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101 results on '"L. Spinoglio"'

1. Molecular gas kinematics in the nuclear region of nearby Seyfert galaxies with ALMA

Author: Kalliopi Dasyra, J. R. De Medeiros, A. Bewketu Belete, R. Slater, C. Cicone, J. A. Fernández-Ontiveros, Claudio Ricci, Francoise Combes, L. Spinoglio, M. Sirressi, Evanthia Hatziminaoglou, Masatoshi Imanishi, Susanne Aalto, Paola Andreani, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA (UMR_8112)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY)
Subjects: Physics, ISM: kinematics and dynamics, [PHYS]Physics [physics], Active galactic nucleus, Continuum (design consultancy), FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), galaxies: individual: MCG-06-30-15, Astrophysics, Rotation, Astrophysics - Astrophysics of Galaxies, Galaxy, galaxies: individual: NGC 4968, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: structure, Emission spectrum, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Lindblad resonance, Line (formation), galaxies: individual: NGC 4845
Abstract: We present the analysis of the molecular gas in the nuclear regions of NGC 4968, NGC 4845, and MCG-06-30-15, with the help of ALMA observations of the CO(2-1) emission line. The aim is to determine the kinematics of the gas in the central (~ 1 kpc) region. We use the 3D-Based Analysis of Rotating Object via Line Observations ($^{3D}$BAROLO) and DiskFit softwares. Circular motions dominate the kinematics of the gas in the central discs, mainly in NGC 4845 and MCG-06-30-15, however there is a clear evidence of non-circular motions in the central ($\sim$ 1 kpc) region of NGC 4845 and NGC 4968. The strongest non-circular motion is detected in the inner disc of NGC 4968 with velocity $\sim 115\, \rm{km\,s^{-1}}$. The bisymmetric model is found to give the best-fit for NGC 4968 and NGC 4845. If the dynamics of NGC 4968 is modeled as a corotation pattern just outside of the bar, the bar pattern speed turns out to be at $\Omega_b$ = $52\, \rm{km\,s^{-1}\,kpc^{-1}}$ the corotation is set at 3.5 kpc and the inner Lindblad resonance (ILR) ring at R = 300pc corresponding to the CO emission ring. The 1.2 mm ALMA continuum is peaked and compact in NGC 4968 and MCG-06-30-15, but their CO(2-1) has an extended distribution. Allowing the CO-to-H$_{2}$ conversion factor $\alpha_{CO}$ between 0.8 and 3.2, typical of nearby galaxies of the same type, the molecular mass M(H$_{2}$) is estimated to be $\sim 3-12\times 10^{7} ~{\rm M_\odot}$ (NGC 4968), $\sim 9-36\times 10^{7}~ {\rm M_\odot}$ (NGC 4845), and $\sim 1-4\times 10^{7}~ {\rm M_\odot}$ (MCG-06-30-15). We conclude that the observed non-circular motions in the disc of NGC 4968 and likely that seen in NGC 4845 is due to the presence of the bar in the nuclear region. At the current spectral and spatial resolution and sensitivity we cannot claim any strong evidence in these sources of the long sought feedback/feeding effect due to the AGN presence., Comment: 14 pages, 11 figures, 3 tables, accepted for publication in the Astronomy & Astrophysics (A&A) journal
Published: 2021

2. Simulating infrared spectro-photometric surveys with a SPRITZ

Author: L. Bisigello, C. Gruppioni, F. Calura, A. Feltre, F. Pozzi, C. Vignali, L. Barchiesi, G. Rodighiero, M. Negrello, F. J. Carrera, K. M. Dasyra, J. A. Fernández-Ontiveros, M. Giard, E. Hatziminaoglou, H. Kaneda, E. Lusso, M. Pereira-Santaella, P. G. Pérez González, C. Ricci, D. Schaerer, L. Spinoglio, L. Wang, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Bisigello L., Gruppioni C., Calura F., Feltre A., Pozzi F., Vignali C., Barchiesi L., Rodighiero G., Negrello M., Carrera F.J., Dasyra K.M., Fernandez-Ontiveros J.A., Giard M., Hatziminaoglou E., Kaneda H., Lusso E., Pereira-Santaella M., Perez Gonzalez P.G., Ricci C., Schaerer D., Spinoglio L., Wang L., Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astronomy, Agenzia Spaziale Italiana, Ministero dell'Istruzione, dell'Università e della Ricerca, Comunidad de Madrid, Agencia Estatal de Investigación (España), and Ministerio de Ciencia, Innovación y Universidades (España)
Subjects: galaxies: active, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, galaxies -techniques, infrared: galaxies, techniques: photometric, photometric, 0103 physical sciences, galaxies, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, infrared: galaxie, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, spectroscopic -techniques, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], evolution -galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: star formation, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, techniques: spectroscopic, active -galaxies, star formation -infrared
Abstract: arXiv:2111.11453v1, Mid- and far-infrared (IR) photometric and spectroscopic observations are fundamental to a full understanding of the dust-obscured Universe and the evolution of both star formation and black hole accretion in galaxies. In this work, using the specifications of the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) as a baseline, we investigate the capability to study the dust-obscured Universe of mid- and far-IR photometry at 34 and 70 µm and low-resolution spectroscopy at 17−36 µm using the state-of-the-art SpectroPhotometric Realisations of Infrared-selected Targets at all-z (SPRITZ) simulation. This investigation is also compared to the expected performance of the Origins Space Telescope and the Galaxy Evolution Probe. The photometric view of the Universe of a SPICA-like mission could cover not only bright objects (e.g. LIR > 1012 L) up to z = 10, but also normal galaxies (LIR < 1011 L) up to z ∼ 4. At the same time, the spectroscopic observations of such mission could also allow us to estimate the redshifts and study the physical properties for thousands of star-forming galaxies and active galactic nuclei by observing the polycyclic aromatic hydrocarbons and a large set of IR nebular emission lines. In this way, a cold, 2.5-m size space telescope with spectro-photometric capability analogous to SPICA, could provide us with a complete three-dimensional (i.e. images and integrated spectra) view of the dust-obscured Universe and the physics governing galaxy evolution up to z ∼ 4., We acknowledge the whole SPICA Collaboration Team. LB, CG, LS and JAFO acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. AF and FC acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001. MPS acknowledges support from the Comunidad de Madrid through the Atracción de Talento Investigador Grant 2018-T1/TIC11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia Maria de Maeztu, ref. MDM-2017-0765.
Published: 2021

3. The role of SPICA-like missions and the Origins Space Telescope in the quest for heavily obscured AGN and synergies with Athena

Author: L. Barchiesi, Giulia Rodighiero, Asantha Cooray, Enrico Piconcelli, Fabio Vito, Francesca Pozzi, I. Delvecchio, A. Feltre, Hidehiro Kaneda, Claudio Ricci, Cristian Vignali, Mattia Negrello, Elisabeta Lusso, Francisco J. Carrera, Miguel Pereira-Santaella, L. Spinoglio, Francesco Tombesi, Giorgio Lanzuisi, J. A. Fernández-Ontiveros, Simona Gallerani, Carlotta Gruppioni, L. Bisigello, Shinki Oyabu, Francesco Calura, Agenzia Spaziale Italiana, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), Comunidad de Madrid, European Commission, Ministero dell'Istruzione, dell'Università e della Ricerca, Barchiesi L., Pozzi F., Vignali C., Carrera F.J., Vito F., Calura F., Bisigello L., Lanzuisi G., Gruppioni C., Lusso E., Delvecchio I., Negrello M., Cooray A., Feltre A., Fernandez-Ontiveros J.A., Gallerani S., Kaneda H., Oyabu S., Pereira-Santaella M., Piconcelli E., Ricci C., Rodighiero G., Spinoglio L., and Tombesi F.
Subjects: Active galactic nucleus, Infrared: galaxie, Astrophysics::High Energy Astrophysical Phenomena, Infrared telescope, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, infrared: galaxies, Spitzer Space Telescope, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Galaxies: star formation, Star formation, Settore FIS/05, Astrophysics::Instrumentation and Methods for Astrophysics, Galaxies: evolution, Astronomy and Astrophysics, Galaxies: active, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, X-rays: diffuse background, Techniques: photometric
Abstract: arXiv:2106.08345v1, SPICA Collaboration Team., In the black hole (BH)–galaxy co-evolution framework, most of the star formation (SF) and the BH accretion are expected to take place in highly obscured conditions. The large amount of gas and dust absorbs most of the UV-to-soft-X radiation and re-emits it at longer wavelengths, mostly in the IR. Thus, obscured active galactic nuclei (AGN) are very difficult to identify in optical or X-ray bands but shine bright in the IR. Moreover, X-ray background (XRB) synthesis models predict that a large fraction of the yet-unresolved XRB is due to the most obscured (Compton thick, CT: NH ≥ 1024 cm−2) of these AGN. In this work, we investigate the synergies between putative IR missions [using SPace Infrared telescope for Cosmology and Astrophysics (SPICA), proposed for European Space Agency (ESA)/M5 but withdrawn in 2020 October, and Origins Space Telescope, OST, as ‘templates’] and the X-ray mission Athena (Advanced Telescope for High ENergy Astrophysics), which should fly in early 2030s, in detecting and characterising AGN, with a particular focus on the most obscured ones. Using an XRB synthesis model, we estimated the number of AGN and the number of those which will be detected in the X-rays by Athena. For each AGN, we associated an optical-to-Far InfraRed (FIR) spectral energy distribution (SED) from observed AGN with both X-ray data and SED decomposition and used these SEDs to check if the AGN will be detected by SPICA-like or OST at IR wavelengths. We expect that, with the deepest Athena and SPICA-like (or OST) surveys, we will be able to photometrically detect in the IR more than 90% of all the AGN (down to L2−10keV ∼ 1042 erg s−1 and up to z ∼ 10) predicted by XRB synthesis modeling, and we will detect at least half of them in the X-rays. The spectroscopic capabilities of the OST can provide ≈51 000 and ≈3 400 AGN spectra with R = 300 at 25–588µm in the wide and deep surveys, respectively, the last one up to z ≈ 4. Athena will be extremely powerful in detecting and discerning moderate- and high-luminosity AGN, allowing us to properly select AGN even when the mid-IR torus emission is ‘hidden’ by the host galaxy contribution. We will constrain the intrinsic luminosity and the amount of obscuration for ∼20% of all the AGN (and ∼50% of those with L2−10keV > 3.2 × 1043 erg s−1) using the X-ray spectra provided by Athena WFI. We find that the most obscured and elusive CT-AGN will be exquisitely sampled by SPICA-like mission or OST and that Athena will allow a fine characterisation of the most luminous ones. This will provide a significant step forward in the process of placing stronger constraints on the yet-unresolved XRB and investigating the BH accretion rate evolution up to very high redshift (z ≥ 4)., FP, CV, CG, LB, and LS acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. MPS acknowledges support from the Comunidad de Madrid, Spain, through Atracción de Talento Investigador Grant 2018-T1/TIC-11035 and PID2019-105423GA-I00 (MCIU/AEI/FEDER,UE). AF acknowledges the support from grant PRIN MIUR2017-20173ML3WW_001.
Published: 2021

4. Physical properties of the ambient medium and of dense cores in the Perseus star-forming region derived from Herschel Gould Belt Survey observations

Author: Stefano Pezzuto, Alexander Men'shchikov, Ph. André, J. Di Francesco, Christine D. Wilson, Sylvain Bontemps, L. Piccotti, Sarah Sadavoy, Frédérique Motte, Vera Konyves, P. Palmeirim, E. Fiorellino, Nicola Schneider, Jason M. Kirk, L. Spinoglio, Davide Elia, J.-Ph. Bernard, Eugenio Schisano, Doris Arzoumanian, G. Li Causi, M. Benedettini, Derek Ward-Thompson, Bilal Ladjelate, FEMIS 2021, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Initial mass function, 010504 meteorology & atmospheric sciences, Extinction (astronomy), FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Power law, 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Stars, Wavelength, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Right ascension
Abstract: (Abridged) In this paper, we present analyses of images taken with the Herschel ESA satellite from 70mu to 500mu. We first constructed column density and dust temperature maps. Next, we identified compact cores in the maps, and characterize the cores using modified blackbody fits to their SEDs: we identified 684 starless cores, of which 199 are bound and potential prestellar cores, and 132 protostars. We also matched the Herschel-identified young stars with GAIA sources to model distance variations across the Perseus cloud. We measure a linear gradient function with right ascension and declination for the entire cloud. From the SED fits, mass and temperature of cores were derived. The core mass function can be modelled with a log-normal distribution that peaks at 0.82~$M_\sun$ suggesting a star formation efficiency of 0.30. The high-mass tail can be modelled with a power law of slope $\sim-2.32$, close to the Salpeter's value. We also identify the filamentary structure of Perseus, confirming that stars form preferentially in filaments. We find that the majority of filaments where star formation is ongoing are transcritical against their own internal gravity because their linear masses are below the critical limit of 16~$M_\sun$pc$^{-1}$ above which we expect filaments to collapse. We find a possible explanation for this result, showing that a filament with a linear mass as low as 8~$M_\sun$pc$^{-1}$ can be already unstable. We confirm a linear relation between star formation efficiency and slope of dust probability density function and a similar relation is also seen with the core formation efficiency. We derive a lifetime for the prestellar core phase of $1.69\pm0.52$~Myr for Perseus but different regions have a wide range in prestellar core fractions, hint that star-formation has started only recently in some clumps. We also derive a free-fall time for prestellar cores of 0.16~Myr., Comparison with Zari et al's (2016) work improved once Eleonora Zari told us that, contrarily to what we wrote, their data are publicly available (this was not written in the first version of their paper put on arxiv, then our misunderstaning). The modification is small, a paragraph on page 11, and does not have any impact on the content of the paper. Modification allowed by A&A editor
Published: 2020

5. A CO molecular gas wind 340 pc away from the Seyfert 2 nucleus in ESO 420-G13 probes an elusive radio jet

Author: J. A. Fernández-Ontiveros, Masatoshi Imanishi, Francoise Combes, L. Spinoglio, Paola Andreani, Evanthia Hatziminaoglou, R. Slater, Miguel Pereira-Santaella, Neil M. Nagar, Kalliopi Dasyra, Susanne Aalto, M. Papachristou, M. Malkan, Claudio Ricci, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Fernández Ontiveros, J. A. [0000-0001-9490-899X], Hatziminaoglou, E. [0000-0003-0917-9636], Spignoglio, L. [0000-0001-8840-1551], Combes, F. [0000-0003-2658-7893], Nagar, N. [0000-0001-6920-662X], Imanishi, M. [0000-0001-6186-8792], Andreani, P. [0000-0001-9493-0169], Agenzia Spaziale Italiana (ASI), Comunidad de Madrid, Hellenic Foundation for Research and Innovation (HFRI), and Comisión Nacional de Investigación Científica y Tecnológica (CONICYT)
Subjects: active [Galaxies], astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ESO 420-G13, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, individual [Galaxies], Line (formation), Physics, individual: ESO 420-G13 [galaxies], Jet (fluid), 010308 nuclear & particles physics, Star formation, jets and outflows [ISM], ISM [Submillimeter], Astronomy and Astrophysics, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Supernova, high angular resolution [Techniques], Radiation pressure, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Outflow, Astronomical and Space Sciences
Abstract: A prominent jet-driven outflow of CO(2-1) molecular gas is found along the kinematic minor axis of the Seyfert 2 galaxy ESO 420-G13, at a distance of $340-600\, \rm{pc}$ from the nucleus. The wind morphology resembles a characteristic funnel shape, formed by a highly collimated filamentary emission at the base, likely tracing the jet propagation through a tenuous medium, until a bifurcation point at $440\, \rm{pc}$ where the jet hits a dense molecular core and shatters, dispersing the molecular gas into several clumps and filaments within the expansion cone. We also trace the jet in ionised gas within the inner $\lesssim 340\, \rm{pc}$ using the [NeII]$_{\rm 12.8 \mu m}$ line emission, where the molecular gas follows a circular rotation pattern. The wind outflow carries a mass of $\sim 8 \times 10^6\, \rm{M_\odot}$ at an average wind projected speed of $\sim 160\, \rm{km\,s^{-1}}$, which implies a mass outflow rate of $\sim 14\, \rm{M_\odot\,yr^{-1}}$. Based on the structure of the outflow and the budget of energy and momentum, we discard radiation pressure from the active nucleus, star formation, and supernovae as possible launching mechanisms. ESO 420-G13 is the second case after NGC 1377 where the presence of a previously unknown jet is revealed due to its interaction with the interstellar medium, suggesting that unknown jets in feeble radio nuclei might be more common than expected. Two possible jet-cloud configurations are discussed to explain the presence of an outflow at such distance from the AGN. The outflowing gas will likely not escape, thus a delay in the star formation rather than quenching is expected from this interaction, while the feedback effect would be confined within the central few hundred parsecs of the galaxy., Comment: 12 pages, 8 figures. Accepted for publication in A&A
Published: 2020

