PACS Evolutionary Probe (PEP) – A<i>Herschel</i>key program

Lutz, D.; Poglitsch, A.; Altiéri, B.; Andreani, P.; Aussel, H.; Berta, S.; Bongiovanni, Á.; Brisbin, D.; Cava, A.; Cepa, J.; Cimatti, A.; Daddi, E.; Domínguez-Sánchez, H.; Elbaz, D.; Schreiber, N. M. Förster; Genzel, R.; Grazian, A.; Gruppioni, C.; Harwit, Martin; Floc’h, E. Le; Magdis, G.; Magnelli, B.; Maiolino, R.; Nordon, R.; Pérez-García, A. M.; Popesso, P.; Pozzi, F.; Riguccini, L.; Rodighiero, G.; Saintonge, A.; Portal, M. Sánchez; Santini, P.; Shao, Li; Sturm, E.; Tacconi, L. J.; Valtchanov, I.; Wetzstein, Michael E.; Wieprecht, E.

doi:10.1051/0004-6361/201117107

Cited by 494 publications

(507 citation statements)

References 72 publications

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“…For the stacking analysis (Section 3) we use the MIPS 24 μm imaging (FWHM;6″) from Sanders et al (2007), while the Herschel PACS and SPIRE maps are from the PACS Evolutionary Probe survey (PEP; Lutz et al 2011) and the Herschel Multi-tiered Extragalactic Survey (HerMES; Oliver et al 2012), respectively. The PACS maps reach depths of 5 and 10.3 mJy beam −1 (3σ) at 100 and 160 μm, respectively (FWHM;6 8 and 11″), and SPIRE 250, 350, and 500 μm depths are 8, 11, and 13 mJy beam −1 (3σ), respectively (FWHM;18 2, 24 9, and 36 3).…”

Section: Data and Sample Selectionmentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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We performed a comprehensive stacking analysis on ∼14,200 quiescent galaxy (QG) candidates at z=0-3 across mid-, far-infrared (MIR and FIR), and radio wavelengths. Identified via their rest-frame NUV−r and r−J colors, the QG candidates (M M 10 9.8 12.2 - =  ) have drastically different IR and radio properties depending on their 24 μm emission strength. The fraction of QG candidates with strong 24 μm emission (equivalent to inferred star formation rates SFR M yr 100, hereafter "IR-bright") increases with redshift and peaks at 15%, and their stacked MIPS 24 μm, Herschel (PACS and SPIRE) and VLA emissions are consistent with being starforming galaxies (SFGs). In contrast, the majority of QG candidates are faint or undetected at 24 μm individually (i.e., SFR 24 <100 M e yr −1 , hereafter "IR-faint"). Their low dust-obscured SFRs derived from Herschel stacking (SFR H  3, 15, 50 M e yr −1 out to z∼1, 2, 3) are >2.5-12.5×lower than compared to SFGs. This is consistent with the quiescence, as expected from their low unobscured SFRs, as inferred from modeling their ultraviolet-to-NIR photometry. The discrepancy between the L IR derived from stacking Herschel and 24 μm indicates that IRfaint QGs have dust SEDs that are different from those of SFGs. For the most massive (M M 10 11    ) IR-faint QGs at z<1.5, the stacked 1.4 GHz emission is in excess of that expected from other SFR indicators, suggesting a widespread presence of low-luminosity active galactic nuclei. Our results reaffirm the existence of a significant population of QGs out to z=3, thus corroborating the need to quench star formation in galaxies at early epochs.

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Section: Data and Sample Selectionmentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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“…The FIR data used in this work were collected by the PACS instrument (Poglitsch et al 2010) on board the Herschel Space Observatory, as part of the PACS Evolutionary Probe (PEP, Lutz et al 2011) survey. Observations of almost the entire COSMOS field were taken in two PACS bands (100 and 160 μm).…”

Section: Herschel Imaging and Photometrymentioning

confidence: 99%

“…3.2. Detailed information on the PEP survey, observed fields, data processing and source extraction can be found in Lutz et al (2011).…”

