Search

Your search keyword '"A. Poglitsch A."' showing total 81 results
Start Over Author "A. Poglitsch A." Publisher edp sciences
81 results on '"A. Poglitsch A."'

1. Star formation and the ISM in infrared bright galaxies - SHINING

Author

Amiel Sternberg, L. Vigroux, Aprajita Verma, Oliver Krause, Albrecht Poglitsch, A. Contursi, Diane Cormier, S. Hailey-Dunsheath, S. C. Madden, M. Haas, Ulrich Klaas, Juergen Schreiber, J. de Jong, Eckhard Sturm, Javier Graciá-Carpio, Eduardo González-Alfonso, Linda J. Tacconi, Dieter Lutz, Markus Nielbock, Reinhard Genzel, and J. Fischer

Subjects
Physics, Active infrared, Infrared, Star formation, Astrophysics::High Energy Astrophysical Phenomena, Metallicity, Spatially resolved, General Engineering, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation)
Abstract

The Herschel Key Project SHINING performs a study of the ISM in star forming and active infrared bright galaxies (starbursts, AGN, (U)LIRGs, interacting and low metallicity galaxies) at local and intermediate redshifts. Here we present some surprising and promising first results from parts of this programme, including spatially resolved PDR diagnostics, line deficit diagnostics, and large scale molecular outflows traced by the OH molecule.

Published
2011
Full Text
View/download PDF

2. The PACS Instrument

Author

B. Altieri and Albrecht Poglitsch

Subjects
Physics, Spectrometer, business.industry, Bolometer, General Engineering, Photodetector, Astronomy and Astrophysics, Field of view, law.invention, Telescope, Photometry (astronomy), Optics, Sampling (signal processing), Space and Planetary Science, law, Spectral resolution, business
Abstract

The Photodetector Array Camera and Spectrometer on Herschel provides imaging line spectroscopy and imaging photometry in the 55–210 μm wavelength band. In photometry mode, two filled silicon bolometer arrays with 16×32 and 32×64 pixels, respectively, are used to simultaneously image two bands, 60–85 μm or 85–130 μm and 130–210 μm, over a field of view of ~1.75'×3.5', with Nyquist beam sampling in each band. In spectroscopy mode, two Ge:Ga photoconductor arrays (stressed and unstressed) with 16×25 pixels, each, are used to image a field of ~50''×50'', resolved into 5×5 pixels, with a spectral resolution of ~175 km s-1 and an instantaneous spectral coverage of ~1500 km s-1. In both modes the performance is expected to be not far from background-noise limited, with sensitivities (5σ in 1 h) of ~4 mJy or 3–20×10-18 W/m2, respectively. We summarise the design of the instrument and its subunits, describe the observing modes in combination with the telescope pointing modes, report results from instrument level performance tests of the Flight Model, and present our current prediction of the in-orbit performance of the instrument.

Published
2008
Full Text
View/download PDF

3. Herschel and Beyond: FIR and Submillimetre Space Missions and Possible Synergies with Antarctic Astronomy

Author

Göran Pilbratt, Albrecht Poglitsch, Matthew Joseph Griffin, and T. de Graauw

Subjects
Physics, Photometry (astronomy), Far infrared, Space and Planetary Science, Payload, General Engineering, Astronomy, Astronomy and Astrophysics, Space astronomy, Space exploration, Space observatory
Abstract

The Herschel Space Observatory is the fourth cornerstone mission in the European Space Agency (ESA) science programme, and is scheduled for launch in late 2008. It will perform imaging photometry and spectroscopy at far infrared and submillimetre wavelengths, covering approximately the 60–670 m range. The three payload instruments are briefly described, and examples of their scientific capabilities are given from the Guaranteed Time Key Projects which have already been approved. Prospects for future far infrared/submillimetre space astronomy are briefly reviewed, and the implications for possible Antarctic facilities operating in this spectral region are discussed.

Published
2008
Full Text
View/download PDF

4. Interstellar medium conditions inz~ 0.2 Lyman-break analogs

Author

Contursi, A., primary, Baker, A. J., additional, Berta, S., additional, Magnelli, B., additional, Lutz, D., additional, Fischer, J., additional, Verma, A., additional, Nielbock, M., additional, Grácia Carpio, J., additional, Veilleux, S., additional, Sturm, E., additional, Davies, R., additional, Genzel, R., additional, Hailey-Dunsheath, S., additional, Herrera-Camus, R., additional, Janssen, A., additional, Poglitsch, A., additional, Sternberg, A., additional, and Tacconi, L. J., additional

Published
2017
Full Text
View/download PDF

5. The Trumpler 14 photodissociation region in the Carina Nebula

Author

Kate Brooks, N. Geis, Albrecht Poglitsch, John W. V. Storey, Nicola Schneider, Pierre Cox, and Leonardo Bronfman

Subjects
Physics, Stars, Nebula, Space and Planetary Science, Molecular cloud, Kuiper Airborne Observatory, Velocity dispersion, Astronomy, Astronomy and Astrophysics, Astrophysics, Photodissociation region, Dust lane, O-type star
Abstract

We report the results of observations of the fine-structure emission lines (C ) 158 µ ma nd (O )6 3µm using FIFI on the Kuiper Airborne Observatory (KAO) and the Long Wavelength Spectrometer (LWS) on board ISO, towards the molecular cloud associated with the stellar cluster Trumpler 14 (Tr 14) in the Carina Nebula. These data are compared with selected CO and CS transitions obtained with the SEST as well as IRAS and MSX images to produce a detailed view of the morphology and the physical conditions prevailing in the photodissociation region (PDR) at the interface between the ionized gas and the molecular dust lane. The relative intensity distribution observed for the various tracers is consistent with the stratification expected for a molecular cloud seen edge-on and exposed to a radiation field of ≈10 4 G0, which is dominated by the most massive stars of Tr 14. The grain photoelectric heating efficiency, � , is estimated to be ≈5 × 10 −3 and is comparable to other galactic PDRs. The molecular gas has a complicated velocity structure with a high velocity dispersion resulting from the impact of the stellar winds arising from Tr 14. There is evidence of small-scale clumping with a very low volume filling factor. Despite the rich concentration of massive O stars in Tr 14 we find that the parameters of the PDR are much less-extreme than those of the Orion and M 17 massive star-forming regions.

Published
2003
Full Text
View/download PDF

6. Excited OH^+, H_2O^+, and H_3O^+ in NGC 4418 and Arp 220

Author

González-Alfonso, E., Fischer, J., Bruderer, S., Müller, H. S. P., Graciá-Carpio, J., Sturm, E., Lutz, D., Poglitsch, A., Feuchtgruber, H., Veilleux, S., Contursi, A., Sternberg, A., Hailey-Dunsheath, S., Verma, A., Christopher, N., Davies, R., Genzel, R., and Tacconi, L.

Abstract

We report on Herschel/PACS observations of absorption lines of OH^+, H_2O^+ and H_3O^+ in NGC 4418 and Arp 220. Excited lines of OH^+ and H_2O^+ with E_(lower) of at least 285 and ~200 K, respectively, are detected in both sources, indicating radiative pumping and location in the high radiation density environment of the nuclear regions. Abundance ratios OH^+/H_2O^+ of 1−2.5 are estimated in the nuclei of both sources. The inferred OH^+ column and abundance relative to H nuclei are (0.5−1) × 10^(16) cm^(-2) and ~ 2 × 10^(-8), respectively. Additionally, in Arp 220, an extended low excitation component around the nuclear region is found to have OH^+/H^2O^+ ~ 5−10. H_3O^+ is detected in both sources with N(H_3O^+) ~ (0.5−2) × 10^(16) cm^(-2), and in Arp 220 the pure inversion, metastable lines indicate a high rotational temperature of ~500 K, indicative of formation pumping and/or hot gas. Simple chemical models favor an ionization sequence dominated by H^+ → O^+ → OH^+ → H_2O^+ → H_3O^+, and we also argue that the H^+ production is most likely dominated by X-ray/cosmic ray ionization. The full set of observations and models leads us to propose that the molecular ions arise in a relatively low density (≳10^4 cm^(-3)) interclump medium, in which case the ionization rate per H nucleus (including secondary ionizations) is ζ > 10^(-13) s^(-1), a lower limit that is several × 10^2 times the highest current rate estimates for Galactic regions. In Arp 220, our lower limit for ζ is compatible with estimates for the cosmic ray energy density inferred previously from the supernova rate and synchrotron radio emission, and also with the expected ionization rate produced by X-rays. In NGC 4418, we argue that X-ray ionization due to an active galactic nucleus is responsible for the molecular ion production.