6. Properties of the dense core population in Orion B as seen by the Herschel Gould Belt survey

Author: P. Didelon, Simon P. Goodwin, Vera Könyves, Stefano Pezzuto, Alexander Men'shchikov, Doris Arzoumanian, Glenn J. White, Ph. André, L. Spinoglio, Bilal Ladjelate, Yoshito Shimajiri, Andrea Bracco, Nicola Schneider, Derek Ward-Thompson, Kazi L.J. Rygl, J. Di Francesco, Sylvain Bontemps, Milena Benedettini, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CEREG (CEREG), Université Louis Pasteur - Strasbourg I, FORMATION STELLAIRE 2019, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Istituto Nazionale di Fisica Nucleare, Sezione di Milano (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Nagoya University, Instituto de Astrofísica e Ciências do Espaço (IASTRO), University of Cologne, Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Victoria [Canada] (UVIC), University of Sheffield [Sheffield], Istituto di Radioastronomia [Bologna] (IRA), Space Science and Technology Department [Didcot] (RAL Space), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Support from the French national programs of CNRS/INSU on stellar and ISM physics (PNPS and PCMI)., ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), ANR-16-CE92-0035,GENESIS,GENeration et Evolution des Structures du milieu InterStellaire(2016), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), European Project: 267934,EC:FP7:ERC,ERC-2010-AdG_20100224,MISTIC(2011), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Istituto Nazionale di Fisica Nucleare [Milano] (INFN), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Istituto di Radioastronomia (IRA), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris)
Subjects: 010504 meteorology & atmospheric sciences, ISM: structure, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, ISM: clouds, Protein filament, Core formation, 0103 physical sciences, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), ComputingMilieux_MISCELLANEOUS, 0105 earth and related environmental sciences, Physics, education.field_of_study, stars: formation, Molecular cloud, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Stars, Wavelength, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ISM: individual objects: Orion B complex, submillimeter: ISM, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Dense core
Abstract: We present a detailed study of the Orion B clouds (d~400 pc), imaged with the PACS/SPIRE cameras at 70-500 $��$m by the Herschel Gould Belt survey (HGBS). We release new high-res. maps of column density and dust temperature. In the filamentary sub-regions NGC2023/2024, NGC2068/2071, and L1622, 1768 starless dense cores were identified, ~28-45% of which are self-gravitating prestellar cores. A total of 76 protostellar dense cores were also found. The typical lifetime of the prestellar cores was found to be $t_{\rm pre}=1.7_{-0.6}^{+0.8}$ Myr. The prestellar core mass function (CMF) peaks at ~0.5 $M_\odot$ and is consistent with a power law with log slope -1.27$\pm$0.24 at the high-mass end, compared to the Salpeter slope of -1.35. In this region, we confirm the existence of a transition in prestellar core formation efficiency (CFE) around a fiducial value A_V_bg~7 mag in background visual extinction, similar to the trend observed with Herschel in other clouds. This is not a sharp threshold, but a smooth transition between a regime with very low prestellar CFE at A_V_bg90% when a more complete sample of filamentary structures is considered. Interestingly, the median separation between nearest core neighbors corresponds to the typical inner filament width of ~0.1 pc commonly observed in nearby molecular clouds. Analysis of the CMF observed as a function of background cloud column density shows that the most massive prestellar cores are spatially segregated in the highest column density areas, and suggests that both higher- and lower-mass prestellar cores may form in denser filaments., In press in Astronomy and Astrophysics. arXiv admin note: text overlap with arXiv:1507.05926
Published: 2019

7. SPICA —A Large Cryogenic Infrared Space Telescope: Unveiling the Obscured Universe

Author: M. Kawada, B. Larsson, D. Arrazola, Brian Jackson, C.M. Bradford, Lee Armus, K. Shinozaki, Hiroshi Shibai, Francisca Kemper, N. Isobe, I. Funaki, R. Huisman, M. Giard, L. Duband, Shiang-Yu Wang, P. Khosropanah, Shinki Oyabu, P. P. Kooijman, R. Shipman, Daisuke Ishihara, I. Charles, L. Rodriguez, V. Reveret, S. Withington, Frank Helmich, Kotaro Kohno, Willem Jellema, Pieter Dieleman, M. Audard, T. Wada, B. Vandenbussche, D. van Loon, A. Di Giorgio, Peter Roelfsema, David A. Naylor, I. Sakon, H. Ogawa, G. de Lange, Franz Kerschbaum, J. Kwon, R. Hijmering, W. M. Laauwen, J. van der Kuur, Jaap Evers, Francisco Najarro, Inga Kamp, Takashi Onaka, Albrecht Poglitsch, T. Yamada, L. M. González Fernández, H. Jacobs, S. C. Madden, Hidehiro Kaneda, Yasuo Doi, Jian-Rong Gao, C. K. Wafelbakker, H. van Weers, M. Eggens, I. Yamamura, L. Spinoglio, H. Matsuhara, Oliver Krause, T. Suzuki, Takao Nakagawa, Matthew Joseph Griffin, F. F. S. van der Tak, H. Sugita, Michael D. Audley, Y. Sato, J. Torres Redondo, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), ISDC Data Centre for Astrophysics, University of Geneva [Switzerland], Institut Nanosciences et Cryogénie (INAC), Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Massachusetts Institute of Technology (MIT), inconnu, Inconnu, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], AUTRES, National Institute for Subatomic Physics [Amsterdam] (NIKHEF), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Departamento de Astrofisica [Madrid], Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Department of Physics, Nara Women's University, Department of Environmental and Materials Engineering, Nagoya Institute, Max-Planck-Institut für Extraterrestrische Physik (MPE), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Antarctic Research a European Network for Astrophysics (ARENA), Nanomaterials Research Institute, foreign laboratories (FL), CERN [Genève], SRON Netherlands Institute for Space Research (SRON), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), NASA Goddard Space Flight Center (GSFC), Astronomy, Université de Genève = University of Geneva (UNIGE), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Grenoble Alpes (UGA), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), and Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA)
Subjects: infrared: galaxies, infrared: general, infrared: planetary systems, instrumentation: photometers, instrumentation: spectrographs, space vehicles: instruments, Astrophysics - Instrumentation and Methods for Astrophysics, instruments [space vehicles], Direct assessment, Infrared, media_common.quotation_subject, Infrared wavelength, FOS: Physical sciences, Spica, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Space (mathematics), 01 natural sciences, galaxies [infrared], infrared: galaxies, Spitzer Space Telescope, 0103 physical sciences, photometers [instrumentation], space vehicles: instruments, 010306 general physics, infrared: planetary systems, planetary systems [infrared], Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, general [infrared], Astrophysics::Galaxy Astrophysics, ComputingMilieux_MISCELLANEOUS, media_common, instrumentation: spectrographs, MISSION, Luminous infrared galaxy, Physics, Science & Technology, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Universe, instrumentation: photometers, SPITZER, Space and Planetary Science, Physical Sciences, Astrophysics::Earth and Planetary Astrophysics, infrared: general, Astrophysics - Instrumentation and Methods for Astrophysics, spectrographs [instrumentation]
Abstract: 著者人数: 70名(所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 芝井, 広; 船木, 一幸; 磯部, 直樹; 川田, 光伸; 權, 靜美; 松原, 英雄; 中川, 貴雄; 小川, 博之; 佐藤, 洋一; 篠崎, 慶亮; 杉田, 寛之; 和田, 武彦; 山田, 亨; 山村, 一誠), Number of authors: 70(Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Shibai, Hiroshi; Funaki, Ikkoh; Isobe, Naoki; Kawada, Mitsunobu; Kwon, Jungmi; Matsuhara, Hideo; Nakagawa, Takao; Ogawa, Hiroyuki; Sato, Yoichi; Shinozaki, Keisuke; Sugita, Hiroyuki; Wada, Takehiko; Yamada, Toru; Yamamura, Issei), 資料番号: SA1180106000
Published: 2018

8. A catalogue of dense cores and young stellar objects in the Lupus complex based on Herschel Gould Belt Survey observations

Author: J. Di Francesco, Davide Elia, F. Louvet, Bilal Ladjelate, Kazi L.J. Rygl, Stefano Pezzuto, Derek Ward-Thompson, Milena Benedettini, P. Palmeirim, Nicola Schneider, L. Spinoglio, E. Schisano, Ph. André, Vera Könyves, Alexander Men'shchikov, Doris Arzoumanian, ITA, GBR, and FRA
Subjects: Physics, stars: formation, Initial mass function, 010504 meteorology & atmospheric sciences, ISM: individual objects: Lupus complex (except planetary nebulae), Star formation, Young stellar object, Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, F500, clouds, Astrophysics, Circumstellar envelope, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Interstellar medium, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, submillimeter: ISM, Protostar, Spectral energy distribution, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: The Herschel Gould Belt Survey key project mapped the bulk of nearby star-forming molecular clouds in five far-infrared bands with the aim of compiling complete census of prestellar cores and young, embedded protostars. In this paper, we present the catalogue of the dense cores and YSOs/protostars extracted from the Herschel maps of the Lupus I, III, and IV molecular clouds. The physical properties of the detected objects were derived by fitting their spectral energy distributions. A total of 532 dense cores, out of which 103 are presumably prestellar in nature, and 38 YSOs/protostars have been detected in the three clouds. Almost all the prestellar cores are associated with filaments against only about one third of the unbound cores and YSOs/protostars. Prestellar core candidates are found even in filaments that are on average thermally sub-critical and over a background column density lower than that measured in other star forming regions so far. The core mass function of the prestellar cores peaks between 0.2 and 0.3 solar masses and it is compatible with the log-normal shape found in other regions. Herschel data reveal several, previously undetected, protostars and new candidates of Class 0 and Class II with transitional disks. We estimate the evolutionary status of the YSOs/protostars using two independent indicators: the $\alpha$ index and the fitting of the spectral energy distribution from near- to far-infrared wavelengths. For 70% of the objects, the evolutionary stages derived with the two methods are in agreement. Lupus is confirmed to be a very low-mass star-forming region, both in terms of the prestellar condensations and of the diffuse medium. Noticeably, in the Lupus clouds we have found star formation activity associated with interstellar medium at low column density, usually quiescent in other (more massive) star forming regions., Comment: 25 pages, 15 ifgures
Published: 2018
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9. The Herschel Exploitation of Local Galaxy Andromeda (HELGA)

Author: George J. Bendo, S. Verstocken, Sébastien Viaene, Antti Tamm, S. C. Madden, P. De Vis, Matthew Smith, Maarten Baes, Médéric Boquien, Elmo Tempel, Peter Camps, Joris Blommaert, L. Spinoglio, Maud Galametz, J. A. Fernández-Ontiveros, A. Cooray, Gianfranco Gentile, Alessandro Boselli, Jacopo Fritz, I. De Looze, Physics, Astronomy and Astrophysics Research Group, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Andromeda Galaxy, ISM [Infrared], FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, TRANSFER SIMULATIONS, 01 natural sciences, Luminosity, Atmospheric radiative transfer codes, Bulge, 0103 physical sciences, ISM [Galaxies], STAR-FORMING GALAXIES, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, COLD DUST, EDGE-ON GALAXIES, individual: M31 [galaxies], 010303 astronomy & astrophysics, Dust, extinction, Astrophysics::Galaxy Astrophysics, SPITZER-SPACE-TELESCOPE, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, SPIRAL GALAXY, Astrophysics - Astrophysics of Galaxies, FORMATION RATES, Galaxy, Interstellar medium, Physics and Astronomy, individual: M 31 [Galaxies], 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), fundamental parameters [Galaxies], galaxies: individual: M 31, galaxies: ISM, infrared: ISM, galaxies: fundamental parameters, dust, extinction, radiative transfer, MILKY-WAY, dust, Astrophysics::Earth and Planetary Astrophysics
Abstract: The radiation of stars heats dust grains in the diffuse interstellar medium and in star-forming regions in galaxies. Modelling this interaction provides information on dust in galaxies, a vital ingredient for their evolution. It is not straightforward to identify the stellar populations heating the dust, and to link attenuation to emission on a sub-galactic scale. Radiative transfer models are able to simulate this dust-starlight interaction in a realistic, three-dimensional setting. We investigate the dust heating mechanisms on a local and global galactic scale, using the Andromeda galaxy (M31) as our laboratory. We perform a series of panchromatic radiative transfer simulations of Andromeda with our code SKIRT. The high inclination angle of M31 complicates the 3D modelling and causes projection effects. However, the observed morphology and flux density are reproduced fairly well from UV to sub-millimeter wavelengths. Our model reveals a realistic attenuation curve, compatible with previous, observational estimates. We find that the dust in M31 is mainly (91 % of the absorbed luminosity) heated by the evolved stellar populations. The bright bulge produces a strong radiation field and induces non-local heating up to the main star-forming ring at 10 kpc. The relative contribution of unevolved stellar populations to the dust heating varies strongly with wavelength and with galactocentric distance.The dust heating fraction of unevolved stellar populations correlates strongly with NUV-r colour and specific star formation rate. These two related parameters are promising probes for the dust heating sources at a local scale., Comment: 16 pages + appendix, 13 figures, accepted for publication in A&A
Published: 2017

10. Erratum: Tracing black hole accretion with SED decomposition and IR lines: from local galaxies to the high-z Universe

Author: C Gruppioni, S Berta, L Spinoglio, M Pereira-Santaella, F Pozzi, P Andreani, M Bonato, G De Zotti, M Malkan, M Negrello, L Vallini, C Vignali, ITA, USA, GBR, DEU, and ESP
Subjects: Space and Planetary Science, Astronomy and Astrophysics
Published: 2018

11. Far-infrared line spectra of active galaxies from the Herschel/PACS Spectrometer: the complete database

Author: Miguel Pereira-Santaella, J. A. Fernández-Ontiveros, Matthew A. Malkan, Paola Andreani, Kalliopi Dasyra, and L. Spinoglio
Subjects: Active galactic nucleus, dwarf [galaxies], Metallicity, astro-ph.GA, nuclei [galaxies], FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, computer.software_genre, 01 natural sciences, Atomic, Physical Chemistry, Particle and Plasma Physics, Seyfert [galaxies], 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Nuclear, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, Database, ISM [galaxies], 010308 nuclear & particles physics, Star formation, starburst [galaxies], Stellar atmosphere, Molecular, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], Astrophysics::Earth and Planetary Astrophysics, computer, Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract: We present a coherent database of spectroscopic observations of far-IR fine-structure lines from the Herschel/PACS archive for a sample of 170 local AGN, plus a comparison sample of 20 starburst galaxies and 43 dwarf galaxies. Published Spitzer/IRS and Herschel/SPIRE line fluxes are included to extend our database to the full 10-600 $\mu m$ spectral range. The observations are compared to a set of CLOUDY photoionisation models to estimate the above physical quantities through different diagnostic diagrams. We confirm the presence of a stratification of gas density in the emission regions of the galaxies, which increases with the ionisation potential of the emission lines. The new [OIV]25.9$\mu m$/[OIII]88$\mu m$ vs [NeIII]15.6$\mu m$/[NeII]12.8$\mu m$ diagram is proposed as the best diagnostic to separate: $i)$ AGN activity from any kind of star formation; and $ii)$ low-metallicity dwarf galaxies from starburst galaxies. Current stellar atmosphere models fail to reproduce the observed [OIV]25.9$\mu m$/[OIII]88$\mu m$ ratios, which are much higher when compared to the predicted values. Finally, the ([NeIII]15.6$\mu m$ + [NeII]12.8$\mu m$)/([SIV]10.5$\mu m$ + [SIII]18.7$\mu m$) ratio is proposed as a promising metallicity tracer to be used in obscured objects, where optical lines fail to accurately measure the metallicity. The diagnostic power of mid- to far-infrared spectroscopy shown here for local galaxies will be of crucial importance to study galaxy evolution during the dust-obscured phase at the peak of the star formation and black-hole accretion activity ($1 < z < 4$). This study will be addressed by future deep spectroscopic surveys with present and forthcoming facilities such as JWST, ALMA, and SPICA., Comment: Accepted for publication in the ApJS
Published: 2016

