Search

Your search keyword '"M. Bethermin"' showing total 32 results
Start Over Author "M. Bethermin"
32 results on '"M. Bethermin"'

1. The ALMA REBELS Survey: Average [CII] 158μm Sizes of Star-forming Galaxies from z~7 to z~4

Author

Y. Fudamoto, R. Smit, R. A. A. Bowler, P. A. Oesch, R. Bouwens, M. Stefanon, H. Inami, R. Endsley, V. Gonzalez, S. Schouws, D. Stark, H. S. B. Algera, M. Aravena, L. Barrufet, E. da Cunha, P. Dayal, A. Ferrara, L. Graziani, J. A. Hodge, A. P. S. Hygate, A. K. Inoue, T. Nanayakkara, A. Pallottini, E. Pizzati, R. Schneider, L. Sommovigo, Y. Sugahara, M. Topping, P. van der Werf, M. Bethermin, P. Cassata, M. Dessauges-Zavadsky, E. Ibar, A. L. Faisst, S. Fujimoto, M. Ginolfi, N. Hathi, G. C. Jones, F. Pozzi, D. Schaerer, Astronomy, Fudamoto, Y., Smit, R., Bowler, R. A. A., Oesch, P. A., Bouwens, R., Stefanon, M., Inami, H., Endsley, R., Gonzalez, V., Schouws, S., Stark, D., Algera, H. S. B., Aravena, M., Barrufet, L., Da Cunha, E., Dayal, P., Ferrara, A., Graziani, L., Hodge, J. A., Hygate, A. P. S., Inoue, A. K., Nanayakkara, T., Pallottini, A., Pizzati, E., Schneider, R., Sommovigo, L., Sugahara, Y., Topping, M., Van Der Werf, P., Bethermin, M., Cassata, P., Dessauges-Zavadsky, M., Ibar, E., Faisst, A. L., Fujimoto, S., Ginolfi, M., Hathi, N., Jones, G. C., Pozzi, F., Schaerer, D., 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), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Settore FIS/05 - Astronomia e Astrofisica, [SDU]Sciences of the Universe [physics], Space and Planetary Science, Interstellar medium, Astrophysics - astrophysics of galaxies, High-redshift galaxies, Astronomy and Astrophysics, Submillimeter astronomy
Abstract

We present the average [C ii] 158 μm emission line sizes of UV-bright star-forming galaxies at z ∼ 7. Our results are derived from a stacking analysis of [C ii] 158 μm emission lines and dust continua observed by the Atacama Large Millimeter/submillimeter Array (ALMA), taking advantage of the large program Reionization Era Bright Emission Line Survey. We find that the average [C ii] emission at z ∼ 7 has an effective radius r e of 2.2 ± 0.2 kpc. It is ≳2× larger than the dust continuum and the rest-frame UV emission, in agreement with recently reported measurements for z ≲ 6 galaxies. Additionally, we compared the average [C ii] size with 4 < z < 6 galaxies observed by the ALMA Large Program to INvestigate [C ii] at Early times (ALPINE). By analyzing [C ii] sizes of 4 < z < 6 galaxies in two redshift bins, we find an average [C ii] size of r e = 2.2 ± 0.2 kpc and r e = 2.5 ± 0.2 kpc for z ∼ 5.5 and z ∼ 4.5 galaxies, respectively. These measurements show that star-forming galaxies, on average, show no evolution in the size of the [C ii] 158 μm emitting regions at redshift between z ∼ 7 and z ∼ 4. This finding suggests that the star-forming galaxies could be morphologically dominated by gas over a wide redshift range.

Published
2022
Full Text
View/download PDF

2. ALPINE: The ALMA [CII] survey of normal star-forming galaxies at 4 <z< 6

Author

Daniel Schaerer, Andreas L. Faisst, Lin Yan, Olivier Le Fevre, M. Bethermin, Alpine Team, John D. Silverman, Paolo Cassata, and Peter Capak

Subjects
Physics, 010308 nuclear & particles physics, Space and Planetary Science, 0103 physical sciences, Astronomy and Astrophysics, Astrophysics, Star (graph theory), 010303 astronomy & astrophysics, 01 natural sciences, Galaxy
Abstract

The ALMA-ALPINE [CII] survey (A2C2S) aims at characterizing the properties of normal star-forming galaxies (SFGs) observed in the [CII]-158μm line in the period of rapid mass assembly at redshifts 4

Published
2019
Full Text
View/download PDF

3. The ALPINE-ALMA [CII] survey

Author

Y. Khusanova, M. Bethermin, O. Le Fèvre, P. Capak, A. L. Faisst, D. Schaerer, J. D. Silverman, P. Cassata, L. Yan, M. Ginolfi, Y. Fudamoto, F. Loiacono, R. Amorin, S. Bardelli, M. Boquien, A. Cimatti, M. Dessauges-Zavadsky, C. Gruppioni, N. P. Hathi, G. C. Jones, A. M. Koekemoer, G. Lagache, R. Maiolino, B. C. Lemaux, P. Oesch, F. Pozzi, D. A. Riechers, M. Romano, M. Talia, S. Toft, D. Vergani, G

Published
2021
Full Text
View/download PDF

4. The ALPINE-ALMA [C II] Survey: [C II] 158 μm Emission Line Luminosity Functions at z ~ 4–6

Author

L. A. M. Tasca, E. Ibar, Peter Capak, Sune Toft, Livia Vallini, Miroslava Dessauges-Zavadsky, Michele Ginolfi, Francesca Pozzi, F. Loiacono, Nimish P. Hathi, Andreas L. Faisst, E. Zucca, A. Cimatti, Anna Sajina, G. Zamorani, Paolo Cassata, G. C. Jones, M. Bethermin, Lin Yan, Margherita Talia, Carlotta Gruppioni, S. Bardelli, John D. Silverman, D. Vergani, O. Le Fevre, Pascal Oesch, G. Lagache, Brian Lemaux, Dominik Riechers, Anton M. Koekemoer, Daniel Schaerer, Yan, L., Sajina, A., Loiacono, F., Lagache, G., Bethermin, M., Faisst, A., Ginolfi, M., Fevre, O. L., Gruppioni, C., Capak, P. L., Cassata, P., Schaerer, D., Silverman, J. D., Bardelli, S., Dessauges-Zavadsky, M., Cimatti, A., Hathi, N. P., Lemaux, B. C., Ibar, E., Jones, G. C., Koekemoer, A. M., Oesch, P. A., Talia, M., Pozzi, F., Riechers, D. A., Tasca, L. A. M., Toft, S., Vallini, L., Vergani, D., Zamorani, G., Zucca, E., Yan L., Sajina A., Loiacono F., Lagache G., Bethermin M., Faisst A., Ginolfi M., Fevre O.L., Gruppioni C., Capak P.L., Cassata P., Schaerer D., Silverman J.D., Bardelli S., Dessauges-Zavadsky M., Cimatti A., Hathi N.P., Lemaux B.C., Ibar E., Jones G.C., Koekemoer A.M., Oesch P.A., Talia M., Pozzi F., Riechers D.A., Tasca L.A.M., Toft S., Vallini L., Vergani D., Zamorani G., Zucca E., Caltech Department of Astronomy [Pasadena], and California Institute of Technology (CALTECH)

Subjects
010504 meteorology & atmospheric sciences, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Population, FOS: Physical sciences, Emission line galaxie, Astrophysics, 01 natural sciences, Luminosity, Warm ionized medium, Warm neutral medium, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Emission spectrum, education, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation), Luminosity function (astronomy), Physics, education.field_of_study, Molecular gas, Luminosity function, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, High-redshift galaxie, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Order of magnitude
Abstract

We present the [CII]158$\mu$m line luminosity functions (LFs) at $z\sim4-6$ using the ALMA observations of 118 sources, which are selected to have UV luminosity $M_{1500A}10^9L_{\odot}$, suggesting that UV-faint but [CII]-bright sources likely make a significant contributions to the [CII] emitter volume density. When we include all the LF estimates, we find that available model predictions underestimate the number densities of [CII] emitters at $z\sim4-6$. Finally, we set a constraint on the molecular gas mass density at $z\sim4-6$, with $\rho_{mol} \sim (2-7)\times10^7M_\odot$\,Mpc$^{-3}$. This is broadly consistent with previous studies., Comment: 17 pages, 9 Figures, Update to match with the published version. Accepted for the publication in ApJ

Published
2020
Full Text
View/download PDF

5. The ALPINE-ALMA [CII] survey: Small Ly$\alpha$-[CII] velocity offsets in main-sequence galaxies at 4.4 < z < 6

Author

G. Rodighiero, H. Mendez-Hernandez, Dominik Riechers, Seiji Fujimoto, E. Zucca, Brian C. Lemaux, Pascal Oesch, Mauro Giavalisco, Nimish P. Hathi, Andrea Cimatti, Chiara Mancini, Daniel Schaerer, L. Morselli, Y. Fudamoto, M. Bethermin, John D. Silverman, Lin Yan, Gareth J. F. Jones, M. Romano, O. Le Fevre, Andreas L. Faisst, S. Bardelli, Peter Capak, Miroslava Dessauges-Zavadsky, Paolo Cassata, Edo Ibar, Margherita Talia, Médéric Boquien, D. Vergani, Anton M. Koekemoer, G. Zamorani, Michele Ginolfi, Francesca Pozzi, 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), 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), 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), Cassata P., Morselli L., Faisst A., Ginolfi M., Bethermin M., Capak P., Le Fevre O., Schaerer D., Silverman J., Yan L., Lemaux B.C., Romano M., Talia M., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Fudamoto Y., Fujimoto S., Giavalisco M., Hathi N.P., Ibar E., Jones G., Koekemoer A.M., Mendez-Hernandez H., Mancini C., Oesch P.A., Pozzi F., Riechers D.A., Rodighiero G., Vergani D., Zamorani G., Zucca E., 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), 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), and 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)

Subjects
submillimeter: galaxies, REDSHIFT EVOLUTION, galaxies [submillimeter], PHYSICAL-PROPERTIES, Context (language use), Astrophysics, 01 natural sciences, LYMAN BREAK GALAXIES, ULTRAVIOLET-SPECTRA, galaxies: high-redshift, 0103 physical sciences, C II, STAR-FORMING GALAXIES, 010303 astronomy & astrophysics, ESCAPE FRACTION, Line (formation), Physics, Very Large Telescope, Line-of-sight, ISM [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, DUST CONTENT, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, COSMOS FIELD, Interstellar medium, Space and Planetary Science, LY-ALPHA RADIATION, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Equivalent width, galaxies: ISM, high-redshift [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Lya line in the UV and the [CII] line in the FIR are widely used tools to identify galaxies and to obtain insights into ISM properties in the early Universe. By combining data obtained with ALMA in band 7 at ~ 320 GHz as part of the ALMA Large Program to INvestigate [CII] at Early Times (ALPINE) with spectroscopic data from DEIMOS at Keck, VIMOS and FORS2 at the VLT, we assembled a unique sample of 53 main-sequence star-forming galaxies at 4.4 < z < 6 in which we detect both the Lya line and the [CII]. We used [CII], observed with ALMA, as a tracer of the systemic velocity of the galaxies, and we find that 90% of the selected objects have Lya-[CII] velocity offsets in the range 0 < Dv_Lya-[CII] < 400 km/s, in line with the few measurements available so far in the early Universe, and significantly smaller than those observed at lower z. We observe ISM-[CII] offsets in the range -500 < Dv_ISM-[CII] < 0 km/s, in line with values at all redshifts. We find significant anticorrelations between Dv_Lya-[CII] and the Lya rest-frame equivalent width EW0(Lya) (or equivalently, the Lya escape fraction f_esc(Lya)). According to available models for the radiative transfer of Lya photons, the escape of Lya photons would be favored in galaxies with high outflow velocities, in agreement with our observations. The uniform shell model would also predict that the Lya escape in galaxies with slow outflows (0 < v_out < 300 km/s) is mainly determined by the neutral hydrogen column density (NHI), while the alternative model by Steidel+10 would favor a combination of NHI and covering fraction as driver of the Lya escape. We suggest that the observed increase in Lya escape that is observed between z~2 and z~6 is not due to a higher incidence of fast outflows at high redshift, but rather to a decrease in average NHI along the line of sight, or alternatively, a decrease in HI covering fraction. [abridged], Comment: 22 pages, 6 figures, accepted for publication in A&A. This version replaces the previous one

Published
2020
Full Text
View/download PDF

6. The ALPINE-ALMA [CII] survey: Survey strategy, observations and sample properties of 118 star-forming galaxies at $4 < z < 6$

Author

M. Bethermin, Carlotta Gruppioni, Shoubaneh Hemmati, Lin Yan, G. Zamorani, Michele Ginolfi, Andreas L. Faisst, E. Zucca, Fabian Walter, G. Lagache, Francesca Pozzi, F. Loiacono, Edo Ibar, Médéric Boquien, Ricardo Amorín, Nick Scoville, Daniel Schaerer, Anton M. Koekemoer, Y. Khusanova, Pascal Oesch, Dominik Riechers, Desika Narayanan, Andrea Cimatti, John D. Silverman, Nimish P. Hathi, Sune Toft, Brian C. Lemaux, Livia Vallini, Chiara Mancini, Miroslava Dessauges-Zavadsky, H. Mendez-Hernandez, R. Thomas, L. Morselli, G. C. Jones, Mauro Giavalisco, L. A. M. Tasca, Paolo Cassata, Roberto Maiolino, Peter Capak, O. Le Fevre, M. Romano, D. Vergani, S. Bardelli, Margherita Talia, Seiji Fujimoto, Y. Fudamoto, 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 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), ALPINE Team, 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), 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), 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), Le Fevre, O., Bethermin, M., Faisst, A., Jones, G. C., Capak, P., Cassata, P., Silverman, J. D., Schaerer, D., Yan, L., Amorin, R., Bardelli, S., Boquien, M., Cimatti, A., Dessauges-Zavadsky, M., Giavalisco, M., Hathi, N. P., Fudamoto, Y., Fujimoto, S., Ginolfi, M., Gruppioni, C., Hemmati, S., Ibar, E., Koekemoer, A., Khusanova, Y., Lagache, G., Lemaux, B. C., Loiacono, F., Maiolino, R., Mancini, C., Narayanan, D., Morselli, L., Mendez-Hernandez, H., Oesch, P. A., Pozzi, F., Romano, M., Riechers, D., Scoville, N., Talia, M., Tasca, L. A. M., Thomas, R., Toft, S., Vallini, L., Vergani, D., Walter, F., Zamorani, G., Zucca, E., Le Fevre O., Bethermin M., Faisst A., Jones G.C., Capak P., Cassata P., Silverman J.D., Schaerer D., Yan L., Amorin R., Bardelli S., Boquien M., Cimatti A., Dessauges-Zavadsky M., Giavalisco M., Hathi N.P., Fudamoto Y., Fujimoto S., Ginolfi M., Gruppioni C., Hemmati S., Ibar E., Koekemoer A., Khusanova Y., Lagache G., Lemaux B.C., Loiacono F., Maiolino R., Mancini C., Narayanan D., Morselli L., Mendez-Hernandez H., Oesch P.A., Pozzi F., Romano M., Riechers D., Scoville N., Talia M., Tasca L.A.M., Thomas R., Toft S., Vallini L., Vergani D., Walter F., Zamorani G., and Zucca E.