Published
2013

7. The role of massive halos in the star formation history of the Universe

Author

Popesso, P., primary, Biviano, A., additional, Finoguenov, A., additional, Wilman, D., additional, Salvato, M., additional, Magnelli, B., additional, Gruppioni, C., additional, Pozzi, F., additional, Rodighiero, G., additional, Ziparo, F., additional, Berta, S., additional, Elbaz, D., additional, Dickinson, M., additional, Lutz, D., additional, Altieri, B., additional, Aussel, H., additional, Cimatti, A., additional, Fadda, D., additional, Ilbert, O., additional, Le Floch, E., additional, Nordon, R., additional, Poglitsch, A., additional, Genel, S., additional, and Xu, C. K., additional

Published
2015
Full Text
View/download PDF

8. The evolution of galaxy star formation activity in massive haloes

Author

Popesso, P., primary, Biviano, A., additional, Finoguenov, A., additional, Wilman, D., additional, Salvato, M., additional, Magnelli, B., additional, Gruppioni, C., additional, Pozzi, F., additional, Rodighiero, G., additional, Ziparo, F., additional, Berta, S., additional, Elbaz, D., additional, Dickinson, M., additional, Lutz, D., additional, Altieri, B., additional, Aussel, H., additional, Cimatti, A., additional, Fadda, D., additional, Ilbert, O., additional, Le Floch, E., additional, Nordon, R., additional, Poglitsch, A., additional, and Xu, C. K., additional

Published
2015
Full Text
View/download PDF

9. Herschel unveils a puzzling uniformity of distant dusty galaxies [Letter]

Author

Elbaz, D., Hwang, H. S., Magnelli, B., Daddi, E., Aussel, H., Altieri, B., Amblard, A., Andreani, P., Arumugam, V., Auld, Robbie Richard, Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodriguez, N., Cava, A., Cepa, J., Chanial, P., Chary, R.-R., Cimatti, A., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Dickinson, M., Dominguez, H., Dowell, C. D., Dunlop, J. S., Dwek, E., Eales, Stephen Anthony, Farrah, D., Förster Schreiber, N., Fox, M., Franceschini, A., Gear, Walter Kieran, Genzel, R., Glenn, J., Griffin, Matthew Joseph, Gruppioni, C., Halpern, M., Hatziminaoglou, E., Ibar, E., Isaak, Kate Gudrun, Ivison, R. J., Lagache, G., Le Borgne, D., Le Floc'h, E., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Maiolino, R., Marchetti, L., Mortier, A. M. J., Nguyen, H. T., Nordon, R., O'Halloran, B., Okumura, K., Oliver, S. J., Omont, A., Page, M. J., Panuzzo, P., Papageorgiou, Andreas, Pearson, C. P., Perez Fournon, I., Pérez García, A. M., Poglitsch, A., Pohlen, Michael, Popesso, P., Pozzi, F., Rawlings, J. I., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Saintonge, A., Sanchez Portal, M., Santini, P., Sauvage, M., Schulz, B., Scott, D., Seymour, N., Shao, L., Shupe, D. L., Smith, A. J., Stevens, J. A., Sturm, E., Symeonidis, M., Tacconi, L., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, QB
Abstract

The Herschel Space Observatory enables us to accurately measure the bolometric output of starburst galaxies and active galactic nuclei (AGN) by directly sampling the peak of their far-infrared (IR) emission. Here we examine whether the spectral energy distribution (SED) and dust temperature of galaxies have strongly evolved over the last 80% of the age of the Universe. We discuss possible consequences for the determination of star-formation rates (SFR) and any evidence for a major change in their star-formation properties. We use Herschel deep extragalactic surveys from 100 to 500 μm to compute total IR luminosities in galaxies down to the faintest levels, using PACS and SPIRE in the GOODS-North field (PEP and HerMES key programs). An extension to fainter luminosities is done by stacking images on 24 μm prior positions. We show that measurements in the SPIRE bands can be used below the statistical confusion limit if information at higher spatial resolution is used, e.g. at 24 μm, to identify “isolated” galaxies whose flux is not boosted by bright neighbors. Below z ~ 1.5, mid-IR extrapolations are correct for star-forming galaxies with a dispersion of only 40% (0.15 dex), therefore similar to z ~ 0 galaxies, over three decades in luminosity below the regime of ultra-luminous IR galaxies (ULIRGs, LIR ≥ 1012 ). This narrow distribution is puzzling when considering the range of physical processes that could have affected the SED of these galaxies. Extrapolations from only one of the 160 μm, 250 μm or 350 μm bands alone tend to overestimate the total IR luminosity. This may be explained by the lack of far-IR constraints around and above ~150 μm (rest-frame) before Herschel on those templates. We also note that the dust temperature of luminous IR galaxies (LIRGs, LIR ≥ 1011 ) around z ~ 1 is mildly colder by 10–15% than their local analogs and up to 20% for ULIRGs at z ~ 1.6 (using a single modified blackbody-fit to the peak far-IR emission with an emissivity index of β = 1.5). Above z = 1.5, distant galaxies are found to exhibit a substantially larger mid- over far-IR ratio, which could either result from stronger broad emission lines or warm dust continuum heated by a hidden AGN. Two thirds of the AGNs identified in the field with a measured redshift exhibit the same behavior as purely star-forming galaxies. Hence a large fraction of AGNs harbor coeval star formation at very high SFR and in conditions similar to purely star-forming galaxies.

Published
2010

10. The far-infrared/radio correlation as probed by Herschel [Letter]

Author

Ivison, R. J., Magnelli, B., Ibar, E., Andreani, P., Elbaz, D., Altieri, B., Amblard, A., Arumugam, V., Auld, Robbie Richard, Aussel, H., Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Cepa, J., Chanial, P., Cimatti, A., Cirasuolo, M., Clements, D. L., Conley, A., Conversi, L., Cooray, A., Daddi, E., Dominguez, H., Dowell, C. D., Dwek, E., Eales, Stephen Anthony, Farrah, D., Förster Schreiber, N., Fox, M., Franceschini, A., Gear, Walter Kieran, Genzel, R., Glenn, J., Griffin, Matthew Joseph, Gruppioni, C., Halpern, M., Hatziminaoglou, E., Isaak, Kate Gudrun, Lagache, G., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Maiolino, R., Marchetti, L., Morrison, G. E., Mortier, A. M. J., Nguyen, H. T., Nordon, R., O'Halloran, B., Oliver, S. J., Omont, A., Owen, F. N., Page, M. J., Panuzzo, P., Papageorgiou, Andreas, Pearson, C. P., Pérez-Fournon, I., Pérez García, A. M., Poglitsch, A., Pohlen, Michael, Popesso, P., Pozzi, F., Rawlings, J. I., Raymond, Gwenifer, Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I. G., Rowan-Robinson, M., Saintonge, A., Sanchez Portal, M., Santini, P., Schulz, B., Scott, D., Seymour, N., Shao, L., Shupe, D. L., Smith, A. J., Stevens, J. A., Sturm, E., Symeonidis, M., Tacconi, L., Trichas, M., Tugwell, K. E., Vaccari, M., Valtchanov, I., Vieira, J., Vigroux, L., Wang, L., Ward, R., Wright, G., Xu, C. K., and Zemcov, M.

Subjects
QB
Abstract

We set out to determine the ratio, qIR, of rest-frame 8–1000-μm flux, SIR, to monochromatic radio flux, S1.4 GHz, for galaxies selected at far-infrared (IR) and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, Td, and to identify any far-IR-bright outliers – useful laboratories for exploring why the far-IR/radio correlation (FIRRC) is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-μm and 1.4-GHz samples, obtained using Herschel and the Very Large Array (VLA) in GOODS-North (-N). We determine bolometric IR output using ten bands spanning λobs = 24–1250 μm, exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an LIR-matched sample, designed to reveal evolution of qIR with redshift, spanning log LIR = 11–12 and z = 0–2, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies in GOODS-N, we see tentative evidence of a break in the flux ratio, qIR, at L1.4 GHz ~ 1022.7 W Hz-1, where active galactic nuclei (AGN) are starting to dominate the radio power density, and of weaker correlations with redshift and Td. From our 250-μm-selected sample we identify a small number of far-IR-bright outliers, and see trends of qIR with L1.4 GHz, LIR, Td and redshift, noting that some of these are inter-related. For our LIR-matched sample, there is no evidence that qIR changes significantly as we move back into the epoch of galaxy formation: we find qIR (1+z)γ, where γ = -0.04±0.03 at z = 0–2; however, discounting the least reliable data at z < 0.5 we find γ = -0.26±0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by 1.

Published
2010

11. Development of a Large Scale Stressed Ge:Ga Detector Array for SAFARI

Author

Walfried Raab, L. Barl, Rainer Höhnle, and Albrecht Poglitsch

Subjects
Physics, Pixel, business.industry, Detector, Field of view, Spica, Large format, Multiplexer, Noise (electronics), Particle detector, Optics, Optoelectronics, business, Electronic circuit
Abstract

We report on the development of a large format stressed gallium doped germanium (Ge:Ge) array for the SAFARI instrument. Building on flight proven PACS heritage, the goal of our development is a 32 pixel stressed Ge:Ga module enabling a 32 × 32 pixel photoconductor array for the wavelength range between 110 and 210 μm. The unprecedented size of this array would allow the use of almost all of the 3.8 × 3.8 arcmin field of view provided for SAFARI in the SPICA focal plane. We are currently in the process of manufacturing the individual components of the 32 pixel demonstration module. This prototype module will feature three selectable read out architectures enabling the evaluation and optimisation of the detector performance as well as a two stage multiplexer to distribute the dissipative heat load on the temperature levels provided by the satellite. Thermal modeling has shown that the heat loads are in compliance with the thermal budgets of the SPICA cryogenic system. The ultimate development goal with optimised read out circuits is an NEP of 1 × 10-18 W/Hz1/2 , which would present a factor of 8 improvement in the noise performance compared to the PACS stressed Ge:Ga array.