12. The bolometric and UV attenuation in normal spiral galaxies of the Herschel Reference Survey⋆

Author: Maarten Baes, Alessandro Boselli, S. C. Madden, O. L. Karczewski, Luca Cortese, I. De Looze, Laure Ciesla, L. Spinoglio, Médéric Boquien, Matthew Smith, George J. Bendo, Sébastien Viaene, Stephen Anthony Eales, Jacopo Fritz, Sterrenkundig Observatorium, Universiteit Gent, University of Manchester [Manchester], University of Cambridge [UK] (CAM), Universidad de Antofagasta, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), The University of Western Australia (UWA), University College of London [London] (UCL), Cardiff University, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universiteit Gent = Ghent University (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: STELLAR MASSES, Infrared, INFRARED-EMISSION, Extinction (astronomy), FOS: Physical sciences, Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, 0103 physical sciences, VIRGO CLUSTER GALAXIES, STAR-FORMING GALAXIES, BAND-SELECTED SAMPLE, Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, infrared: ISM, Spiral galaxy, DUST ATTENUATION, ISM [galaxies], 010308 nuclear & particles physics, Star formation, extinction, fundamental parameters [Galaxy], STARBURST GALAXIES, ISM [infrared], Astronomy and Astrophysics, Galaxy: fundamental parameters, Astrophysics - Astrophysics of Galaxies, Galaxy, FORMATION RATES, Stars, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract: The dust in nearby galaxies absorbs a fraction of the UV-optical-near-infrared radiation produced by stars. This energy is consequently re-emitted in the infrared. We investigate the portion of the stellar radiation absorbed by spiral galaxies from the HRS by modelling their UV-to-submillimetre spectral energy distributions. Our models provide an attenuated and intrinsic SED from which we find that on average 32 % of all starlight is absorbed by dust. We define the UV heating fraction as the percentage of dust luminosity that comes from absorbed UV photons and find that this is 56 %, on average. This percentage varies with morphological type, with later types having significantly higher UV heating fractions. We find a strong correlation between the UV heating fraction and specific star formation rate and provide a power-law fit. Our models allow us to revisit the IRX-AFUV relations, and derive these quantities directly within a self-consistent framework. We calibrate this relation for different bins of NUV-r colour and provide simple relations to relate these parameters. We investigated the robustness of our method and we conclude that the derived parameters are reliable within the uncertainties which are inherent to the adopted SED model. This calls for a deeper investigation on how well extinction and attenuation can be determined through panchromatic SED modelling., Comment: 14 pages, 7 figures. Accepted for publication in Astronomy & Astrophysics
Published: 2016

13. The imprint of rapid star formation quenching on the spectral energy distributions of galaxies

Author: Maarten Baes, Laure Ciesla, Ciro Pappalardo, I. De Looze, Alessandro Boselli, Matthieu Béthermin, David Elbaz, Corentin Schreiber, J. A. Fernández-Ontiveros, Sébastien Viaene, Vassilis Charmandaris, Médéric Boquien, V. Buat, Samuel Boissier, L. Spinoglio, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), University of Crete [Heraklion] (UOC), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Southern Observatory (ESO), Sterrenkundig Observatorium, Universiteit Gent, Universidad de Antofagasta, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Observatório Astronómico de Lisboa, L.C. benefited from the thales project 383549 that is jointly funded by the European Union and the Greek Government in the framework of the program 'Education and lifelong learning'., European Project: 312725,EC:FP7:SPA,FP7-SPACE-2012-1,ASTRODEEP(2013), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University (UGENT), National Observatory of Athens, and Institute for Space Applications and Remote Sensing
Subjects: HERSCHEL REFERENCE SURVEY, ACTIVE GALACTIC NUCLEI, Active galactic nucleus, Stellar mass, FOS: Physical sciences, POPULATION SYNTHESIS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, LYMAN BREAK GALAXIES, 0103 physical sciences, BAND-SELECTED SAMPLE, fundamental parameters [galaxies], Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, MAIN-SEQUENCE, 010303 astronomy & astrophysics, RED SEQUENCE, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, galaxies: fundamental parameters, VIRGO CLUSTER, Virgo Cluster, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Ram pressure, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, STELLAR MASS, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: [Abridged] In high density environment, the gas content of galaxies is stripped, leading to a rapid quenching of their star formation activity. This dramatic environmental effect is generally not taken into account in the SFHs usually assumed to perform spectral energy distribution (SED) fitting of these galaxies, yielding to a poor fit of their stellar emission and, consequently, a biased estimate of the SFR. We aim at reproducing the SFH of galaxies that underwent a rapid star formation quenching using a truncated delayed SFH that we implemented in the SED fitting code CIGALE. We show that the ratio between the instantaneous SFR and the SFR just before the quenching ($r_{SFR}$) is well constrained as long as rest frame UV data are available. This SED modelling is applied to the Herschel Reference Survey (HRS) containing isolated galaxies and sources falling in the dense environment of the Virgo cluster. The latter are HI-deficient due to ram pressure stripping. We show that the truncated delayed SFH successfully reproduces their SED while typical SFH assumptions fail. A good correlation is found between $r_{SFR}$ and HI-def, the parameter quantifying the gas deficiency of cluster galaxies, meaning that SED fitting results can be used to provide a tentative estimate of the gas deficiency of galaxies for which HI observations are not available. The HRS galaxies are placed on the SFR-$M_*$ diagram showing that the HI-deficient sources lie in the quiescent region confirming previous studies. Using the $r_{SFR}$ parameter, we derive the SFR of these sources before quenching and show that they were previously on the main sequence relation. We show that the $r_{SFR}$ parameter is also well recovered for deeply obscured high redshift sources, as well as in absence of IR data. SED fitting is thus a powerful tool to identify galaxies that underwent a rapid star formation quenching., accepted for publication in A&A. 13 pages, 14 figures
Published: 2016

14. Herschel observations of Cen A: stellar heating of two extragalactic dust clouds

Author: David Elbaz, Matthew Smith, Michael Pohlen, Christine D. Wilson, George J. Bendo, Tom Oosterloo, Maarten Baes, Jonathan Ivor Davies, A. Cooray, Kate Gudrun Isaak, M. J. Page, Christian Struve, Maud Galametz, L. Spinoglio, Raffaella Morganti, E. E. Rigby, Alessandro Boselli, Stephen Anthony Eales, Robbie Richard Auld, Luca Cortese, and Haley Louise Gomez
Subjects: Physics, Jet (fluid), Active galactic nucleus, 010308 nuclear & particles physics, Spectral density, Flux, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Wavelength, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Black-body radiation, 010303 astronomy & astrophysics
Abstract: We present the first results of a multi-wavelength survey, incoporating Herschel-SPIRE, Spitzer, GALEX and ATCA observations, of a 1 deg x 1 deg field centred on Centaurus A. As well as detecting the inner lobes of the active galactic nucleus (AGN) jet and counterjet, we have found two clouds, bright at sub-mm wavelengths, ~15 kpc from the centre of Cen A that are co-aligned with the jets. Flux measurements at Herschel wavelengths have proved vital in constraining fits to the Spectral Energy Distributions (SEDs). The clouds are well fit by a single-temperature, modified blackbody spectrum (beta=2) indicating that we are looking at two cold dust clouds on the outskirts of Cen A. The temperature and masses of the clouds are: T_{north} = 12.6^{+1.1}_{-1.2} K, T_{south} = 15.1^{+1.7}_{-1.6} K; log(M_{north} / M_o) = 5.8^{+0.2}_{-0.2}, log(M_{south} / M_o) = 5.6^{+0.2}_{-0.2} and the gas-dust ratio for both clouds is ~100. The measured values for the northern dust cloud are consistent with previous measurements from ISO while the southern cloud is a new sub-mm detection. The two dust clouds are located at the termini of the partial HI ring that surrounds Cen A which is also where the gas column density peaks... abridged
Published: 2012

15. A census of dense cores in the Aquila cloud complex: SPIRE/PACS observations from the Herschel Gould Belt survey⋆,⋆⋆,⋆⋆⋆

Author: Vera Könyves, P. Didelon, Matthew James Griffin, T. Hill, P. Palmeirim, Alexander Men'shchikov, Doris Arzoumanian, Stefano Pezzuto, Sarah Sadavoy, Kenneth A. Marsh, Glenn J. White, Ph. André, E. Schisano, Yoshito Shimajiri, J. Di Francesco, L. Spinoglio, Sylvain Bontemps, Peter G. Martin, Milena Benedettini, J.-Ph. Bernard, Nicola Schneider, Derek Ward-Thompson, Kazi L.J. Rygl, Jason M. Kirk, Frédérique Motte, A. Roy, Anaëlle Maury, Bilal Ladjelate, Helene Roussel, Q. Nguyen Luong, Nicolas Peretto, Davide Elia, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, FORMATION STELLAIRE 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, Department of Physics and Astronomy [Victoria], University of Victoria [Canada] (UVIC), School of Physics and Astronomy [Cardiff], Cardiff University, Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Joint ALMA Observatory (JAO), National Radio Astronomy Observatory (NRAO)-European Southern Observatory (ESO), Jeremiah Horrocks Institute for Mathematics, Physics and Astronomy [Preston], University of Central Lancashire [Preston] (UCLAN), Canadian Institute for Theoretical Astrophysics (CITA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Bologna (OABO), Department of Physics and Astronomy [Milton Keynes], The Open University [Milton Keynes] (OU), ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), European Project: 267934,EC:FP7:ERC,ERC-2010-AdG_20100224,MISTIC(2011), Laboratory for Atmospheric and Space Physics [Boulder] (LASP), University of Colorado [Boulder], San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, University of California [Los Angeles] (UCLA), University of California, Service des Photons, Atomes et Molécules (SPAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), SLAC National Accelerator Laboratory (SLAC), Stanford University, Stanford Linear Accelerator Center (SLAC), Stanford University [Stanford], Smithsonian Institution-Harvard University [Cambridge], Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Harvard University-Smithsonian Institution, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), ITA, GBR, FRA, DEU, CAN, CHL, JPN, and NLD
Subjects: Initial mass function, ISM: structure, Stars: formation, Young stellar object, FOS: Physical sciences, Budget control, F500, Efficiency, Astrophysics, Surveys, Population statistics, ISM : clouds, 7. Clean energy, Submillimeter: isms, Gravitation, ISM: individual objects, Functions, Protostar, Spatial distribution, QB, Physics, Star formation, Information dissemination, Molecular cloud, Astronomy and Astrophysics, Stars, Astrophysics - Astrophysics of Galaxies, Spire, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Coremaking, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA]
Abstract: We present and discuss the results of the Herschel Gould Belt survey (HGBS) observations in an 11 deg2 area of the Aquila molecular cloud complex at d 260 pc, imaged with the SPIRE and PACS photometric cameras in parallel mode from 70 μm to 500 μm. Using the multi-scale, multi-wavelength source extraction algorithm getsources, we identify a complete sample of starless dense cores and embedded (Class 0-I) protostars in this region, and analyze their global properties and spatial distributions. We find a total of 651 starless cores, 60% ± 10% of which are gravitationally bound prestellar cores, and they will likely form stars inthe future. We also detect 58 protostellar cores. The core mass function (CMF) derived for the large population of prestellar cores is very similar in shape to the stellar initial mass function (IMF), confirming earlier findings on a much stronger statistical basis and supporting the view that there is a close physical link between the stellar IMF and the prestellar CMF. The global shift in mass scale observed between the CMF and the IMF is consistent with a typical star formation efficiency of 40% at the level of an individual core. By comparing the numbers of starless cores in various density bins to the number of young stellar objects (YSOs), we estimate that the lifetime of prestellar cores is 1 Myr, which is typically 4 times longer than the core free-fall time, and that it decreases with average core density. We find a strong correlation between the spatial distribution of prestellar cores and the densest filaments observed in the Aquila complex. About 90% of the Herschel-identified prestellar cores are located above a background column density corresponding to AV 7, and 75% of them lie within filamentary structures with supercritical masses per unit length ≳16 M☉/pc. These findings support a picture wherein the cores making up the peak of the CMF (and probably responsible for the base of the IMF) result primarily from the gravitational fragmentation of marginally supercritical filaments. Given that filaments appear to dominate the mass budget of dense gas at AV> 7, our findings also suggest that the physics of prestellar core formation within filaments is responsible for a characteristic "efficiency" {SFR/M_dense ̃ 5+2-2 × 10-8 yr-1} for the star formation process in dense gas. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.Figures 18, 19, and Appendices are available in electronic form at http://www.aanda.orgHerschel column density and temperature maps (FITS format) and full Tables A.1 and A.2 are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/584/A91
Published: 2015

16. Linking dust emission to fundamental properties in galaxies: the low-metallicity picture

Author: Laure Ciesla, V. Doublier-Pritchard, Anthony P. Jones, Nanyao Y. Lu, L. Spinoglio, George J. Bendo, Maarten Baes, I. De Looze, Luca Cortese, Alessandro Boselli, Frédéric Galliano, Diane Cormier, Maud Galametz, O. Ł. Karczewski, A. Cooray, A. Rémy-Ruyer, Vianney Lebouteiller, Suzanne C. Madden, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), ANR-11-BS56-0023,SYMPATICO,SYnthetic MultiPhase Analysis of The Ism of Cosmic Objects(2011), European Project: 606847,EC:FP7:SPA,FP7-SPACE-2013-1,DUSTPEDIA(2014), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universiteit Gent, and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: HERSCHEL REFERENCE SURVEY, ACTIVE GALACTIC NUCLEI, dwarf [galaxies], Infrared, Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxies [infrared], Luminosity, infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, 0103 physical sciences, COMPACT DWARF GALAXIES, evolution, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Black-body radiation, TO-GAS RATIO, 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Dwarf galaxy, Physics, infrared: ISM, 010308 nuclear & particles physics, extinction, Sigma, ISM [infrared], Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, galaxies: dwarf, Mass ratio, Astrophysics - Astrophysics of Galaxies, Galaxy, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, LARGE-MAGELLANIC-CLOUD, Astrophysics::Earth and Planetary Astrophysics, dust, galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: In this work, we aim at providing a consistent analysis of the dust properties from metal-poor to metal-rich environments by linking them to fundamental galactic parameters. We consider two samples of galaxies: the Dwarf Galaxy Survey (DGS) and KINGFISH, totalling 109 galaxies, spanning almost 2 dex in metallicity. We collect infrared (IR) to submillimetre (submm) data for both samples and present the complete data set for the DGS sample. We model the observed spectral energy distributions (SED) with a physically-motivated dust model to access the dust properties. Using a different SED model (modified blackbody), dust composition (amorphous carbon), or wavelength coverage at submm wavelengths results in differences in the dust mass estimate of a factor two to three, showing that this parameter is subject to non-negligible systematic modelling uncertainties. For eight galaxies in our sample, we find a rather small excess at 500 microns (< 1.5 sigma). We find that the dust SED of low-metallicity galaxies is broader and peaks at shorter wavelengths compared to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The PAH mass fraction and the dust temperature distribution are found to be driven mostly by the specific star-formation rate, SSFR, with secondary effects from metallicity. The correlations between metallicity and dust mass or total-IR luminosity are direct consequences of the stellar mass-metallicity relation. The dust-to-stellar mass ratios of metal-rich sources follow the well-studied trend of decreasing ratio for decreasing SSFR. The relation is more complex for highly star-forming low-metallicity galaxies and depends on the chemical evolutionary stage of the source (i.e., gas-to-dust mass ratio). Dust growth processes in the ISM play a key role in the dust mass build-up with respect to the stellar content at high SSFR and low metallicity. (abridged), 44 pages (20 pages main body plus 5 Appendices), 11 figures, 9 tables, accepted for publication in A&A
Published: 2015

17. Investigations of dust heating in M81, M83 and NGC 2403 with the Herschel Space Observatory

Author: Marc Sauvage, Haley Louise Gomez, S. C. Madden, Bernhard Schulz, Helene Roussel, David L. Clements, Vianney Lebouteiller, Luca Cortese, Maud Galametz, George J. Bendo, Aliakbar Dariush, Christine D. Wilson, Maarten Baes, L. Spinoglio, Matthew Smith, A. Cooray, K. Foyle, Nanyao Y. Lu, M. J. Page, Erin Mentuch, B. O'Halloran, A. Remy, Alessandro Boselli, and Michael Pohlen
Subjects: Physics, Spiral galaxy, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Radiation, 01 natural sciences, Galaxy, Starlight, Stars, Spitzer Space Telescope, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Surface brightness, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We use Spitzer Space Telescope and Herschel Space Observatory far-infrared data along with ground-based optical and near-infrared data to understand how dust heating in the nearby face-on spiral galaxies M81, M83, and NGC 2403 is affected by the starlight from all stars and by the radiation from star forming regions. We find that 70/160 micron surface brightness ratios tend to be more strongly influenced by star forming regions. However, the 250/350 micron and 350/500 micron surface brightness ratios are more strongly affected by the light from the total stellar populations, suggesting that the dust emission at >250 microns originates predominantly from a component that is colder than the dust seen at
Published: 2011