Section: Herschel Imaging and Photometrymentioning

confidence: 99%

The mean star-forming properties of QSO host galaxies

Rosario

Trakhtenbrot

Lutz

et al. 2013

A&A

Self Cite

126

112

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Quasi-stellar objects (QSOs) occur in galaxies in which supermassive black holes (SMBHs) are growing substantially through rapid accretion of gas. Many popular models of the co-evolutionary growth of galaxies and black holes predict that QSOs are also sites of substantial recent star formation (SF), mediated by important processes, such as major mergers, which rapidly transform the nature of galaxies. A detailed study of the star-forming properties of QSOs is a critical test of these models. We present a far-infrared Herschel/PACS study of the mean star formation rate (SFR) of a sample of spectroscopically observed QSOs to z ∼ 2 from the COSMOS extragalactic survey. This is the largest sample to date of moderately luminous QSOs (with nuclear luminosities that lie around the knee of the luminosity function) studied using uniform, deep far-infrared photometry. We study trends of the mean SFR with redshift, black hole mass, nuclear bolometric luminosity, and specific accretion rate (Eddington ratio). To minimize systematics, we have undertaken a uniform determination of SMBH properties, as well as an analysis of important selection effects of spectroscopic QSO samples that influence the interpretation of SFR trends. We find that the mean SFRs of these QSOs are consistent with those of normal massive star-forming galaxies with a fixed scaling between SMBH and galaxy mass at all redshifts. No strong enhancement in SFR is found even among the most rapidly accreting systems, at odds with several co-evolutionary models. Finally, we consider the qualitative effects on mean SFR trends from different assumptions about the SF properties of QSO hosts and from redshift evolution of the SMBH-galaxy relationship. While currently limited by uncertainties, valuable constraints on AGN-galaxy co-evolution can emerge from our approach.

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“…For this reason, we use the Herschel/PACS catalog of the COSMOS field, which was extracted using the positions of 24 μm sources as a prior. The data comes from the PACS evolutionary probe survey (PEP, Lutz et al 2011). We fitted the 100 μm and 160 μm PACS flux densities with Magdis et al (2012) templates in order to derive L IR of each galaxy and assume the same conversion factor between L IR and SFR as for MIPS.…”

Section: Herschel/pacs Datamentioning

confidence: 99%

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

Béthermin

Kilbinger

Daddi

et al. 2014

A&A

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Using a sample of 25 683 star-forming and 2821 passive galaxies at z ∼ 2, selected in the COSMOS field following the BzK color criterion, we study the hosting halo mass and environment of galaxies as a function of their physical properties. Spitzer and Herschel allow us to obtain accurate star formation rate estimates for starburst galaxies. We measure the autocorrelation and cross-correlation functions of various galaxy subsamples and infer the properties of their hosting halos using both a halo occupation model and the linear bias at large scale. We find that passive and star-forming galaxies obey a similarly rising relation between the halo and stellar mass. The mean host halo mass of star-forming galaxies increases with the star formation rate between 30 M yr −1 and 200 M yr −1 , but flattens for higher values, except if we select only main-sequence galaxies. This reflects the expected transition from a regime of secular coevolution of the halos and the galaxies to a regime of episodic starburst. We find similar large-scale biases for mainsequence, passive, and starburst galaxies at equal stellar mass, suggesting that these populations live in halos of the same mass. However, we detect an excess of clustering on small scales for passive galaxies and showed, by measuring the large-scale bias of close pairs of passive galaxies, that this excess is caused by a small fraction (∼16%) of passive galaxies being hosted by massive halos (∼3 × 10 13 M ) as satellites. Finally, extrapolating the growth of halos hosting the z ∼ 2 population, we show that M ∼ 10 10 M galaxies at z ∼ 2 will evolve, on average, into massive (M ∼ 10 11 M ), field galaxies in the local Universe and M ∼ 10 11 M galaxies at z = 2 into local, massive, group galaxies. We also identify two z ∼ 2 populations which should end up in today's clusters: massive (>M ∼ 10 11 M ), strongly star-forming (>200 M yr −1 ), main-sequence galaxies, and close pairs of massive, passive galaxies.

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PACS Evolutionary Probe (PEP) – AHerschelkey program

Cited by 494 publications

References 72 publications

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

The mean star-forming properties of QSO host galaxies

Clustering, host halos, and environment ofz ~ 2 galaxies as a function of their physical properties

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