Subjects
formation [galaxies], Population, REDSHIFT, BILLION YEARS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, COOL GAS, Far infrared, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, galaxies: formation, MAIN-SEQUENCE, FIELD, education, 010303 astronomy & astrophysics, Reionization, BLACK-HOLES, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Physics, EVOLUTION SURVEY COSMOS, education.field_of_study, 010308 nuclear & particles physics, James Webb Space Telescope, Astronomy and Astrophysics, FRAMEWORK, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, C II EMISSION, SIMULATIONS, Reference sample, Space and Planetary Science, galaxies: star formation, Spectral energy distribution, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies], galaxies: evolution, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The ALMA-ALPINE [CII] survey is aimed at characterizing the properties of a sample of normal star-forming galaxies (SFGs). The ALMA Large Program to INvestigate (ALPINE) features 118 galaxies observed in the [CII]-158$\mu$m line and far infrared (FIR) continuum emission during the period of rapid mass assembly, right after the end of the HI reionization, at redshifts of 45). Based on a visual inspection of the [CII] data cubes together with the large wealth of ancillary data, we find a surprisingly wide range of galaxy types, including 40% that are mergers, 20% extended and dispersion-dominated, 13% compact, and 11% rotating discs, with the remaining 16% too faint to be classified. This diversity indicates that a wide array of physical processes must be at work at this epoch, first and foremost, those of galaxy mergers. This paper sets a reference sample for the gas distribution in normal SFGs at 4, Comment: 20 pages, 13 figures, 1 table, accepted by A&A

Published
2020
Full Text
View/download PDF

7. A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47⋆

Author

Matthew A. Malkan, Scott Chapman, M. Bethermin, Manuel Aravena, Amit Vishwas, M. Archipley, Axel Weiss, M. Strandet, D. J. M. Cunningham, J. Fu, Chian-Chou Chen, Carlos De Breuck, Yordanka Apostolovski, A. C. Mangian, Gordon J. Stacey, Sreevani Jarugula, Cassie Reuter, Kedar A. Phadke, Joaquin Vieira, 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
submillimeter: galaxies, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Metallicity, FOS: Physical sciences, galaxies [submillimeter], Astrophysics, Star (graph theory), Astronomy & Astrophysics, 01 natural sciences, Submillimeter Array, Gravitation, galaxies: high-redshift, 0103 physical sciences, ISM [submillimeter], 010303 astronomy & astrophysics, Line (formation), Physics, ISM [galaxies], 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), submillimeter: ISM, Millimeter, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], galaxies: ISM, high-redshift [galaxies], Astronomical and Space Sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present a study of six far-infrared fine structure lines in the z=4.225 lensed dusty star-forming galaxy SPT0418-47 to probe the physical conditions of its InterStellar Medium (ISM). In particular, we report Atacama Pathfinder EXperiment (APEX) detections of the [OI]145um and [OIII]88um lines and Atacama Compact Array (ACA) detections of the [NII]122 and 205um lines. The [OI]145um / [CII]158um line ratio is ~5x higher compared to the average of local galaxies. We interpret this as evidence that the ISM is dominated by photo-dissociation regions with high gas densities. The line ratios, and in particular those of [OIII]88um and [NII]122um imply that the ISM in SPT0418-47 is already chemically enriched close to solar metallicity. While the strong gravitational amplification was required to detect these lines with APEX, larger samples can be observed with the Atacama Large Millimeter/submillimeter Array (ALMA), and should allow to determine if the observed dense, solar metallicity ISM is common among these highly star-forming galaxies., Accepted for publication in Astronomy & Astrophysics. Revised to match language-edited version and adding 1 missing citation

Published
2019
Full Text
View/download PDF

8. The Close AGN Reference Survey (CARS) Discovery of a global [C II] 158 mu m line excess in AGN HE 1353-1917

Author

M. Singha, Christian Fischer, Gerold Busch, P. N. Appleton, Randolf Klein, M. Bethermin, Brent Groves, Miguel A. Pérez-Torres, Tanya Urrutia, J. Scharwächter, Francoise Combes, Bernd Husemann, Timothy A. Davis, Scott M. Croom, Grant R. Tremblay, Massimo Gaspari, C. P. O'Dea, I. Smirnova-Pinchukova, 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), German Research Foundation, National Aeronautics and Space Administration (US), European Southern Observatory, Ministerio de Economía y Competitividad (España), and European Commission

Subjects
Galaxies: Seyfert, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, seyfert [galaxies], 01 natural sciences, Luminosity, Ionization, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, ism [infrared], 14. Life underwater, Disc, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Line (formation), Physics, Infrared: ISM, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Galaxies: star formation, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Interstellar medium, ISM: jets and outflows, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Astrophysics of Galaxies (astro-ph.GA), jets and outflows [ism], Outflow, Astrophysics::Earth and Planetary Astrophysics, star formation [galaxies]
Abstract

Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited. Open Access funding provided by Max Planck Society., The [C II]lambda 158 mu m line is one of the strongest far-infrared (FIR) lines and an important coolant in the interstellar medium of galaxies that is accessible out to high redshifts. The excitation of [C II] is complex and can best be studied in detail at low redshifts. Here we report the discovery of the highest global [C II] excess with respect to the FIR luminosity in the nearby AGN host galaxy HE 1353-1917. This galaxy is exceptional among a sample of five targets because the AGN ionization cone and radio jet directly intercept the cold galactic disk. As a consequence, a massive multiphase gas outflow on kiloparsec scales is embedded in an extended narrow-line region. Because HE 1353-1917 is distinguished by these special properties from our four bright AGN, we propose that a global [C II] excess in AGN host galaxies could be a direct signature of a multiphase AGN-driven outflow with a high mass-loading factor.© I. Smirnova-Pinchukova et al. 2019, We thank the anonymous referee for helpful comments that improved the quality of the manuscript. Based on observations made with the NASA/DLR Stratospheric Observatory for Infrared Astronomy (SOFIA). SOFIA is jointly operated by the Universities Space Research Association, Inc. (USRA), under NASA contract NNA17BF53C, and the Deutsches SOFIA Institut (DSI) under DLR contract 50 OK 0901 to the University of Stuttgart. Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO programme 094. B-0345(A) and 095. B-0015(A). M. G. is supported by the Lyman Spitzer Jr. Fellowship (Princeton University) and by NASA Chandra GO7-18121X and GO8-19104X. M. P. T. acknowledges support from the Spanish MINECO through grant AYA2015-63939-C2-1-P.

Published
2019
Full Text
View/download PDF

9. Multi-wavelength de-blended Herschel view of the statistical properties of dusty star-forming galaxies across cosmic time

Author

Lingyu Wang, W. I. Cowley, Carlotta Gruppioni, James W. Trayford, Peter Hurley, Michał J. Michałowski, W. J. Pearson, M. Bethermin, Astronomy, 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
submillimeter: galaxies, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, Measure (mathematics), infrared: galaxies, Luminosity, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Physics, Luminous infrared galaxy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, galaxies: luminosity function, Wavelength, [SDU]Sciences of the Universe [physics], mass function, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: abundances, Astrophysics::Earth and Planetary Astrophysics, galaxies: evolution
Abstract

We aim to study the statistical properties of dusty star-forming galaxies, such as their number counts, luminosity functions (LF) and dust-obscured star-formation rate density (SFRD). We use state-of-the-art de-blended Herschel catalogue in the COSMOS field, generated by combining the Bayesian source extraction tool XID+ and informative prior on the spectral energy distributions, to measure the number counts and LFs at far-infrared (FIR) and sub-millimetre (sub-mm) wavelengths. Thanks to our de-confusion technique and deep multi-wavelength photometry, we are able to achieve more accurate measurements while probing ten times below the confusion limit. Our number counts at 250 microns agree well with previous Herschel studies. However, our counts at 350 and 500 microns are considerably below previous Herschel results. This is due to previous studies suffering from source confusion which worsens towards longer wavelength. Our number counts at 450 and 870 microns show excellent agreement with previous determinations derived from single dish and interferometric observations. Our measurements of the monochromatic LF and the total IR LF agree well with previous results. The increased dynamic range of our measurements allows us to better measure the faint-end slope of the LF and measure the dust-obscured SFRD out to z~6. We find that the fraction of dust obscured star-formation activity is at its highest around z~1 which then decreases towards both low and high redshift. We do not find a shift of balance between z~3 and z~4 in the cosmic star-formation history from being dominated by unobscured star formation at higher redshift to obscured star formation at lower redshift. However, we do find 3, Comment: 21 pages, 10 figures, 8 table, accepted for publication in A&A

Published
2019
Full Text
View/download PDF

11. Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2

Author

Masato Onodera, E. Daddi, Francesco Valentino, Maurilio Pannella, Daizhong Liu, A. Cimatti, Raphael Gobat, A. Finoguenov, Alvio Renzini, Nobuo Arimoto, V. Strazzullo, M. T. Sargent, R. Coogan, Helmut Dannerbauer, Mark Dickinson, M. Bethermin, Department of Physics, Ludwig-Maximilians-Universität München (LMU), 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, 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), National Optical Astronomy Observatory (NOAO), Max-Planck-Institut für Extraterrestrische Physik (MPE), National Astronomical Observatory of Japan (NAOJ), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Institute for Astronomy [Zürich], Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Astronomy Centre [Brighton], University of Sussex, Département d'Astrophysique (ex SAP) (DAP), 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, 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), Pontificia Universidad Católica de Valparaíso (PUCV), Dark Cosmology Centre (DARK), Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), INAF - Osservatorio Astronomico di Padova (OAPD), Istituto Nazionale di Astrofisica (INAF), Seoul National University [Seoul] (SNU), Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Instituto de Astrofisica de Canarias (IAC), Max Planck Institute for Astronomy (MPIA), 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), Strazzullo, V., Coogan, R. T., Daddi, E., Sargent, M. T., Gobat, R., Valentino, F., Bethermin, M., Pannella, M., Dickinson, M., Renzini, A., Arimoto, N., Cimatti, A., Dannerbauer, H., Finoguenov, A., Liu, D., Onodera, M., University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)-Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU), Università degli Studi di Bologna, NOAO, and Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich)

Subjects
galaxies: clusters: individual, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, galaxies: clusters: individual: Cl J1449+0856, galaxies: evolution, galaxies: high-redshift, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxie, Z=1.46, 0103 physical sciences, STAR-FORMING GALAXIES, Continuum (set theory), Brightest cluster galaxy, RED-SEQUENCE, education, 010303 astronomy & astrophysics, evolution [galaxies], QB, Line (formation), Physics, education.field_of_study, PROTOCLUSTER, 010308 nuclear & particles physics, Star formation, Center (category theory), STARBURST GALAXIES, Astronomy and Astrophysics, Astronomy and Astrophysic, ALPHA EMITTERS, 115 Astronomy, Space science, Galaxy, Redshift, DENSE ENVIRONMENTS, EVOLUTION, galaxies: clusters: individual ( ClJ1449+0856), [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Space and Planetary Science, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), MOLECULAR GAS-RESERVOIRS, clusters: individual: Cl J1449+0856 [galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], high-redshift [galaxies]
Abstract

We present ALMA observations of the 870$\mu$m continuum and CO(4-3) line emission in the core of the galaxy cluster ClJ1449+0856 at z=2, a NIR-selected, X-ray detected system in the mass range of typical progenitors of today's massive clusters. The 870$\mu$m map reveals six F$_{870\mu m}$ > 0.5 mJy sources spread over an area of 0.07 arcmin$^2$, giving an overdensity of a factor ~10 (6) with respect to blank field counts down to F$_{870\mu m}$ > 1 (0.5) mJy. On the other hand, deep CO(4-3) follow-up confirms membership of three of these sources, but suggests that the remaining three, including the brightest 870$\mu$m sources in the field (F$_{870\mu m}\gtrsim$2 mJy), are likely interlopers. The measurement of 870$\mu$m continuum and CO(4-3) line fluxes at the positions of previously-known cluster members provides a deep probe of dusty star formation occurring in the core of this high-redshift structure, adding up to a total SFR~700$\pm$100 M$_{\odot}$/yr and yielding an integrated star formation rate density of ~10$^4$ M$_{\odot}$/yr/Mpc$^3$, five orders of magnitude larger than in the field at the same epoch, due to the concentration of star-forming galaxies in the small volume of the dense cluster core. The combination of these observations with previously available HST imaging highlights the presence in this same volume of a population of galaxies with already suppressed star formation. This diverse composition of galaxy populations in ClJ1449+0856 is especially highlighted at the very cluster center, where a complex assembly of quiescent and star-forming sources is likely forming the future Brightest Cluster Galaxy., Comment: 11 pages, 6 figures, ApJ in press

Published
2018
Full Text
View/download PDF

12. Fast molecular outflow from a dusty star-forming galaxy in the early Universe

Author

Manuel Aravena, Christopher C. Hayward, Kedar A. Phadke, Antony A. Stark, Scott Chapman, Chenxing Dong, J. Sreevani, Warren R. Morningstar, Jingzhe Ma, M. Bethermin, Justin Spilker, Daniel P. Marrone, D. Narayanan, Joaquin Vieira, Yashar D. Hezaveh, M. A. Malkan, Axel Weiss, K. Litke, Chian-Chou Chen, C. De Breuck, Tim B. Miller, Anthony H. Gonzalez, D. J. M. Cunningham, 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), Université de Lyon, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), 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 Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
010504 meteorology & atmospheric sciences, General Science & Technology, astro-ph.GA, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Supermassive black hole, Multidisciplinary, Star formation, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), Redshift, Galaxy, Stars, Supernova, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Radiation pressure, 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract

