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Author

A. Feltre

Bio: A. Feltre is an academic researcher from University of Padua. The author has contributed to research in topics: Physics & Galaxy. The author has an hindex of 7, co-authored 11 publications receiving 2668 citations.

Papers
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Journal ArticleDOI
TL;DR: In this article, the relative contribution of star formation rate (SFR)-driven and starburst-driven galaxies to the global SFR density in the redshift interval 1.5 1000 M ☉ yr-1 was quantified.
Abstract: Two main modes of star formation are know to control the growth of galaxies: a relatively steady one in disk-like galaxies, defining a tight star formation rate (SFR)-stellar mass sequence, and a starburst mode in outliers to such a sequence which is generally interpreted as driven by merging. Such starburst galaxies are rare but have much higher SFRs, and it is of interest to establish the relative importance of these two modes. PACS/Herschel observations over the whole COSMOS and GOODS-South fields, in conjunction with previous optical/near-IR data, have allowed us to accurately quantify for the first time the relative contribution of the two modes to the global SFR density in the redshift interval 1.5 1000 M ☉ yr-1, off-sequence sources significantly contribute to the SFR density (46% ± 20%). We conclude that merger-driven starbursts play a relatively minor role in the formation of stars in galaxies, whereas they may represent a critical phase toward the quenching of star formation and morphological transformation in galaxies.

927 citations

Journal ArticleDOI
Seb Oliver1, James J. Bock2, James J. Bock3, Bruno Altieri4, Alexandre Amblard5, V. Arumugam6, Herve Aussel7, Tom Babbedge8, Alexandre Beelen9, Matthieu Béthermin9, Matthieu Béthermin7, Andrew Blain2, Alessandro Boselli10, C. Bridge2, Drew Brisbin11, V. Buat10, Denis Burgarella10, N. Castro-Rodríguez12, N. Castro-Rodríguez13, Antonio Cava14, P. Chanial7, Michele Cirasuolo15, David L. Clements8, A. Conley16, L. Conversi4, Asantha Cooray17, Asantha Cooray2, C. D. Dowell2, C. D. Dowell3, Elizabeth Dubois1, Eli Dwek18, Simon Dye19, Stephen Anthony Eales20, David Elbaz7, Duncan Farrah1, A. Feltre21, P. Ferrero12, P. Ferrero13, N. Fiolet9, N. Fiolet22, M. Fox8, Alberto Franceschini21, Walter Kieran Gear20, E. Giovannoli10, Jason Glenn16, Yan Gong17, E. A. González Solares23, Matthew Joseph Griffin20, Mark Halpern24, Martin Harwit, Evanthia Hatziminaoglou, Sebastien Heinis10, Peter Hurley1, Ho Seong Hwang7, A. Hyde8, Edo Ibar15, O. Ilbert10, K. G. Isaak25, Rob Ivison15, Rob Ivison6, Guilaine Lagache9, E. Le Floc'h7, L. R. Levenson2, L. R. Levenson3, B. Lo Faro21, Nanyao Y. Lu2, S. C. Madden7, Bruno Maffei26, Georgios E. Magdis7, G. Mainetti21, Lucia Marchetti21, G. Marsden24, J. Marshall2, J. Marshall3, A. M. J. Mortier8, Hien Nguyen2, Hien Nguyen3, B. O'Halloran8, Alain Omont22, Mat Page27, P. Panuzzo7, Andreas Papageorgiou20, H. Patel8, Chris Pearson28, Chris Pearson29, Ismael Perez-Fournon12, Ismael Perez-Fournon13, Michael Pohlen20, Jonathan Rawlings27, Gwenifer Raymond20, Dimitra Rigopoulou29, Dimitra Rigopoulou30, L. Riguccini7, D. Rizzo8, Giulia Rodighiero21, Isaac Roseboom6, Isaac Roseboom1, Michael Rowan-Robinson8, M. Sanchez Portal4, Benjamin L. Schulz2, Douglas Scott24, Nick Seymour27, Nick Seymour31, D. L. Shupe2, A. J. Smith1, Jamie Stevens32, M. Symeonidis27, Markos Trichas33, K. E. Tugwell27, Mattia Vaccari21, Ivan Valtchanov4, Joaquin Vieira2, Marco P. Viero2, L. Vigroux22, Lifan Wang1, Robyn L. Ward1, Julie Wardlow17, G. Wright15, C. K. Xu2, Michael Zemcov2, Michael Zemcov3 
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ∼380deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy programme designed to map a set of nested fields totalling ∼380 deg^2. Fields range in size from 0.01 to ∼20 deg^2, using the Herschel-Spectral and Photometric Imaging Receiver (SPIRE) (at 250, 350 and 500 μm) and the Herschel-Photodetector Array Camera and Spectrometer (PACS) (at 100 and 160 μm), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the reprocessed optical and ultraviolet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multiwavelength understanding of galaxy formation and evolution. The survey will detect of the order of 100 000 galaxies at 5σ in some of the best-studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to facilitate redshift determination, rapidly identify unusual objects and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include the total infrared emission of galaxies, the evolution of the luminosity function, the clustering properties of dusty galaxies and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