18. On the origin of M81 group extended dust emission

Author: Bernhard Schulz, L. Spinoglio, Maud Galametz, Andreas Papageorgiou, Jason Glenn, Jonathan Ivor Davies, Marc Sauvage, N. Lu, Matthew Joseph Griffin, Eli Dwek, Robbie Richard Auld, D. Elbaz, Seb Oliver, M. J. Barlow, Herve Wozniak, Laure Ciesla, B. O'Halloran, L. R. Levenson, Ismael Perez-Fournon, Alessandro Boselli, A. Rykala, M. Bradford, M. Trichas, Christine D. Wilson, Frédéric Galliano, Walter Kieran Gear, Naseem Rangwala, George J. Bendo, Maximilien R. P. Schirm, Maarten Baes, Mat Page, A. Cooray, Jamie Stevens, Mattia Vaccari, Koryo Okumura, N. Sacchi, Sundar Srinivasan, T. J. Parkin, Diane Cormier, Suzanne C. Madden, Pasquale Panuzzo, N. Castro-Rodriguez, V. Buat, E. E. Rigby, Michael Pohlen, Kate Gudrun Isaak, M. Symeonidis, Matthew Smith, Helene Roussel, David L. Clements, Luca Cortese, L. Vigroux, James J. Bock, Stephane Charlot, Sacha Hony, Gillian S. Wright, Haley Louise Gomez, Pierre Chanial, Stephen Anthony Eales, and Werner W. Zeilinger
Subjects: Physics, Infrared, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Minute of arc, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Wavelength, Space and Planetary Science, Group (periodic table), Cirrus, Optical emission spectroscopy, Astrophysics::Galaxy Astrophysics, Dust emission
Abstract: Galactic cirrus emission at far-infrared wavelengths affects many extragalactic observations. Separating this emission from that associated with extragalactic objects is both important and difficult. In this paper we discuss a particular case, the M81 group, and the identification of diffuse structures prominent in the infrared, but also detected at optical wavelengths. The origin of these structures has previously been controversial, ranging from them being the result of a past interaction between M81 and M82 or due to more local Galactic emission. We show that over of order a few arcminute scales the far-infrared (Herschel 250 &\mu&m) emission correlates spatially very well with a particular narrow velocity (2-3 km/s) component of the Galactic HI. We find no evidence that any of the far-infrared emission associated with these features actually originates in the M81 group. Thus we infer that the associated diffuse optical emission must be due to galactic light back scattered off dust in our galaxy. Ultra-violet observations pick out young stellar associations around M81, but no detectable far-infrared emission. We consider in detail one of the Galactic cirrus features, finding that the far-infrared HI relation breaks down below arc minute scales and that at smaller scales there can be quite large dust temperature variations.
Published: 2010

19. The dense cores and filamentary structure of the molecular cloud in Corona Australis: Herschel SPIRE and PACS observations from the Herschel Gould Belt Survey

Author: Glenn J. White, Ph. André, Vera Könyves, Nicola Schneider, Alexander Men'shchikov, Jason M. Kirk, Milena Benedettini, J. Di Francesco, Stefano Pezzuto, Doris Arzoumanian, Kate Pattle, Sergio Molinari, P. Palmeirim, Andrea Bracco, D. Bresnahan, S. P. S. Eyres, L. Spinoglio, Bilal Ladjelate, Derek Ward-Thompson, ITA, GBR, FRA, and CAN
Subjects: Physics, 010504 meteorology & atmospheric sciences, Mass distribution, Spectrometer, F510, Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, F500, Astrophysics, Spatial distribution, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Corona, Wavelength, Spire, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Protostar, 14. Life underwater, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We present a catalogue of prestellar and starless cores within the Corona Australis molecular cloud using photometric data from the Herschel Space Observatory. At a distance of d~130 pc, Corona Australis is one of the closest star-forming regions. Herschel has taken multi-wavelength data of Corona Australis with both the SPIRE and PACS photometric cameras in a parallel mode with wavelengths in the range 70 {\mu}m to 500 {\mu}m. A complete sample of starless and prestellar cores and embedded protostars is identified. Other results from the Herschel Gould Belt Survey have shown spatial correlation between the distribution of dense cores and the filamentary structure within the molecular clouds. We go further and show correlations between the properties of these cores and their spatial distribution within the clouds, with a particular focus on the mass distribution of the dense cores with respect to their filamentary proximity. We find that only lower-mass starless cores form away from filaments, while all of the higher-mass prestellar cores form in close proximity to, or directly on the filamentary structure. This result supports the paradigm that prestellar cores mostly form on filaments. We analyse the mass distribution across the molecular cloud, finding evidence that the region around the Coronet appears to be at a more dynamically advanced evolutionary stage to the rest of the clumps within the cloud., Comment: Article Accepted September 2017
Published: 2018

20. The Herschel Reference Survey

Author: Jason Glenn, E. Dwek, George J. Bendo, Jamie Stevens, Alessandro Boselli, N. Sacchi, Mat Page, Walter Kieran Gear, L. Vigroux, Ismael Perez-Fournon, Maximilien R. P. Schirm, K. Okumura, P. Chanial, K. G. Isaak, A. Rykala, Diane Cormier, James J. Bock, Jonathan Ivor Davies, E. E. Rigby, Marc Sauvage, Stephane Charlot, Matthew Smith, Michael Pohlen, N. Castro-Rodriguez, G. Wright, L. Spinoglio, N. Rangwala, Louis Levenson, Robbie Richard Auld, D. Elbaz, Matthew Joseph Griffin, Helene Roussel, David L. Clements, Christine D. Wilson, B. O'Halloran, Benjamin L. Schulz, Luca Cortese, V. Buat, Werner W. Zeilinger, Frédéric Galliano, Haley Louise Gomez, Stephen Anthony Eales, Maarten Baes, M. Bradford, P. Panuzzo, Nanyao Y. Lu, M. J. Barlow, M. Symeonidis, Suzanne C. Madden, S. J. Oliver, Sacha Hony, T. J. Parkin, Herve Wozniak, Andreas Papageorgiou, Maud Galametz, and Mattia Vaccari
Subjects: Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, media_common.quotation_subject, FOS: Physical sciences, Astronomy and Astrophysics, Sample (statistics), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Virgo Cluster, Galaxy, Universe, Interstellar medium, Stars, Space and Planetary Science, Range (statistics), Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, media_common
Abstract: The Herschel Reference Survey is a guaranteed time Herschel key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350 and 500 micron. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K-band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the centre of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass and environment, (ii) the connection between the dust content and composition and the other phases of the interstellar medium and (iii) the origin and evolution of dust in galaxies. In this paper, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multi-frequency data to carry out an analysis of the statistical properties of the sample., Comment: Accepted for publication on PASP
Published: 2010

21. Detection of two power-law tails in the probability distribution functions of massive GMCs

Author: Nicola Schneider, D. Russeil, S. Pezzuto, Frédérique Motte, Volker Ossenkopf, L. Spinoglio, M. Benedettini, S. Bontemps, Timea Csengeri, T. Rayner, Alain Abergel, J. Di Francesco, P. Didelon, Philipp Girichidis, L. D. Anderson, A. Rivera-Ingraham, Ralf S. Klessen, Matthew Joseph Griffin, Pascal Tremblin, T. Hill, A. Zavagno, D. Arzoumanian, Ph. André, FORMATION STELLAIRE 2015, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Universität zu Köln = University of Cologne, Max-Planck-Institut für Astrophysik (MPA), Max-Planck-Gesellschaft, School of Physics and Astronomy [Cardiff], Cardiff University, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), National Radio Astronomy Observatory [Green Bank] (NRAO), National Radio Astronomy Observatory (NRAO), Department of Physics and Astronomy [Morgantown], West Virginia University [Morgantown], Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), Max-Planck-Institut für Radioastronomie (MPIFR), NRC Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Zentrum für Astronomie der Universität Heidelberg (ZAH), Universität Heidelberg [Heidelberg] = Heidelberg University, Operations Department (ESAC), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA)-Agence Spatiale Européenne = European Space Agency (ESA), University of Exeter, ANR-11-BS56-0010,STARFICH,Vers une vision unifiée de la formation stellaire dans les galaxies : Origine de la structure filamentaire du milieu interstellaire, des cœurs pré-stellaires et des amas protostellaires vus avec Herschel(2011), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Procédés, Matériaux et Energie Solaire ( PROMES ), Université de Perpignan Via Domitia ( UPVD ) -Centre National de la Recherche Scientifique ( CNRS ), Institut d'astrophysique spatiale ( IAS ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), National Radio Astronomy Observatory [Green Bank] ( NRAO ), National Radio Astronomy Observatory ( NRAO ), School of Physics & Astronomy [Cardiff], Laboratoire d'Astrophysique de Marseille ( LAM ), Aix Marseille Université ( AMU ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National d'Etudes Spatiales ( CNES ) -Centre National de la Recherche Scientifique ( CNRS ), Procédés, Matériaux et Energie Solaire (PROMES), Université de Perpignan Via Domitia (UPVD)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Maison de la Simulation (MDLS), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Recherche en Informatique et en Automatique (Inria)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: Physics, dust extinction, Angular momentum, extinction, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Power law, Astrophysics - Astrophysics of Galaxies, ISM: clouds, Space and Planetary Science, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics of Galaxies (astro-ph.GA), Gravitational collapse, Log-normal distribution, Optical depth (astrophysics), Range (statistics), Probability distribution, clouds dust, ISM, Astrophysics::Galaxy Astrophysics
Abstract: We report the novel detection of complex high-column density tails in the probability distribution functions (PDFs) for three high-mass star-forming regions (CepOB3, MonR2, NGC6334), obtained from dust emission observed with Herschel. The low column density range can be fit with a lognormal distribution. A first power-law tail starts above an extinction (Av) of ~6-14. It has a slope of alpha=1.3-2 for the rho~r^-alpha profile for an equivalent density distribution (spherical or cylindrical geometry), and is thus consistent with free-fall gravitational collapse. Above Av~40, 60, and 140, we detect an excess that can be fitted by a flatter power law tail with alpha>2. It correlates with the central regions of the cloud (ridges/hubs) of size ~1 pc and densities above 10^4 cm^-3. This excess may be caused by physical processes that slow down collapse and reduce the flow of mass towards higher densities. Possible are: 1. rotation, which introduces an angular momentum barrier, 2. increasing optical depth and weaker cooling, 3. magnetic fields, 4. geometrical effects, and 5. protostellar feedback. The excess/second power-law tail is closely linked to high-mass star-formation though it does not imply a universal column density threshold for the formation of (high-mass) stars., MNRAS Letters, accepted 20.7.2015, in press
Published: 2015

22. The Herschel Comprehensive (U)LIRG Emission Survey (HERCULES): CO Ladders, Fine Structure Lines, and Neutral Gas Cooling

Author: Aaron S. Evans, J. Fischer, Fabian Walter, L. Spinoglio, Andrew I. Harris, Lee Armus, Emmanuel M. Xilouris, Susanne Aalto, Marco Spaans, Howard A. Smith, Eduardo González-Alfonso, M. H. D. van der Wiel, Gordon J. Stacey, David A. Naylor, Thomas R. Greve, M. J. F. Rosenberg, C. Kramer, Vassilis Charmandaris, Tanio Díaz-Santos, Frank P. Israel, P. van der Werf, Yu Gao, Carsten Henkel, David B. Sanders, K. G. Isaak, A. Weiß, Sylvain Veilleux, M. C. Wiedner, I. Veenendaal, Rowin Meijerink, Leiden Observatory [Leiden], Universiteit Leiden, Chalmers University of Technology [Göteborg], Institute for Space Applications and Remote Sensing (ISARS/NOA), National Observatory of Athens (NOA), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Universidad Diego Portales [Santiago] (UDP), Neurobiologie des signaux intercellulaires (NSI), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Institute of Earthquake Science, Universidad de Alcalá - University of Alcalá (UAH), Institut für Physik (Institut für Physik), University of Potsdam = Universität Potsdam, School of Physics and Astronomy [Cardiff], Cardiff University, Instituto de RadioAstronomía Milimétrica (IRAM), Centre National de la Recherche Scientifique (CNRS), Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), University of Maryland [College Park], University of Maryland System, Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Département de Physique, Albert-Ludwigs-Universität Freiburg, Universiteit Leiden [Leiden], École normale supérieure - Paris (ENS Paris), Universität Potsdam, and Kapteyn Astronomical Institute
Subjects: molecular data, Infrared, FOS: Physical sciences, Astrophysics, 01 natural sciences, Luminosity, Far infrared, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, photon-dominated region: PDR, Line (formation), Physics, Luminous infrared galaxy, [PHYS]Physics [physics], galaxies: individual: ULIRGs, 010308 nuclear & particles physics, Order (ring theory), Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM
Abstract: (Ultra) luminous infrared galaxies ((U)LIRGs) are objects characterized by their extreme infrared (8-1000 μm) luminosities (L LIRG > 1011 L ☉ and L ULIRG > 1012 L ☉). The Herschel Comprehensive ULIRG Emission Survey (PI: van der Werf) presents a representative flux-limited sample of 29 (U)LIRGs that spans the full luminosity range of these objects (1011 L ☉ IR 13 L ☉). With the Herschel Space Observatory, we observe [C II] 157 μm, [O I] 63 μm, and [O I] 145 μm line emission with Photodetector Array Camera and Spectrometer, CO J = 4-3 through J = 13-12, [C I] 370 μm, and [C I] 609 μm with SPIRE, and low-J CO transitions with ground-based telescopes. The CO ladders of the sample are separated into three classes based on their excitation level. In 13 of the galaxies, the [O I] 63 μm emission line is self absorbed. Comparing the CO excitation to the InfraRed Astronomical Satellite 60/100 μm ratio and to far infrared luminosity, we find that the CO excitation is more correlated to the far infrared colors. We present cooling budgets for the galaxies and find fine-structure line flux deficits in the [C II], [Si II], [O I], and [C I] lines in the objects with the highest far IR fluxes, but do not observe this for CO 4 upp Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
Published: 2015

23. Herschel observations of B1-bS and B1-bN: two ﬁrst hydrostatic core candidates in the Perseus star-forming cloud

Author: S. Pezzuto, D. Elia, E. Schisano, J. Di Francesco, S. Sadavoy, P. André, M. Benedettini, J. P. Bernard, A. M. di Giorgio, A. Facchini, M. Hennemann, T. Hill, V. Könyves, S. Molinari, F. Motte, Q. Nguyen Luong, N. Peretto, M. Pestalozzi, D. Polychroni, K. L. J. Rygl, P. Saraceno, N. Schneider, L. Spinoglio, L. Testi, D. Ward Thompson, G. J. White, STRAFELLA, Francesco, S., Pezzuto, D., Elia, E., Schisano, Strafella, Francesco, J., Di Francesco, S., Sadavoy, P., André, M., Benedettini, J. P., Bernard, A. M., di Giorgio, A., Facchini, M., Hennemann, T., Hill, V., Könyve, S., Molinari, F., Motte, Q., Nguyen Luong, N., Peretto, M., Pestalozzi, D., Polychroni, K. L. J., Rygl, P., Saraceno, N., Schneider, L., Spinoglio, L., Testi, D., Ward Thompson, and G. J., White
Subjects: protostelle, formazione stellare
Abstract: We report far-infrared Herschel observations obtained between 70 μm and 500 μm of two star-forming dusty condensations, B1-bS and B1-bN, in the B1 region of the Perseus star-forming cloud. In the western part of the Perseus cloud, B1-bS is the only source detected in all six PACS and SPIRE photometric bands, but it is not visible in the Spitzer map at 24 μm. B1-bN is clearly detected between 100 μm and 250 μm. We have ﬁtted the spectral energy distributions of these sources to derive their physical properties, and ﬁnd that a simple greybody model fails to reproduce the observed spectral energy distributions. At least a two-component model is required, consisting of a central source surrounded by a dusty envelope. The properties derived from the ﬁt, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-ﬁt models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the ﬁrst hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow studying the mutual interactions between two forming stars at a very early stage of their evolution.
Published: 2012