Galaxies grow inefficiently, with only a few percent of the available gas converted into stars each free-fall time. Feedback processes, such as outflowing winds driven by radiation pressure, supernovae or supermassive black hole accretion, can act to halt star formation if they heat or expel the gas supply. We report a molecular outflow launched from a dust-rich star-forming galaxy at redshift 5.3, one billion years after the Big Bang. The outflow reaches velocities up to 800 km/s relative to the galaxy, is resolved into multiple clumps, and carries mass at a rate within a factor of two of the star formation rate. Our results show that molecular outflows can remove a large fraction of the gas available for star formation from galaxies at high redshift., Comment: Author's version of paper to appear in Science on 7 September 2018

Published
2018
Full Text
View/download PDF

13. The Herschel PEP/HerMES Luminosity Function. I: Probing the Evolution of PACS selected Galaxies to z~4

Author

V. Arumugam, Ismael Perez-Fournon, M. Bethermin, Andreas Papageorgiou, Alberto Franceschini, Mattia Vaccari, A. M. Pérez García, Lucia Pozzetti, G. Wright, B. O'Halloran, P. Chanial, Giulia Rodighiero, Pierluigi Monaco, P. Popesso, E. Zucca, Michael Pohlen, Benjamin Magnelli, K. G. Isaak, Lucia Marchetti, Eckhard Sturm, Bruno Maffei, Michael Rowan-Robinson, Matthew Joseph Griffin, Michael Zemcov, Marco Scodeggio, C. K. Xu, Lian-Tao Wang, Antonio Cava, O. Le Fevre, K. E. Tugwell, M. Magliocchetti, Dimitra Rigopoulou, Albrecht Poglitsch, S. C. Madden, Bruno Altieri, Raanan Nordon, M. Carollo, Rob Ivison, Alexandre Amblard, N. Castro-Rodríguez, R. Genzel, James J. Bock, Vincenzo Mainieri, Linda J. Tacconi, Alvio Renzini, Anthony J. Smith, Francesca Pozzi, David J. Rosario, Chris Pearson, Mark Sargent, A. Boselli, Denis Burgarella, G. Mainetti, Edo Ibar, C. D. Dowell, Ivan Delvecchio, H. Aussel, A. Conley, Benjamin L. Schulz, Simon J. Lilly, Jamie Stevens, H. T. Nguyen, V. Buat, Guilaine Lagache, D. Elbaz, Nick Seymour, Asantha Cooray, Alessandro Cimatti, Douglas Scott, M. J. Page, Louis Levenson, M. Sánchez-Portal, Evanthia Hatziminaoglou, David L. Clements, Nanyao Y. Lu, M. Symeonidis, S. Berta, L. Riguccini, L. Vigroux, Ivan Valtchanov, Emanuele Daddi, Roberto Maiolino, Eli Dwek, J. Cepa, Stephen Anthony Eales, H. Dominguez-Sanchez, G. Zamorani, Dieter Lutz, P. Panuzzo, S. Bardelli, D. L. Shupe, Carlotta Gruppioni, E. Le Floc'h, Isaac Roseboom, Seb Oliver, Ángel Bongiovanni, P. Andreani, Alvaro Iribarrem, Thierry Contini, N. M. Foerster Schreiber, Jason Glenn, Markos Trichas, O. Ilbert, C., Gruppioni, F., Pozzi, G., Rodighiero, I., Delvecchio, S., Berta, L., Pozzetti, G., Zamorani, P., Andreani, A., Cimatti, O., Ilbert, E., Le Floc'h, D., Lutz, B., Magnelli, L., Marchetti, Monaco, Pierluigi, R., Nordon, S., Oliver, P., Popesso, L., Riguccini, I., Roseboom, D. J., Rosario, M., Sargent, M., Vaccari, B., Altieri, H., Aussel, A., Bongiovanni, J., Cepa, E., Daddi, H., Dominguez Sanchez, D., Elbaz, N., Forster Schreiber, R., Genzel, A., Iribarrem, M., Magliocchetti, R., Maiolino, A., Poglitsch, A., Perez Garcia, M., Sanchez Portal, E., Sturm, L., Tacconi, I., Valtchanov, A., Amblard, V., Arumugam, M., Bethermin, J., Bock, A., Boselli, V., Buat, D., Burgarella, N., Castro Rodriguez, A., Cava, P., Chanial, D. L., Clement, A., Conley, A., Cooray, C. D., Dowell, E., Dwek, S., Eale, A., Franceschini, J., Glenn, M., Griffin, E., Hatziminaoglou, E., Ibar, K., Isaak, R. J., Ivison, G., Lagache, L., Levenson, N., Lu, S., Madden, B., Maffei, G., Mainetti, H. T., Nguyen, B., O'Halloran, M. J., Page, P., Panuzzo, A., Papageorgiou, C. P., Pearson, I., Perez Fournon, M., Pohlen, D., Rigopoulou, M., Rowan Robinson, B., Schulz, D., Scott, N., Seymour, D. L., Shupe, A. J., Smith, J. A., Steven, M., Symeonidi, M., Tricha, K. E., Tugwell, L., Vigroux, L., Wang, G., Wright, C. K., Xu, M., Zemcov, S., Bardelli, M., Carollo, T., Contini, O., Le Fevre, S., Lilly, V., Mainieri, A., Renzini, M., Scodeggio, E., Zucca, C. Gruppioni, F. Pozzi, G. Rodighiero, I. Delvecchio, S. Berta, L. Pozzetti, G. Zamorani, P. Andreani, A. Cimatti, O. Ilbert, E. Le Floc'h, D. Lutz, B. Magnelli, L. Marchetti, P. Monaco, R. Nordon, S. Oliver, P. Popesso, L. Riguccini, I. Roseboom, D. J. Rosario, M. Sargent, M. Vaccari, B. Altieri, H. Aussel, A. Bongiovanni, J. Cepa, E. Daddi, H. Dominguez-Sanchez, D. Elbaz, N. Forster Schreiber, R. Genzel, A. Iribarrem, M. Magliocchetti, R. Maiolino, A. Poglitsch, A. Perez Garcia, M. Sanchez-Portal, E. Sturm, L. Tacconi, I. Valtchanov, A. Amblard, V. Arumugam, M. Bethermin, J. Bock, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodriguez, A. Cava, P. Chanial, D. L. Clement, A. Conley, A. Cooray, C. D. Dowell, E. Dwek, S. Eale, A. Franceschini, J. Glenn, M. Griffin, E. Hatziminaoglou, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, H. T. Nguyen, B. O'Halloran, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Perez-Fournon, M. Pohlen, D. Rigopoulou, M. Rowan-Robinson, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Steven, M. Symeonidi, M. Tricha, K. E. Tugwell, L. Vigroux, L. Wang, G. Wright, C. K. Xu, M. Zemcov, S. Bardelli, M. Carollo, T. Contini, O. Le Fevre, S. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, and E. Zucca

Subjects
Astrofísica, Active galactic nucleus, Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: active, FOS: Physical sciences, galaxies: starburst, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, galaxies: evolution, galaxies: luminosity function, mass function, cosmology: observations, infrared: galaxies, 01 natural sciences, galaxies [infrared], Luminosity, 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, evolution [galaxies], QB, Luminosity function (astronomy), luminosity function [galaxies], Physics, Luminous infrared galaxy, Supermassive black hole, cosmology: observation, Spiral galaxy, 010308 nuclear & particles physics, starburst [galaxies], Astronomy, Astronomy and Astrophysics, Galaxy, Astronomía, Space and Planetary Science, active [galaxies], Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology]
Abstract

We exploit the deep and extended far infrared data sets (at 70, 100 and 160 um) of the Herschel GTO PACS Evolutionary Probe (PEP) Survey, in combination with the HERschel Multi tiered Extragalactic Survey (HerMES) data at 250, 350 and 500 um, to derive the evolution of the restframe 35 um, 60 um, 90 um, and total infrared (IR) luminosity functions (LFs) up to z~4. We detect very strong luminosity evolution for the total IR LF combined with a density evolution. In agreement with previous findings, the IR luminosity density increases steeply to z~1, then flattens between z~1 and z~3 to decrease at z greater than 3. Galaxies with different SEDs, masses and sSFRs evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to the IR luminosity density. Galaxies occupying the well established SFR/stellar mass main sequence (MS) are found to dominate both the total IR LF and luminosity density at all redshifts, with the contribution from off MS sources (0.6 dex above MS) being nearly constant (~20% of the total IR luminosity density) and showing no significant signs of increase with increasing z over the whole 0.8, Comment: 32 pages, 20 figures, 9 tables. Published in MNRAS. Replaced Fig. 8 (small scaling bug in the previous version)

Published
2013
Full Text
View/download PDF

14. The redshift distribution of dusty star forming galaxies from the SPT survey

Author

T. M. Crawford, Bitten Gullberg, Antony A. Stark, C. M. Bradford, W. B. Everett, John E. Carlstrom, Jingzhe Ma, Anthony H. Gonzalez, C. De Breuck, Christopher D. Fassnacht, R. M. Furstenau, M. L. N. Ashby, K. M. Rotermund, Andrew Nadolski, Julia Kamenetzky, Scott Chapman, M. Bethermin, Yashar D. Hezaveh, M. A. Malkan, Niraj Welikala, M. Strandet, J. S. Spilker, Daniel P. Marrone, Manuel Aravena, Karl M. Menten, K. Litke, Thomas R. Greve, Joaquin Vieira, Eric J. Murphy, J. E. Aguirre, and Axel Weiß

Subjects
Brightness, astro-ph.GA, Strong gravitational lensing, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Physical Chemistry, 01 natural sciences, Submillimeter Array, Atomic, Particle and Plasma Physics, 0103 physical sciences, Nuclear, 010303 astronomy & astrophysics, evolution [galaxies], molecules [ISM], Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, observations [cosmology], early universe, South Pole Telescope, Gravitational lens, 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, Astrophysics::Earth and Planetary Astrophysics, high-redshift [galaxies], Astronomical and Space Sciences, Physical Chemistry (incl. Structural)
Abstract

We use the Atacama Large Millimeter/submillimeter Array (ALMA) in Cycle 1 to determine spectroscopic redshifts of high-redshift dusty star-forming galaxies (DSFGs) selected by their 1.4 mm continuum emission in the South Pole Telescope (SPT) survey. We present ALMA 3 mm spectral scans between 84 and 114 GHz for 15 galaxies and targeted ALMA 1 mm observations for an additional eight sources. Our observations yield 30 new line detections from CO, [C i], [N ii], H_2O and NH_3. We further present Atacama Pathfinder Experiment [C ii] and CO mid-J observations for seven sources for which only a single line was detected in spectral-scan data from ALMA Cycle 0 or Cycle 1. We combine the new observations with previously published and new millimeter/submillimeter line and photometric data of the SPT-selected DSFGs to study their redshift distribution. The combined data yield 39 spectroscopic redshifts from molecular lines, a success rate of >85%. Our sample represents the largest data set of its kind today and has the highest spectroscopic completeness among all redshift surveys of high-z DSFGs. The median of the redshift distribution is z = 3.9 ± 0.4, and the highest-redshift source in our sample is at z = 5.8. We discuss how the selection of our sources affects the redshift distribution, focusing on source brightness, selection wavelength, and strong gravitational lensing. We correct for the effect of gravitational lensing and find the redshift distribution for 1.4 mm selected sources with a median redshift of z = 3.1 ± 0.3. Comparing to redshift distributions selected at shorter wavelengths from the literature, we show that selection wavelength affects the shape of the redshift distribution.

Published
2016
Full Text
View/download PDF

15. The faint end of the 250 μ m luminosity function at z < 0.5

Author

M. Bethermin, L. Wang, Seb Oliver, Cedric G. Lacey, Loretta Dunne, S. J. Maddox, Simon Dye, Peder Norberg, Duncan Farrah, N. Bourne, Marco Viero, Asantha Cooray, Steve Eales, W. I. Cowley, Jon Loveday, and Astronomy

Subjects
submillimeter: galaxies, Astrophysics::High Energy Astrophysical Phenomena, Stacking, HERMES, DUST, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Luminosity, CENSUS, MAPS, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, STRIPE 82, 010303 astronomy & astrophysics, QC, galaxies: statistics, Astrophysics::Galaxy Astrophysics, Density evolution, QB, Luminosity function (astronomy), REDSHIFT SURVEY, Physics, methods: statistical, 010308 nuclear & particles physics, HERSCHEL-ATLAS, Astronomy and Astrophysics, CATALOG, EVOLUTION, Redshift, Galaxy, GALAXIES, galaxies: luminosity function, Distribution function, mass function, Space and Planetary Science, galaxies: abundances, High Energy Physics::Experiment, galaxies: evolution
Abstract

Aims. We aim to study the 250 micron luminosity function (LF) down to much fainter luminosities than achieved by previous efforts. Methods. We developed a modified stacking method to reconstruct the 250 micron LF using optically selected galaxies from the SDSS survey and Herschel maps of the GAMA equatorial fields and Stripe 82. Our stacking method not only recovers the mean 250 micron luminosities of galaxies that are too faint to be individually detected, but also their underlying distribution functions. Results. We find very good agreement with previous measurements in the overlapping luminosity range. More importantly, we are able to derive the LF down to much fainter luminosities (around 25 times fainter) than achieved by previous studies. We find strong positive luminosity evolution \propto (1 + z)^4.89\pm1.07 and moderate negative density evolution \propto (1 + z)^-1.02\pm0.54 over the redshift range z=[0.02, 0.5].