852 citations

Journal ArticleDOI
Seb Oliver1, James J. Bock2, James J. Bock3, Bruno Altieri4, Alexandre Amblard5, V. Arumugam6, Herve Aussel7, Tom Babbedge8, Alexandre Beelen, Matthieu Béthermin7, Andrew Blain2, Alessandro Boselli9, C. Bridge2, Drew Brisbin10, V. Buat9, Denis Burgarella9, N. Castro-Rodríguez11, N. Castro-Rodríguez12, Antonio Cava13, P. Chanial7, Michele Cirasuolo14, David L. Clements8, A. Conley15, L. Conversi4, Asantha Cooray16, Asantha Cooray2, C. D. Dowell2, C. D. Dowell3, Elizabeth Dubois1, Eli Dwek17, Simon Dye18, Stephen Anthony Eales19, David Elbaz7, Duncan Farrah1, A. Feltre20, P. Ferrero12, P. Ferrero11, N. Fiolet21, M. Fox8, Alberto Franceschini20, Walter Kieran Gear19, E. Giovannoli9, Jason Glenn15, Yan Gong16, E. A. González Solares22, Matthew Joseph Griffin19, Mark Halpern23, Martin Harwit, Evanthia Hatziminaoglou, Sebastien Heinis9, Peter Hurley1, Ho Seong Hwang7, A. Hyde8, Edo Ibar14, O. Ilbert9, K. G. Isaak24, Rob Ivison14, Rob Ivison6, Guilaine Lagache, E. Le Floc'h7, L. R. Levenson2, L. R. Levenson3, B. Lo Faro20, Nanyao Y. Lu2, S. C. Madden7, Bruno Maffei25, Georgios E. Magdis7, G. Mainetti20, Lucia Marchetti20, G. Marsden23, J. Marshall2, J. Marshall3, A. M. J. Mortier8, Hien Nguyen2, Hien Nguyen3, B. O'Halloran8, Alain Omont21, Mat Page26, P. Panuzzo7, Andreas Papageorgiou19, H. Patel8, Chris Pearson27, Chris Pearson28, Ismael Perez-Fournon11, Ismael Perez-Fournon12, Michael Pohlen19, Jonathan Rawlings26, Gwenifer Raymond19, Dimitra Rigopoulou29, Dimitra Rigopoulou27, L. Riguccini7, D. Rizzo8, Giulia Rodighiero20, Isaac Roseboom6, Isaac Roseboom1, Michael Rowan-Robinson8, M. Sanchez Portal4, Benjamin L. Schulz2, Douglas Scott23, Nick Seymour30, Nick Seymour26, D. L. Shupe2, A. J. Smith1, Jamie Stevens31, M. Symeonidis26, Markos Trichas32, K. E. Tugwell26, Mattia Vaccari20, Ivan Valtchanov4, Joaquin Vieira2, Marco P. Viero2, L. Vigroux21, Lifan Wang1, Robyn L. Ward1, Julie Wardlow16, G. Wright14, C. K. Xu2, Michael Zemcov3, Michael Zemcov2 
TL;DR: The Herschel Multi-tiered Extragalactic Survey (HerMES) is a legacy program designed to map a set of nested fields totalling ~380 deg^2 as mentioned in this paper.
Abstract: The Herschel Multi-tiered Extragalactic Survey, HerMES, is a legacy program designed to map a set of nested fields totalling ~380 deg^2. Fields range in size from 0.01 to ~20 deg^2, using Herschel-SPIRE (at 250, 350 and 500 \mu m), and Herschel-PACS (at 100 and 160 \mu m), with an additional wider component of 270 deg^2 with SPIRE alone. These bands cover the peak of the redshifted thermal spectral energy distribution from interstellar dust and thus capture the re-processed optical and ultra-violet radiation from star formation that has been absorbed by dust, and are critical for forming a complete multi-wavelength understanding of galaxy formation and evolution. The survey will detect of order 100,000 galaxies at 5\sigma in some of the best studied fields in the sky. Additionally, HerMES is closely coordinated with the PACS Evolutionary Probe survey. Making maximum use of the full spectrum of ancillary data, from radio to X-ray wavelengths, it is designed to: facilitate redshift determination; rapidly identify unusual objects; and understand the relationships between thermal emission from dust and other processes. Scientific questions HerMES will be used to answer include: the total infrared emission of galaxies; the evolution of the luminosity function; the clustering properties of dusty galaxies; and the properties of populations of galaxies which lie below the confusion limit through lensing and statistical techniques. This paper defines the survey observations and data products, outlines the primary scientific goals of the HerMES team, and reviews some of the early results.