24. The Nature of the Mid-Infrared Population from Optical Identifications of the ELAIS-S1 Sample

Author: F. La Franca, C. Gruppioni, I. Matute, F. Pozzi, C. Lari, M. Mignoli, G. Zamorani, D. M. Alexander, F. Cocchia, L. Danese, A. Franceschini, P. Héraudeau, J. K. Kotilainen, M. J. D. Linden-Vørnle, S. Oliver, M. Rowan-Robinson, S. Serjeant, L. Spinoglio, A. Verma, La Franca F., Gruppioni C., Matute I., Pozzi F., Lari C., Mignoli M., Zamorani G., Alexander D. M., Cocchia F., Danese L., Franceschini A., Héraudeau P., Kotilainen J. K., Linden-Vørnle M. J. D., Oliver S., Rowan-Robinson M., Serjeant S., Spinoglio L., Verma A., LA FRANCA, Fabio, Gruppioni, C, Matute, I, Pozzi, F, Lari, C, Mignoli, M, Zamorani, G, Alexander, Dm, Cocchia, F, Danese, L, Franceschini, A, Heraudeau, P, Kotilainen, Jk, Linden Vornle, Mjd, Oliver, S, Robinson, Mr, Serjeant, S, Spinoglio, L, Verma, A., and Astronomy
Subjects: 15 MU-M, galaxies : evolution, galaxies : active, Young stellar object, Population, Mid infrared, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, ENERGY-DISTRIBUTIONS, STAR-FORMATION RATE, Spectral line, Luminosity, galaxies : distances and redshifts, DATA REDUCTION, education, Astrophysics::Galaxy Astrophysics, SPECTROPHOTOMETRIC STANDARDS, Physics, education.field_of_study, infrared : galaxies, FRANCE REDSHIFT SURVEY, Astrophysics (astro-ph), STARBURST GALAXIES, Astronomy and Astrophysics, Galaxy, cosmology : observations, AREA ISO SURVEY, Space and Planetary Science, DEEP-FIELD-SOUTH, SOURCE COUNTS, galaxies : starburst
Abstract: We present a multi-wavelength catalog (15 um, R, K-band, 1.4 GHz flux) plus spectroscopic identifications for 406 15 um sources detected in the ELAIS region S1, over the flux density range 0.5, Comment: Scheduled on AJ, Vol. 127/6, 2004 June. Table 2 (+ 15um sources coordinates) at http://www.fis.uniroma3.it/~ELAIS_S/lafrancabab.tab2.dat . Table 3 at http://www.fis.uniroma3.it/~ELAIS_S/lafrancabab.tab3.dat . Other related data and papers at http://www.fis.uniroma3.it/~ELAIS_S/ . Few luminosities in Table 2 corrected
Published: 2004

25. Extreme dust disks in Arp 220 as revealed by ALMA

Author: Jason Glenn, Naseem Rangwala, Miguel Pereira-Santaella, Christine D. Wilson, L. Spinoglio, and P. R. Maloney
Subjects: Physics, Active galactic nucleus, Opacity, 010308 nuclear & particles physics, Extinction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Submillimeter Array, Astrophysics - Astrophysics of Galaxies, Galaxy, Luminosity, medicine.anatomical_structure, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, medicine, 010303 astronomy & astrophysics, Nucleus, Cosmic dust
Abstract: We present new images of Arp 220 from the Atacama Large Millimeter/submillimeter Array with the highest combination of frequency (691 GHz) and resolution ($0.36 \times 0.20^{\prime\prime}$) ever obtained for this prototypical ultraluminous infrared galaxy. The western nucleus is revealed to contain warm (200 K) dust that is optically thick ($\tau_{434\mu m} = 5.3$), while the eastern nucleus is cooler (80 K) and somewhat less opaque ($\tau_{434\mu m} = 1.7$). We derive full-width half-maximum diameters of $ 76 \times \le 70$ pc and $123 \times 79$ pc for the western and eastern nucleus, respectively. The two nuclei combined account for ($83 ^{+65}_{-38}$ (calibration) $^{+0}_{-34}$ (systematic))% of the total infrared luminosity of Arp 220. The luminosity surface density of the western nucleus ($ \log(\sigma T^4) = 14.3\pm 0.2 ^{+0}_{-0.7}$ in units of L$_\odot$ kpc$^{-2}$) appears sufficiently high to require the presence of an AGN or a "hot starburst", although the exact value depends sensitively on the brightness distribution adopted for the source. Although the role of any central AGN remains open, the inferred mean gas column densities of $0.6-1.8 \times 10^{25}$ cm$^{-2}$ mean that any AGN in Arp 220 must be Compton-thick., Comment: Accepted to ApJ Letters
Published: 2014

26. FISICA (Far Infrared Space Interferometer Critical Assessment) metrological problems and system requirements for interferometric observations from space

Author: Emiliano Fiorenza, Francesco Santoli, L. Spinoglio, C. Magnafico, Carlo Lefevre, L. Iafolla, and Valerio Iafolla
Subjects: Physics, System requirements, Interferometry, Far infrared, Electronic engineering, Systems engineering, Instrumentation (computer programming), Space (commercial competition), Outcome (probability), Low technology, Metrology
Abstract: FISICA (Far Infrared Space Interferometer Critical Assessment) is an FP7 program of the European community that aims to bring together the leading international experts on FIR (Far InfraRed) space instrumentation, in the effort to identify the scientific questions connected to high spatial resolution observations in the FIR and to translate these questions into a technological definition of a FIR space mission. To this finality the technologies relevant for a space interferometer which are at a low Technology Readiness Level will be studied and analyzed, trying to implement the appropriate solutions to current problems. The outcome of this study will advance the knowledge and technology required for a future FIR mission, consolidating the scientific community and bringing world-wide expertise to the EU consortium.
Published: 2014

27. THE PHYSICAL CHARACTERISTICS OF THE GAS IN THE DISK OF CENTAURUS A USING THE HERSCHEL SPACE OBSERVATORY

Author: Christine D. Wilson, I. De Looze, Médéric Boquien, L. Spinoglio, Alessandro Boselli, M. R. P. Schirm, Matthew Smith, Helene Roussel, Maarten Baes, Vianney Lebouteiller, Suzanne C. Madden, D. Cormier, O. Ł. Karczewski, Maud Galametz, T. J. Parkin, McMaster University [Hamilton, Ontario], Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universität Heidelberg [Heidelberg] = Heidelberg University, University of Cambridge [UK] (CAM), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), AUTRES, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Universiteit Gent, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universität Heidelberg [Heidelberg], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)
Subjects: ULTRALUMINOUS INFRARED GALAXIES, C-II, Centaurus A, Doubly ionized oxygen, MU-M, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, PHOTODISSOCIATION REGIONS, 01 natural sciences, PHOTON-DOMINATED REGIONS, 0103 physical sciences, STAR-FORMING GALAXIES, EARLY-TYPE GALAXIES, Emission spectrum, Spectroscopy, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, QB, Physics, individual (Centaurus A) [galaxies], Spiral galaxy, ISM [galaxies], INTERSTELLAR-MEDIUM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, ISM [infrared], Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, MOLECULAR GAS, Interstellar medium, Physics and Astronomy, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), NGC 5128, Elliptical galaxy, lines and bands [ISM]
Abstract: We search for variations in the disk of Centaurus A of the emission from atomic fine structure lines using Herschel PACS and SPIRE spectroscopy. In particular we observe the [C II](158 $\mu$m), [N II](122 and 205 $\mu$m), [O I](63 and 145 $\mu$m) and [O III](88 $\mu$m) lines, which all play an important role in cooling the gas in photo-ionized and photodissociation regions. We determine that the ([C II]+[O I]$_{63}$)/$F_{TIR}$ line ratio, a proxy for the heating efficiency of the gas, shows no significant radial trend across the observed region, in contrast to observations of other nearby galaxies. We determine that 10 - 20% of the observed [C II] emission originates in ionized gas. Comparison between our observations and a PDR model shows that the strength of the far-ultraviolet radiation field, $G_0$, varies between $10^{1.75}$ and $10^{2.75}$ and the hydrogen nucleus density varies between $10^{2.75}$ and $10^{3.75}$ cm$^{-3}$, with no significant radial trend in either property. In the context of the emission line properties of the grand-design spiral galaxy M51 and the elliptical galaxy NGC 4125, the gas in Cen A appears more characteristic of that in typical disk galaxies rather than elliptical galaxies., Comment: Accepted for publication in the Astrophysical Journal. 22 pages, 10 figures, 5 tables
Published: 2014

28. Reconstructing the density and temperature structure of prestellar cores from

Author: A. Roy, Ph. Andrxe9, P. Palmeirim, M. Attard, V. Kxf6nyves, N. Schneider, N. Peretto, A. Men’shchikov, D. Ward-Thompson, J. Kirk, M. Griffin, K. Marsh, A. Abergel, D. Arzoumanian, M. Benedettini, T. Hill, F. Motte, Q. Nguyen Luong, S. Pezzuto, A. Rivera-Ingraham, H. Roussel, K. L. J. Rygl, L. Spinoglio, D. Stamatellos, and G. White
Published: 2014

29. Insights into gas heating and cooling in the disc of NGC 891 from Herschel far-infrared spectroscopy

Author: I. De Looze, Alessandro Boselli, George J. Bendo, Sébastien Viaene, Jacopo Fritz, A. Cooray, S. C. Madden, T. M. Hughes, K. Foyle, Vianney Lebouteiller, Maarten Baes, M. R. P. Schirm, D. Cormier, O. Ł. Karczewski, L. Spinoglio, C. D. Wilson, Nanyao Y. Lu, T. J. Parkin, Sterrenkundig Observatorium, Universiteit Gent, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Universiteit Gent = Ghent University (UGENT), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
Subjects: galaxies: spiral, Hydrogen, Flux, chemistry.chemical_element, FOS: Physical sciences, Astrophysics, PHOTODISSOCIATION REGIONS, galaxies [infrared], infrared: galaxies, MU-M LINE, MICRON LINE DEFICIT, galaxies: individual: NGC 891, STAR-FORMING GALAXIES, Spectroscopy, Optical depth, C-II EMISSION, Physics, Spiral galaxy, ISM [galaxies], INTERSTELLAR-MEDIUM, Astronomy and Astrophysics, HUBBLE-SPACE-TELESCOPE, Gas heating, Photoelectric effect, Astrophysics - Astrophysics of Galaxies, ISM: lines and bands, spiral [galaxies], SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, chemistry, Space and Planetary Science, individual: NGC 891 [galaxies], Astrophysics of Galaxies (astro-ph.GA), MULTIBAND IMAGING PHOTOMETER, Far infrared spectroscopy, lines and bands [ISM], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], NEARBY SPIRAL GALAXIES, galaxies: ISM
Abstract: We present Herschel PACS and SPIRE spectroscopy of the most important far-infrared cooling lines in the nearby edge-on spiral galaxy, NGC 891: [CII] 158 $��$m, [NII] 122, 205 $��$m, [OI] 63, 145 $��$m, and [OIII] 88 $��$m. We find that the photoelectric heating efficiency of the gas, traced via the ([CII]+[OII]63)/$F_{\mathrm{TIR}}$ ratio, varies from a mean of 3.5$\times$10$^{-3}$ in the centre up to 8$\times$10$^{-3}$ at increasing radial and vertical distances in the disc. A decrease in ([CII]+[OII]63)/$F_{\mathrm{TIR}}$ but constant ([CII]+[OI]63)/$F_{\mathrm{PAH}}$ with increasing FIR colour suggests that polycyclic aromatic hydrocarbons (PAHs) may become important for gas heating in the central regions. We compare the observed flux of the FIR cooling lines and total IR emission with the predicted flux from a PDR model to determine the gas density, surface temperature and the strength of the incident far-ultraviolet (FUV) radiation field, $G_{0}$. Resolving details on physical scales of ~0.6 kpc, a pixel-by-pixel analysis reveals that the majority of the PDRs in NGC 891's disc have hydrogen densities of 1 < log ($n$/cm$^{-3}$) < 3.5 experiencing an incident FUV radiation field with strengths of 1.7 < log $G_0$ < 3. Although these values we derive for most of the disc are consistent with the gas properties found in PDRs in the spiral arms and inter-arm regions of M51, observed radial trends in $n$ and $G_0$ are shown to be sensitive to varying optical thickness in the lines, demonstrating the importance of accurately accounting for optical depth effects when interpreting observations of high inclination systems. With an empirical relationship between the MIPS 24 $��$m and [NII] 205 $��$m emission, we estimate an enhancement of the FUV radiation field strength in the far north-eastern side of the disc., Accepted for publication in A&A. 25 pages, including 17 figures and 3 tables, abstract abridged for arXiv
Published: 2014
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30. Dust spectral energy distributions of nearby galaxies: an insight from the Herschel Reference Survey

Author: Luca Cortese, Stephen Anthony Eales, S. C. Madden, Alessandro Boselli, George J. Bendo, Maarten Baes, Matthew Smith, Sébastien Viaene, Sebastien Heinis, Laure Ciesla, I. De Looze, S. di Serego Alighieri, V. Buat, Daniele Pierini, A. Rémy-Ruyer, Thomas M. Hughes, Simone Bianchi, Catherine Vlahakis, Médéric Boquien, Frédéric Galliano, L. Spinoglio, Maud Galametz, Mattia Vaccari, Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Sterrenkundig Observatorium, Universiteit Gent, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Universiteit Gent = Ghent University (UGENT)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, Infrared, Metallicity, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, STAR-FORMING GALAXIES, Astrophysics::Solar and Stellar Astrophysics, Surface brightness, SMALL-MAGELLANIC-CLOUD, education, Astrophysics::Galaxy Astrophysics, QB, SPITZER-SPACE-TELESCOPE, Physics, education.field_of_study, ISM [galaxies], extinction, Astronomy and Astrophysics, MID-IR EMISSION, VIRGO CLUSTER, Astrophysics - Astrophysics of Galaxies, FAR-INFRARED PROPERTIES, Galaxy, Stars, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, dust, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], SPIRAL GALAXIES, LOW-METALLICITY ENVIRONMENTS, INTERSTELLAR DUST, galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We gather infrared (IR) photometric data from 8 to 500 microns (Spitzer, WISE, IRAS and Herschel) for all of the HRS galaxies. Draine & Li (2007) models are fit to the data from which the stellar contribution has been carefully removed. We find that our photometric coverage is sufficient to constrain all of the models parameters and that a strong constraint on the 20-60 microns range is mandatory to estimate the relative contribution of the photo-dissociation regions to the IR SED. The SED models tend to systematically under-estimate the observed 500 microns flux densities, especially for low mass systems. We provide the output parameters for all of the galaxies: the minimum intensity of the interstellar radiation field (ISRF), the fraction of PAH, the relative contribution of PDR and evolved stellar population to the dust heating, the $M_{dust}$ and the $L_{IR}$. For a subsample of gas-rich galaxies, we analyze the relations between these parameters and the integrated properties of galaxies, such as $M_*$, SFR, metallicity, H$\alpha$ and H-band surface brightness, and the FUV attenuation. A good correlation between the fraction of PAH and the metallicity is found implying a weakening of the PAH emission in galaxies with low metallicities. The intensity of the IRSF and the H-band and H$\alpha$ surface brightnesses are correlated, suggesting that the diffuse dust component is heated by both the young stars in star forming regions and the diffuse evolved population. We use these results to provide a new set of IR templates calibrated with Herschel observations on nearby galaxies and a mean SED template to provide the z=0 reference for cosmological studies. For the same purpose, we put our sample on the SFR-$M_*$ diagram. The templates are compared to the most popular IR SED libraries, enlightening a large discrepancy between all of them in the 20-100 microns range., Comment: 37 pages, 17 figures, 11 tables, accepted for publication in A&A
Published: 2014

31. Reconstructing the density and temperature structure of prestellar cores from $Herschel$ data: A case study for B68 and L1689B

