PACS Evolutionary Probe (PEP) – a Herschel key program

By D. Lutz, Albrecht Poglitsch, B. Altieri, P. Andreani, H. Aussel, S. Berta, A. Bongiovanni, D. Brisbin, A. Cava, J. Cepa and 28 more. 2011

415 citations recorded by the source corpus.

Deep far-infrared photometric surveys studying galaxy evolution and the nature of the cosmic infrared background are a key strength of the Herschel mission. We describe the scientific motivation for the PACS Evolutionary Probe (PEP) guaranteed time key program and its role within the entire set of Herschel surveys, and the field selection that includes popular multiwavelength fields such as GOODS, COSMOS, Lockman Hole, ECDFS, and EGS. We provide an account of the observing strategies and data reduction methods used. An overview of first science results illustrates the potential of PEP in providing calorimetric star formation rates for high-redshift galaxy populations, thus testing and superseding previous extrapolations from other wavelengths, and enabling a wide range of galaxy evolution studies.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/d59d1c3a1abadcbc3785a929d0a392f2375c5a80

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In Astronomy and Astrophysics

1. P. Hopkins
2. L. Hernquist
3. D. M. Alexander
4. R. Somerville
5. R. Dav'e
6. P. V. van Dokkum
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Citations in the corpus

• AN ALMA SURVEY OF SUB-MILLIMETER GALAXIES IN THE EXTENDED CHANDRA DEEP FIELD SOUTH: PHYSICAL PROPERTIES DERIVED FROM ULTRAVIOLET-TO-RADIO MODELING (2015, methodology): “The ECDF-S was imaged with Herschel at 70, 100, and 160 μmwith PACS as part of the PACS Evolutionary Probe (PEP) survey (Lutz et al. 2011).”
• An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, background): “These data and deblended catalogs are described in Lutz et al. (2011) and Magnelli et al. (2013) and reach 1-σ sensitivities of 0.2–0.4 mJy (CDFS) and 1–2.6mJy (ECDFS).”
• 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).”
• The Herschel view of the dominant mode of galaxy growth from z = 4 to the present day (2014, methodology): “The PACS images are the result of the combined observation of both GOODS–Herschel and PACS evolutionary probe (PEP; Lutz et al. 2011), while SPIRE images were obtained as part of the HerMES program (Oliver et al. 2012).”
• Panchromatic spectral energy distributions of Herschel sources (2013, methodology): “The sensitivity reached by the Photodetector Array Camera and Spectrometer (PACS, Poglitsch et al. 2010) and the Spectraland Photometric Imaging REceiver (SPIRE, Griffin et al. 2010) instruments aboardHerschel has guaranteed the detection not only of the most extreme star-forming galaxies, with star”
• Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, methodology): “The PACS (photodetecting array camera and spectrometer, Poglitsch et al. 2010) evolutionary probe survey (PEP, Lutz et al. 2011) mapped the COSMOS field with the Herschel1 space observatory (Pilbratt et al. 2010) at 100 and 160 μm with a pointsource sensitivity of 1.5 mJy and 3.3 mJy and a PSF FWHM…”
• 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).”
• X-shooter reveals powerful outflows in z ∼ 1.5 X-ray selected obscured quasi-stellar objects (2014, background): “Four of the targets (XID5321, XID2028, XID60053 and XID54466) are detected in the PEP (PACS Evolutionary Probe) survey by Herschel/PACS in at least one band (Lutz et al. 2011; Santini et al. 2012).”
• SUBMILLIMETER GALAXIES AS PROGENITORS OF COMPACT QUIESCENT GALAXIES (2014, methodology): “…(AzTEC, LABOCA, MAMBO, SMA, CARMA, PdBI) and FIR (Spitzer MIPS, Herschel PACS and SPIRE) observations of the COSMOS field (Sanders et al. 2007; Lutz et al. 2011; Oliver et al. 2012; Scott et al. 2008; Aretxaga et al. 2011; Bertoldi et al. 2007; Younger et al. 2007, 2008; Smolčić et al.…”