Published
2016
Full Text
View/download PDF

16. A higher efficiency of converting gas to stars push galaxies at z ~ 1.6 well above the star-forming main sequence

Author

E. Daddi, Daizhong Liu, Anton M. Koekemoer, M. Bethermin, Chiara Feruglio, D. Lutz, Masato Onodera, D. B. Sanders, Nobuo Arimoto, M. T. Sargent, Georgios E. Magdis, G. Rodighiero, Tohru Nagao, J. S. Kartaltepe, G. Zamorani, John D. Silverman, Chiara Mancini, S. Berta, W. Rujopakarn, Daichi Kashino, and Alvio Renzini

Subjects
Physics, galaxies: high-redshift, galaxies: ISM, galaxies: star formation, galaxies: starburst, Astronomy and Astrophysics, Space and Planetary Science, Stellar mass, Star formation, Plateau de Bure Interferometer, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy merger, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Stars, Astrophysics of Galaxies (astro-ph.GA), Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

Local starbursts have a higher efficiency of converting gas into stars, as compared to typical star-forming galaxies at a given stellar mass, possibly indicative of different modes of star formation. With the peak epoch of galaxy formation occurring at z > 1, it remains to be established whether such an efficient mode of star formation is occurring at high-redshift. To address this issue, we measure the molecular gas content of seven high-redshift (z ~ 1.6) starburst galaxies with the Atacama Large (sub-)Millimeter Array and IRAM/Plateau de Bure Interferometer. Our targets are selected from the sample of Herschel far-infrared detected galaxies having star formation rates (~300-800 Msolar/yr) elevated (>4x) above the star-forming `main sequence', and included in the FMOS-COSMOS near-infrared spectroscopic survey of star-forming galaxies at z ~ 1.6 with Subaru. We detect CO emission in all cases at high levels of significance, indicative of high gas fractions (~30-50%). Even more compelling, we firmly establish with a clean and systematic selection that starbursts, identified as main-sequence outliers, at high redshift generally have a lower ratio of CO to total infrared luminosity as compared to typical main-sequence star-forming galaxies, although with a smaller offset than expected based on past studies of local starbursts. We put forward a hypothesis that there exists a continuous increase in star formation efficiency with elevation from the main sequence with galaxy mergers as a possible physical driver. Along with a heightened star formation efficiency, our high-redshift sample is similar in other respects to local starbursts such as being metal rich and having a higher ionization state of the interstellar medium., Published in ApJ Letters; 6 pages, 4 figures

Published
2015

17. The 2014 ALMA Long Baseline Campaign: An Overview

Author

ALMA Partnership, E. B. Fomalont, C. Vlahakis, S. Corder, A. Remijan, D. Barkats, R. Lucas, T. R. Hunter, C. L. Brogan, Y. Asaki, S. Matsushita, W. R. F. Dent, R. E. Hills, N. Phillips, A. M. S. Richards, P. Cox, R. Amestica, D. Broguiere, W. Cotton, A. S. Hales, R. Hiriart, A. Hirota, J. A. Hodge, C. M. V. Impellizzeri, J. Kern, R. Kneissl, E. Liuzzo, N. Marcelino, R. Marson, A. Mignano, K. Nakanishi, B. Nikolic, J. E. Perez, L. M. Pérez, I. Toledo, R. Aladro, B. Butler, J. Cortes, P. Cortes, V. Dhawan, J. Di Francesco, D. Espada, F. Galarza, D. Garcia-Appadoo, L. Guzman-Ramirez, E. M. Humphreys, T. Jung, S. Kameno, R. A. Laing, S. Leon, J. Mangum, G. Marconi, H. Nagai, L.-A. Nyman, M. Radiszcz, J. A. Rodón, T. Sawada, S. Takahashi, R. P. J. Tilanus, T. van Kempen, B. Vila Vilaro, L. C. Watson, T. Wiklind, F. Gueth, K. Tatematsu, A. Wootten, A. Castro-Carrizo, E. Chapillon, G. Dumas, I. de Gregorio-Monsalvo, H. Francke, J. Gallardo, J. Garcia, S. Gonzalez, J. E. Hibbard, T. Hill, T. Kaminski, A. Karim, M. Krips, Y. Kurono, C. Lopez, S. Martin, L. Maud, F. Morales, V. Pietu, K. Plarre, G. Schieven, L. Testi, L. Videla, E. Villard, N. Whyborn, M. A. Zwaan, F. Alves, P. Andreani, A. Avison, M. Barta, F. Bedosti, G. J. Bendo, F. Bertoldi, M. Bethermin, A. Biggs, J. Boissier, J. Brand, S. Burkutean, V. Casasola, J. Conway, L. Cortese, B. Dabrowski, T. A. Davis, M. Diaz Trigo, F. Fontani, R. Franco-Hernandez, G. Fuller, R. Galvan Madrid, A. Giannetti, A. Ginsburg, S. F. Graves, E. Hatziminaoglou, M. Hogerheijde, P. Jachym, I. Jimenez Serra, M. Karlicky, P. Klaasen, M. Kraus, D. Kunneriath, C. Lagos, S. Longmore, S. Leurini, M. Maercker, B. Magnelli, I. Marti Vidal, M. Massardi, A. Maury, S. Muehle, S. Muller, T. Muxlow, E. O’Gorman, R. Paladino, D. Petry, J. Pineda, S. Randall, J. S. Richer, A. Rossetti, A. Rushton, K. Rygl, A. Sanchez Monge, R. Schaaf, P. Schilke, T. Stanke, M. Schmalzl, F. Stoehr, S. Urban, E. van Kampen, W. Vlemmings, K. Wang, W. Wild, Y. Yang, S. Iguchi, T. Hasegawa, M. Saito, J. Inatani, N. Mizuno, S. Asayama, G. Kosugi, K.-I. Morita, K. Chiba, S. Kawashima, S. K. Okumura, N. Ohashi, R. Ogasawara, S. Sakamoto, T. Noguchi, Y.-D. Huang, S.-Y. Liu, F. Kemper, P. M. Koch, M.-T. Chen, Y. Chikada, M. Hiramatsu, D. Iono, M. Shimojo, S. Komugi, J. Kim, A.-R. Lyo, E. Muller, C. Herrera, R. E. Miura, J. Ueda, J. Chibueze, Y.-N. Su, A. Trejo-Cruz, K.-S. Wang, H. Kiuchi, N. Ukita, M. Sugimoto, R. Kawabe, M. Hayashi, S. Miyama, P. T. P. Ho, N. Kaifu, M. Ishiguro, A. J. Beasley, S. Bhatnagar, J. A. Braatz III, D. G. Brisbin, N. Brunetti, C. Carilli, J. H. Crossley, L. D’Addario, J. L. Donovan Meyer, D. T. Emerson, A. S. Evans, P. Fisher, K. Golap, D. M. Griffith, A. E. Hale, D. Halstead, E. J. Hardy, M. C. Hatz, M. Holdaway, R. Indebetouw, P. R. Jewell, A. A. Kepley, D.-C. Kim, M. D. Lacy, A. K. Leroy, H. S. Liszt, C. J. Lonsdale, B. Matthews, M. McKinnon, B. S. Mason, G. Moellenbrock, A. Moullet, S. T. Myers, J. Ott, A. B. Peck, J. Pisano, S. J. E. Radford, W. T. Randolph, U. Rao Venkata, M. G. Rawlings, R. Rosen, S. L. Schnee, K. S. Scott, N. K. Sharp, K. Sheth, R. S. Simon, T. Tsutsumi, S. J. Wood, National Radio Astronomy Observatory (NRAO), Joint ALMA Observatory (JAO), European Southern Observatory (ESO)-National Radio Astronomy Observatory (NRAO), Institute for Ethnomedicine, University of Wyoming (UW), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Chimie des métaux de transition et catalyse (CMTC), Centre National de la Recherche Scientifique (CNRS)-Université Louis Pasteur - Strasbourg I, Istituto di Radioastronomia [Bologna] (IRA), Istituto Nazionale di Astrofisica (INAF), Institut Jacques Monod (IJM (UMR_7592)), Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ESO, European Southern Observatory (ESO), Department of Organic and Polymeric Materials, Tokyo Institute of Technology [Tokyo] (TITECH), Biogeochemistry Research Centre, School of Chemistry, Onsala Space Observatory, Chalmers University of Technology [Göteborg], Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), AMOR 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), Departamento de Analisis Matematico, Universidad de Málaga [Málaga] = University of Málaga [Málaga], Unité de recherche Zoologie Forestière (URZF), Institut National de la Recherche Agronomique (INRA), IFP Energies nouvelles (IFPEN), Fastopt GmbH, D-20357 Hamburg, Germany, Mathématiques Appliquées Paris 5 (MAP5 - UMR 8145), Université Paris Descartes - Paris 5 (UPD5)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Centre National de la Recherche Scientifique (CNRS), Departament de Ecologia, Universitat d'Alacant, Centro de Estudios Ambientales del Mediterraneo, INAF - Osservatorio Astrofisico di Arcetri (OAA), Faculty of Medicine, Universidad de Chile = University of Chile [Santiago] (UCHILE), Université Pierre et Marie Curie - Paris 6 (UPMC), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition (ICAN), Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [AP-HP], Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU)-Sorbonne Université (SU), Laboratoire de génie électrique de Paris (LGEP), Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Ecole Supérieure d'Electricité - SUPELEC (FRANCE)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), Max-Planck-Institut für Radioastronomie (MPIFR), Northern Illinois University (NORTHERN ILLINOIS UNIVERSITY), Northern Illinois University, Centre for Astrophysics Research [Hatfield], University of Hertfordshire [Hatfield] (UH), Jodrell Bank Centre for Astrophysics (JBCA), University of Manchester [Manchester], foreign laboratories (FL), CERN [Genève], Departements of Medicine and Microbiology, University of Alabama [Tuscaloosa] (UA), Swinburne University of Technology (Hawthorn campus), San Pedro de Atacama Celestial Explorations (SPACE), San Pedro de Atacama Celestial Explorations, General Electric Medical Systems [Buc] (GE Healthcare), General Electric Medical Systems, Laboratoire de Radiopathologie (LRP), Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de la Santé et de la Recherche Médicale (INSERM), Università degli Studi di Milano [Milano] (UNIMI), Altération génétique des cancers, chimioprévention et réponse thérapeutique, Physikalisches Institut [Köln], Universität zu Köln, Ministère de la santé, National Astronomical Observatory of Japan (NAOJ), National Institute for Materials Science (NIMS), Espaces acoustiques et cognitifs (EAC), Sciences et Technologies de la Musique et du Son (STMS), Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche et Coordination Acoustique/Musique (IRCAM)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Département de Mathématiques et Applications - ENS Paris (DMA), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Department of Chemistry and Biochemistry [Bern], University of Bern, Academia Sinica, Department of Marine Organic Biogeochemistry, Royal Netherlands Institute for Sea Research (NIOZ), Faculty of Geosciences, Utrecht University, Faculty of Geosciences, Brain Mind Institute (BMI - EPFL), Ecole Polytechnique Fédérale de Lausanne (EPFL), Departamento de Ingenieria Eléctrica (DIE), Universidad de Concepción [Chile], Laboratório de Bioinformática, Embrapa Recursos Genéticos e Biotecnologia, Graduate School of Engineering [The Univ of Tokyo] (UTokyo), The University of Tokyo (UTokyo), Kyushu University [Fukuoka], Mitsubishi Research Institute, Inc., Department of Computer Science and Automation [Bangalore] (CSA), Indian Institute of Science [Bangalore] (IISc Bangalore), National Radio Astronomy Observatory [Socorro] (NRAO), Occupational Physiology Laboratory (Vandœuvre-Les -Nancy, France), Computational Science and Engineering Department [Daresbury] (STFC), Science & Technologie Facilities Council, University College of London [London] (UCL), Centre for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong [Australia], Safety science group, Delft University of Technology (TU Delft), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble (CIC-IT Grenoble (CIT803)), CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Grenoble Alpes (UGA), Northern Research Station, Forest Research [Great Britain], Department of Helsinki Institute for Information Technology Communications and Networking, Aalto University, University of Washington [Seattle], Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de la Santé et de la Recherche Médicale (INSERM), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Astronomy, Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Research Unit on Cardiovascular and Metabolic Diseases (ICAN), Università degli Studi di Milano = University of Milan (UNIMI), Universität zu Köln = University of Cologne, Universidad de Concepción - University of Concepcion [Chile], Kyushu University, Istituto di Radioastronomia (IRA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Universidad de Málaga [Málaga], Unité de recherche Zoologie Forestière (UZF), Science et Technologie du Lait et de l'Oeuf (STLO), Institut National de la Recherche Agronomique (INRA)-AGROCAMPUS OUEST, Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions (INSMI)-Université Paris Descartes - Paris 5 (UPD5), University of Chile [Santiago], Université Pierre et Marie Curie - Paris 6 (UPMC)-Assistance publique - Hôpitaux de Paris (AP-HP) (APHP)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Pitié-Salpêtrière [APHP], Université Paris-Sud - Paris 11 (UP11)-Université Pierre et Marie Curie - Paris 6 (UPMC)-SUPELEC-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), Jodrell Bank Centre for Astrophysics, School of Physics, Università degli studi di Milano [Milano], National Institute of Materials Science, Equipe Espaces acoustiques et cognitifs, Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-IRCAM-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS), Department of Chemistry and Biochemistry, Graduate School of Engineering [Tokyo], The University of Tokyo, Center for Atmospheric Chemistry [Wollongong] (CAC), University of Wollongong, CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM)-Université Joseph Fourier - Grenoble 1 (UJF), Forest Research, Sorbonne Université (SU)-Assistance publique - Hôpitaux de Paris (AP-HP) (AP-HP)-Sorbonne Université (SU), École normale supérieure - Paris (ENS Paris), Université Grenoble Alpes (UGA)-Institut National de la Santé et de la Recherche Médicale (INSERM)-CHU Grenoble, Joint ALMA Office (JAO), ALMA, Institut Jacques Monod (IJM), Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Mathématiques et de leurs Interactions-Université Paris Descartes - Paris 5 (UPD5), ALMA Observatory, Laboratoire d'analyse et d'architecture des systèmes [Toulouse] (LAAS), Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UPS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Institut National Polytechnique [Toulouse] (INP), Center for Brain Simulation, Ecole Polytechnique Fédérale de Lausanne, Université Joseph Fourier - Grenoble 1 (UJF)-CHU Grenoble-Institut National de la Santé et de la Recherche Médicale (INSERM), National Radio Astronomy Observatory ( NRAO ), Joint ALMA Office ( JAO ), University of Wyoming ( UW ), Max-Planck-Institut für Astronomie ( MPIA ), Chimie des métaux de transition et catalyse ( CMTC ), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique ( CNRS ), Istituto di Radioastronomia ( IRA ), Istituto Nazionale di Astrofisica ( INAF ), Institut Jacques Monod ( IJM ), Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), European Southern Observatory ( ESO ), Tokyo Institute of Technology [Tokyo] ( TITECH ), Institut de RadioAstronomie Millimétrique ( IRAM ), 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 national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ), Unité de recherche Zoologie Forestière ( UZF ), Institut National de la Recherche Agronomique ( INRA ), IFP Energies nouvelles ( IFPEN ), Science et Technologie du Lait et de l'Oeuf ( STLO ), Institut National de la Recherche Agronomique ( INRA ) -AGROCAMPUS OUEST, Mathématiques Appliquées à Paris 5 ( MAP5 - UMR 8145 ), Université Paris Descartes - Paris 5 ( UPD5 ) -Institut National des Sciences Mathématiques et de leurs Interactions-Centre National de la Recherche Scientifique ( CNRS ), INAF - Osservatorio Astrofisico di Arcetri ( OAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ), Unité de Recherche sur les Maladies Cardiovasculaires, du Métabolisme et de la Nutrition = Institute of cardiometabolism and nutrition ( ICAN ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Assistance publique - Hôpitaux de Paris (AP-HP)-Institut National de la Santé et de la Recherche Médicale ( INSERM ) -CHU Pitié-Salpêtrière [APHP], Laboratoire de génie électrique de Paris ( LGEP ), Université Paris-Sud - Paris 11 ( UP11 ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -SUPELEC-Centre National de la Recherche Scientifique ( CNRS ), Czech Academy of Sciences [Prague] ( ASCR ), Max-Planck-Institut für Radioastronomie ( MPIFR ), Northern Illinois University ( NORTHERN ILLINOIS UNIVERSITY ), Canadian Space Agency, foreign laboratories ( FL ), University of Alabama [Tuscaloosa] ( UA ), San Pedro de Atacama Celestial Explorations ( SPACE ), General Electric Medical Systems [Buc] ( GE Healthcare ), Laboratoire de Radiopathologie ( LRP ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ), Max Planck Institute for Biochemistry, Max-Planck-Institut, Department of Virology, Global COE Program, Nagasaki University-Institute of Tropical Medicine, Sciences et Technologies de la Musique et du Son ( STMS ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -IRCAM-Centre National de la Recherche Scientifique ( CNRS ), Département de Mathématiques et Applications - ENS Paris ( DMA ), École normale supérieure - Paris ( ENS Paris ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'analyse et d'architecture des systèmes [Toulouse] ( LAAS ), Centre National de la Recherche Scientifique ( CNRS ) -Université Toulouse III - Paul Sabatier ( UPS ), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut National des Sciences Appliquées - Toulouse ( INSA Toulouse ), Institut National des Sciences Appliquées ( INSA ) -Institut National des Sciences Appliquées ( INSA ) -Institut National Polytechnique [Toulouse] ( INP ), Royal Netherlands Institute for Sea Research ( NIOZ ), Departamento de Ingenieria Eléctrica ( DIE ), AUTRES, Department of Computer Science and Automation [Bangalore] ( CSA ), Indian Institute of Science [Bangalore] ( IISc Bangalore ), National Radio Astronomy Observatory [Socorro] ( NRAO ), Computational Science and Engineering Department [Daresbury] ( STFC ), University College of London [London] ( UCL ), Center for Atmospheric Chemistry [Wollongong] ( CAC ), Delft University of Technology ( TU Delft ), Service Hématologie, Hôpital Morvan [Brest]-Centre Hospitalier Régional Universitaire de Brest ( CHRU Brest ), Centre d'Investigation Clinique - Innovation Technologique - INSERM - CHU de Grenoble ( CIC-IT Grenoble (CIT803) ), and Université Joseph Fourier - Grenoble 1 ( UJF ) -Institut National de la Santé et de la Recherche Médicale ( INSERM ) -Centre Hospitalier Universitaire de Grenoble

