Building the cosmic infrared background brick by brick with Herschel/PEP. ⋆

By S. Berta, B. Magnelli, R. Nordon, D. Lutz, S. Wuyts, B. Altieri, P. Andreani, H. Aussel, H. Castañeda, J. Cepa and 17 more. 2011

156 citations recorded by the source corpus.

The cosmic infrared background (CIB) includes roughly half of the energy radiated by all galaxies at all wavelengths across cosmic time, as observed at the present epoch. The PACS Evolutionary Probe (PEP) survey is exploited here to study the CIB and its redshift differential, at 70, 100 and 160 μm, where the background peaks. Combining PACS observations of the GOODS-S, GOODS-N, Lockman Hole and COSMOS areas, we define number counts spanning over more than two orders of magnitude in flux: from ∼ 1m Jy to few hundreds mJy. Stacking of 24 μm sources and P(D) statistics extend the analysis down to ∼0.2 mJy. Taking advantage of the wealth of ancillary data in PEP fields, differential number counts d 2 N/dS /dz and CIB are studied up to z = 5. Based on these counts, we discuss the effects of confusion on PACS blank field observations and provide confusion limits for the three bands considered. While most of the available backward evolution models predict the total PACS number counts with reasonable success, the consistency to redshift distributions and CIB derivatives can still be significantly improved. The new high-quality PEP data highlight the need to include redshift-dependent constraints in future modeling. The total CIB surface brightness emitted above PEP 3σ flux limits is νIν = 4.52 ± 1.18, 8.35 ± 0.95 and 9.49 ± 0.59 [nW m −2 sr −1 ] at 70, 100, and 160 μm, respectively. These values correspond to 58 ± 7% and 74± 5% of the COBE/DIRBE CIB direct measurements at 100 and 160 μm. Employing the P(D) analysis, these fractions increase to ∼65% and ∼89%. More than half of the resolved CIB was emitted at redshift z ≤ 1. The 50%-light redshifts lie at z = 0.58, 0.67 and 0.73 at the three PACS wavelengths. The distribution moves towards earlier epochs at longer wavelengths: while the 70 μ mC IB is mainly produced by z ≤ 1.0 objects, the contribution of z > 1.0 sources reaches 50% at 160 μm. Most of the CIB resolved in the three PACS bands was emitted by galaxies with infrared luminosities in the range 10 11 −10 12 L� .

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/f11d448b48fbb5a8dd46b07a9de22151cd32c5ae