Author: Dimitris Stamatellos, Kazi L.J. Rygl, Stefano Pezzuto, T. Hill, Frédérique Motte, A. Abergel, A. Rivera-Ingraham, Glenn J. White, Ph. André, Doris Arzoumanian, Helene Roussel, Alexander Men'shchikov, Vera Könyves, Nicolas Peretto, Kenneth A. Marsh, Derek Ward-Thompson, L. Spinoglio, Milena Benedettini, Matthew Joseph Griffin, M. Attard, P. Palmeirim, Nicola Schneider, Jason M. Kirk, A. Roy, Q. Nguyen Luong, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Oristars, Oristars (291294), European Project: 291294,EC:FP7:ERC,ERC-2011-ADG_20110209,ORISTARS(2012), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Opacity, Extinction (astronomy), FOS: Physical sciences, F500, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Lambda, ISM: individual objects: B68, ISM: individual objects: L1689B, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Continuum (set theory), Astrophysics::Galaxy Astrophysics, QB, Physics, Line-of-sight, stars: formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], extinction, Drop (liquid), Center (category theory), Astronomy and Astrophysics, submillimeter: general, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Utilizing multi-wavelength dust emission maps acquired with $Herschel$, we reconstruct local volume density and dust temperature profiles for the prestellar cores B68 and L1689B using inverse-Abel transform based technique. We present intrinsic radial dust temperature profiles of starless cores directly from dust continuum emission maps disentangling the effect of temperature variations along the line of sight which was previously limited to the radiative transfer calculations. The reconstructed dust temperature profiles show a significant drop in core center, a flat inner part, and a rising outward trend until the background cloud temperature is reached. The central beam-averaged dust temperatures obtained for B68 and L1689B are 9.3 $\pm$ 0.5 K and 9.8 $\pm$0.5 K, respectively, which are lower than the temperatures of 11.3 K and 11.6 K obtained from direct SED fitting. The best mass estimates derived by integrating the volume density profiles of B68 and L1689B are 1.6 M_sol and 11 M_sol, respectively. Comparing our results for B68 with the near-infrared extinction studies, we find that the dust opacity law adopted by the HGBS project, $\kappa_{\lambda} =0.1(\lambda/300 \mu m)^{-2}$, agrees to within 50% with the dust extinction constraints, Comment: 10 pages, 7 figures, Accepted for publication to A&A
Published: 2014

32. Ionization compression impact on dense gas distribution and star formation, Probability density functions around H ii regions as seen by Herschel

Author: Nicolas Peretto, J. Di Francesco, T. Giannini, Vincent Minier, Timea Csengeri, A. Rivera-Ingraham, A. P. Marston, Pascal Tremblin, Q. Nguyen Luong, P. Didelon, L. D. Anderson, T. Hill, Annie Zavagno, Nicola Schneider, Doris Arzoumanian, Frédérique Motte, Sylvain Bontemps, Milena Benedettini, Kazi L.J. Rygl, D. Russeil, L. Spinoglio, Martin Hennemann, Glenn J. White, Ph. André, Edouard Audit, FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), foreign laboratories (FL), CERN [Genève], Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Antarctic Research a European Network for Astrophysics (ARENA), Engineering Department, University of Cambridge [UK] (CAM), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Equation of state, H II region, Initial mass function, ISM: structure, Stars: formation, FOS: Physical sciences, Probability density function, Context (language use), Different effects, Astrophysics, Flattening, Ionization of gases, Clouds, Impact ionization, H II regions, QC, Astrophysics::Galaxy Astrophysics, QB, Physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Equations of state, Log-normal distribution, Methods:observational, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Stars, Compression zones, Astrophysics - Astrophysics of Galaxies, Probability distributions, 13. Climate action, Space and Planetary Science, C (programming language), Astrophysics of Galaxies (astro-ph.GA), Gases, Distribution functions
Abstract: Ionization feedback should impact the probability distribution function (PDF) of the column density around the ionized gas. We aim to quantify this effect and discuss its potential link to the Core and Initial Mass Function (CMF/IMF). We used in a systematic way Herschel column density maps of several regions observed within the HOBYS key program: M16, the Rosette and Vela C molecular cloud, and the RCW 120 H ii region. We fitted the column density PDFs of all clouds with two lognormal distributions, since they present a double-peak or enlarged shape in the PDF. Our interpretation is that the lowest part of the column density distribution describes the turbulent molecular gas while the second peak corresponds to a compression zone induced by the expansion of the ionized gas into the turbulent molecular cloud. The condensations at the edge of the ionized gas have a steep compressed radial profile, sometimes recognizable in the flattening of the power-law tail. This could lead to an unambiguous criterion able to disentangle triggered from pre-existing star formation. In the context of the gravo-turbulent scenario for the origin of the CMF/IMF, the double peaked/enlarged shape of the PDF may impact the formation of objects at both the low-mass and the high-mass end of the CMF/IMF. In particular a broader PDF is required by the gravo-turbulent scenario to fit properly the IMF with a reasonable initial Mach number for the molecular cloud. Since other physical processes (e.g. the equation of state and the variations among the core properties) have already been suggested to broaden the PDF, the relative importance of the different effects remains an open question., Accepted in A&A
Published: 2014

33. A resolved analysis of cold dust and gas in the nearby edge-on spiral NGC 891

Author: Jonathan Ivor Davies, Alessandro Boselli, L. Spinoglio, F. Allaert, George J. Bendo, Jacopo Fritz, A. Rémy-Ruyer, Maud Galametz, Gianfranco Gentile, Sébastien Viaene, T. M. Hughes, Médéric Boquien, T. J. Parkin, Matthew Smith, I. De Looze, Suzanne C. Madden, David L. Clements, Christine D. Wilson, Maarten Baes, Joris Verstappen, Simone Bianchi, Sterrenkundig Observatorium, Universiteit Gent = Ghent University (UGENT), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysics, and Astronomy and Astrophysics Research Group
Subjects: HERSCHEL REFERENCE SURVEY, submillimeter: galaxies, galaxies: spiral, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, LOCAL GALAXY ANDROMEDA, galaxies [infrared], 01 natural sciences, infrared: galaxies, POLYCYCLIC AROMATIC-HYDROCARBONS, CO-TO-H-2 CONVERSION FACTOR, VIRGO CLUSTER SURVEY, 0103 physical sciences, galaxies: individual: NGC 891, Emissivity, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, SPITZER-SPACE-TELESCOPE, Physics, Spectral index, NEUTRAL HYDROGEN OBSERVATIONS, Spiral galaxy, ISM [galaxies], Mass distribution, 010308 nuclear & particles physics, Star formation, CLERK-MAXWELL-TELESCOPE, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, spiral [galaxies], Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), individual: NGC 891 [galaxies], MULTIBAND IMAGING PHOTOMETER, Hydrogen line, Spectral energy distribution, LARGE-MAGELLANIC-CLOUD, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We investigate the connection between dust and gas in the nearby edge-on spiral galaxy NGC 891. High resolution Herschel PACS and SPIRE 70, 100, 160, 250, 350, and 500 $\mu$m images are combined with JCMT SCUBA 850 $\mu$m observations to trace the far-infrared/submillimetre spectral energy distribution (SED). Maps of the HI 21 cm line and CO(J=3-2) emission trace the atomic and molecular hydrogen gas, respectively. We fit one-component modified blackbody models to the integrated SED, finding a global dust mass of 8.5$\times$10$^{7}$ M$_{\odot}$ and an average temperature of 23$\pm$2 K. We also fit the pixel-by-pixel SEDs to produce maps of the dust mass and temperature. The dust mass distribution correlates with the total stellar population as traced by the 3.6 $\mu$m emission. The derived dust temperature, which ranges from approximately 17 to 24 K, is found to correlate with the 24 $\mu$m emission. Allowing the dust emissivity index to vary, we find an average value of $\beta$ = 1.9$\pm$0.3. We confirm an inverse relation between the dust emissivity spectral index and dust temperature, but do not observe any variation of this relationship with vertical height from the mid-plane of the disk. A comparison of the dust properties with the gaseous components of the ISM reveals strong spatial correlations between the surface mass densities of dust and the molecular hydrogen and total gas surface densities. Observed asymmetries in the dust temperature, and the H$_{2}$-to-dust and total gas-to-dust ratios hint that an enhancement in the star formation rate may be the result of larger quantities of molecular gas available to fuel star formation in the NE compared to the SW. Whilst the asymmetry likely arises from dust obscuration due to the geometry of the line-of-sight projection of the spiral arms, we cannot exclude an enhancement in the star formation rate in the NE side of the disk., Comment: Accepted for publication in A&A. 21 pages, including 13 figures and 4 tables
Published: 2014

34. Gas-to-Dust mass ratios in local galaxies over a 2 dex metallicity range

Author: Svitlana Zhukovska, Maarten Baes, Thomas M. Hughes, Frédéric Galliano, I. Delooze, S. C. Madden, Ryosuke Asano, M. Bocchio, Tsutomu T. Takeuchi, L. Spinoglio, A. Rémy-Ruyer, D. Cormier, O. Ł. Karczewski, Médéric Boquien, Vianney Lebouteiller, V. Doublier-Pritchard, George J. Bendo, Anthony P. Jones, Alessandro Boselli, Maud Galametz, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), ANR-11-BS56-0023,SYMPATICO,SYnthetic MultiPhase Analysis of The Ism of Cosmic Objects(2011), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)
Subjects: HERSCHEL REFERENCE SURVEY, Cosmology and Nongalactic Astrophysics (astro-ph.CO), dwarf [galaxies], Metallicity, media_common.quotation_subject, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, GRAIN-SIZE DISTRIBUTION, 01 natural sciences, POLYCYCLIC AROMATIC-HYDROCARBONS, CO-TO-H-2 CONVERSION FACTOR, MOLECULAR INTERSTELLAR-MEDIUM, COMPACT DWARF GALAXIES, 0103 physical sciences, evolution, STAR-FORMING GALAXIES, Range (statistics), 010303 astronomy & astrophysics, evolution [galaxies], Astrophysics::Galaxy Astrophysics, media_common, Dwarf galaxy, Physics, infrared: ISM, ISM [galaxies], 010308 nuclear & particles physics, Star formation, extinction, ISM [infrared], Astronomy and Astrophysics, galaxies: dwarf, Mass ratio, RADIO TELESCOPE OBSERVATIONS, Astrophysics - Astrophysics of Galaxies, Galaxy, Universe, SPECTRAL ENERGY-DISTRIBUTION, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), LARGE-MAGELLANIC-CLOUD, dust, Dispersion (chemistry), galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: This paper analyses the behaviour of the gas-to-dust mass ratio (G/D) of local Universe galaxies over a large metallicity range. We combine three samples: the Dwarf Galaxy Survey, the KINGFISH survey and a subsample from Galametz et al. (2011) totalling 126 galaxies, covering a 2 dex metallicity range, with 30% of the sample with 12+log(O/H) < 8.0. The dust masses are homogeneously determined with a semi-empirical dust model, including submm constraints. The atomic and molecular gas masses are compiled from the literature. Two XCO are used to estimate molecular gas masses: the Galactic XCO, and a XCO depending on the metallicity (as Z^{-2}). Correlations with morphological types, stellar masses, star formation rates and specific star formation rates are discussed. The trend between G/D and metallicity is empirically modelled using power-laws (slope of -1 and free) and a broken power-law. We compare the evolution of the G/D with predictions from chemical evolution models. We find that out of the five tested galactic parameters, metallicity is the galactic property driving the observed G/D. The G/D versus metallicity relation cannot be represented by a power-law with a slope of -1 over the whole metallicity range. The observed trend is steeper for metallicities lower than ~ 8.0. A large scatter is observed in the G/D for a given metallicity, with a dispersion of 0.37 dex in metallicity bins of ~0.1 dex. The broken power-law reproduces best the observed G/D and provides estimates of the G/D that are accurate to a factor of 1.6. The good agreement of the G/D and its scatter with the three tested chemical evolution models shows that the scatter is intrinsic to galactic properties, reflecting the different star formation histories, dust destruction efficiencies, dust grain size distributions and chemical compositions across the sample. (abriged), 23 pages, 12 figures, accepted in Astronomy & Astrophysics
Published: 2013

35. Pillars and globules at the edges of H ii regions

Author: Timea Csengeri, P. Didelon, L. Spinoglio, Annie Zavagno, J. P. Bernard, A. P. Marston, Helene Roussel, Edouard Audit, L. D. Anderson, Nicola Schneider, J. Di Francesco, Martin Hennemann, Frédérique Motte, Pascal Tremblin, Vincent Minier, Tracey Hill, Sylvain Bontemps, Jonathan Williams, Glenn J. White, Q. Nguyen Luong, Ph. André, Davide Elia, T. Sousbie, Vera Könyves, Nicolas Peretto, Doris Arzoumanian, A. Rivera-Ingraham, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Maison de la Simulation (MDLS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut National de Recherche en Informatique et en Automatique (Inria)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Engineering Department, University of Cambridge [UK] (CAM), Medical Research Council (MRC) Centre for Neuropsychiatric Genetics and Genomics, Neurosciences and Mental Health Research Institute, Department of Psychological Medicine and Neurology, School of Medicine, Cardiff University, Cardiff, UK, Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), and Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)
Subjects: HII regions, Numerical models, ISM: structure, Infrared imaging, Velocity, Shell (structure), FOS: Physical sciences, Astrophysics, Curvature, 01 natural sciences, Ionization of gases, ISM: individual objects: Rosette, ISM: individual objects: M 16, ISM: individual objects, Clouds, Ionization, H II regions, 0103 physical sciences, Shells (structures), Ism: individual objects: rosettes, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, ISM: kinematics and dynamics, Nebula, 010308 nuclear & particles physics, Turbulence, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Methods:observational, Astronomy and Astrophysics, Computer simulation, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Stars, Astrophysics - Astrophysics of Galaxies, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Gases, methods: observational, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: Pillars and globules are present in many high-mass star-forming regions, such as the Eagle nebula (M16) and the Rosette molecular cloud, and understanding their origin will help characterize triggered star formation. The formation mechanisms of these structures are still being debated. Recent numerical simulations have shown how pillars can arise from the collapse of the shell in on itself and how globules can be formed from the interplay of the turbulent molecular cloud and the ionization from massive stars. The goal here is to test this scenario through recent observations of two massive star-forming regions, M16 and Rosette. The column density structure of the interface between molecular clouds and H ii regions was characterized using column density maps obtained from far-infrared imaging of the Herschel HOBYS key programme. Then, the DisPerSe algorithm was used on these maps to detect the compressed layers around the ionized gas and pillars in different evolutionary states. Finally, their velocity structure was investigated using CO data, and all observational signatures were tested against some distinct diagnostics established from simulations. The column density profiles have revealed the importance of compression at the edge of the ionized gas. The velocity properties of the structures, i.e. pillars and globules, are very close to what we predict from the numerical simulations. We have identified a good candidate of a nascent pillar in the Rosette molecular cloud that presents the velocity pattern of the shell collapsing on itself, induced by a high local curvature. Globules have a bulk velocity dispersion that indicates the importance of the initial turbulence in their formation, as proposed from numerical simulations. Altogether, this study re-enforces the picture of pillar formation by shell collapse and globule formation by the ionization of highly turbulent clouds., Comment: Accepted in A&A
Published: 2013

36. Far-IR Spectrophotometry of HH Flows with the ISO Long-Wavelength Spectrometer

Author: R. Liseau, T. Giannini, B. Nisini, P. Saraceno, L. Spinoglio, B. Larsson, D. Lorenzetti, and E. Tommasi
Abstract: Full Iso-Lws spectral scans between about 45 to 190 μm of 17 individual HH objects in 7 star forming regions have revealed essentially only [O I] 63 μm line emission, implying that the Fircooling of these objects is totally dominated by this line alone. In this case, J-shock models can be used to determine the mass loss rates of the HH exciting sources. These mass loss rates are in reasonably good agreement with those estimated for the accompanying CO flows, providing first observational evidence that HH and molecular flows are driven by the same agent. The Lmech – Lbol relation, based on our results with the Lws, implies that young stellar objects of lower mass are loosing mass at relatively higher rates than their more massive counterparts.
Published: 1997

37. Regional variations in the dense gas heating and cooling in M51 from Herschel far-infrared spectroscopy

Author: Suzanne C. Madden, Maarten Baes, Marc Sauvage, A. Cooray, K. Foyle, M. R. P. Schirm, T. J. Parkin, Alessandro Boselli, D. Cormier, Helene Roussel, I. De Looze, O. Ł. Karczewski, Médéric Boquien, Christine D. Wilson, L. Spinoglio, Vianney Lebouteiller, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Hydrogen density, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Photon, FOS: Physical sciences, Flux, Astrophysics, PHOTODISSOCIATION REGIONS, 01 natural sciences, 0103 physical sciences, Spectroscopy, 010303 astronomy & astrophysics, Physics, INTERSTELLAR-MEDIUM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Molecular cloud, Astronomy and Astrophysics, Gas heating, Astrophysics - Astrophysics of Galaxies, Galaxy, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Far infrared spectroscopy, MOLECULAR CLOUDS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present Herschel PACS and SPIRE spectroscopy of the most important far-infrared cooling lines in M51, [CII](158 \mu m), [NII](122 & 205 \mu m), [OI](63 and 145 \mu m) and [OIII](88 \mu m). We compare the observed flux of these lines with the predicted flux from a photon dominated region model to determine characteristics of the cold gas such as density, temperature and the far-ultraviolet radiation field, G_0, resolving details on physical scales of roughly 600 pc. We find an average [CII]/F_TIR of 4 x 10^{-3}, in agreement with previous studies of other galaxies. A pixel-by-pixel analysis of four distinct regions of M51 shows a radially decreasing trend in both the far-ultraviolet (FUV) radiation field, G_0 and the hydrogen density, n, peaking in the nucleus of the galaxy, then falling off out to the arm and interarm regions. We see for the first time that the FUV flux and gas density are similar in the differing environments of the arm and interarm regions, suggesting that the inherent physical properties of the molecular clouds in both regions are essentially the same., Comment: 24 pages, 7 figures, 9 tables; accepted for publication in the Astrophysical Journal
Published: 2013