Published
2009
Full Text
View/download PDF

12. Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

Author

S. Berta, A. M. Pérez García, Franz E. Bauer, Giulia Rodighiero, Miguel Sánchez-Portal, Lijing Shao, Andrea Cimatti, Andrea Grazian, N. M. Förster Schreiber, Reinhard Genzel, Dieter Lutz, Albrecht Poglitsch, Emanuele Daddi, Roberto Maiolino, E. Sturm, Benjamin Magnelli, Mara Salvato, David M. Alexander, Bruno Altieri, David J. Rosario, L. Riguccini, Paola Popesso, Marcella Brusa, Francesca Pozzi, Raanan Nordon, P. Santini, V. Mainieri, David Elbaz, J. Cepa, Paola Andreani, Linda J. Tacconi, Adriano Fontana, W. N. Brandt, Herve Aussel, Ivan Valtchanov, E. Le Floc'h, Stijn Wuyts, Ángel Bongiovanni, Santini P., Rosario, D. J., Shao L., Lutz D., Maiolino R., Alexander D. M., Altieri B., Andreani P., Aussel H., Bauer F. E., Berta S., Bongiovanni A., Brandt W. N., Brusa M., Cepa J., Cimatti A., Daddi E., Elbaz D., Fontana A., Förster Schreiber N. M., Genzel R., Grazian A., Le Floc'h E., Magnelli B., Mainieri V., Nordon R., Pérez Garcia A. M., Poglitsch A., Popesso P., Pozzi F., Riguccini L., Rodighiero G., Salvato M., Sanchez-Portal M., Sturm E., Tacconi L. J., Valtchanov I., and Wuyts S.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, infrared: galaxies, galaxies: high-redshift, Space and Planetary Science, galaxies: star formation, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We compare the average star formation (SF) activity in X-ray selected AGN hosts with mass-matched control inactive galaxies,including star forming and quiescent sources, at 0.510sigma) for bright AGNs. However, when comparing to star forming galaxies only, AGN hosts are broadly consistent with the locus of their `main sequence'. We investigate the relative far-IR luminosity distributions of active and inactive galaxies, and find a higher fraction of PACS detected, hence normal and highly star forming systems among AGN hosts. Although different interpretations are possible, we explain our findings as a consequence of a twofold AGN growth path: faint AGNs evolve through secular processes, with instantaneous AGN accretion not tightly linked to the current total SF in the host, while luminous AGNs co-evolve with their hosts through periods of enhanced AGN activity and SF, possibly through major mergers. While an increased SF with respect to non-AGNs of similar mass is expected in the latter, we interpret the modest SF offsets measured in low-Lx AGN hosts as either a) generated by non-synchronous accretion and SF histories in a merger scenario or b) due to possible connections between instantaneous SF and accretion that can be induced by smaller scale (non-major merger) mechanisms. Far-IR luminosity distributions favour the latter scenario., Comment: Final version

Published
2012
Full Text
View/download PDF

13. The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Author

Andrea Biviano, David Elbaz, Giulia Rodighiero, Antonio Cava, Kim-Vy Tran, Carlotta Gruppioni, Dario Fadda, Paola Popesso, Dieter Lutz, Ivan Valtchanov, Kalliopi Dasyra, Helmut Dannerbauer, Francesca Pozzi, S. Berta, Lijing Shao, Alexis Finoguenov, E. Le Floc'h, Jeyhan S. Kartaltepe, D. Coia, Amélie Saintonge, Ho Seong Hwang, Shannon G. Patel, L. Riguccini, Raanan Nordon, N. M. Förster Schreiber, Ivano Baronchelli, Albrecht Poglitsch, Paola Andreani, Reinhard Genzel, Benjamin Magnelli, O. Ilbert, Linda J. Tacconi, Roger Leiton, Bruno Altieri, Andrea Cimatti, Mara Salvato, E. Daddi, Herve Aussel, M. Sanchez Portal, Mark Dickinson, Adam Tomczak, Georgios E. Magdis, Peter Capak, Popesso P., Biviano A., Rodighiero G., Baronchelli I., Salvato M., Saintonge A., Finoguenov A., Magnelli B., Gruppioni C., Pozzi F., Lutz D., Elbaz D., Altieri B., Andreani P., Aussel H., Berta S., Capak P., Cava A., Cimatti A., Coia D., Daddi E., Dannerbauer H., Dickinson M., Dasyra K., Fadda D., Förster Schreiber N., Genzel R., Hwang H. S., Kartaltepe J., Ilbert O., Le Floch E., Leiton R., Magdis, G., Nordon R., Patel S., Poglitsch A., Riguccini L., Sanchez Portal M., Shao L., Tacconi L., Tomczak A., Tran K., and Valtchanov I.

Subjects
Physics, Luminous infrared galaxy, education.field_of_study, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Population, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Redshift, Galaxy, galaxies: clusters: general, galaxies: high-redshift, Space and Planetary Science, Galaxy group, galaxies: evolution, education, Low Mass, Astrophysics::Galaxy Astrophysics, Galaxy cluster, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (\Sigma(SFR/M)) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift ~1.6. We use deep far-infrared PACS data at 100 and 160 um to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ~10^{15} M_{\odot}, and 9 groups/poor clusters with mass ~ 5 x 10^{13} M_{\odot}. Estimates of the field \Sigma(SFR/M) are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe. The field \Sigma(SFR/M) increases with redshift up to z~1 and it is constant thereafter. The evolution of the \Sigma(SFR/M)-z relation in galaxy systems is much faster than in the field. Up to redshift z~0.2, the field has a higher \Sigma(SFR/M) than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar \Sigma(SFR/M), while massive clusters have significantly lower \Sigma(SFR/M) than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z~1.6, where the group \Sigma(SFR/M) lies above the field \Sigma(SFR/M)-z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching., Comment: 8 pages, 3 figures, accepted for publication on A&A

Published
2012
Full Text
View/download PDF

14. Building the cosmic infrared background brick by brick withHerschel/PEP

Author

Bruno Altieri, Albrecht Poglitsch, Stijn Wuyts, Linda J. Tacconi, Ivan Valtchanov, Raanan Nordon, Miguel Sánchez-Portal, Paola Andreani, N. M. Foerster Schreiber, J. Cepa, Reinhard Genzel, E. Le Floc'h, Giulia Rodighiero, E. Sturm, Benjamin Magnelli, Herve Aussel, Francesca Pozzi, Ismael Perez-Fournon, Andrea Cimatti, S. Berta, Héctor O. Castañeda, Paola Popesso, David Elbaz, L. Riguccini, Dieter Lutz, Emanuele Daddi, Roberto Maiolino, Berta S., Magnelli B., Nordon R., Lutz D., Wuyts S., Altieri B., Andreani P., Aussel H., Castañeda H., Cepa J., Cimatti A., Daddi E., Elbaz D., Förster Schreiber N. M., Genzel R., Le Floc'h E., Maiolino R., Pérez-Fournon I., Poglitsch A., Popesso P., Pozzi F., Riguccini L., Rodighiero G., Sanchez-Portal M., Sturm E., Tacconi L. J., and Valtchanov I.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Infrared, infrared: galaxie, FOS: Physical sciences, Flux, Astronomy and Astrophysics, cosmic background radiation, Astrophysics, infrared: diffuse background, Galaxy, Redshift, Wavelength, Space and Planetary Science, Cosmic infrared background, galaxies: statistic, Surface brightness, galaxies: evolution, Order of magnitude, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The cosmic infrared background (CIB) includes roughly half of the energy radiated by all galaxies at all wavelengths across cosmic time, as observed at the present epoch. The PACS Evolutionary Probe (PEP) survey is exploited here to study the CIB and its redshift differential, at 70, 100 and 160 micron, where the background peaks. Combining PACS observations of the GOODS-S, GOODS-N, Lockman Hole and COSMOS areas, we define number counts spanning over more than two orders of magnitude in flux: from ~1 mJy to few hundreds mJy. Stacking of 24 micron sources and P(D) statistics extend the analysis down to ~0.2 mJy. Taking advantage of the wealth of ancillary data in PEP fields, differential number counts and CIB are studied up to z=5. Based on these counts, we discuss the effects of confusion on PACS blank field observations and provide confusion limits for the three bands considered. The total CIB surface brightness emitted above PEP 3 sigma flux limits is 4.52 +/- 1.18, 8.35 +/- 0.95 and 9.49 +/- 0.59 [nW/m2/sr] at 70, 100, and 160 micron, respectively. These values correspond to 58 +/- 7% and 74 +/- 5% of the COBE/DIRBE CIB direct measurements at 100 and 160 micron. Employing the P(D) analysis, these fractions increase to ~65% and ~89%. More than half of the resolved CIB was emitted at redshift z1.0 sources reaches 50% at 160 micron. Most of the CIB resolved in the three PACS bands was emitted by galaxies with infrared luminosities in the range 1e11-1e12 L(sun)., Proposed for acceptance on A&A