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Citations in the corpus

• THE LESSER ROLE OF STARBURSTS IN STAR FORMATION AT z = 2 (2011, methodology): “The PACS data in GOODS are deeper than those in COSMOS, reaching 5σ detection levels of 1.8, 2.0 and 4.0 mJy at 70, 100 and 160 µm, respectively (Berta et al. 2011).”
• The Herschel census of infrared SEDs through cosmic time (2013, methodology): “…of the capabilities of this observatory (some examples from the multitude of Herschel papers on this topic: Amblard et al. 2010; Buat et al. 2010; Berta et al. 2010, 2011; Dye et al. 2010; Eales et al. 2010b; Gruppioni et al. 2010; Hwang et al. 2010; Ivison et al. 2010; Magdis et al. 2010, 2011;…”
• EXPLAINING THE [C ii]157.7 μm DEFICIT IN LUMINOUS INFRARED GALAXIES—FIRST RESULTS FROM A HERSCHEL/PACS STUDY OF THE GOALS SAMPLE (2013, background): “…galaxies comprise the bulk of the cosmic infrared background and dominate star-formation activity between 0.5 < z < 2 (Caputi et al. 2007; Magnelli et al. 2011; Murphy et al. 2011; Berta et al. 2011) and (2) AGN activity may preferentially occur during episodes of enhanced nuclear star formation.”
• RESOLVING THE RADIO SOURCE BACKGROUND: DEEPER UNDERSTANDING THROUGH CONFUSION (2012, methodology): “The Herschel PACS Evolutionary Probe (PEP) resolved 74 ± 5 % of the λ = 160µm background into individually detected galaxies stronger than about 3 mJy, and Berta et al. (2011) used a P (D) analysis to raise the resolved fraction to ∼ 89% above ∼ 0.3 mJy.”
• GOODS–Herschel: an infrared main sequence for star-forming galaxies (2011, background): “6) and on the other hand measured average PACS 100µm and 160µm flux densities for the sources with noHerscheldetection by stacking sub-images of 60′′ on a side at their 24µm prior positions.”
• The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, methodology): “These multi-wavelength catalogues also include photometric redshift estimates computed using all optical and near-infrared data available (see Berta et al. 2011; Grazian et al. 2006; Santini et al. 2009).”
• Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “…widely used in describing the statistical properties of galaxy populations, for example while interpreting and modeling observed number counts (e.g. Berta et al. 2011, 2010; Béthermin et al. 2011; Franceschini et al. 2010) or assessing luminosity functions at different wavelengths (e.g. Gruppioni…”
• The mean star formation rate of X-ray selected active galaxies and its evolution from z~2.5: results from PEP-Herschel (2012, background): “In the other two fields the 3σ flux limit at 100/160µm is 3.0/5.7 mJy in GOODS-N and 5.0/10.2 mJy in COSMOS (Berta et al. 2011).”
• The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4 (2013, methodology): “On average, the 160-µm selection favours higher redshifts than the 100-µm one (see also Berta et al. 2011).”
• The SINS/zC-SINF Survey of z ∼ 2 Galaxy Kinematics: SINFONI Adaptive Optics–assisted Data and Kiloparsec-scale Emission-line Properties (2018, methodology): “…that exponentially declining models are actually trying to mimic a secularly increasing SFR. 2 IR photometry was taken from the PEP survey catalog in GOODSSouth and COSMOS (Lutz et al. 2011; Berta et al. 2011) with updated MIPS data from the COSMOS2015 catalog (Laigle et al. 2016) where relevant.”
• THE EVOLVING INTERSTELLAR MEDIUM OF STAR-FORMING GALAXIES SINCE z = 2 AS PROBED BY THEIR INFRARED SPECTRAL ENERGY DISTRIBUTIONS (2012, unknown): “Despite the simple and straightforward nature of these templates, we note that Béthermin et al. (2012b) find that they manage to reproduce recent Herschel source counts (e.g., Berta et al. 2011; Béthermin et al. 2012), including counts measured in redshift slices.”
• PACS Evolutionary Probe (PEP) – a Herschel key program (2011, methodology): “…analysis of source confusion (Dole et al. 2004) suggests that with the 100µm and 160µm number counts turning over at a depth that is reached with PEP (Berta et al. 2010, 2011), deeper observations can still be extracted reliably, in particular when using position priorsf om very deep 24µm data…”
• The evolution of the dust temperatures of galaxies in the SFR–M∗ plane up to z ~ 2 (2013, methodology): “All these properties are given in Berta et al. (2011) and Roseboom et al. (2010, see also Lutz et al. 2011; and Oliver et al. 2012).”
• Accreting supermassive black holes in the COSMOS field and the connection to their host galaxies (2012, methodology): “Here, we use the deep COSMOS PACS 100- and 160-µm observations of the PEP12 (Lutz et al. 2011) guaranteed time key programme, reaching a 3σ limit of ∼4 and ∼10 mJy at 100 and 160 µm, respectively (see Berta et al. 2011).”
• VALIDATION OF THE EQUILIBRIUM MODEL FOR GALAXY EVOLUTION TO z ∼ 3 THROUGH MOLECULAR GAS AND DUST OBSERVATIONS OF LENSED STAR-FORMING GALAXIES (2013, methodology): “For the GOODSN comparison sample, we retrieve the ACS photometry from the multi-wavelength catalog of Berta et al. (2011) 8 and compute SFRUV from Eq.”
• Enhanced star formation rates in AGN hosts with respect to inactive galaxies from PEP-Herschel observations (2012, methodology): “…GOODS-S were computed by fitting the multiwavelength photometry to the PEGASE 2.0 templates (Fioc & Rocca-Volmerange 1997, see details in Grazian et al. 2006 updated as in Santini et al. 2009) and by adopting the EAZY code (Brammer et al. 2008) in GOODS-N and COSMOS (details in Berta et al. 2011).”
• The extragalactic background light revisited and the cosmic photon–photon opacity (Corrigendum) (2017, background): “…peak of dust emission from galaxies; the peak EBL emission at 160 µm, while estimated to exceed 20 nW/m2/sr by AF2008 based on Spitzer data, is now lowered to νI(ν) ∼ 14 nW/m2/sr, in good agreement with several other independent determinations (e.g., Lagache et al. 1999; Berta et al. 2011).”
• A UNIFIED EMPIRICAL MODEL FOR INFRARED GALAXY COUNTS BASED ON THE OBSERVED PHYSICAL EVOLUTION OF DISTANT GALAXIES (2012, background): “This observable is close to the monochromatic LF, but requires fewer corrections (K-corrections, Vmax) which could bias the results (possible biases from photometric redshifts and source identification are discussed in Berta et al. 2011 and Béthermin et al. 2012b).”