707 citations

Journal ArticleDOI
TL;DR: In this paper, a broad-band spectral energy distribution decomposition was performed to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy.
Abstract: We study a sample of Herschel selected galaxies within the Great Observatories Origins Deep Survey-South and the Cosmic Evolution Survey fields in the framework of the Photodetector Array Camera and Spectrometer (PACS) Evolutionary Probe project. Starting from the rich multiwavelength photometric data sets available in both fields, we perform a broad-band spectral energy distribution decomposition to disentangle the possible active galactic nucleus (AGN) contribution from that related to the host galaxy. We find that 37 per cent of the Herschel-selected sample shows signatures of nuclear activity at the 99 per cent confidence level. The probability of revealing AGN activity increases for bright (L_(1−1000) > 10^(11) L_⊙) star-forming galaxies at z > 0.3, becoming about 80 per cent for the brightest (L_(1−1000) > 10^(12) L_⊙) infrared (IR) galaxies at z ≥ 1. Finally, we reconstruct the AGN bolometric luminosity function and the supermassive black hole growth rate across cosmic time up to z ∼ 3 from a far-IR perspective. This work shows general agreement with most of the panchromatic estimates from the literature, with the global black hole growth peaking at z ∼ 2 and reproducing the observed local black hole mass density with consistent values of the radiative efficiency ϵ_(rad) (∼0.07).

196 citations

Journal ArticleDOI
TL;DR: In this paper, the authors explore the impact of the presence of an active galactic nucleus (AGN) on the mid and far-infrared properties of galaxies as well as the effects of simultaneous AGN and starburst activity in the same galaxies.
Abstract: In this work, we explore the impact of the presence of an active galactic nucleus (AGN) on the mid- and far-infrared (IR) properties of galaxies as well as the effects of simultaneous AGN and starburst activity in the same galaxies. To do this, we apply a multicomponent, multiband spectral synthesis technique to a sample of 250 μm selected galaxies of the Herschel Multi-tiered Extragalactic Survey (HerMES), with Infrared Spectrograph (IRS) spectra available for all galaxies. Our results confirm that the inclusion of the IRS spectra plays a crucial role in the spectral analysis of galaxies with an AGN component improving the selection of the best-fitting hot dust (torus) model. We find a correlation between the obscured star formation rate, SFR_IR, derived from the IR luminosity of the starburst component, and SFRPAH, derived from the luminosity of the PAH features, L_PAH, with SFR_FIR taking higher values than SFR_PAH. The correlation is different for AGN- and starburst-dominated objects. The ratio of L_PAH to that of the starburst component, L_PAH/L_SB, is almost constant for AGN-dominated objects but decreases with increasing L_SB for starburst-dominated objects. SFR_FIR increases with the accretion luminosity, L_acc, with the increase less prominent for the very brightest, unobscured AGN-dominated sources. We find no correlation between the masses of the hot (AGN-heated) and cold (starburst-heated) dust components. We interpret this as a non-constant fraction of gas driven by the gravitational effects to the AGN while the starburst is ongoing. We also find no evidence of the AGN affecting the temperature of the cold dust component, though this conclusion is mostly based on objects with a non-dominant AGN component. We conclude that our findings do not provide evidence that the presence of AGN affects the star formation process in the host galaxy, but rather that the two phenomena occur simultaneously over a wide range of luminosities.