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], techniques: high angular resolution, Astronomy and Astrophysics, submillimeter: general, telescopes, Submillimeter Array, [ SDU.ASTR.CO ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Space and Planetary Science, techniques: interferometric, Environmental science, Millimeter, Baseline (configuration management), instrumentation: interferometers, QB, Remote sensing
Abstract

著者人数: 248名, Accepted: 2015-04-10, 資料番号: SA1150145000

Published
2015
Full Text
View/download PDF

18. ISM Properties of a Massive Dusty Star-forming Galaxy Discovered at z ∼ 7

Author

Yashar D. Hezaveh, Manuel Aravena, M. Bethermin, Christopher C. Hayward, Timothy R. Miller, C. De Breuck, John E. Carlstrom, Anthony H. Gonzalez, M. Strandet, Jingzhe Ma, Karl M. Menten, Kedar A. Phadke, J. S. Spilker, K. Litke, Chian-Chou Chen, M. L. N. Ashby, Joaquin Vieira, K. M. Rotermund, C. M. Bradford, Eric J. Murphy, Bitten Gullberg, D. Narayanan, Scott Chapman, Daniel P. Marrone, D. J. M. Cunningham, Christopher D. Fassnacht, Thomas R. Greve, M. A. Malkan, Axel Weiß, J. Sreevani, Matt Bothwell, 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), California Institute of Technology (CALTECH), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, 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), Centre for Fusion Space and Astrophysics [Coventry] (CFSA), University of Warwick [Coventry], AUTRES, Niels Bohr Institute [Copenhagen] (NBI), Faculty of Science [Copenhagen], University of Copenhagen = Københavns Universitet (UCPH)-University of Copenhagen = Københavns Universitet (UCPH), Millimeter and Submillimeter Astronomy, Max-Planck-Institut für Radioastronomie (MPIFR), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Smithsonian Institution-Harvard University [Cambridge], 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), and University of Copenhagen = Københavns Universitet (KU)-University of Copenhagen = Københavns Universitet (KU)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], astro-ph.GA, FOS: Physical sciences, Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Photometry (optics), 0103 physical sciences, Radiative transfer, 010303 astronomy & astrophysics, Reionization, Physics, 010308 nuclear & particles physics, Star formation, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, early universe, Redshift, Galaxy, Interstellar medium, South Pole Telescope, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], star formation [galaxies], high-redshift [galaxies], Astronomical and Space Sciences
Abstract

We report the discovery and constrain the physical conditions of the interstellar medium of the highest-redshift millimeter-selected dusty star-forming galaxy (DSFG) to date, SPT-S J031132-5823.4 (hereafter SPT0311-58), at $z=6.900 +/- 0.002$. SPT0311-58 was discovered via its 1.4mm thermal dust continuum emission in the South Pole Telescope (SPT)-SZ survey. The spectroscopic redshift was determined through an ALMA 3mm frequency scan that detected CO(6-5), CO(7-6) and [CI](2-1), and subsequently confirmed by detections of CO(3-2) with ATCA and [CII] with APEX. We constrain the properties of the ISM in SPT0311-58 with a radiative transfer analysis of the dust continuum photometry and the CO and [CI] line emission. This allows us to determine the gas content without ad hoc assumptions about gas mass scaling factors. SPT0311-58 is extremely massive, with an intrinsic gas mass of $M_{\rm gas} = 3.3 \pm 1.9 \times10^{11}\,M_{\odot}$. Its large mass and intense star formation is very rare for a source well into the Epoch of Reionization., Accepted by ApJL, Fixed compilation problem in v.2

Published
2017
Full Text
View/download PDF

19. The evolution of the dust temperatures of galaxies in the SFR-M plane up to z sim 2

Author

E. Le Floc'h, S. Berta, Alex Conley, H. Aussel, P. Andreani, David J. Rosario, E. Daddi, Rob Ivison, N. M. Förster Schreiber, G. Rodighiero, A. Cimatti, Eckhard Sturm, I. Valtchanov, P. Popesso, M. J. Page, Linda J. Tacconi, S. J. Oliver, L. Wang, Georgios E. Magdis, Francesca Pozzi, P. Santini, L. Riguccini, Benjamin Magnelli, Amelie Saintonge, M. Sánchez-Portal, D. Elbaz, J. J. Bock, Isaac Roseboom, Dieter Lutz, Bruno Altieri, Albrecht Poglitsch, Douglas Scott, Roberto Maiolino, Ángel Bongiovanni, Stijn Wuyts, M. Bethermin, J. Cepa, Raanan Nordon, M. Symeonidis, A. M. Pérez García, R. Genzel, Magnelli, B., Lutz, D., Saintonge, A., Berta, S., Santini, P., Symeonidis, M., Altieri, B., Andreani, P., Aussel, H., Béthermin, M., Bock, J., Bongiovanni, A., Cepa, J., Cimatti, A., Conley, A., Daddi, E., Elbaz, D., Förster Schreiber, N. M., Genzel, R., Ivison, R. J., Le Floc'h, E., Magdis, G., Maiolino, R., Nordon, R., Oliver, S. J., Page, M., Pérez García, A., Poglitsch, A., Popesso, P., Pozzi, F., Riguccini, L., Rodighiero, G., Rosario, D., Roseboom, I., Sanchez-Portal, M., Scott, D., Sturm, E., Tacconi, L. J., Valtchanov, I., Wang, L., and Wuyts, S

Subjects
Physics, 010308 nuclear & particles physics, Plane (geometry), Infrared, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, Redshift, Space observatory, Galaxy, galaxies: evolution, infrared: galaxies, galaxies: starburst, QB0460, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, evolution, infrared: galaxies, galaxies: starburst [galaxies], Astrophysics::Galaxy Astrophysics
Abstract

We study the evolution of the dust temperature of galaxies in the SFR− M∗ plane up to z ~ 2 using far-infrared and submillimetre observations from the Herschel Space Observatory taken as part of the PACS Evolutionary Probe (PEP) and Herschel Multi-tiered Extragalactic Survey (HerMES) guaranteed time key programmes. Starting from a sample of galaxies with reliable star-formation rates (SFRs), stellar masses (M_∗) and redshift estimates, we grid the SFR− M_∗parameter space in several redshift ranges and estimate the mean dust temperature (T_(dust)) of each SFR–M_∗ − z bin. Dust temperatures are inferred using the stacked far-infrared flux densities (100–500 μm) of our SFR–M_∗ − z bins. At all redshifts, the dust temperature of galaxies smoothly increases with rest-frame infrared luminosities (L_(IR)), specific SFRs (SSFR; i.e., SFR/M_∗), and distances with respect to the main sequence (MS) of the SFR− M_∗ plane (i.e., Δlog (SSFR)_(MS) = log [SSFR(galaxy)/SSFR_(MS)(M_∗,z)]). The T_(dust) − SSFR and T_(dust) − Δlog (SSFR)_(MS) correlations are statistically much more significant than the T_(dust) − LIR one. While the slopes of these three correlations are redshift-independent, their normalisations evolve smoothly from z = 0 and z ~ 2. We convert these results into a recipe to derive T_(dust) from SFR, M_∗ and z, valid out to z ~ 2 and for the stellar mass and SFR range covered by our stacking analysis. The existence of a strong T_(dust) − Δlog (SSFR)_(MS) correlation provides us with several pieces of information on the dust and gas content of galaxies. Firstly, the slope of the T_(dust) − Δlog (SSFR)_(MS) correlation can be explained by the increase in the star-formation efficiency (SFE; SFR/M_(gas)) with Δlog (SSFR)_(MS) as found locally by molecular gas studies. Secondly, at fixed Δlog (SSFR)_(MS), the constant dust temperature observed in galaxies probing wide ranges in SFR and M_∗ can be explained by an increase or decrease in the number of star-forming regions with comparable SFE enclosed in them. And thirdly, at high redshift, the normalisation towards hotter dust temperature of the T_(dust) − Δlog (SSFR)_(MS) correlation can be explained by the decrease in the metallicities of galaxies or by the increase in the SFE of MS galaxies. All these results support the hypothesis that the conditions prevailing in the star-forming regions of MS and far-above-MS galaxies are different. MS galaxies have star-forming regions with low SFEs and thus cold dust, while galaxies situated far above the MS seem to be in a starbursting phase characterised by star-forming regions with high SFEs and thus hot dust.

Published
2014
Full Text
View/download PDF

20. Herschel reveals the obscured star formation in HiZELS H\xa0 emitters at z = 1.47

Author

E. Ibar, D. Sobral, P. N. Best, R. J. Ivison, I. Smail, V. Arumugam, S. Berta, M. Bethermin, J. Bock, A. Cava, A. Conley, D. Farrah, J. Geach, S. Ikarashi, K. Kohno, E. Le Floc'h, D. Lutz, G. Magdis, B. Magnelli, G. Marsden, S. J. Oliver, M. J. Page, F. Pozzi, L. Riguccini, B. Schulz, N. Seymour, A. J. Smith, M. Symeonidis, L. Wang, J. Wardlow, and M. Zemcov

Published
2013

22. Erratum: The Herschel PEP/HerMES Luminosity Function - I. Probing the Evolution of PACS selected Galaxies to z = 4

Author

P. Chania, G. Mainetti, M. Bethermin, I. Ṕerez-Fournon, Matthew Joseph Griffin, L. Vigroux, H. Aussel, J. J. Bock, Andreas Papageorgiou, Vincenzo Mainieri, Anthony J. Smith, A. Conley, Benjamin Magnelli, Bruno Altieri, Asantha Cooray, Marcella Carollo, Raanan Nordon, V. Buat, Linda J. Tacconi, V. Arumugam, B. O'Halloran, E. Ibar, Alberto Franceschini, Alexandre Amblard, Francesca Pozzi, S. Bardelli, David J. Rosario, Bruno Maffei, Dimitra Rigopoulou, Mattia Vaccari, G. Wright, K. G. Isaak, Simon J. Lilly, Lucia Marchetti, Dieter Lutz, S. Berta, Ángel Bongiovanni, Albrecht Poglitsch, Michael Rowan-Robinson, I. Valtchanov, Alvaro Iribarrem, E. Zucca, Michael Pohlen, C. K. Xu, Marco Scodeggio, P. Popesso, Guilaine Lagache, G. Rodighiero, Thierry Contini, M. J. Page, Emanuele Daddi, Eckhard Sturm, Roberto Maiolino, S. C. Madden, N. M. Förster Schreiber, Jason Glenn, E. Le Floc'h, David L. Shupe, Lucia Pozzetti, Michael Zemcov, Alvio Renzini, M. Magliocchetti, Eli Dwek, N. Castro-Rodŕlguez, Douglas Scott, Louis Levenson, C. D. Dowell, R. Genzel, D. Elbaz, Nick Seymour, Rob Ivison, Jamie Stevens, Andrea Cimatti, Antonio Cava, Evanthia Hatziminaoglou, H. T. Nguyen, Nanyao Y. Lu, M. Symeonidis, Paola Andreani, Alessandro Boselli, O. Le Fevre, K. E. Tugwell, L. Riguccini, P. Panuzzo, A. Ṕerez Garćla, G. Zamorani, Chris Pearson, M. Sánchez-Portal, David L. Clements, Steve Eales, Denis Burgarella, L. Monaco, Ivan Delvecchio, J. Cepa, H. Doḿlnguez-Śanchez, M. T. Sargent, Benjamin L. Schulz, S. J. Oliver, Lian-Tao Wang, Carlotta Gruppioni, Isaac Roseboom, Markos Trichas, and O. Ilbert

Subjects
Luminous infrared galaxy, Physics, Radio galaxy, Física atmosférica, Astronomy, Astronomy and Astrophysics, Astrophysics, Disc galaxy, Galaxy, Space and Planetary Science, Galaxy group, Galaxy formation and evolution, Elliptical galaxy, Luminosity function (astronomy)
Abstract

This is an erratum to the paper ‘The Herschel PEP/HerMES Luminosity Function – I: Probing the Evolution of PACS selected Galaxies to z ≃ 4’, by Gruppioni et al., published in MNRAS, 432, 23 (2013).