Published
2011
Full Text
View/download PDF

15. The star-formation rates of 1.5 < z < 2.5 massive galaxies

Author

N. M. Förster Schreiber, S. Berta, H. Dominguez, L. Riguccini, Giulia Rodighiero, Eckhard Sturm, Roberto Maiolino, Georgios E. Magdis, Lijing Shao, D. Elbaz, Benjamin Magnelli, Andrea Cimatti, E. Daddi, Raanan Nordon, Herve Aussel, P. Santini, Paola Andreani, Dieter Lutz, Andrea Grazian, A. M. Pérez García, Amélie Saintonge, Ángel Bongiovanni, I. Valtchanov, Ekkehard Wieprecht, P. Popesso, Linda J. Tacconi, Francesca Pozzi, J. Cepa, M. Wetzstein, M. Sánchez-Portal, Reinhard Genzel, Albrecht Poglitsch, Antonio Cava, Bruno Altieri, R. Nordon, D. Lutz, L. Shao, B. Magnelli, S. Berta, B. Altieri, P. Andreani, H. Aussel, A. Bongiovanni, A. Cava, J. Cepa, A. Cimatti, E. Daddi, H. Dominguez, D. Elbaz, N. M. Förster Schreiber, R. Genzel, A.Grazian, G. Magdi, R. Maiolino R., A. M. Pérez García, A. Poglitsch A., P. Popesso, F. Pozzi, L. Riguccini, and G. Rodighiero

Subjects
Physics, Luminous infrared galaxy, cosmology: observation, Star formation, Extinction (astronomy), Theoretical models, galaxies: starburst, Astronomy and Astrophysics, Astrophysics, Galaxy, Redshift, infrared: galaxies, Space and Planetary Science, Galaxy formation and evolution, galaxies: evolution, galaxies: fundamental parameter
Abstract

The star formation rate (SFR) is a key parameter in the study of galaxy evolution. The accuracy of SFR measurements at z ∼ 2 has been questioned following a disagreement between observations and theoretical models. The latter predict SFRs at this redshift that are typically a factor 4 or more lower than the measurements. We present star-formation rates based on calorimetric measurements of the far-infrared (FIR) luminosities for massive 1.5 < z < 2.5, normal star-forming galaxies (SFGs), which do not depend on extinction corrections and/or extrapolations of spectral energy distributions. The measurements are based on observations in GOODS-N with the Photodetector Array Camera and Spectrometer (PACS) onboard Herschel, as part of the PACS evolutionary probe (PEP) project, that resolve for the first time individual SFGs at these redshifts at FIR wavelengths. We compare FIR-based SFRs to the more commonly used 24 μm and UV SFRs. We find that SFRs from 24 μm alone are higher by a factor of ∼4-7.5 than the true SFRs. This overestimation depends on luminosity: gradually increasing for log L(24 μm) > 12.2 L ⊙. The SFGs and AGNs tend to exhibit the same 24 μm excess. The UV SFRs are in closer agreement with the FIR-based SFRs. Using a Calzetti UV extinction correction results in a mean excess of up to 0.3 dex and a scatter of 0.35 dex from the FIR SFRs. The previous UV SFRs are thus confirmed and the mean excess, while narrowing the gap, is insufficient to explain the discrepancy between the observed SFRs and simulation predictions. © 2010 ESO.

Published
2010
Full Text
View/download PDF

16. Star formation in AGN hosts in GOODS-N

Author

Bruno Altieri, Emmanouel Rovilos, Marcella Brusa, V. Mainieri, Franz E. Bauer, Reinhard Genzel, Giulia Rodighiero, Andrea Grazian, N. M. Förster Schreiber, Albrecht Poglitsch, Francesca Pozzi, Paola Santini, Amélie Saintonge, David M. Alexander, Carlotta Gruppioni, Dieter Lutz, M. Wetzstein, L. Riguccini, E. Sturm, W. N. Brandt, Emanuele Daddi, Lijing Shao, Benjamin Magnelli, Roberto Maiolino, Ángel Bongiovanni, H. Dominguez-Sanchez, Linda J. Tacconi, Georgios E. Magdis, Mara Salvato, Ivan Valtchanov, S. Berta, Raanan Nordon, A. M. Pérez García, J. Cepa, Norbert Geis, Andrea Cimatti, Paola Popesso, Antonio Cava, E. Wieprecht, Herve Aussel, M. Sanchez Portal, David Elbaz, Paola Andreani, Shao L., Lutz D., Nordon R., Maiolino R., Alexander D. M., Altieri B., Andreani P., Aussel H., Bauer F. E., Berta S., Bongiovanni A., Brandt W. N., Brusa M., Cava A., Cepa J., Cimatti A., Daddi E., Dominguez-Sanchez H., Elbaz D., Förster Schreiber N. M., Geis N., Genzel R., Grazian A., Gruppioni C., Magdis G., Magnelli B., Mainieri V., Pérez García A. M., Poglitsch A., Popesso P., Pozzi F., Riguccini L., Rodighiero G., Rovilos E., Saintonge A., Salvato M., Sanchez Portal M., Santini P., Sturm E., Tacconi L. J., Valtchanov I., Wetzstein M., and Wieprecht E.

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star formation, Astrophysics::High Energy Astrophysical Phenomena, Conjunction (astronomy), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Galaxy, Redshift, Luminosity, Space and Planetary Science, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Sensitive Herschel far-infrared observations can break degeneracies that were inherent to previous studies of star formation in high-z AGN hosts. Combining PACS 100 and 160um observations of the GOODS-N field with 2Msec Chandra data, we detect ~20% of X-ray AGN individually at >3sig. The host far-infrared luminosity of AGN with L2-10~10^43erg/s increases with redshift by an order of magnitude from z=0 to z~1. In contrast, there is little dependence of far-infrared luminosity on AGN luminosity, for L2-10~1. We do not find a dependence of far-infrared luminosity on X-ray obscuring column, for our sample which is dominated by L2-10, Comment: Accepted for publication in A&A Herschel issue. 4 pages, 6 figures

Published
2010
Full Text
View/download PDF

17. The far-infrared/radio correlation as probed by Herschel

Author

Ivison, R., Magnelli, B., Ibar, E., Andreani, P., Elbaz, D., Altieri, B., Amblard, A., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Cepa, J., Chanial, P., Cimatti, A., Cirasuolo, M., Clements, D., Conley, A., Conversi, L., Cooray, A., Daddi, E., Dominguez, H., Dowell, C., Dwek, E., Eales, S., Farrah, D., FörsterSchreiber, N., Fox, M., Franceschini, A., Gear, W., Genzel, R., Glenn, J., Griffin, M., Gruppioni, C., Halpern, M., Hatziminaoglou, E., Isaak, K., Lagache, G., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Maiolino, R., Marchetti, L., Morrison, G., Mortier, A., Nguyen, H., Nordon, R., O'Halloran, B., Oliver, S., Omont, A., Owen, F., Page, M., Panuzzo, P., Papageorgiou, A., Pearson, C., Pérez-Fournon, I., García, A., Poglitsch, A., Pohlen, M., Popesso, P., Pozzi, F., Rawlings, J., Raymond, G., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I., Rowan-Robinson, M., Saintonge, A., SanchezPorta, M., Santini, P., Schulz, B., Scott, D., Seymour, Nick, Shao, L., Ivison, R., Magnelli, B., Ibar, E., Andreani, P., Elbaz, D., Altieri, B., Amblard, A., Arumugam, V., Auld, R., Aussel, H., Babbedge, T., Berta, S., Blain, A., Bock, J., Bongiovanni, A., Boselli, A., Buat, V., Burgarella, D., Castro-Rodríguez, N., Cava, A., Cepa, J., Chanial, P., Cimatti, A., Cirasuolo, M., Clements, D., Conley, A., Conversi, L., Cooray, A., Daddi, E., Dominguez, H., Dowell, C., Dwek, E., Eales, S., Farrah, D., FörsterSchreiber, N., Fox, M., Franceschini, A., Gear, W., Genzel, R., Glenn, J., Griffin, M., Gruppioni, C., Halpern, M., Hatziminaoglou, E., Isaak, K., Lagache, G., Levenson, L., Lu, N., Lutz, D., Madden, S., Maffei, B., Magdis, G., Mainetti, G., Maiolino, R., Marchetti, L., Morrison, G., Mortier, A., Nguyen, H., Nordon, R., O'Halloran, B., Oliver, S., Omont, A., Owen, F., Page, M., Panuzzo, P., Papageorgiou, A., Pearson, C., Pérez-Fournon, I., García, A., Poglitsch, A., Pohlen, M., Popesso, P., Pozzi, F., Rawlings, J., Raymond, G., Rigopoulou, D., Riguccini, L., Rizzo, D., Rodighiero, G., Roseboom, I., Rowan-Robinson, M., Saintonge, A., SanchezPorta, M., Santini, P., Schulz, B., Scott, D., Seymour, Nick, and Shao, L.

