The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations

By B. Magnelli, P. Popesso, S. Berta, Francesca Pozzi, D. Elbaz, D. Lutz, Mark Dickinson, B. Altieri, P. Andreani, H. Aussel and 27 more. 2013

337 citations recorded by the source corpus.

We present results from the deepest Herschel-Photodetector Array Camera and Spectrometer (PACS) far-infrared blank field extragalactic survey, obtained by combining observations of the Great Observatories Origins Deep Survey (GOODS) fields from the PACS Evolutionary Probe (PEP) and GOODS-Herschel key programmes. We describe data reduction and theconstruction of images and catalogues. In the deepest parts of the GOODS-S field, the catalogues reach 3σ depths of 0.9, 0.6 and 1.3 mJy at 70, 100 and 160 μm, respectively, and resolve ~75% of the cosmic infrared background at 100 μm and 160 μm into individually detected sources. We use these data to estimate the PACS confusion noise, to derive the PACS number counts down to unprecedented depths, and to determine the infrared luminosity function of galaxies down to L_(IR) = 10^(11) L⊙ at z ~ 1 and L_(IR) = 10^(12) L⊙ at z ~ 2, respectively. For the infrared luminosity function of galaxies, our deep Herschel far-infrared observations are fundamental because they provide more accurate infrared luminosity estimates than those previously obtained from mid-infrared observations. Maps and source catalogues (>3σ) are now publicly released. Combined with the large wealth of multi-wavelength data available for the GOODS fields, these data provide a powerful new tool for studying galaxy evolution over a broad range of redshifts.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/dee7141e1f8057634f8548e2b5af5119c1b851de

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In Astronomy and Astrophysics

1. P. V. van Dokkum
2. P. Hopkins
3. L. Hernquist
4. M. Franx
5. R. Somerville
6. D. M. Alexander
7. A. Dekel
8. R. Dav'e

In Instrumentation

1. P. V. van Dokkum
2. M. Franx
3. C. Conroy
4. Christopher J. Conselice
5. P. Hopkins
6. A. Dekel
7. I. Labbé
8. R. Somerville

Citations in the corpus

• An ALMA survey of the SCUBA-2 CLS UDS field: physical properties of 707 sub-millimetre galaxies (2019, methodology): “Due to the coarse resolution of the Herschel/SPIRE maps (∼ 18-, 25-, and 36-arcsec FWHM at 250, 350, and 500 μm, respectively), we need to account for the effect of source blending (Roseboom et al. 2012; Magnelli et al. 2013).”
• An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, methodology): “We match our ALESS catalog with those from Magnelli et al. (2013) (with a matching radius of 1.5′′) and include the 70–160 µm photometry for the ALESS SMGs from the CDFS and the ECDFS wherever possible in our analysis below.”
• CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, background): “…de Bure interferometer (Daddi et al 2008; 2010a; D10 hereafter; Tacconi et al 2010; 2013; Geach et al 2011) and confirmed by gas mass estimates obtained via the conversion of dust masses (Magdis et al 2011; 2012; Santini et al 2014; Scoville et al 2014; Magnelli et al 2013; Genzel et al 2014).”
• GOODS-ALMA: 1.1 mm galaxy survey (2018, methodology): “Herschel images come from a 206.3 h GOODS– South observational program (Elbaz et al. 2011) and combined by Magnelli et al. (2013) with the PACS Evolutionary Probe (PEP) observations (Lutz et al. 2011).”
• Dusty Star Forming Galaxies at High Redshift (2014, neutral): “…et al., 2010a; Berta et al., 2011), 100 µm (Héraudeau et al., 2004; Rodighiero and Franceschini, 2004; Kawara et al., 2004; Berta et al., 2011; Magnelli et al., 2013), 160 µm (Dole et al., 2004; Kawara et al., 2004; Béthermin et al., 2010a; Berta et al., 2011; Magnelli et al., 2013), 250…”
• The HDUV Survey: A Revised Assessment of the Relationship between UV Slope and Dust Attenuation for High-redshift Galaxies (2017, methodology): “…general could have been anticipated from the implied low number density of LIR & 1012 L objects from the IR luminosity function (Reddy et al. 2008; Magnelli et al. 2013) and the high number density of UV-faint galaxies inferred from the UV luminosity function (Reddy et al. 2008; Reddy & Steidel…”
• ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, methodology): “Such sources are known to contribute a substantial fraction of the SFR density at z ∼ 0-2 (Karim et al. 2011; Magnelli et al. 2013; Madau & Dickinson 2014).”
• A remarkably flat relationship between the average star formation rate and AGN luminosity for distant X-ray AGN. (2015, methodology): “We first match the positions of the optical counterparts of the X-ray sources to the MIPS 24 μm positions in the catalogues of Magnelli et al. (2013).3 To choose the matching radii between catalogues, we measure the number of total matches as a function of radius and estimate the fraction of…”
• THE KMOS3D SURVEY: DESIGN, FIRST RESULTS, AND THE EVOLUTION OF GALAXY KINEMATICS FROM 0.7 ⩽ z ⩽ 2.7 (2014, background): “The fields further benefit from multi-wavelength coverage from the X-ray to far-IR and radio (e.g. Ueda et al. 2008; Lutz et al. 2011; Xue et al. 2011; Civano et al. 2012; Magnelli et al. 2013).”
• AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “Swinbank et al. (2014) obtain the PACS fluxes for the ALESS SMGs by matching them with the PEP catalog extracted by Magnelli et al. (2013).”
• Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, background): “This trend can be understood considering the rise of the clustering of the galaxy responsible for the cosmic infrared background (Planck Collaboration XXX 2014) and a rather stable number density of emitters especially below z = 1 (Béthermin et al. 2011; Magnelli et al. 2013; Gruppioni et al. 2013).”
• BULGE GROWTH AND QUENCHING SINCE z = 2.5 IN CANDELS/3D-HST (2014, methodology): “The latter method uses detected emission in either UV + PACS for PACS-detected galaxies (Lutz et al. 2011; Magnelli et al. 2013) or UV + MIPS 24µm for MIPS-detected galaxies to compute the sum of the obscured and unobscured SFR.”
• A CANDELS–3D-HST SYNERGY: RESOLVED STAR FORMATION PATTERNS AT 0.7 < z < 1.5 (2013, background): “The latter span up to 30+ medium and broad bands from 0.3 to 8 micron (e.g., Ilbert et al. 2009; Whitaker et al. 2011; Spitler et al. 2012), complemented further by mid-to-far-infrared photometry, probing dustobscured star formation within at least the more massive SFGs (e.g., Magnelli et al. 2013).”
• The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “The PACS fluxes are taken from the public PEP DR1 catalog (Magnelli et al. 2013), and were extracted using the same procedure as in GOODS–North.”