Published
2013

23. Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density

Author

V. Buat, Duncan Farrah, M. J. Page, Francesca Pozzi, Asantha Cooray, Raanan Nordon, James Dunlop, S. J. Oliver, Benjamin Magnelli, Denis Burgarella, S. Berta, E. Le Floc'h, D. Lutz, Sebastien Heinis, P. Popesso, L. Riguccini, Marco Viero, Carlotta Gruppioni, Alberto Franceschini, Mattia Vaccari, O. Cucciati, M. Bethermin, J. J. Bock, 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), INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), 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), D. Burgarella, V. Buat, C. Gruppioni, O. Cucciati, S. Heini, S. Berta, M. Béthermin, J. Bock, A. Cooray, J. S. Dunlop, D. Farrah, A. Franceschini, E. Le Floc’h, D. Lutz, B. Magnelli, R. Nordon, S. J. Oliver, M. J. Page, P. Popesso, F. Pozzi, L. Riguccini, M. Vaccari, M. Viero, 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)), and 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)

Subjects
Stellar mass, media_common.quotation_subject, galaxies: starburst, Astrophysics, Plateau (mathematics), 01 natural sciences, infrared: galaxies, 0103 physical sciences, 010303 astronomy & astrophysics, media_common, Physics, cosmology: observation, 010308 nuclear & particles physics, Star formation, Attenuation, infrared: galaxie, Astronomy and Astrophysics, early Universe, Redshift, Galaxy, Universe, Space and Planetary Science, Homogeneous, galaxies: star formation, cosmology: observations, ultraviolet: galaxies, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we were able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). By integrating SFRDTOT, we followed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing a complete view of star formation from the local Universe to z ~ 4 and, using assumptions on earlier star formation history, compares this evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formation in galaxies. Our main conclusions are that: 1) the dust attenuation AFUV is found to increase from z = 0 to z ~ 1.2 and then starts to decrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z ~ 2. At z > 2, we observe either a plateau or a small increase up to z ~ 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRDTOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) using assumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3.6 to zform = 10, we integrated SFRDTOT and obtained a good agreement with the published SMDs.

Published
2013
Full Text
View/download PDF

24. Connecting stellar mass and star-formation rate to dark matter halo mass out to z ~ 2

Author

M. Bethermin, G. Marsden, Rob Ivison, Duncan Farrah, Marco Viero, Asantha Cooray, S. J. Oliver, E. Ibar, A. Amblard, Michael Zemcov, Lingyu Wang, Mark Halpern, Sebastien Heinis, Michael Rowan-Robinson, Austin Smith, Isaac Roseboom, J. J. Bock, O. Ilbert, Benjamin L. Schulz, and Alex Conley

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Accretion (astrophysics), Redshift, Dark matter halo, Space and Planetary Science, 0103 physical sciences, Elliptical galaxy, Astrophysics::Solar and Stellar Astrophysics, Halo, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We have constructed an extended halo model (EHM) which relates the total stellar mass and star-formation rate (SFR) to halo mass (M_h). An empirical relation between the distribution functions of total stellar mass of galaxies and host halo mass, tuned to match the spatial density of galaxies over 0, Comment: 15 pages, 12 figures, accepted for publication in MNRAS

Published
2012

25. HerMES: deep number counts at 250 μm, 350 μm and 500 μm in the COSMOS and GOODS-N fields and the build-up of the cosmic infrared background

Author

G. Marsden, A. Amblard, A. Omont, D. L. Clements, S. Berta, Andrew Smith, Rob Ivison, Sebastien Heinis, Steve Eales, J. Kartaltepe, Lucia Marchetti, Michael Rowan-Robinson, S. J. Oliver, Joaquin Vieira, Matthew Joseph Griffin, Louis Levenson, H. T. Nguyen, G. Lagache, Asantha Cooray, M. Bethermin, M. Pohlen, Marco Viero, K. E. Tugwell, E. Ibar, Duncan Farrah, Michael Zemcov, J. J. Bock, Andreas Papageorgiou, M. Symeonidis, Evanthia Hatziminaoglou, Douglas Scott, A. Boselli, N. Castro-Rodriguez, V. Arumugam, V. Buat, Mara Salvato, Benjamin L. Schulz, Alberto Franceschini, Mattia Vaccari, C. K. Xu, Chris Pearson, Georgios E. Magdis, D. Rigopoulou, Jason Glenn, I. Perez-Fournon, M. J. Page, Isaac Roseboom, David L. Shupe, Lingyu Wang, B. O'Halloran, Antonio Cava, O. Ilbert, I. Valtchanov, P. Panuzzo, Caitlin M. Casey, C. D. Dowell, Nick Seymour, Alex Conley, H. Aussel, M. Trichas, E. Le Floc'h, 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), 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), Center for Astrophysics and Space Astronomy [Boulder] (CASA), University of Colorado [Boulder], NASA Ames Research Center (ARC), Max-Planck-Institut für Extraterrestrische Physik (MPE), Computing and Mathematical Sciences [Pasadena]], California Institute of Technology (CALTECH), Dipartimento di Astronomia [Padova], Universita degli Studi di Padova, School of Physics and Astronomy [Cardiff], Cardiff University, AUTRES, Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, UPGAL, European Project: 240039,EC:FP7:ERC,ERC-2009-StG,UPGAL(2009), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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), 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), Royal Observatory Edinburgh (ROE), University of Edinburgh, University of Hawai'i [Honolulu] (UH), Instituto de Astrofisica de Canarias (IAC), Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Imperial College London, University of California [Irvine] (UC Irvine), University of California (UC), Caltech Department of Astronomy [Pasadena], Astronomy Centre, University of Sussex, Università degli Studi di Padova = University of Padua (Unipd), European Southern Observatory (ESO), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica e Astronomia 'Galileo Galilei', University of British Columbia (UBC), Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), 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), University of Lethbridge, Max Planck Institute for Extraterrestrial Physics (MPE), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, Agence Spatiale Européenne = European Space Agency (ESA), and Dipartimento di Astronomia

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Redshift, Galaxy, Spire, Space and Planetary Science, Cosmic infrared background, 0103 physical sciences, Galaxy formation and evolution, Source counts, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Photometric redshift, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

ABRIGED Herschel/SPIRE has provided confusion limited maps of deep fields at 250, 350, and 500um, as part of the HerMES survey. Due to confusion, only a small fraction of the Cosmic Infrared Background can be resolved into individually-detected sources. Our goal is to produce deep galaxy number counts and redshift distributions below the confusion limit, which we then use to place strong constraints on the origins of the cosmic infrared background and on models of galaxy evolution. We individually extracted the bright SPIRE with a method using the positions, the flux densities, and the redshifts of the 24um sources as a prior, and derived the number counts and redshift distributions of the bright SPIRE sources. For fainter SPIRE sources, we reconstructed the number counts and the redshift distribution below the confusion limit using the deep 24um catalogs associated with photometric redshift and information provided by the stacking of these sources into the deep SPIRE maps. Finally, by integrating all these counts, we studied the contribution of the galaxies to the CIB as a function of their flux density and redshift. Through stacking, we managed to reconstruct the source counts per redshift slice down to ~2 mJy in the three SPIRE bands, which lies about a factor 10 below the 5sigma confusion limit. None of the pre-existing population models are able to reproduce our results at better than 3sigma. Finally, we extrapolate our counts to zero flux density in order to derive an estimate of the total contribution of galaxies to the CIB, finding 10.1, 6.5, and 2.8 nW/m2/sr at 250, 350, and 500um, respectively. These values agree well with FIRAS absolute measurements, suggesting our number counts and their extrapolation are sufficient to explain the CIB. Finally, combining our results with other works, we estimate the energy budget contained in the CIB between 8 and 1000um: 26 nW/m2/sr., 25 pages, 17 figures, 15 tables, accepted by A&A, bug with Fig. 3 fixed

Published
2012
Full Text
View/download PDF

26. Planck intermediate results VII. Statistical properties of infrared and radio extragalactic sources from the Planck Early Release Compact Source Catalogue at frequencies between 100 and 857 GHz

Author

Collaboration, P, Ade, P, Aghanim, N, Argueso, F, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Balbi, A, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Bhatia, R, Bonaldi, A, Bond, J, Borrill, J, Bouchet, F, Burigana, C, Cabella, P, Cardoso, J, Catalano, A, Cayon, L, Chamballu, A, Chary, R, Chen, X, Chiang, L, Christensen, P, Clements, D, Colafrancesco, S, Colombi, S, Colombo, L, Coulais, A, Crill, B, Cuttaia, F, Danese, L, Davis, R, De Bernardis, P, De Gasperis, G, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Dorl, U, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Finelli, F, Forni, O, Fosalba, P, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Hansen, F, Harrison, D, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Jaffe, T, Jaffe, A, Jagemann, T, Jones, W, Juvela, M, Keihanen, E, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurinsky, N, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Lilje, P, Lopez-Caniego, M, Macias-Perez, J, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Mitra, S, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Nørgaard-Nielsen, H, Norgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rowan-Robinson, M, Rubino-Martin, J, Rusholme, B, Sajina, A, Sandri, M, Savini, G, Scott, D, Smoot, G, Starck, J, Sudiwala, R, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Turler, M, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, White, M, Yvon, D, Zacchei, A, Zonca, A, Planck Collaboration, P.A.R. Ade, N. Aghanim, F. Argueso, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A.J. Banday, R.B. Barreiro, E. Battaner, K. Benabed, A. Benoit, J.P. Bernard, M. Bersanelli, M. Bethermin, R. Bhatia, A. Bonaldi, J.R. Bond, J. Borrill, F.R. Bouchet, C. Burigana, P. Cabella, J.F. Cardoso, A. Catalano, L. Cayon, A. Chamballu, R.R. Chary, X. Chen, L.Y. Chiang, P.R. Christensen, D.L. Clements, S. Colafrancesco, S. Colombi, L.P.L. Colombo, A. Coulais, B.P. Crill, F. Cuttaia, L. Danese, R.J. Davis, Paolo De Bernardis, G. De Gasperis, G. De Zotti, J. Delabrouille, C. Dickinson, J.M. Diego, H. Dole, S. Donzelli, O. Dore, U. Dorl, M. Douspis, X. Dupac, G. Efstathiou, T.A. Ensslin, H.K. Eriksen, F. Finelli, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, G. Giardino, Y. Giraud-Heraud, J. Gonzalez-Nuevo, K.M. Gorski, A. Gregorio, A. Gruppuso, F.K. Hansen, D. Harrison, S. Henrot-Versille, C. Hernandez-Monteagudo, D. Herranz, S.R. Hildebrandt, E. Hivon, M. Hobson, W.A. Holmes, T.R. Jaffe, A.H. Jaffe, T. Jagemann, W.C. Jones, M. Juvela, E. Keihanen, T.S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, N. Kurinsky, H. Kurki-Suonio, G. Lagache, A. Lahteenmaki, J.M. Lamarre, A. Lasenby, C.R. Lawrence, R. Leonardi, P.B. Lilje, M. Lopez-Caniego, J.F. Macias-Perez, D. Maino, N. Mandolesi, M. Maris, D.J. Marshall, E. Martinez-Gonzalez, Silvia Masi, M. Massardi, S. Matarrese, P. Mazzotta, Alessandro Melchiorri, L. Mendes, A. Mennella, S. Mitra, M.A. Miville-Deschenes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J.A. Murphy, P. Naselsky, Federico Nati, P. Natoli, H.U. Nørgaard-Nielsen, H.U. Norgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, Francesco Piacentini, M. Piat, E. Pierpaoli, S. Plaszczynski, E. Pointecouteau, Gianluca Polenta, N. Ponthieu, L. Popa, T. Poutanen, G.W. Pratt, S. Prunet, J.L. Puget, J.P. Rachen, W.T. Reach, R. Rebolo, M. Reinecke, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, M. Rowan-Robinson, J.A. Rubino-Martin, B. Rusholme, A. Sajina, M. Sandri, Giorgio Savini, D. Scott, G.F. Smoot, J.L. Starck, R. Sudiwala, A.S. Suur-Uski, J.F. Sygnet, J.A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, M. Turler, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L.A. Wade, B.D. Wandelt, M. White, D. Yvon, A. Zacchei, A. Zonca, Collaboration, P, Ade, P, Aghanim, N, Argueso, F, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Balbi, A, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Bhatia, R, Bonaldi, A, Bond, J, Borrill, J, Bouchet, F, Burigana, C, Cabella, P, Cardoso, J, Catalano, A, Cayon, L, Chamballu, A, Chary, R, Chen, X, Chiang, L, Christensen, P, Clements, D, Colafrancesco, S, Colombi, S, Colombo, L, Coulais, A, Crill, B, Cuttaia, F, Danese, L, Davis, R, De Bernardis, P, De Gasperis, G, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Dorl, U, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Finelli, F, Forni, O, Fosalba, P, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Hansen, F, Harrison, D, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Jaffe, T, Jaffe, A, Jagemann, T, Jones, W, Juvela, M, Keihanen, E, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurinsky, N, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Lilje, P, Lopez-Caniego, M, Macias-Perez, J, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Mitra, S, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Nørgaard-Nielsen, H, Norgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rowan-Robinson, M, Rubino-Martin, J, Rusholme, B, Sajina, A, Sandri, M, Savini, G, Scott, D, Smoot, G, Starck, J, Sudiwala, R, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Turler, M, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, White, M, Yvon, D, Zacchei, A, Zonca, A, Planck Collaboration, P.A.R. Ade, N. Aghanim, F. Argueso, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. Balbi, A.J. Banday, R.B. Barreiro, E. Battaner, K. Benabed, A. Benoit, J.P. Bernard, M. Bersanelli, M. Bethermin, R. Bhatia, A. Bonaldi, J.R. Bond, J. Borrill, F.R. Bouchet, C. Burigana, P. Cabella, J.F. Cardoso, A. Catalano, L. Cayon, A. Chamballu, R.R. Chary, X. Chen, L.Y. Chiang, P.R. Christensen, D.L. Clements, S. Colafrancesco, S. Colombi, L.P.L. Colombo, A. Coulais, B.P. Crill, F. Cuttaia, L. Danese, R.J. Davis, Paolo De Bernardis, G. De Gasperis, G. De Zotti, J. Delabrouille, C. Dickinson, J.M. Diego, H. Dole, S. Donzelli, O. Dore, U. Dorl, M. Douspis, X. Dupac, G. Efstathiou, T.A. Ensslin, H.K. Eriksen, F. Finelli, O. Forni, P. Fosalba, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, G. Giardino, Y. Giraud-Heraud, J. Gonzalez-Nuevo, K.M. Gorski, A. Gregorio, A. Gruppuso, F.K. Hansen, D. Harrison, S. Henrot-Versille, C. Hernandez-Monteagudo, D. Herranz, S.R. Hildebrandt, E. Hivon, M. Hobson, W.A. Holmes, T.R. Jaffe, A.H. Jaffe, T. Jagemann, W.C. Jones, M. Juvela, E. Keihanen, T.S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, N. Kurinsky, H. Kurki-Suonio, G. Lagache, A. Lahteenmaki, J.M. Lamarre, A. Lasenby, C.R. Lawrence, R. Leonardi, P.B. Lilje, M. Lopez-Caniego, J.F. Macias-Perez, D. Maino, N. Mandolesi, M. Maris, D.J. Marshall, E. Martinez-Gonzalez, Silvia Masi, M. Massardi, S. Matarrese, P. Mazzotta, Alessandro Melchiorri, L. Mendes, A. Mennella, S. Mitra, M.A. Miville-Deschenes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J.A. Murphy, P. Naselsky, Federico Nati, P. Natoli, H.U. Nørgaard-Nielsen, H.U. Norgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, F. Pajot, R. Paladini, D. Paoletti, B. Partridge, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, Francesco Piacentini, M. Piat, E. Pierpaoli, S. Plaszczynski, E. Pointecouteau, Gianluca Polenta, N. Ponthieu, L. Popa, T. Poutanen, G.W. Pratt, S. Prunet, J.L. Puget, J.P. Rachen, W.T. Reach, R. Rebolo, M. Reinecke, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, M. Rowan-Robinson, J.A. Rubino-Martin, B. Rusholme, A. Sajina, M. Sandri, Giorgio Savini, D. Scott, G.F. Smoot, J.L. Starck, R. Sudiwala, A.S. Suur-Uski, J.F. Sygnet, J.A. Tauber, L. Terenzi, L. Toffolatti, M. Tomasi, M. Tristram, M. Tucci, M. Turler, L. Valenziano, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L.A. Wade, B.D. Wandelt, M. White, D. Yvon, A. Zacchei, and A. Zonca