Abstract

We set out to determine the ratio, qIR, of rest-frame 8-1000-µm flux, SIR, to monochromatic radio flux, S 1.4 GHz, for galaxies selected at far-infrared (IR) and radio wavelengths, to search for signs that the ratio evolves with redshift, luminosity or dust temperature, Td, and to identify any far-IR-bright outliers - useful laboratories for exploring why the far-IR/radio correlation (FIRRC) is generally so tight when the prevailing theory suggests variations are almost inevitable. We use flux-limited 250-µm and 1.4-GHz samples, obtained using Herschel and the Very Large Array (VLA) in GOODS-North (-N). We determine bolometric IR output using ten bands spanning ?obs = 24-1250 µm, exploiting data from PACS and SPIRE (PEP; HerMES), as well as Spitzer, SCUBA, AzTEC and MAMBO. We also explore the properties of an L IR-matched sample, designed to reveal evolution of qIR with redshift, spanning log LIR = 11-12 L? and z = 0-2, by stacking into the radio and far-IR images. For 1.4-GHz-selected galaxies in GOODS-N, we see tentative evidence of a break in the flux ratio, q IR, at L1.4 GHz ~ 1022.7 W Hz-1, where active galactic nuclei (AGN) are starting to dominate the radio power density, and of weaker correlations with redshift and Td. From our 250-µm-selected sample we identify a small number of far-IR-bright outliers, and see trends of qIR with L1.4 GHz, LIR, Td and redshift, noting that some of these are inter-related. For our LIR-matched sample, there is no evidence that qIR changes significantly as we move back into the epoch of galaxy formation: we find qIR (1+z)?, where ? = -0.04±0.03 at z = 0-2; however, discounting the least reliable data at z < 0.5 we find ? = -0.26±0.07, modest evolution which may be related to the radio background seen by ARCADE 2, perhaps driven by <10-µJy radio activity amongst ordinary star-forming galaxies at z>1. © ESO 2010.

Published
2010

18. The evolution of the dust temperatures of galaxies in the SFR–M∗plane up toz ~ 2

Author

Magnelli, B., primary, Lutz, D., additional, Saintonge, A., additional, Berta, S., additional, Santini, P., additional, Symeonidis, M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Béthermin, M., additional, Bock, J., additional, Bongiovanni, A., additional, Cepa, J., additional, Cimatti, A., additional, Conley, A., additional, Daddi, E., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Ivison, R. J., additional, Le Floc’h, E., additional, Magdis, G., additional, Maiolino, R., additional, Nordon, R., additional, Oliver, S. J., additional, Page, M., additional, Pérez García, A., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Rosario, D., additional, Roseboom, I., additional, Sanchez-Portal, M., additional, Scott, D., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wang, L., additional, and Wuyts, S., additional

Published
2014
Full Text
View/download PDF

19. The Mrk 231 molecular outflow as seen in OH

Author

González-Alfonso, E., primary, Fischer, J., additional, Graciá-Carpio, J., additional, Falstad, N., additional, Sturm, E., additional, Meléndez, M., additional, Spoon, H. W. W., additional, Verma, A., additional, Davies, R. I., additional, Lutz, D., additional, Aalto, S., additional, Polisensky, E., additional, Poglitsch, A., additional, Veilleux, S., additional, and Contursi, A., additional

Published
2013
Full Text
View/download PDF

20. The deepestHerschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations

Author

Magnelli, B., primary, Popesso, P., additional, Berta, S., additional, Pozzi, F., additional, Elbaz, D., additional, Lutz, D., additional, Dickinson, M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Béthermin, M., additional, Bongiovanni, A., additional, Cepa, J., additional, Charmandaris, V., additional, Chary, R.-R., additional, Cimatti, A., additional, Daddi, E., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Gruppioni, C., additional, Harwit, M., additional, Hwang, H. S., additional, Ivison, R. J., additional, Magdis, G., additional, Maiolino, R., additional, Murphy, E., additional, Nordon, R., additional, Pannella, M., additional, Pérez García, A., additional, Poglitsch, A., additional, Rosario, D., additional, Sanchez-Portal, M., additional, Santini, P., additional, Scott, D., additional, Sturm, E., additional, Tacconi, L. J., additional, and Valtchanov, I., additional

Published
2013
Full Text
View/download PDF

21. Excited OH+, H2O+, and H3O+in NGC 4418 and Arp 220

Author

González-Alfonso, E., primary, Fischer, J., additional, Bruderer, S., additional, Müller, H. S. P., additional, Graciá-Carpio, J., additional, Sturm, E., additional, Lutz, D., additional, Poglitsch, A., additional, Feuchtgruber, H., additional, Veilleux, S., additional, Contursi, A., additional, Sternberg, A., additional, Hailey-Dunsheath, S., additional, Verma, A., additional, Christopher, N., additional, Davies, R., additional, Genzel, R., additional, and Tacconi, L., additional

Published
2013
Full Text
View/download PDF

22. Spectroscopic FIR mapping of the disk and galactic wind of M 82 withHerschel-PACS

Author

Contursi, A., primary, Poglitsch, A., additional, Grácia Carpio, J., additional, Veilleux, S., additional, Sturm, E., additional, Fischer, J., additional, Verma, A., additional, Hailey-Dunsheath, S., additional, Lutz, D., additional, Davies, R., additional, González-Alfonso, E., additional, Sternberg, A., additional, Genzel, R., additional, and Tacconi, L., additional

Published
2013
Full Text
View/download PDF

24. The mean star formation rate of X-ray selected active galaxies and its evolution fromz ~ 2.5: results from PEP-Herschel

Author

Rosario, D.J., primary, Santini, P., additional, Lutz, D., additional, Shao, L., additional, Maiolino, R., additional, Alexander, D.M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Bauer, F.E., additional, Berta, S., additional, Bongiovanni, A., additional, Brandt, W.N., additional, Brusa, M., additional, Cepa, J., additional, Cimatti, A., additional, Cox, T.J., additional, Daddi, E., additional, Elbaz, D., additional, Fontana, A., additional, Förster Schreiber, N.M., additional, Genzel, R., additional, Grazian, A., additional, Le Floch, E., additional, Magnelli, B., additional, Mainieri, V., additional, Netzer, H., additional, Nordon, R., additional, Pérez Garcia, I., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Salvato, M., additional, Sanchez-Portal, M., additional, Sturm, E., additional, Tacconi, L.J., additional, Valtchanov, I., additional, and Wuyts, S., additional

Published
2012
Full Text
View/download PDF

25. Herschel-PACS far-infrared detections of Lyman-αemitters at 2.0 ≲ z ≲ 3.5

Author

Oteo, I., primary, Bongiovanni, A., additional, Pérez García, A. M., additional, Cepa, J., additional, Ederoclite, A., additional, Sánchez-Portal, M., additional, Pintos-Castro, I., additional, Pérez-Martínez, R., additional, Berta, S., additional, Magnelli, B., additional, Popesso, P., additional, Pozzi, F., additional, Poglitsch, A., additional, Lutz, D., additional, Genzel, R., additional, Tacconi, L., additional, Förster Schreiber, N., additional, Sturm, E., additional, Elbaz, D., additional, Aussel, H., additional, Daddi, E., additional, Andreani, P., additional, Cimatti, A., additional, Maiolino, R., additional, Altieri, B., additional, and Valtchanov, I., additional

Published
2012
Full Text
View/download PDF

26. Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O, H218O, OH,18OH, O I, HCN, and NH3

Author

González-Alfonso, E., primary, Fischer, J., additional, Graciá-Carpio, J., additional, Sturm, E., additional, Hailey-Dunsheath, S., additional, Lutz, D., additional, Poglitsch, A., additional, Contursi, A., additional, Feuchtgruber, H., additional, Veilleux, S., additional, Spoon, H. W. W., additional, Verma, A., additional, Christopher, N., additional, Davies, R., additional, Sternberg, A., additional, Genzel, R., additional, and Tacconi, L., additional

Published
2012
Full Text
View/download PDF

27. Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschelobservations

Author

Santini, P., primary, Rosario, D. J., additional, Shao, L., additional, Lutz, D., additional, Maiolino, R., additional, Alexander, D. M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Bauer, F. E., additional, Berta, S., additional, Bongiovanni, A., additional, Brandt, W. N., additional, Brusa, M., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Elbaz, D., additional, Fontana, A., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Grazian, A., additional, Le Floc’h, E., additional, Magnelli, B., additional, Mainieri, V., additional, Nordon, R., additional, Pérez Garcia, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Salvato, M., additional, Sanchez-Portal, M., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, and Wuyts, S., additional