• A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “…obtained 2 PI M. Dickinson, see http://www.noao.edu/noao/fidel/ through the GOODS-Herschel (Elbaz et al. 2011) and the PACS Evolutionary Probe (PEP; Lutz et al. 2011) surveys, while SPIRE (Griffin et al. 2010) images at 250µm, 350µm and 500µm, reaching 5.86, 6.34 and 6.88 mJy respectively…”
• Bolometric luminosities and Eddington ratios of X-ray selected active galactic nuclei in the XMM-COSMOS survey (2012, background): “Firstly, the inclusion ofHerscheldata at 100µm and 160µm (Lutz et al. 2011) in the SED-fitting code is of fundamental importance to better constrain the far-infrared emission and, therefore, the AGN emission in the mid-infrared for Type-2 AGN.”
• COMBINED CO AND DUST SCALING RELATIONS OF DEPLETION TIME AND MOLECULAR GAS FRACTIONS WITH COSMIC TIME, SPECIFIC STAR-FORMATION RATE, AND STELLAR MASS (2014, methodology): “6 CO 2-1 detections of z=1-1.2 main-sequence SFGs selected from the HerschelPEP survey (Lutz et al. 2011), obtained with the IRAM PdBI (Magnelli et al. 2012a); 7.”
• Evolution of Interstellar Medium, Star Formation, and Accretion at High Redshift (2017, methodology): “COSMOS was observed at 100 µm and 160 µm by Herschel PACS (Poglitsch et al. 2010) as part of the PACS Evolutionary Probe program (PEP; Lutz et al. 2011)), and down to the confusion limit at 250 µm, 350 µm, and 500 µm by Herschel SPIRE (Griffin et al. 2010) as part of the Herschel Multi-tiered…”
• The Herschel Multi-tiered Extragalactic Survey: HerMES (2012, methodology): “An optimized sampling over wavelength is achieved by combining HerMES with the PACS Evolutionary Probe (PEP; Lutz et al., 2011) survey.”
• A Herschel view of the far-infrared properties of submillimetre galaxies (2012, methodology): “The reliability, completeness and cotamination of our PACS and SPIRE catalogues were tested via Monte-Carlo simulations (see Lutz et al., 2011 and Oliver etal.”
• VALIDATION OF THE EQUILIBRIUM MODEL FOR GALAXY EVOLUTION TO z ∼ 3 THROUGH MOLECULAR GAS AND DUST OBSERVATIONS OF LENSED STAR-FORMING GALAXIES (2013, methodology): “We processed the PACS data to maps using standard procedures similar to those described for the PEP project in Lutz et al. (2011), in build 7.0.1786 of the Herschel HIPE software (Ott 2010).”
• The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, methodology): “…it applies a recentring correction to the pointing product of Herschel using reference positions of 24 µm sources with accurate astrometry (see Lutz et al. 2011) from deep Article number, page 3 of 22 observations with the Multiband Imaging Photometer (MIPS; Rieke et al. 2004) onboard the…”
• GOODS-Herschel: the far-infrared view of star formation in active galactic nucleus host galaxies since z ≈ 3 (2011, background): “Wide, but less deep, infrared surveys such as PEP (Lutz et al. 2011) and HERMES (P.I.: S. Oliver) are needed to fully explore the average infrared properties of both higher luminosity (i.e.,LX> 1044 ergs s−1) or, alternatively, lower redshift (i.e.,z. 0.5) AGNs.”
• THE LESSER ROLE OF STARBURSTS IN STAR FORMATION AT z = 2 (2011, methodology): “SFR-selected Herschel samples Herschel-PACS observations cover 2.04 square degrees over the COSMOS field down to a 5σ limit of 8 and 17 mJy at 100 and 160 µm, respectively, well above confusion limits (Lutz et al. 2011).”
• Tracing the cosmic growth of supermassive black holes to z ∼ 3 with Herschel (2014, methodology): “This is the reason why we exploit observations carried out within the PACS Evolutionary Probe (PEP1, Lutz et al. 2011) and the Herschel Multi-tiered Extragalactic Survey (HerMES, Oliver et al. 2012) in two different regions: the Great Observatories Origins Deep Survey-South (GOODS- S, Elbaz et al.…”