Abstract

We make use of the Planck all-sky survey to derive number counts and spectral indices of extragalactic sources - infrared and radio sources - from the Planck Early Release Compact Source Catalogue (ERCSC) at 100 to 857 GHz (3mm to 350 mu m). Three zones (deep, medium and shallow) of approximately homogeneous coverage are used to permit a clean and controlled correction for incompleteness, which was explicitly not done for the ERCSC, as it was aimed at providing lists of sources to be followed up. Our sample, prior to the 80% completeness cut, contains between 217 sources at 100 GHz and 1058 sources at 857 GHz over about 12 800 to 16 550 deg(2) (31 to 40% of the sky). After the 80% completeness cut, between 122 and 452 and sources remain, with flux densities above 0.3 and 1.9 Jy at 100 and 857 GHz. The sample so defined can be used for statistical analysis. Using the multi-frequency coverage of the Planck High Frequency Instrument, all the sources have been classified as either dust-dominated (infrared galaxies) or synchrotron-dominated (radio galaxies) on the basis of their spectral energy distributions (SED). Our sample is thus complete, flux-limited and color-selected to differentiate between the two populations. We find an approximately equal number of synchrotron and dusty sources between 217 and 353 GHz; at 353 GHz or higher (or 217 GHz and lower) frequencies, the number is dominated by dusty (synchrotron) sources, as expected. For most of the sources, the spectral indices are also derived. We provide for the first time counts of bright sources from 353 to 857 GHz and the contributions from dusty and synchrotron sources at all HFI frequencies in the key spectral range where these spectra are crossing. The observed counts are in the Euclidean regime. The number counts are compared to previously published data (from earlier Planck results, Herschel, BLAST, SCUBA, LABOCA, SPT, and ACT) and models taking into account both radio or infrared galaxies, and covering a

Published
2013

27. THE HIDDEN 'AGN MAIN SEQUENCE': EVIDENCE FOR A UNIVERSAL BLACK HOLE ACCRETION TO STAR FORMATION RATE RATIO SINCE z ∼ 2 PRODUCING AN M BH - M * RELATION

Author

E. Daddi, M. Bethermin, Ryan C. Hickox, D. Elbaz, Maurilio Pannella, M. T. Sargent, D. M. Alexander, Stéphanie Juneau, and James Mullaney

Subjects
Physics, Supermassive black hole, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, 010308 nuclear & particles physics, Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Redshift, Galaxy, Accretion (astrophysics), Black hole, Space and Planetary Science, Bulge, 0103 physical sciences, 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Using X-ray stacking analyses we estimate the average amounts of supermassive black hole (SMBH) growth taking place in star-forming galaxies (SFGs) at z~1 and z~2 as a function of galaxy stellar mass (M*). We find the average SMBH growth rate follows remarkably similar trends with M* and redshift as the average star-formation rates (SFRs) of their host galaxies (i.e., (i.e., dM_BH/dt ~ M*^(0.86+/-0.39) for the z~1 sample and dM_BH/dt ~ M*^(1.05+/-0.36) for the z~2 sample). It follows that the ratio of SMBH growth rate to SFR is (a) flat with respect to M* (b) not evolving with redshift and (c) close to the ratio required to maintain/establish a SMBH to M* ratio of ~10^{-3} as also inferred from today's M_BH-M_bulge relationship. We interpret this as evidence that SMBHs have, on average, grown in-step with their host galaxies since at least z~2, irrespective of host galaxy mass and AGN triggering mechanism. As such, we suggest that the same secular processes that drive the bulk of star formation are also responsible for the majority of SMBH growth. From this, we speculate that it is the availability of gas reservoirs that regulate both cosmological SMBH growth and star formation., Comment: 6 Pages, 3 Figures, ApJL accepted after minor changes

Published
2012
Full Text
View/download PDF

28. Submillimeter number counts at 250 μm, 350 μm and 500 μm in BLAST data

Author

M. Cousin, M. Bethermin, N. Bavouzet, and H. Dole

Subjects
Telescope, Physics, Luminous infrared galaxy, Photometry (optics), Wavelength, Space and Planetary Science, law, Astronomy and Astrophysics, Astrophysics, law.invention
Abstract

BLAST (Balloon-borne Large-Aperture Submillimeter Telescope) performed the first deep and wide extragalactic survey at 250, 350 and 500 um. The extragalactic number counts at these wavelengths are important constraints for modeling the infrared galaxies evolution. [...] We use three methods to identify the submillimeter sources. 1) Blind extraction. [...] The photometry is computed with a new simple and quick PSF fitting routine (FASTPHOT). [...] 2) Extraction with prior. [...] 3) A stacking analysis. [...] With the blind extraction, we reach 97, 83 and 76 mJy at resp. 250, 350 and 500 um with a 95% completeness. With the prior extraction, we reach 76 mJy (resp. 63 and 49 mJy) at 250 um (resp. 350 and 500 um). With the stacking analysis, we reach 6.2 mJy (resp. 5.2 and 3.5 mJy) at 250 um (resp. 350 and 500 um). The differential submillimeter number counts are derived, and start showing a turnover at flux densities decreasing with increasing wavelength. There is a very good agreement with the P(D) analysis of Patanchon et al. (2009). At bright fluxes (>100 mJy), the Lagache et al. (2004) and Le Borgne et al. (2009) models slightly overestimate the observed counts, but there is a very good agreement near the peak of differential number counts. [...] Counts are available at: this http URL

Published
2010
Full Text
View/download PDF

29. Deciphering the Activity and Quiescence of High-redshift Cluster Environments: ALMA Observations of Cl J1449+0856 at z = 2.

Author

V. Strazzullo, R. T. Coogan, E. Daddi, M. T. Sargent, R. Gobat, F. Valentino, M. Bethermin, M. Pannella, M. Dickinson, A. Renzini, N. Arimoto, A. Cimatti, H. Dannerbauer, A. Finoguenov, D. Liu, and M. Onodera

Subjects
GALACTIC redshift, GALAXY clusters, ASTRONOMICAL observations, SUPERGIANT stars
Abstract

We present Atacama Large Millimeter/submillimeter Array observations of the 870 μm continuum and CO(4–3) line emission in the core of the galaxy cluster Cl J1449+0856 at z = 2, a near-IR-selected, X-ray-detected system in the mass range of typical progenitors of today’s massive clusters. The 870 μm map reveals six F870μm > 0.5 mJy sources spread over an area of 0.07 arcmin2, giving an overdensity of a factor of ∼10 (6) with respect to blank-field counts down to F870μm > 1 mJy (>0.5 mJy). On the other hand, deep CO(4–3) follow-up confirms membership of three of these sources but suggests that the remaining three, including the brightest 870 μm sources in the field (F870μm ≳ 2 mJy), are likely interlopers. The measurement of 870 μm continuum and CO(4–3) line fluxes at the positions of previously known cluster members provides a deep probe of dusty star formation occurring in the core of this high-redshift structure, adding up to a total star formation rate of ∼700 ± 100 M⊙ yr−1 and yielding an integrated star formation rate density of ∼104M⊙ yr−1 Mpc−3, five orders of magnitude larger than in the field at the same epoch, due to the concentration of star-forming galaxies in the small volume of the dense cluster core. The combination of these observations with previously available Hubble Space Telescope imaging highlights the presence in this same volume of a population of galaxies with already suppressed star formation. This diverse composition of galaxy populations in Cl J1449+0856 is especially highlighted at the very cluster center, where a complex assembly of quiescent and star-forming sources is likely forming the future brightest cluster galaxy. [ABSTRACT FROM AUTHOR]

Published
2018
Full Text
View/download PDF

30. GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4.

Author

M. Pannella, D. Elbaz, E. Daddi, M. Dickinson, H. S. Hwang, C. Schreiber, V. Strazzullo, H. Aussel, M. Bethermin, V. Buat, V. Charmandaris, A. Cibinel, S. Juneau, R. J. Ivison, D. Le Borgne, E. Le Floc’h, R. Leiton, L. Lin, G. Magdis, and G. E. Morrison

Subjects
ATMOSPHERIC attenuation, STAR formation, GALACTIC dynamics, REDSHIFT, STARBURSTS
Abstract

We use deep panchromatic data sets in the GOODS-N field, from GALEX to the deepest Herschel far-infrared (FIR) and VLA radio continuum imaging, to explore the evolution of star-formation activity and dust attenuation properties of star-forming galaxies to z ≃ 4, using mass-complete samples. Our main results can be summarized as follows: (i) the slope of the star-formation rate–M* correlation is consistent with being constant ≃0.8 up to z ≃ 1.5, while its normalization keeps increasing with redshift; (ii) for the first time we are able to explore the FIR–radio correlation for a mass-selected sample of star-forming galaxies: the correlation does not evolve up to z ≃ 4; (iii) we confirm that galaxy stellar mass is a robust proxy for UV dust attenuation in star-forming galaxies, with more massive galaxies being more dust attenuated. Strikingly, we find that this attenuation relation evolves very weakly with redshift, with the amount of dust attenuation increasing by less than 0.3 mag over the redshift range [0.5–4] for a fixed stellar mass; (iv) the correlation between dust attenuation and the UV spectral slope evolves with redshift, with the median UV slope becoming bluer with redshift. By z ≃ 3, typical UV slopes are inconsistent, given the measured dust attenuations, with the predictions of commonly used empirical laws. (v) Finally, building on existing results, we show that gas reddening is marginally larger (by a factor of around 1.3) than the stellar reddening at all redshifts probed. Our results support a scenario where the ISM conditions of typical star-forming galaxies evolve with redshift, such that at z ≥ 1.5 Main Sequence galaxies have ISM conditions moving closer to those of local starbursts. [ABSTRACT FROM AUTHOR]

Published
2015
Full Text
View/download PDF

31. Herschel reveals the obscured star formation in HiZELS H\alpha\ emitters at z=1.47

Author

M. J. Page, V. Arumugam, S. J. Oliver, Francesca Pozzi, Benjamin Magnelli, Kotaro Kohno, Ian Smail, M. Symeonidis, Duncan Farrah, Dieter Lutz, Nick Seymour, A. Conley, Georgios E. Magdis, James E. Geach, Michael Zemcov, Lingyu Wang, L. Riguccini, Julie Wardlow, S. Berta, Antonio Cava, Rob Ivison, Austin Smith, E. Le Floc'h, J. J. Bock, G. Marsden, David Sobral, Philip Best, Edo Ibar, Matthieu Béthermin, Benjamin L. Schulz, Soh Ikarashi, E. Ibar, D. Sobral, P. N. Best, R. J. Ivison, I. Smail, V. Arumugam, S. Berta, M. Bethermin, J. Bock, A. Cava, A. Conley, D. Farrah, J. Geach, S. Ikarashi, K. Kohno, E. Le Floc'h, D. Lutz, G. Magdi, B. Magnelli, G. Marsden, S. J. Oliver, M. J. Page, F. Pozzi, L. Riguccini, B. Schulz, N. Seymour, A. J. Smith, M. Symeonidi, L. Wang, J. Wardlow, and M. Zemcov