Published
2012
Full Text
View/download PDF

28. AHerschelview of the far-infrared properties of submillimetre galaxies

Author

Magnelli, B., primary, Lutz, D., additional, Santini, P., additional, Saintonge, A., additional, Berta, S., additional, Albrecht, M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Bertoldi, F., additional, Béthermin, M., additional, Bongiovanni, A., additional, Capak, P., additional, Chapman, S., additional, Cepa, J., additional, Cimatti, A., additional, Cooray, A., additional, Daddi, E., additional, Danielson, A. L. R., additional, Dannerbauer, H., additional, Dunlop, J. S., additional, Elbaz, D., additional, Farrah, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Hwang, H. S., additional, Ibar, E., additional, Ivison, R. J., additional, Le Floc’h, E., additional, Magdis, G., additional, Maiolino, R., additional, Nordon, R., additional, Oliver, S. J., additional, Pérez García, A., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Rosario, D., additional, Roseboom, I., additional, Salvato, M., additional, Sanchez-Portal, M., additional, Scott, D., additional, Smail, I., additional, Sturm, E., additional, Swinbank, A. M., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wang, L., additional, and Wuyts, S., additional

Published
2012
Full Text
View/download PDF

29. The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Author

Popesso, P., primary, Biviano, A., additional, Rodighiero, G., additional, Baronchelli, I., additional, Salvato, M., additional, Saintonge, A., additional, Finoguenov, A., additional, Magnelli, B., additional, Gruppioni, C., additional, Pozzi, F., additional, Lutz, D., additional, Elbaz, D., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Berta, S., additional, Capak, P., additional, Cava, A., additional, Cimatti, A., additional, Coia, D., additional, Daddi, E., additional, Dannerbauer, H., additional, Dickinson, M., additional, Dasyra, K., additional, Fadda, D., additional, Förster Schreiber, N., additional, Genzel, R., additional, Hwang, H. S., additional, Kartaltepe, J., additional, Ilbert, O., additional, Le Floch, E., additional, Leiton, R., additional, Magdis, G., additional, Nordon, R., additional, Patel, S., additional, Poglitsch, A., additional, Riguccini, L., additional, Sanchez Portal, M., additional, Shao, L., additional, Tacconi, L., additional, Tomczak, A., additional, Tran, K., additional, and Valtchanov, I., additional

Published
2012
Full Text
View/download PDF

30. The effect of environment on star forming galaxies at redshift 1 First insight from PACS (Corrigendum)

Author

Popesso, P., primary, Rodighiero, G., additional, Saintonge, A., additional, Santini, P., additional, Grazian, A., additional, Lutz, D., additional, Brusa, M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Berta, S., additional, Bongiovanni, A., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez, H., additional, Elbaz, D., additional, Förster Schreiber, N., additional, Genzel, R., additional, Gruppioni, C., additional, Magdis, G., additional, Maiolino, R., additional, Magnelli, B., additional, Nordon, R., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Pozzi, F., additional, Riguccini, L., additional, Sanchez-Portal, M., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, Wieprecht, E., additional, and Wetzstein, M., additional

Published
2011
Full Text
View/download PDF

31. PACS Evolutionary Probe (PEP) – AHerschelkey program

Author

Lutz, D., primary, Poglitsch, A., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Berta, S., additional, Bongiovanni, A., additional, Brisbin, D., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez-Sanchez, H., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Grazian, A., additional, Gruppioni, C., additional, Harwit, M., additional, Le Floc’h, E., additional, Magdis, G., additional, Magnelli, B., additional, Maiolino, R., additional, Nordon, R., additional, Pérez García, A. M., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Sanchez Portal, M., additional, Santini, P., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wetzstein, M., additional, and Wieprecht, E., additional

Published
2011
Full Text
View/download PDF

32. Building the cosmic infrared background brick by brick withHerschel/PEP

Author

Berta, S., primary, Magnelli, B., additional, Nordon, R., additional, Lutz, D., additional, Wuyts, S., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Castañeda, H., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Le Floc’h, E., additional, Maiolino, R., additional, Pérez-Fournon, I., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Sanchez-Portal, M., additional, Sturm, E., additional, Tacconi, L. J., additional, and Valtchanov, I., additional

Published
2011
Full Text
View/download PDF

33. Star formation and the ISM in infrared bright galaxies - SHINING

Author

Sturm, E., primary, Poglitsch, A., additional, Contursi, A., additional, Graciá-Carpio, J., additional, Fischer, J., additional, González-Alfonso, E., additional, Genzel, R., additional, Hailey-Dunsheath, S., additional, Lutz, D., additional, Tacconi, L., additional, deJong, J., additional, Sternberg, A., additional, Verma, A., additional, Madden, S., additional, Vigroux, L., additional, Cormier, D., additional, Klaas, U., additional, Nielbock, M., additional, Krause, O., additional, Schreiber, J., additional, and Haas, M., additional

Published
2011
Full Text
View/download PDF

34. Herschel-PACS far-infrared detections of Lyman-αemitters at 2.0 ≲ z ≲ 3.5

Author

M. Sánchez-Portal, Eckhard Sturm, N. M. Förster Schreiber, J. Cepa, Ángel Bongiovanni, Linda J. Tacconi, A. Cimatti, Benjamin Magnelli, Roberto Maiolino, Francesca Pozzi, H. Aussel, I. Valtchanov, P. Popesso, A. Ederoclite, Ricardo Pérez-Martínez, Dieter Lutz, Reinhard Genzel, A. M. Pérez García, D. Elbaz, I. Pintos-Castro, Albrecht Poglitsch, S. Berta, I. Oteo, Bruno Altieri, E. Daddi, and P. Andreani

Subjects
Physics, education.field_of_study, Spectrometer, Population, Astronomy and Astrophysics, Astrophysics, Mutually exclusive events, Redshift, Space observatory, Galaxy, Luminosity, Space and Planetary Science, Spectral energy distribution, education
Abstract

In this work we analyze the physical properties of a sample of 56 spectroscopically selected star-forming (SF) Ly$\alpha$ emitting galaxies at 2.0$\lesssim$z$\lesssim$3.5 using both a spectral energy distribution (SED) fitting procedure from rest-frame UV to mid-IR and direct 160$\mu$m observations taken with the Photodetector Array Camera & Spectrometer (PACS) instrument onboard \emph{Herschel Space Observatory}. We define LAEs as those Ly$\alpha$ emitting galaxies whose rest-frame Ly$\alpha$ equivalent widths (Ly$\alpha$ EW$_{rest-frame}$) are above 20\AA, the typical threshold in narrow-band searches. Ly$\alpha$ emitting galaxies with Ly$\alpha$ EW$_{rest-frame}$ are called non-LAEs. As a result of an individual SED fitting for each object, we find that the studied sample of LAEs contains galaxies with ages mostly below 100Myr and a wide variety of dust attenuations, SFRs, and stellar masses. The heterogeneity in the physical properties is also seen in the morphology, ranging from bulge-like galaxies to highly clumpy systems. In this way, we find that LAEs at 2.0$\lesssim$z$\lesssim$3.5 are very diverse, and do not have a bimodal nature, as suggested in previous works. Furthermore, the main difference between LAEs and non-LAEs is their dust attenuation, because LAEs are not as dusty as non-LAEs. On the FIR side, four galaxies of the sample (two LAEs and two non-LAEs) have PACS-FIR counterparts. Their total IR luminosity place all of them in the ULIRG regime and are all dusty objects, with A$_{1200}$$\gtrsim$4mag. This is an indication from direct FIR measurements that dust and Ly$\alpha$ emission are not mutually exclusive. This population of red and dusty LAEs is not seen at z$\sim$0.3, suggesting an evolution with redshift of the IR nature of galaxies selected via their Ly$\alpha$ emission.