38. WHAT DETERMINES THE DENSITY STRUCTURE OF MOLECULAR CLOUDS? A CASE STUDY OF ORION B WITH

Author: N. Schneider, Ph. Andrxe9, V. Kxf6nyves, S. Bontemps, F. Motte, C. Federrath, D. Ward-Thompson, D. Arzoumanian, M. Benedettini, E. Bressert, P. Didelon, J. Di Francesco, M. Griffin, M. Hennemann, T. Hill, P. Palmeirim, S. Pezzuto, N. Peretto, A. Roy, K. L. J. Rygl, L. Spinoglio, and G. White
Published: 2013

39. What determines the density structure of molecular clouds ? A case study of Orion B with Herschel

Author: P. Palmeirim, Vera Könyves, M. Hennemann, Nicola Schneider, Frédérique Motte, Glenn J. White, Ph. André, Doris Arzoumanian, A. Roy, J. Di Francesco, M. Benedettini, Sylvain Bontemps, Nicolas Peretto, Christoph Federrath, Matthew Joseph Griffin, Kazi L.J. Rygl, Stefano Pezzuto, Eli Bressert, Tracey Hill, L. Spinoglio, Derek Ward-Thompson, Pierre Didelon, FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, School of Physics and Astronomy [Cardiff], Cardiff University, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)
Subjects: Physics, 010308 nuclear & particles physics, Turbulence, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Magnetic field, law.invention, Polaris, 13. Climate action, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), Intermittency, 0103 physical sciences, Log-normal distribution, Probability distribution, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: A key parameter to the description of all star formation processes is the density structure of the gas. In this letter, we make use of probability distribution functions (PDFs) of Herschel column density maps of Orion B, Aquila, and Polaris, obtained with the Herschel Gould Belt survey (HGBS). We aim to understand which physical processes influence the PDF shape, and with which signatures. The PDFs of Orion B (Aquila) show a lognormal distribution for low column densities until Av 3 (6), and a power-law tail for high column densities, consistent with a rho r^-2 profile for the equivalent spherical density distribution. The PDF of Orion B is broadened by external compression due to the nearby OB stellar aggregates. The PDF of a quiescent subregion of the non-star-forming Polaris cloud is nearly lognormal, indicating that supersonic turbulence governs the density distribution. But we also observe a deviation from the lognormal shape at Av>1 for a subregion in Polaris that includes a prominent filament. We conclude that (i) the point where the PDF deviates from the lognormal form does not trace a universal Av-threshold for star formation, (ii) statistical density fluctuations, intermittency and magnetic fields can cause excess from the lognormal PDF at an early cloud formation stage, (iii) core formation and/or global collapse of filaments and a non-isothermal gas distribution lead to a power-law tail, and (iv) external compression broadens the column density PDF, consistent with numerical simulations., Astrophysical Journal Letters, received: 2012 December 30; accepted 2013 February 26
Published: 2013

40. Towards understanding the relation between the gas and the attenuation in galaxies at kpc scales

Author: I. De Looze, Maarten Baes, Alessandro Boselli, V. Buat, George J. Bendo, Christine D. Wilson, Laure Ciesla, A. Cooray, Samuel Boissier, Stephen Anthony Eales, Matthew Smith, L. Spinoglio, Vianney Lebouteiller, Médéric Boquien, Luca Cortese, Jin Koda, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University (UGENT), University of Manchester [Manchester], Department of Physics and Astronomy [Irvine], University of California [Irvine] (UC Irvine), University of California (UC)-University of California (UC), European Southern Observatory (ESO), School of Physics and Astronomy [Cardiff], Cardiff University, Stony Brook University [SUNY] (SBU), State University of New York (SUNY), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Astrofisica e Planetologia Spaziali - INAF (IAPS), Istituto Nazionale di Astrofisica (INAF), McMaster University [Hamilton, Ontario], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universiteit Gent [Ghent], University of California [Irvine] (UCI), University of California-University of California, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Universiteit Gent = Ghent University [Belgium] (UGENT)
Subjects: Surface (mathematics), Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, INITIAL MASS FUNCTION, FOS: Physical sciences, Scale (descriptive set theory), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, HIGH-REDSHIFT GALAXIES, Luminosity, infrared: galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, Optical depth, Astrophysics::Galaxy Astrophysics, QB, Physics, radio lines: galaxies, 010308 nuclear & particles physics, extinction, Attenuation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Trace gas, Physics and Astronomy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), ultraviolet: galaxies, dust, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: [abridged] Aims. The aim of the present paper is to provide new and more detailed relations at the kpc scale between the gas surface density and the face-on optical depth directly calibrated on galaxies, in order to compute the attenuation not only for semi-analytic models but also observationally as new and upcoming radio observatories are able to trace gas ever farther in the Universe. Methods. We have selected a sample of 4 nearby resolved galaxies and a sample of 27 unresolved galaxies from the Herschel Reference Survey and the Very Nearby Galaxies Survey, for which we have a large set of multi-wavelength data from the FUV to the FIR including metallicity gradients for resolved galaxies, along with radio HI and CO observations. For each pixel in resolved galaxies and for each galaxy in the unresolved sample, we compute the face-on optical depth from the attenuation determined with the CIGALE SED fitting code and an assumed geometry. We determine the gas surface density from HI and CO observations with a metallicity-dependent XCO factor. Results. We provide new, simple to use, relations to determine the face-on optical depth from the gas surface density, taking the metallicity into account, which proves to be crucial for a proper estimate. The method used to determine the gas surface density or the face-on optical depth has little impact on the relations except for galaxies that have an inclination over 50d. Finally, we provide detailed instructions on how to compute the attenuation practically from the gas surface density taking into account possible information on the metallicity. Conclusions. Examination of the influence of these new relations on simulated FUV and IR luminosity functions shows a clear impact compared to older oft-used relations, which in turn could affect the conclusions drawn from studies based on large scale cosmological simulations., Comment: 24 pages, 21 figures, accepted for publication in A&A
Published: 2013

41. The Herschel and JCMT Gould Belt Surveys: Constraining Dust Properties in the Perseus B1 Clump with PACS, SPIRE, and SCUBA-2

Author: Doug Johnstone, Cassandra Fallscheer, L. Spinoglio, Leonardo Testi, Rachel Friesen, Nicholas F. H Tothill, Kazi L.J. Rygl, E. Drabek, J. Di Francesco, Glenn J. White, Stefano Pezzuto, Jane S. Greaves, Vera Könyves, Doris Arzoumanian, Ana Duarte-Cabral, Jennifer Hatchell, Milena Benedettini, Martin Hennemann, Sarah Sadavoy, Joseph C. Mottram, Tim Jenness, Brenda C. Matthews, N. Schneider-Bontemps, D. Nutter, Philippe André, A. Roy, T. Hill, Malcolm J. Currie, Derek Ward-Thompson, J.-P. Bernard, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, BC V9E 2E7 Canada, Natl Res Council Canada, Herzberg Inst Astrophys, Victoria, School of Physics and Astronomy [Cardiff], Cardiff University, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Opération Cétacés, Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1, Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: FOS: Physical sciences, Astrophysics, 01 natural sciences, ISM: clouds, stars: low-mass, 0103 physical sciences, Emissivity, Dense material, 14. Life underwater, 010303 astronomy & astrophysics, QB, Physics, stars: formation, stars: protostars, 010308 nuclear & particles physics, extinction, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Long wavelength, Spire, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), dust
Abstract: We present Herschel observations from the Herschel Gould Belt Survey and SCUBA-2 science verification observations from the JCMT Gould Belt Survey of the B1 clump in the Perseus molecular cloud. We determined the dust emissivity index using four different techniques to combine the Herschel PACS+SPIRE data at 160 - 500 microns with the SCUBA-2 data at 450 microns and 850 microns. Of our four techniques, we found the most robust method was to filter-out the large-scale emission in the Herschel bands to match the spatial scales recovered by the SCUBA-2 reduction pipeline. Using this method, we find beta ~ 2 towards the filament region and moderately dense material and lower beta values (beta > 1.6) towards the dense protostellar cores, possibly due to dust grain growth. We find that beta and temperature are more robust with the inclusion of the SCUBA-2 data, improving estimates from Herschel data alone by factors of ~ 2 for beta and by ~ 40% for temperature. Furthermore, we find core mass differences of < 30% compared to Herschel-only estimates with an adopted beta = 2, highlighting the necessity of long wavelength submillimeter data for deriving accurate masses of prestellar and protostellar cores., 19 figures, 4 Appendices, Accepted to the Astrophysical Journal
Published: 2013

42. Herschel view of the Taurus B211/3 filament and striations: Evidence of filamentary growth?

Author: P. Palmeirim, Ph. André, J. Kirk, D. Ward-Thompson, D. Arzoumanian, V. Könyves, P. Didelon, N. Schneider, M. Benedettini, S. Bontemps, J. Di Francesco, D. Elia, M. Griffin, M. Hennemann, T. Hill, P. G. Martin, A. Men’shchikov, S. Molinari, F. Motte, Q. Nguyen Luong, D. Nutter, N. Peretto, S. Pezzuto, A. Roy, K. L. J. Rygl, L. Spinoglio, G. L. White, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, FORMATION STELLAIRE 2013, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR)
Subjects: ISM structure, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Isothermal process, Gravitation, Protein filament, 0103 physical sciences, Perpendicular, ISM individual objects, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, 010308 nuclear & particles physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, Star formation, B211–ISM clouds, Astronomy and Astrophysics, Optical polarization, Polytropic process, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Magnetic field, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: We present first results from the Herschel Gould Belt survey for the B211/L1495 region in the Taurus molecular cloud. Thanks to their high sensitivity and dynamic range, the Herschel images reveal the structure of the dense, star-forming filament B211 with unprecedented detail, along with the presence of striations perpendicular to the filament and generally oriented along the magnetic field direction as traced by optical polarization vectors. Based on the column density and dust temperature maps derived from the Herschel data, we find that the radial density profile of the B211 filament approaches a power-law behavior {\rho} {\propto} r^(-2.0{\pm}0.4) at large radii and that the temperature profile exhibits a marked drop at small radii. The observed density and temperature profiles of the B211 filament are in good agreement with a theoretical model of a cylindrical filament undergoing gravitational contraction with a polytropic equation of state: P {\propto} {\rho}^{\gamma} and T {\propto} {\rho}^({\gamma}-1), with {\gamma}=0.97{\pm}0.01, Comment: 9 pages, 7 figures. Accepted for publication by Astronomy and Astrophysics
Published: 2013

43. EFFICACY OF LOW LEVEL LASER THERAPY FOR SYMPATHETIC REFLEX DYSTROPHY SYNDROME IN GERIATRIC PATIENTS

Author: E Hartman, G Castronuovo, S Giavelli, A Fava, L Pisani, L Spinoglio, and A Zingone
Subjects: medicine.medical_specialty, business.industry, medicine.medical_treatment, Anesthesia, Biomedical Engineering, medicine, Dystrophy, Surgery, business, Low level laser therapy, Sympathetic reflex
Published: 1996

44. Herschel observations of B1-bS and B1-bN: two first hydrostatic core candidates in the Perseus star-forming cloud

Author: Martin Hennemann, Sarah Sadavoy, Kazi L.J. Rygl, Davide Elia, Glenn J. White, Ph. André, J. P. Bernard, Frédérique Motte, L. Spinoglio, Milena Benedettini, M. R. Pestalozzi, A. Facchini, Vera Könyves, Quang Nguyen-Luong, Derek Ward-Thompson, Nicolas Peretto, Paolo Saraceno, Leonardo Testi, Sergio Molinari, Francesco Strafella, A. Di Giorgio, Stefano Pezzuto, E. Schisano, T. Hill, Nicola Schneider, J. Di Francesco, D. Polychroni, Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), foreign laboratories (FL), CERN [Genève], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Consiglio Nazionale delle Ricerche (CNR), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées
Subjects: 010504 meteorology & atmospheric sciences, Phase (waves), FOS: Physical sciences, Astrophysics, Star (graph theory), 01 natural sciences, law.invention, law, 0103 physical sciences, 010303 astronomy & astrophysics, QB, 0105 earth and related environmental sciences, Envelope (waves), Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Spectral density, Astronomy and Astrophysics, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Spire, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Hydrostatic equilibrium
Abstract: We report far-IR Herschel observations obtained between 70 $\mu$m and 500 $\mu$m of two star-forming dusty condensations, B1-bS and B1-bN, in the B1 region of the Perseus star-forming cloud. In the Western part of the Perseus cloud, B1-bS is the only source detected in all of the 6 PACS and SPIRE photometric bands without being visible in the Spitzer map at 24 $\mu$m. B1-bN is clearly detected between 100 $\mu$m and 250 $\mu$m. We have fitted the spectral energy distributions of these sources to derive their physical properties, and find that a simple greybody model fails to reproduce the observed SEDs. At least a two-component model, consisting of a central source surrounded by a dusty envelope is required. The properties derived from the fit, however, suggest that the central source is not a Class 0 object. We then conclude that while B1-bS and B1-bN appear to be more evolved than a pre-stellar core, the best-fit models suggest that their central objects are younger than a Class 0 source. Hence, they may be good candidates to be examples of the first hydrostatic core phase. The projected distance between B1-bS and B1-bN is a few Jeans lengths. If their physical separation is close to this value, this pair would allow the mutual interactions between two forming stars at a very early stage of their evolution to be studied., Comment: 14 pages, 4 figures. Accepted for publication in A&A, main journal
Published: 2012
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45. THE HERSCHEL EXPLOITATION OF LOCAL GALAXY ANDROMEDA (HELGA). II. DUST AND GAS IN ANDROMEDA

Author: M. W. L. Smith, S. A. Eales, H. L. Gomez, J. Roman-Duval, J. Fritz, R. Braun, M. Baes, G. J. Bendo, J. A. D. L. Blommaert, M. Boquien, A. Boselli, D. L. Clements, A. R. Cooray, L. Cortese, I. de Looze, G. P. Ford, W. K. Gear, G. Gentile, K. D. Gordon, J. Kirk, V. Lebouteiller, S. Madden, E. Mentuch, B. O’Halloran, M. J. Page, B. Schulz, L. Spinoglio, J. Verstappen, C. D. Wilson, D. A. Thilker, AUTRES, Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), Technische Universität Dresden (TUD), Universiteit Gent [Ghent], Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), European Southern Observatory (ESO), School of Physics and Astronomy, Cardiff University, School of Physics and Astronomy [Cardiff], Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California-University of California, Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Sterrenkundig Observatorium, Universiteit Gent, McMaster University [Hamilton, Ontario], Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Technische Universität Dresden = Dresden University of Technology (TU Dresden), Universiteit Gent = Ghent University [Belgium] (UGENT), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Universiteit Gent = Ghent University (UGENT), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), University of California (UC)-University of California (UC), Réseau nanophotonique et optique, and Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar population, Milky Way, Metallicity, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Bulge, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, Astronomy and Astrophysics, Radius, Astrophysics - Astrophysics of Galaxies, Galaxy, Andromeda, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an analysis of the dust and gas in Andromeda, using Herschel images sampling the entire far-infrared peak. We fit a modified-blackbody model to ~4000 quasi-independent pixels with spatial resolution of ~140pc and find that a variable dust-emissivity index (beta) is required to fit the data. We find no significant long-wavelength excess above this model suggesting there is no cold dust component. We show that the gas-to-dust ratio varies radially, increasing from ~20 in the center to ~70 in the star-forming ring at 10kpc, consistent with the metallicity gradient. In the 10kpc ring the average beta is ~1.9, in good agreement with values determined for the Milky Way (MW). However, in contrast to the MW, we find significant radial variations in beta, which increases from 1.9 at 10kpc to ~2.5 at a radius of 3.1kpc and then decreases to 1.7 in the center. The dust temperature is fairly constant in the 10kpc ring (ranging from 17-20K), but increases strongly in the bulge to ~30K. Within 3.1kpc we find the dust temperature is highly correlated with the 3.6 micron flux, suggesting the general stellar population in the bulge is the dominant source of dust heating there. At larger radii, there is a weak correlation between the star formation rate and dust temperature. We find no evidence for 'dark gas' in M31 in contrast to recent results for the MW. Finally, we obtained an estimate of the CO X-factor by minimising the dispersion in the gas-to-dust ratio, obtaining a value of (1.9+/-0.4)x10^20 cm^-2 [K kms^-1]^-1., Comment: 19 pages, 18 figures. Submitted to ApJ April 2012; Accepted July 2012
Published: 2012