Subjects
Stellar mass, galaxies: starburst, Astrophysics, 01 natural sciences, star formation [Galaxies], Physical cosmology, high-redshift [Galaxies], statistics [Galaxies], galaxies [Infrared], galaxies: high-redshift, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Luminous infrared galaxy, Physics, 010308 nuclear & particles physics, Star formation, infrared: galaxie, Astronomy, Astronomy and Astrophysics, Galaxy, Redshift, Stars, starburst [Galaxies], Space and Planetary Science, galaxies: star formation, galaxies: statistic, submillimetre: galaxies, galaxies. [Submillimetre], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We describe the far-infrared (FIR; rest-frame 8--1000\mu m) properties of a sample of 443 H\alpha-selected star-forming galaxies in the COSMOS and UDS fields detected by the HiZELS imaging survey. Sources are identified using narrow-band filters in combination with broad-band photometry to uniformly select H\alpha\ (and [OII] if available) emitters in a narrow redshift slice at z = 1.47+/-0.02. We use a stacking approach in Spitzer, Herschel (from PEP and HerMES surveys) and AzTEC images to describe their typical FIR properties. We find that HiZELS galaxies with observed H\alpha\ luminosities of ~ 10^{8.1-9.1} Lo have bolometric FIR luminosities of typical LIRGs, L_FIR ~ 10^{11.48+/-0.05} Lo. Combining the H\alpha\ and FIR luminosities, we derive median SFR = 32+/-5 Mo/yr and H\alpha\ extinctions of A(H\alpha) = 1.0+/-0.2 mag. Perhaps surprisingly, little difference is seen in typical HiZELS extinction levels compared to local star-forming galaxies. We confirm previous empirical stellar mass (M*) to A(H\alpha) relations and the little or no evolution up to z = 1.47. For HiZELS galaxies, we provide an empirical parametrisation of the SFR as a function of (u-z)_rest colours and 3.6\mu m photometry. We find that the observed H\alpha\ luminosity is a dominant SFR tracer when (u-z)_rest ~< 0.9 mag or when 3.6\mu m photometry > 22 mag (Vega) or when M* < 10^9.7 Mo. We do not find any correlation between the [OII]/H\alpha\ and FIR luminosity, suggesting that this emission line ratio does not trace the extinction of the most obscured star-forming regions. The luminosity-limited HiZELS sample tends to lie above of the so-called `main sequence' for star-forming galaxies, especially at low M*. This work suggests that obscured star formation is linked to the assembly of M*, with deeper potential wells in massive galaxies providing dense, heavily obscured environments in which stars can form rapidly., Comment: abridged abstract

Published
2013

32. Planck intermediate results VII. Statistical properties of infrared and radio extragalactic sources from the Planck Early Release Compact Source Catalogue at frequencies between 100 and 857 GHz

Author

Cardoso, J.-F., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Patanchon, G., Piat, M., Rosset, C., Smoot, G.F., Lähteenmäki, A., Poutanen, T., Kunz, M., Natoli, P., Polenta, G., Mandolesi, N., Ashdown, M., Hobson, M., Lasenby, A., Bhatia, R., Kneissl, R., Bond, J.R., Miville-Deschênes, M.-A., Banday, A.J., Bernard, J.-P., Forni, O., Giard, M., Jaffe, T.R., Montier, L., Pointecouteau, E., Ristorcelli, I., Doré, O., Hildebrandt, S.R., Rocha, G., Lilje, P.B., Hernández-Monteagudo, C., Borrill, J., Rebolo, R., Yvon, D., Nørgaard-Nielsen, Hans Ulrik, Atrio-Barandela, F., Toffolatti, L., Argüeso, F., Rachen, J.P., Scott, D., Colombo, L.P.L., Pierpaoli, E., Kurinsky, N., Sajina, A., Juvela, M., Keihänen, E., Kurki-Suonio, H., Suur-Uski, A.-S., Jones, W.C., White, M., Knox, L., Zonca, A., Wandelt, B.D., Cayón, L., Matarrese, S., Burigana, C., De Bernardis, P., Masi, S., Melchiorri, A., Nati, F., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Gregorio, A., Balbi, A., De Gasperis, G., Mazzotta, P., Vittorio, N., Cabella, P., Christensen, P.R., Naselsky, P., Rubiño-Martín, J.A., Dupac, X., Jagemann, T., Leonardi, R., Mendes, L., Giardino, G., Tauber, J.A., Partridge, B., De Zotti, G., Colafrancesco, S., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Zacchei, A., Massardi, M., Cuttaia, F., Finelli, F., Franceschi, E., Gruppuso, A., Morgante, G., Paoletti, D., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Tomasi, M., Ponthieu, N., Türler, M., Mitra, S., Chamballu, A., Clements, D.L., Jaffe, A.H., Mortlock, D., Novikov, D., Rowan-Robinson, M., Chary, R.-R., Chen, X., Paladini, R., Rusholme, B., Benoît, A., Dole, H., Aghanim, N., Aumont, J., Douspis, M., Lagache, G., Pajot, F., Puget, J.-L., Benabed, K., Bouchet, F.R., Colombi, S., Hivon, E., Moneti, A., Prunet, S., Sygnet, J.-F., Fosalba, P., Popa, L., Chiang, L.-Y., Efstathiou, G., Harrison, D., Eriksen, H.K., Hansen, F.K., Barreiro, R.B., Diego, J.M., González-Nuevo, J., Herranz, D., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Wade, L.A., Bonaldi, A., Davis, R.J., Dickinson, C., Noviello, F., Henrot-Versillé, S., Perdereau, O., Plaszczynski, S., Tristram, M., Tucci, M., Catalano, A., Coulais, A., Lamarre, J.-M., Arnaud, M., Bethermin, M., Marshall, D.J., Pratt, G.W., Starck, J.-L., MacÍas-Pérez, J.F., Perotto, L., Renault, C., Van Tent, B., Kisner, T.S., Dörl, U., Enßlin, T.A., Knoche, J., Reinecke, M., Riller, T., Murphy, J.A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., Perrotta, F., Ade, P.A.R., Munshi, D., Sudiwala, R., Osborne, S., Reach, W.T., Battaner, E., Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-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 de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), PLANCK, Department of Physics, Helsinki Institute of Physics, Collaboration, P, Ade, P, Aghanim, N, Argueso, F, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Balbi, A, Banday, A, Barreiro, R, Battaner, E, Benabed, K, Benoit, A, Bernard, J, Bersanelli, M, Bethermin, M, Bhatia, R, Bonaldi, A, Bond, J, Borrill, J, Bouchet, F, Burigana, C, Cabella, P, Cardoso, J, Catalano, A, Cayon, L, Chamballu, A, Chary, R, Chen, X, Chiang, L, Christensen, P, Clements, D, Colafrancesco, S, Colombi, S, Colombo, L, Coulais, A, Crill, B, Cuttaia, F, Danese, L, Davis, R, De Bernardis, P, De Gasperis, G, De Zotti, G, Delabrouille, J, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Dore, O, Dorl, U, Douspis, M, Dupac, X, Efstathiou, G, Ensslin, T, Eriksen, H, Finelli, F, Forni, O, Fosalba, P, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giardino, G, Giraud-Heraud, Y, Gonzalez-Nuevo, J, Gorski, K, Gregorio, A, Gruppuso, A, Hansen, F, Harrison, D, Henrot-Versille, S, Hernandez-Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Jaffe, T, Jaffe, A, Jagemann, T, Jones, W, Juvela, M, Keihanen, E, Kisner, T, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurinsky, N, Kurki-Suonio, H, Lagache, G, Lahteenmaki, A, Lamarre, J, Lasenby, A, Lawrence, C, Leonardi, R, Lilje, P, Lopez-Caniego, M, Macias-Perez, J, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martinez-Gonzalez, E, Masi, S, Massardi, M, Matarrese, S, Mazzotta, P, Melchiorri, A, Mendes, L, Mennella, A, Mitra, S, Miville-Deschenes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Nørgaard-Nielsen, H, Norgaard-Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Rowan-Robinson, M, Rubino-Martin, J, Rusholme, B, Sajina, A, Sandri, M, Savini, G, Scott, D, Smoot, G, Starck, J, Sudiwala, R, Suur-Uski, A, Sygnet, J, Tauber, J, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Turler, M, Valenziano, L, Van Tent, B, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, White, M, Yvon, D, Zacchei, A, Zonca, A, Hélium : du fondamental aux applications (NEEL - HELFA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), P. A. R., Ade, N., Aghanim, F., Argüeso, M., Arnaud, M., Ashdown, F., Atrio Barandela, J., Aumont, C., Baccigalupi, A., Balbi, A. J., Banday, R. B., Barreiro, E., Battaner, K., Benabed, A., Benoît, J. P., Bernard, M., Bersanelli, M., Bethermin, R., Bhatia, A., Bonaldi, J. R., Bond, J., Borrill, F. R., Bouchet, C., Burigana, P., Cabella, J. F., Cardoso, A., Catalano, L., Cayón, A., Chamballu, R. R., Chary, X., Chen, L. Y., Chiang, P. R., Christensen, D. L., Clement, S., Colafrancesco, S., Colombi, L. P. L., Colombo, A., Coulai, B. P., Crill, F., Cuttaia, L., Danese, R. J., Davi, P., de Bernardi, G., de Gasperi, G., de Zotti, J., Delabrouille, C., Dickinson, J. M., Diego, H., Dole, S., Donzelli, O., Doré, U., Dörl, M., Douspi, X., Dupac, G., Efstathiou, T. A., Enßlin, H. K., Eriksen, F., Finelli, O., Forni, P., Fosalba, M., Fraili, E., Franceschi, S., Galeotta, K., Ganga, M., Giard, G., Giardino, Y., Giraud Héraud, J., González Nuevo, K. M., Górski, Gregorio, Anna, A., Gruppuso, F. K., Hansen, D., Harrison, S., Henrot Versillé, C., Hernández Monteagudo, D., Herranz, S. R., Hildebrandt, E., Hivon, M., Hobson, W. A., Holme, T. R., Jaffe, A. H., Jaffe, T., Jagemann, W. C., Jone, M., Juvela, E., Keihänen, T. S., Kisner, R., Kneissl, J., Knoche, L., Knox, M., Kunz, N., Kurinsky, H., Kurki Suonio, G., Lagache, A., Lähteenmäki, J. M., Lamarre, A., Lasenby, C. R., Lawrence, R., Leonardi, P. B., Lilje, M., López Caniego, J. F., Macías Pérez, D., Maino, N., Mandolesi, M., Mari, D. J., Marshall, E., Martínez González, S., Masi, M., Massardi, S., Matarrese, P., Mazzotta, A., Melchiorri, L., Mende, A., Mennella, S., Mitra, M. A., Miville Deschêne, A., Moneti, L., Montier, G., Morgante, D., Mortlock, D., Munshi, J. A., Murphy, P., Naselsky, F., Nati, P., Natoli, H. U., Nørgaard Nielsen, F., Noviello, D., Novikov, I., Novikov, S., Osborne, F., Pajot, R., Paladini, D., Paoletti, B., Partridge, F., Pasian, G., Patanchon, O., Perdereau, L., Perotto, F., Perrotta, F., Piacentini, M., Piat, E., Pierpaoli, S., Plaszczynski, E., Pointecouteau, G., Polenta, N., Ponthieu, L., Popa, T., Poutanen, G. W., Pratt, S., Prunet, J. L., Puget, J. P., Rachen, W. T., Reach, R., Rebolo, M., Reinecke, C., Renault, S., Ricciardi, T., Riller, I., Ristorcelli, G., Rocha, C., Rosset, M., Rowan Robinson, J. A., Rubiño Martín, B., Rusholme, A., Sajina, M., Sandri, G., Savini, D., Scott, G. F., Smoot, J. L., Starck, R., Sudiwala, A. S., Suur Uski, J. F., Sygnet, J. A., Tauber, L., Terenzi, L., Toffolatti, M., Tomasi, M., Tristram, M., Tucci, M., Türler, L., Valenziano, B., Van Tent, P., Vielva, F., Villa, N., Vittorio, L. A., Wade, B. D., Wandelt, M., White, D., Yvon, A., Zacchei, A., Zonca, Anne Lähteenmäki Group, Aalto-yliopisto, Aalto University, HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Universidad de Cantabria

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, cosmology: observations, surveys, galaxies: statistics, galaxies: evolution, galaxies: star formation, galaxies: active, Astrophysics, Surveys, 01 natural sciences, 7. Clean energy, Cosmology: observation, Spectral line, Luminosity, statistics [Galaxies], Radio astronomy, observations [Cosmology], Survey, 010303 astronomy & astrophysics, media_common, Physics, Cosmology: observations, Galaxies: evolution, Galaxies: active, CMB cold spot, active [galaxies], symbols, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, star formation [galaxies], Astrophysics - Cosmology and Nongalactic Astrophysics, observation [cosmology], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Galaxies: statistics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, education, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, survey, statistic [galaxies], Planck, evolution [galaxies], Astrophysics::Galaxy Astrophysics, Luminous infrared galaxy, Galaxies: star formation, 010308 nuclear & particles physics, Galaxies: statistic, Spectral density, Astronomy and Astrophysics, Galaxies, 115 Astronomy, Space science, Galaxy, 13. Climate action, Space and Planetary Science, Sky
Abstract

We make use of the Planck all-sky survey to derive number counts and spectral indices of extragalactic sources-infrared and radio sources-from the Planck Early Release Compact Source Catalogue (ERCSC) at 100 to 857 GHz (3 mm to 350 μm). Three zones (deep, medium and shallow) of approximately homogeneous coverage are used to permit a clean and controlled correction for incompleteness, which was explicitly not done for the ERCSC, as it was aimed at providing lists of sources to be followed up. Our sample, prior to the 80% completeness cut, contains between 217 sources at 100 GHz and 1058 sources at 857 GHz over about 12 800 to 16 550 deg2 (31 to 40% of the sky). After the 80% completeness cut, between 122 and 452 and sources remain, with flux densities above 0.3 and 1.9 Jy at 100 and 857 GHz. The sample so defined can be used for statistical analysis. Using the multi-frequency coverage of the Planck High Frequency Instrument, all the sources have been classified as either dust-dominated (infrared galaxies) or synchrotron-dominated (radio galaxies) on the basis of their spectral energy distributions (SED). Our sample is thus complete, flux-limited and color-selected to differentiate between the two populations. We find an approximately equal number of synchrotron and dusty sources between 217 and 353 GHz; at 353 GHz or higher (or 217 GHz and lower) frequencies, the number is dominated by dusty (synchrotron) sources, as expected. For most of the sources, the spectral indices are also derived. We provide for the first time counts of bright sources from 353 to 857 GHz and the contributions from dusty and synchrotron sources at all HFI frequencies in the key spectral range where these spectra are crossing. The observed counts are in the Euclidean regime. The number counts are compared to previously published data (from earlier Planck results, Herschel, BLAST, SCUBA, LABOCA, SPT, and ACT) and models taking into account both radio or infrared galaxies, and covering a large range of flux densities. We derive the multi-frequency Euclidean level-the plateau in the normalised differential counts at high flux-density-and compare it to WMAP, Spitzer and IRAS results. The submillimetre number counts are not well reproduced by current evolution models of dusty galaxies, whereas the millimetre part appears reasonably well fitted by the most recent model for synchrotron-dominated sources. Finally we provide estimates of the local luminosity density of dusty galaxies, providing the first such measurements at 545 and 857 GHz. © 2013 ESO., The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU).

Published
2013
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results