Published
2012
Full Text
View/download PDF

35. Herschel/PACS spectroscopy of NGC 4418 and Arp 220: H2O, H218O, OH,18OH, O I, HCN, and NH3

Author

A. Verma, R. D. Davies, Linda J. Tacconi, Sylvain Veilleux, D. Lutz, Amiel Sternberg, Albrecht Poglitsch, J. Fischer, S. Hailey-Dunsheath, R. Genzel, A. Contursi, Henrik Spoon, N. Christopher, Eduardo González-Alfonso, Javier Graciá-Carpio, Helmut Feuchtgruber, and Eckhard Sturm

Subjects
Luminous infrared galaxy, Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Absorption spectroscopy, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Oxygen isotope ratio cycle, Redshift, Space and Planetary Science, Isotopologue, Spectroscopy, Excitation, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Herschel/PACS spectroscopy of the luminous infrared galaxies NGC4418 and Arp220 reveals high excitation in H2O, OH, HCN, and NH3. In NGC4418, absorption lines were detected with E_low>800 K (H2O), 600 K (OH), 1075 K (HCN), and 600 K (NH3), while in Arp220 the excitation is somewhat lower. While outflow signatures in moderate excitation lines are seen in Arp220 as reported in previous studies, in NGC4418 the lines tracing its outer regions are redshifted relative to the nucleus, suggesting an inflow with Mdot~100 K) nuclear continuum components, together with a more extended component that is much more prominent and massive in Arp220. A chemical dichotomy is found in both sources: on the one hand, the nuclear regions have high H2O abundances, ~10^{-5}, and high HCN/H2O and HCN/NH3 column density ratios of 0.1-0.4 and 2-5, respectively, indicating a chemistry typical of evolved hot cores where grain mantle evaporation has occurred. On the other hand, the high OH abundance, with OH/H2O ratios of ~0.5, indicates the effects of X-rays and/or cosmic rays. The nuclear media have surface brightnesses >~10^{13} Lsun/kpc^2 and are estimated to be thick (N_H>~10^{25} cm^{-2}). While NGC4418 shows weak absorption in H2^{18}O and ^{18}OH, with a ^{16}O-to-^{18}O ratio of >~250-500, the strong absorption of the rare isotopologues in Arp220 indicates ^{16}O-to-^{18}O of 70-130. Further away from the nuclear regions, the H2O abundance decreases to, Comment: 31 pages, 20 figures. Accepted for publication in Astronomy and Astrophysics

Published
2012
Full Text
View/download PDF

36. HerschelFIR counterparts of selected Lyαemitters atz~ 2.2

Author

Bongiovanni, Á., primary, Oteo, I., additional, Cepa, J., additional, Pérez García, A. M., additional, Sánchez-Portal, M., additional, Ederoclite, A., additional, Aguerri, J. A. L., additional, Alfaro, E. J., additional, Altieri, B., additional, Andreani, P., additional, Aparicio-Villegas, M. T., additional, Aussel, H., additional, Benítez, N., additional, Berta, S., additional, Broadhurst, T., additional, Cabrera-Caño, J., additional, Castander, F. J., additional, Cava, A., additional, Cerviño, M., additional, Chulani, H., additional, Cimatti, A., additional, Cristóbal-Hornillos, D., additional, Daddi, E., additional, Dominguez, H., additional, Elbaz, D., additional, Fernández-Soto, A., additional, Förster Schreiber, N., additional, Genzel, R., additional, Gómez, M. F., additional, González Delgado, R. M., additional, Grazian, A., additional, Gruppioni, C., additional, Herreros, J. M., additional, Iglesias Groth, S., additional, Infante, L., additional, Lutz, D., additional, Magnelli, B., additional, Magdis, G., additional, Maiolino, R., additional, Márquez, I., additional, Martínez, V. J., additional, Masegosa, J., additional, Moles, M., additional, Molino, A., additional, Nordon, R., additional, del Olmo, A., additional, Perea, J., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Prada, F., additional, Quintana, J. M., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Sánchez, S. F., additional, Santini, P., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L., additional, and Valtchanov, I., additional

Published
2010
Full Text
View/download PDF

37. Cold dust clumps in dynamically hot gas

Author

Kim, S., primary, Kwon, E., additional, Madden, S. C., additional, Meixner, M., additional, Hony, S., additional, Panuzzo, P., additional, Sauvage, M., additional, Roman-Duval, J., additional, Gordon, K. D., additional, Engelbracht, C., additional, Israel, F. P., additional, Misselt, K., additional, Okumura, K., additional, Li, A., additional, Bolatto, A., additional, Skibba, R., additional, Galliano, F., additional, Matsuura, M., additional, Bernard, J.-P., additional, Bot, C., additional, Galametz, M., additional, Hughes, A., additional, Kawamura, A., additional, Onishi, T., additional, Paradis, D., additional, Poglitsch, A., additional, Reach, W. T., additional, Robitaille, T., additional, Rubio, M., additional, and Tielens, A. G. G. M., additional

Published
2010
Full Text
View/download PDF

39. Herschel-PACS spectroscopy of IR-bright galaxies at high redshift

Author

Sturm, E., primary, Verma, A., additional, Graciá-Carpio, J., additional, Hailey-Dunsheath, S., additional, Contursi, A., additional, Fischer, J., additional, González-Alfonso, E., additional, Poglitsch, A., additional, Sternberg, A., additional, Genzel, R., additional, Lutz, D., additional, Tacconi, L., additional, Christopher, N., additional, and de Jong, J., additional

Published
2010
Full Text
View/download PDF

40. The dust content of high-zsubmillimeter galaxies revealed byHerschel

Author

Santini, P., primary, Maiolino, R., additional, Magnelli, B., additional, Silva, L., additional, Grazian, A., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Berta, S., additional, Bongiovanni, A., additional, Brisbin, D., additional, Calura, F., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dannerbauer, H., additional, Dominguez-Sanchez, H., additional, Elbaz, D., additional, Fontana, A., additional, Förster Schreiber, N., additional, Genzel, R., additional, Granato, G. L., additional, Gruppioni, C., additional, Lutz, D., additional, Magdis, G., additional, Magliocchetti, M., additional, Matteucci, F., additional, Nordon, R., additional, Pérez Garcia, I., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Sanchez-Portal, M., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L., additional, and Valtchanov, I., additional

Published
2010
Full Text
View/download PDF

41. The star-formation rates of 1.5 < z < 2.5 massive galaxies

Author

Nordon, R., primary, Lutz, D., additional, Shao, L., additional, Magnelli, B., additional, Berta, S., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Bongiovanni, A., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez, H., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Grazian, A., additional, Magdis, G., additional, Maiolino, R., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Sanchez-Portal, M., additional, Santini, P., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, Wetzstein, M., additional, and Wieprecht, E., additional

Published
2010
Full Text
View/download PDF

42. Dissecting the cosmic infra-red background withHerschel/PEP

Author

Berta, S., primary, Magnelli, B., additional, Lutz, D., additional, Altieri, B., additional, Aussel, H., additional, Andreani, P., additional, Bauer, O., additional, Bongiovanni, A., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez, H., additional, Elbaz, D., additional, Feuchtgruber, H., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Gruppioni, C., additional, Katterloher, R., additional, Magdis, G., additional, Maiolino, R., additional, Nordon, R., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Santini, P., additional, Sanchez-Portal, M., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wetzstein, M., additional, and Wieprecht, E., additional

Published
2010
Full Text
View/download PDF

43. Herschelunveils a puzzling uniformity of distant dusty galaxies

Author

Elbaz, D., primary, Hwang, H. S., additional, Magnelli, B., additional, Daddi, E., additional, Aussel, H., additional, Altieri, B., additional, Amblard, A., additional, Andreani, P., additional, Arumugam, V., additional, Auld, R., additional, Babbedge, T., additional, Berta, S., additional, Blain, A., additional, Bock, J., additional, Bongiovanni, A., additional, Boselli, A., additional, Buat, V., additional, Burgarella, D., additional, Castro-Rodriguez, N., additional, Cava, A., additional, Cepa, J., additional, Chanial, P., additional, Chary, R.-R., additional, Cimatti, A., additional, Clements, D. L., additional, Conley, A., additional, Conversi, L., additional, Cooray, A., additional, Dickinson, M., additional, Dominguez, H., additional, Dowell, C. D., additional, Dunlop, J. S., additional, Dwek, E., additional, Eales, S., additional, Farrah, D., additional, Förster Schreiber, N., additional, Fox, M., additional, Franceschini, A., additional, Gear, W., additional, Genzel, R., additional, Glenn, J., additional, Griffin, M., additional, Gruppioni, C., additional, Halpern, M., additional, Hatziminaoglou, E., additional, Ibar, E., additional, Isaak, K., additional, Ivison, R. J., additional, Lagache, G., additional, Le Borgne, D., additional, Le Floc'h, E., additional, Levenson, L., additional, Lu, N., additional, Lutz, D., additional, Madden, S., additional, Maffei, B., additional, Magdis, G., additional, Mainetti, G., additional, Maiolino, R., additional, Marchetti, L., additional, Mortier, A. M. J., additional, Nguyen, H. T., additional, Nordon, R., additional, O'Halloran, B., additional, Okumura, K., additional, Oliver, S. J., additional, Omont, A., additional, Page, M. J., additional, Panuzzo, P., additional, Papageorgiou, A., additional, Pearson, C. P., additional, Perez Fournon, I., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Pohlen, M., additional, Popesso, P., additional, Pozzi, F., additional, Rawlings, J. I., additional, Rigopoulou, D., additional, Riguccini, L., additional, Rizzo, D., additional, Rodighiero, G., additional, Roseboom, I. G., additional, Rowan-Robinson, M., additional, Saintonge, A., additional, Sanchez Portal, M., additional, Santini, P., additional, Sauvage, M., additional, Schulz, B., additional, Scott, D., additional, Seymour, N., additional, Shao, L., additional, Shupe, D. L., additional, Smith, A. J., additional, Stevens, J. A., additional, Sturm, E., additional, Symeonidis, M., additional, Tacconi, L., additional, Trichas, M., additional, Tugwell, K. E., additional, Vaccari, M., additional, Valtchanov, I., additional, Vieira, J., additional, Vigroux, L., additional, Wang, L., additional, Ward, R., additional, Wright, G., additional, Xu, C. K., additional, and Zemcov, M., additional