46. Herschel-SPIRE Imaging Spectroscopy of Molecular Gas in M82

Author: Maximilien R. P. Schirm, Pasquale Panuzzo, Maarten Baes, Asantha Cooray, Alessandro Boselli, S. C. Madden, Ronin Wu, Naseem Rangwala, Christine D. Wilson, M. Bradford, George J. Bendo, P. R. Maloney, Julia Kamenetzky, L. Spinoglio, Kate Gudrun Isaak, Jason Glenn, Vianney Lebouteiller, Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], McMaster University [Hamilton, Ontario], Universiteit Gent = Ghent University (UGENT), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), California Institute of Technology (CALTECH), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Universiteit Gent = Ghent University [Belgium] (UGENT), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), and Universiteit Gent [Ghent]
Subjects: Physics, 010504 meteorology & atmospheric sciences, Absorption spectroscopy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Spectral line, Interstellar medium, chemistry.chemical_compound, chemistry, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Radiative transfer, Emission spectrum, Atomic carbon, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: We present new Herschel-SPIRE imaging spectroscopy (194-671 microns) of the bright starburst galaxy M82. Covering the CO ladder from J=4-3 to J=13-12, spectra were obtained at multiple positions for a fully sampled ~ 3 x 3 arcminute map, including a longer exposure at the central position. We present measurements of 12CO, 13CO, [CI], [NII], HCN, and HCO+ in emission, along with OH+, H2O+ and HF in absorption and H2O in both emission and absorption, with discussion. We use a radiative transfer code and Bayesian likelihood analysis to model the temperature, density, column density, and filling factor of multiple components of molecular gas traced by 12CO and 13CO, adding further evidence to the high-J lines tracing a much warmer (~ 500 K), less massive component than the low-J lines. The addition of 13CO (and [CI]) is new and indicates that [CI] may be tracing different gas than 12CO. No temperature/density gradients can be inferred from the map, indicating that the single-pointing spectrum is descriptive of the bulk properties of the galaxy. At such a high temperature, cooling is dominated by molecular hydrogen. Photon-dominated region (PDR) models require higher densities than those indicated by our Bayesian likelihood analysis in order to explain the high-J CO line ratios, though cosmic-ray enhanced PDR models can do a better job reproducing the emission at lower densities. Shocks and turbulent heating are likely required to explain the bright high-J emission., Accepted to The Astrophysical Journal. 17 pages + 20 pages of appendix figures
Published: 2012

47. The dust scaling relations of the Herschel Reference Survey

Author: Alessandro Boselli, Maarten Baes, Edvige Corbelli, David L. Clements, Luca Cortese, Stefano Zibetti, S. di Serego Alighieri, Catherine Vlahakis, Médéric Boquien, Jonathan Ivor Davies, Maud Galametz, Haley Louise Gomez, Daniele Pierini, Suzanne C. Madden, Laura Magrini, Stephen Anthony Eales, A. Cooray, Matthew Smith, Michael Pohlen, Leslie K. Hunt, Thomas M. Hughes, Simone Bianchi, L. Spinoglio, George J. Bendo, Laure Ciesla, Ciro Pappalardo, Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: HI SOURCE CATALOG, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, FAST ALPHA SURVEY, galaxies [submillimeter], FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, POLYCYCLIC AROMATIC-HYDROCARBONS, VIRGO CLUSTER GALAXIES, 0103 physical sciences, Cluster (physics), Astrophysics::Solar and Stellar Astrophysics, NEARBY GALAXIES, 010303 astronomy & astrophysics, Scaling, evolution [galaxies], Astrophysics::Galaxy Astrophysics, QB, Physics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], extinction, 010308 nuclear & particles physics, Galactic Center, Astronomy and Astrophysics, clusters: individual: Virgo [galaxies], BAND SURFACE PHOTOMETRY, Mass ratio, STAR-FORMATION HISTORY, Galaxy, GAS MASS-RATIO, Interstellar medium, Physics and Astronomy, Space and Planetary Science, Magnitude (astronomy), DIGITAL SKY SURVEY, LATE-TYPE GALAXIES, dust, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We combine new Herschel/SPIRE sub-millimeter observations with existing multiwavelength data to investigate the dust scaling relations of the Herschel Reference Survey, a magnitude-, volume-limited sample of ~300 nearby galaxies in different environments. We show that the dust-to-stellar mass ratio anti-correlates with stellar mass, stellar mass surface density and NUV-r colour across the whole range of parameters covered by our sample. Moreover, the dust-to-stellar mass ratio decreases significantly when moving from late- to early-type galaxies. These scaling relations are similar to those observed for the HI gas-fraction, supporting the idea that the cold dust is tightly coupled to the cold atomic gas component in the interstellar medium. We also find a weak increase of the dust-to-HI mass ratio with stellar mass and colour but no trend is seen with stellar mass surface density. By comparing galaxies in different environments we show that, although these scaling relations are followed by both cluster and field galaxies, HI-deficient systems have, at fixed stellar mass, stellar mass surface density and morphological type systematically lower dust-to-stellar mass and higher dust-to-HI mass ratios than HI-normal/field galaxies. This provides clear evidence that dust is removed from the star-forming disk of cluster galaxies but the effect of the environment is less strong than what is observed in the case of the HI disk. Such effects naturally arise if the dust disk is less extended than the HI and follows more closely the distribution of the molecular gas phase, i.e., if the dust-to-atomic gas ratio monotonically decreases with distance from the galactic center., Comment: 18 pages, 15 figures, 2 tables. Accepted for publication on A&A
Published: 2012

48. The Herschel view of the on-going star formation in the Vela-C molecular cloud

Author: D. Lorenzetti, D. Polychroni, Sylvain Bontemps, Milena Benedettini, Davide Elia, Kazi L.J. Rygl, Ph. André, G. J. White, Sergio Molinari, J. Di Francesco, Nicola Schneider, T. Hill, T. Giannini, Jason M. Kirk, Derek Ward-Thompson, Vincent Minier, Cassandra Fallscheer, L. Spinoglio, A. Di Giorgio, Stefano Pezzuto, M. R. Pestalozzi, Q. Nguyen Luong, E. Schisano, Frédérique Motte, Paolo Saraceno, Leonardo Testi, Martin Hennemann, foreign laboratories (FL), CERN [Genève], INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), European Southern Observatory (ESO), School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), Osservatorio di Astrofisica di Roma (OAR), Consiglio Nazionale delle Ricerche (CNR), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), and Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)
Subjects: individual objects, stars, FOS: Physical sciences, Astrophysics, clouds, Astrophysics::Cosmology and Extragalactic Astrophysics, Vela, 01 natural sciences, Power law, circumstellar matter, Virial theorem, 0103 physical sciences, Protostar, Astrophysics::Solar and Stellar Astrophysics, submillimeter, Vela-C, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, QB, Physics, Mass distribution, 010308 nuclear & particles physics, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Molecular cloud, formation, Astronomy and Astrophysics, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science
Abstract: As part of the Herschel guaranteed time key program 'HOBYS', we present the photometric survey of the star forming region Vela-C, one of the nearest sites of low-to-high-mass star formation in the Galactic plane. Vela-C has been observed with PACS and SPIRE in parallel mode between 70 um and 500 um over an area of about 3 square degrees. A photometric catalogue has been extracted from the detections in each band, using a threshold of 5 sigma over the local background. Out of this catalogue we have selected a robust sub-sample of 268 sources, of which 75% are cloud clumps and 25% are cores. Their Spectral Energy Distributions (SEDs) have been fitted with a modified black body function. We classify 48 sources as protostellar and 218 as starless. For two further sources, we do not provide a secure classification, but suggest they are Class 0 protostars. From SED fitting we have derived key physical parameters. Protostellar sources are in general warmer and more compact than starless sources. Both these evidences can be ascribed to the presence of an internal source(s) of moderate heating, which also causes a temperature gradient and hence a more peaked intensity distribution. Moreover, the reduced dimensions of protostellar sources may indicate that they will not fragment further. A virial analysis of the starless sources gives an upper limit of 90% for the sources gravitationally bound and therefore prestellar. We fit a power law N(logM) prop M^-1.1 to the linear portion of the mass distribution of prestellar sources. This is in between that typical of CO clumps and those of cores in nearby star-forming regions. We interpret this as a result of the inhomogeneity of our sample, which is composed of comparable fractions of clumps and cores., 9 pages, 7 figures, accepted by A&A
Published: 2012

49. The spine of the swan: A Herschel study of the DR21 ridge and filaments in Cygnus X

Author: Frédérique Motte, Martin Hennemann, Jin-Zeng Li, Kazi L.J. Rygl, T. Sousbie, F. Louvet, Sergio Molinari, Nicolas Peretto, Vincent Minier, Marc Sauvage, Nicola Schneider, Alexander Men'shchikov, Stefano Pezzuto, L. D. Anderson, Timea Csengeri, E. Schisano, Sylvain Bontemps, Glenn J. White, Ph. André, T. Hill, Peter G. Martin, Derek Ward-Thompson, Doris Arzoumanian, P. Didelon, J. Di Francesco, P. Palmeirim, Q. Nguyen Luong, A. P. Marston, Vera Könyves, J.-Ph. Bernard, D. Russeil, L. Spinoglio, Annie Zavagno, Davide Elia, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, FORMATION STELLAIRE 2012, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Groupe d'Etudes des Matériaux Hétérogènes (GEMH), Université de Limoges (UNILIM)-Institut des Procédés Appliqués aux Matériaux (IPAM), Université de Limoges (UNILIM)-Université de Limoges (UNILIM), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Herzberg Institute of Astrophysics, National Research Council of Canada (NRC), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), Laboratoire de Modélisation Multi-échelles des Combustibles (LM2C), Service d'Etudes de Simulation du Comportement du combustibles (SESC), Département d'Etudes des Combustibles (DEC), CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction de l'Energie Nucléaire (CEA-DEN), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Département d'Etudes des Combustibles (DEC), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Istituto di Fisica dello Spazio Interplanetario (IFSI), Consiglio Nazionale delle Ricerche (CNR), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), School of Physics and Astronomy [Cardiff], Cardiff University, Engineering Department, University of Cambridge [UK] (CAM), Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-CEA-Direction des Energies (ex-Direction de l'Energie Nucléaire) (CEA-DES (ex-DEN)), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)
Subjects: Physics, 010504 meteorology & atmospheric sciences, Molecular line, Star formation, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Inflow, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Stars, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Protostar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: In order to characterise the cloud structures responsible for the formation of high-mass stars, we present Herschel observations of the DR21 environment. Maps of the column density and dust temperature unveil the structure of the DR21 ridge and several connected filaments. The ridge has column densities larger than 1e23/cm^2 over a region of 2.3 pc^2. It shows substructured column density profiles and branching into two major filaments in the north. The masses in the studied filaments range between 130 and 1400 Msun whereas the mass in the ridge is 15000 Msun. The accretion of these filaments onto the DR21 ridge, suggested by a previous molecular line study, could provide a continuous mass inflow to the ridge. In contrast to the striations seen in e.g., the Taurus region, these filaments are gravitationally unstable and form cores and protostars. These cores formed in the filaments potentially fall into the ridge. Both inflow and collisions of cores could be important to drive the observed high-mass star formation. The evolutionary gradient of star formation running from DR21 in the south to the northern branching is traced by decreasing dust temperature. This evolution and the ridge structure can be explained by two main filamentary components of the ridge that merged first in the south., 8 pages, 5 figures, accepted for publication as a Letter in Astronomy and Astrophysics
Published: 2012

50. The Herschel Exploitation of Local Galaxy Andromeda (HELGA). I: Global far-infrared and sub-mm morphology

Author: A. Remy, M. J. Page, Stephen Anthony Eales, Jacopo Fritz, Walter Kieran Gear, I. De Looze, Haley Louise Gomez, B. O'Halloran, Alessandro Boselli, Karl D. Gordon, George J. Bendo, C. D. Wilson, Vianney Lebouteiller, Frédéric Galliano, Joris Verstappen, C. Waelkens, A. Cooray, Gianfranco Gentile, Mattia Vaccari, Joris Blommaert, S. C. Madden, Helene Roussel, David L. Clements, Luca Cortese, Maarten Baes, Matthew Smith, L. Spinoglio, David A. Thilker, Robert Braun, Médéric Boquien, G. P. Ford, Jason M. Kirk, J. Roman Duval, Laboratoire de Biophotonique et Pharmacologie - UMR 7213 (LBP), Centre National de la Recherche Scientifique (CNRS)-Réseau nanophotonique et optique, Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS), AUTRES, Technische Universität Dresden = Dresden University of Technology (TU Dresden), Universiteit Gent = Ghent University (UGENT), Sterrenkundig Observatorium, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), School of Physics and Astronomy [Cardiff], Cardiff University, Department of Chemistry and Biochemistry, University of California [Los Angeles] (UCLA), University of California (UC)-University of California (UC), aucun, Macif, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Department of Physics and Astronomy [Baltimore], Johns Hopkins University (JHU), Dipartimento di Astronomia [Padova], Università degli Studi di Padova = University of Padua (Unipd), Department of Physics and Astronomy [South Africa], University of the Western Cape (UWC), McMaster University [Hamilton, Ontario], Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Technische Universität Dresden (TUD), Universiteit Gent [Ghent], Universiteit Gent, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), School of Physics and Astronomy, University of California-University of California, Dipartimento di Astronomia, Universita degli Studi di Padova, Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Universiteit Gent = Ghent University [Belgium] (UGENT), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and University of the Western Cape
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, Metallicity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, SPIRE INSTRUMENT, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, CONVERSION FACTOR, EXTENDED SURVEY HERM33ES, 01 natural sciences, STAR-FORMATION, Far infrared, 0103 physical sciences, 010303 astronomy & astrophysics, individual: M31 [galaxies], Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, QB, Physics, Spiral galaxy, ISM [galaxies], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Star formation, MESSIER 31, M31, ISM [infrared], Astronomy and Astrophysics, Galaxy, ATOMIC GAS, Andromeda, BACKGROUND EXPERIMENT, Physics and Astronomy, Space and Planetary Science, Cirrus, LARGE-MAGELLANIC-CLOUD, Astrophysics::Earth and Planetary Astrophysics, INTERSTELLAR DUST, Data reduction, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We have obtained Herschel images at five wavelengths from 100 to 500 micron of a ~5.5x2.5 degree area centred on the local galaxy M31 (Andromeda), our nearest neighbour spiral galaxy, as part of the Herschel guaranteed time project "HELGA". The main goals of HELGA are to study the characteristics of the extended dust emission, focusing on larger scales than studied in previous observations of Andromeda at an increased spatial resolution, and the obscured star formation. In this paper we present data reduction and Herschel maps, and provide a description of the far-infrared morphology, comparing it with features seen at other wavelengths. We use high--resolution maps of the atomic hydrogen, fully covering our fields, to identify dust emission features that can be associated to M31 with confidence, distinguishing them from emission coming from the foreground Galactic cirrus. Thanks to the very large extension of our maps we detect, for the first time at far-infrared wavelengths, three arc-like structures extending out to ~21, ~26 and ~31 kpc respectively, in the south-western part of M31. The presence of these features, hosting ~2.2e6 Msol of dust, is safely confirmed by their detection in HI maps. Overall, we estimate a total dust mass of ~5.8e7 Msol, about 78% of which is contained in the two main ring-like structures at 10 and 15 kpc, at an average temperature of 16.5 K. We find that the gas-to-dust ratio declines exponentially as a function of the galacto-centric distance, in agreement with the known metallicity gradient, with values ranging from 66 in the nucleus to ~275 in the outermost region. [Abridged], Comment: 15 Pages, 9 Figures. Accepted for publication in Astronomy and Astrophysics. A high resolution version of the paper can be found at http://wazn.ugent.be/jfritz/HelgaI_final.pdf
Published: 2011
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