54 citations


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Journal ArticleDOI
TL;DR: In this article, the authors review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch.
Abstract: Over the past two decades, an avalanche of data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z~1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ~1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization.

3,104 citations

Journal ArticleDOI
TL;DR: In this paper, the authors review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch.
Abstract: Over the past two decades, an avalanche of data from multiwavelength imaging and spectroscopic surveys has revolutionized our view of galaxy formation and evolution. Here we review the range of complementary techniques and theoretical tools that allow astronomers to map the cosmic history of star formation, heavy element production, and reionization of the Universe from the cosmic "dark ages" to the present epoch. A consistent picture is emerging, whereby the star-formation rate density peaked approximately 3.5 Gyr after the Big Bang, at z~1.9, and declined exponentially at later times, with an e-folding timescale of 3.9 Gyr. Half of the stellar mass observed today was formed before a redshift z = 1.3. About 25% formed before the peak of the cosmic star-formation rate density, and another 25% formed after z = 0.7. Less than ~1% of today's stars formed during the epoch of reionization. Under the assumption of a universal initial mass function, the global stellar mass density inferred at any epoch matches reasonably well the time integral of all the preceding star-formation activity. The comoving rates of star formation and central black hole accretion follow a similar rise and fall, offering evidence for co-evolution of black holes and their host galaxies. The rise of the mean metallicity of the Universe to about 0.001 solar by z = 6, one Gyr after the Big Bang, appears to have been accompanied by the production of fewer than ten hydrogen Lyman-continuum photons per baryon, a rather tight budget for cosmological reionization.

1,626 citations

Journal ArticleDOI
TL;DR: In this article, the authors investigate the evolution of the star-forming galaxy (SFG) main sequence (MS) in stellar mass and star formation rate (SFR) out to z ~ 6.4 Gyr.
Abstract: Using a compilation of 25 studies from the literature, we investigate the evolution of the star-forming galaxy (SFG) main sequence (MS) in stellar mass and star formation rate (SFR) out to z ~ 6. After converting all observations to a common set of calibrations, we find a remarkable consensus among MS observations (~0.1 dex 1σ interpublication scatter). By fitting for time evolution of the MS in bins of constant mass, we deconvolve the observed scatter about the MS within each observed redshift bin. After accounting for observed scatter between different SFR indicators, we find the width of the MS distribution is ~0.2 dex and remains constant over cosmic time. Our best fits indicate the slope of the MS is likely time-dependent, with our best-fit log SFR(M_*, t) = (0.84 ± 0.02 – 0.026 ± 0.003 × t)log M_* – (6.51 ± 0.24 – 0.11 ± 0.03 × t), where t is the age of the universe in Gyr. We use our fits to create empirical evolutionary tracks in order to constrain MS galaxy star formation histories (SFHs), finding that (1) the most accurate representations of MS SFHs are given by delayed-τ models, (2) the decline in fractional stellar mass growth for a "typical" MS galaxy today is approximately linear for most of its lifetime, and (3) scatter about the MS can be generated by galaxies evolving along identical evolutionary tracks assuming an initial 1σ spread in formation times of ~1.4 Gyr.

1,336 citations

Journal ArticleDOI
TL;DR: In the last decade, observations of the cool interstellar medium (ISM) in distant galaxies via molecular and atomic fine structure line (FSL) emission have gone from a curious look into a few extreme, rare objects to a mainstream tool for studying galaxy formation out to the highest redshifts as mentioned in this paper.
Abstract: Over the past decade, observations of the cool interstellar medium (ISM) in distant galaxies via molecular and atomic fine structure line (FSL) emission have gone from a curious look into a few extreme, rare objects to a mainstream tool for studying galaxy formation out to the highest redshifts. Molecular gas has been observed in close to 200 galaxies at z > 1, including numerous AGN host-galaxies out to z ∼ 7, highly star-forming submillimeter galaxies, and increasing samples of main-sequence color-selected star-forming galaxies at z ∼ 1.5 to 2.5. Studies have moved well beyond simple detections to dynamical imaging at kiloparsec-scale resolution and multiline, multispecies studies that determine the physical conditions in the ISM in early galaxies. Observations of the cool gas are the required complement to studies of the stellar density and star-formation history of the Universe as they reveal the phase of the ISM that immediately precedes star formation in galaxies. Current observations suggest that t...

1,041 citations