Published
2010
Full Text
View/download PDF

44. HERschelInventory of The Agents of Galaxy Evolution (HERITAGE): The Large Magellanic Cloud dust

Author

Meixner, M., primary, Galliano, F., additional, Hony, S., additional, Roman-Duval, J., additional, Robitaille, T., additional, Panuzzo, P., additional, Sauvage, M., additional, Gordon, K., additional, Engelbracht, C., additional, Misselt, K., additional, Okumura, K., additional, Beck, T., additional, Bernard, J.-P., additional, Bolatto, A., additional, Bot, C., additional, Boyer, M., additional, Bracker, S., additional, Carlson, L. R., additional, Clayton, G. C., additional, R. Chen, C.-H., additional, Churchwell, E., additional, Fukui, Y., additional, Galametz, M., additional, Hora, J. L., additional, Hughes, A., additional, Indebetouw, R., additional, Israel, F. P., additional, Kawamura, A., additional, Kemper, F., additional, Kim, S., additional, Kwon, E., additional, Lawton, B., additional, Li, A., additional, Long, K. S., additional, Marengo, M., additional, Madden, S. C., additional, Matsuura, M., additional, Oliveira, J. M., additional, Onishi, T., additional, Otsuka, M., additional, Paradis, D., additional, Poglitsch, A., additional, Riebel, D., additional, Reach, W. T., additional, Rubio, M., additional, Sargent, B., additional, Sewiło, M., additional, Simon, J. D., additional, Skibba, R., additional, Smith, L. J., additional, Srinivasan, S., additional, Tielens, A. G. G. M., additional, van Loon, J. Th., additional, Whitney, B., additional, and Woods, P. M., additional

Published
2010
Full Text
View/download PDF

45. Star formation in AGN hosts in GOODS-N

Author

Shao, L., primary, Lutz, D., additional, Nordon, R., additional, Maiolino, R., additional, Alexander, D. M., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Bauer, F. E., additional, Berta, S., additional, Bongiovanni, A., additional, Brandt, W. N., additional, Brusa, M., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez-Sanchez, H., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Geis, N., additional, Genzel, R., additional, Grazian, A., additional, Gruppioni, C., additional, Magdis, G., additional, Magnelli, B., additional, Mainieri, V., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Rovilos, E., additional, Saintonge, A., additional, Salvato, M., additional, Sanchez Portal, M., additional, Santini, P., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wetzstein, M., additional, and Wieprecht, E., additional

Published
2010
Full Text
View/download PDF

46. The effects of star formation on the low-metallicity ISM: NGC 4214 mapped withHerschel/PACS spectroscopy

Author

Cormier, D., primary, Madden, S. C., additional, Hony, S., additional, Contursi, A., additional, Poglitsch, A., additional, Galliano, F., additional, Sturm, E., additional, Doublier, V., additional, Feuchtgruber, H., additional, Galametz, M., additional, Geis, N., additional, de Jong, J., additional, Okumura, K., additional, Panuzzo, P., additional, and Sauvage, M., additional

Published
2010
Full Text
View/download PDF

47. The Photodetector Array Camera and Spectrometer (PACS) on the HerschelSpace Observatory

Author

Poglitsch, A., primary, Waelkens, C., additional, Geis, N., additional, Feuchtgruber, H., additional, Vandenbussche, B., additional, Rodriguez, L., additional, Krause, O., additional, Renotte, E., additional, van Hoof, C., additional, Saraceno, P., additional, Cepa, J., additional, Kerschbaum, F., additional, Agnèse, P., additional, Ali, B., additional, Altieri, B., additional, Andreani, P., additional, Augueres, J.-L., additional, Balog, Z., additional, Barl, L., additional, Bauer, O. H., additional, Belbachir, N., additional, Benedettini, M., additional, Billot, N., additional, Boulade, O., additional, Bischof, H., additional, Blommaert, J., additional, Callut, E., additional, Cara, C., additional, Cerulli, R., additional, Cesarsky, D., additional, Contursi, A., additional, Creten, Y., additional, De Meester, W., additional, Doublier, V., additional, Doumayrou, E., additional, Duband, L., additional, Exter, K., additional, Genzel, R., additional, Gillis, J.-M., additional, Grözinger, U., additional, Henning, T., additional, Herreros, J., additional, Huygen, R., additional, Inguscio, M., additional, Jakob, G., additional, Jamar, C., additional, Jean, C., additional, de Jong, J., additional, Katterloher, R., additional, Kiss, C., additional, Klaas, U., additional, Lemke, D., additional, Lutz, D., additional, Madden, S., additional, Marquet, B., additional, Martignac, J., additional, Mazy, A., additional, Merken, P., additional, Montfort, F., additional, Morbidelli, L., additional, Müller, T., additional, Nielbock, M., additional, Okumura, K., additional, Orfei, R., additional, Ottensamer, R., additional, Pezzuto, S., additional, Popesso, P., additional, Putzeys, J., additional, Regibo, S., additional, Reveret, V., additional, Royer, P., additional, Sauvage, M., additional, Schreiber, J., additional, Stegmaier, J., additional, Schmitt, D., additional, Schubert, J., additional, Sturm, E., additional, Thiel, M., additional, Tofani, G., additional, Vavrek, R., additional, Wetzstein, M., additional, Wieprecht, E., additional, and Wiezorrek, E., additional

Published
2010
Full Text
View/download PDF

48. Herscheldeep far-infrared counts through Abell 2218 cluster-lens

Author

Altieri, B., primary, Berta, S., additional, Lutz, D., additional, Kneib, J.-P., additional, Metcalfe, L., additional, Andreani, P., additional, Aussel, H., additional, Bongiovanni, A., additional, Cava, A., additional, Cepa, J., additional, Ciesla, L., additional, Cimatti, A., additional, Daddi, E., additional, Dominguez, H., additional, Elbaz, D., additional, Förster Schreiber, N. M., additional, Genzel, R., additional, Gruppioni, C., additional, Magnelli, B., additional, Magdis, G., additional, Maiolino, R., additional, Nordon, R., additional, Pérez García, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Richard, J., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Santini, P., additional, Sanchez-Portal, M., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L. J., additional, Valtchanov, I., additional, Wetzstein, M., additional, and Wieprecht, E., additional

Published
2010
Full Text
View/download PDF

49. PEP: FirstHerschelprobe of dusty galaxy evolution up to z ~ 3

Author

Gruppioni, C., primary, Pozzi, F., additional, Andreani, P., additional, Rodighiero, G., additional, Cimatti, A., additional, Altieri, B., additional, Aussel, H., additional, Berta, S., additional, Bongiovanni, A., additional, Brisbin, D., additional, Cava, A., additional, Cepa, J., additional, Daddi, E., additional, Dominguez-Sanchez, H., additional, Elbaz, D., additional, Förster Schreiber, N., additional, Genzel, R., additional, Le Floc'h, E., additional, Lutz, D., additional, Magdis, G., additional, Magliocchetti, M., additional, Magnelli, B., additional, Maiolino, R., additional, Nordon, R., additional, Peréz-García, A. M., additional, Poglitsch, A., additional, Popesso, P., additional, Riguccini, L., additional, Saintonge, A., additional, Sanchez-Portal, M., additional, Santini, P., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L., additional, and Valtchanov, I., additional

Published
2010
Full Text
View/download PDF

50. Far-infrared properties of submillimeter and optically faint radio galaxies

Author

Magnelli, B., primary, Lutz, D., additional, Berta, S., additional, Altieri, B., additional, Andreani, P., additional, Aussel, H., additional, Castañeda, H., additional, Cava, A., additional, Cepa, J., additional, Cimatti, A., additional, Daddi, E., additional, Dannerbauer, H., additional, Dominguez, H., additional, Elbaz, D., additional, Förster Schreiber, N., additional, Genzel, R., additional, Grazian, A., additional, Gruppioni, C., additional, Magdis, G., additional, Maiolino, R., additional, Nordon, R., additional, Pérez Fournon, I., additional, Pérez García, I., additional, Poglitsch, A., additional, Popesso, P., additional, Pozzi, F., additional, Riguccini, L., additional, Rodighiero, G., additional, Saintonge, A., additional, Santini, P., additional, Sanchez-Portal, M., additional, Shao, L., additional, Sturm, E., additional, Tacconi, L., additional, Valtchanov, I., additional, Wieprecht, E., additional, and Wiezorrek, E., additional

Published
2010
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results