Modelling galaxy and AGN evolution in the infrared: black hole accretion versus star formation activity

Gruppioni, C.; Pozzi, F.; Zamorani, G.; Vignali, C.

doi:10.1111/j.1365-2966.2011.19006.x

Cited by 40 publications

(53 citation statements)

References 109 publications

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“…total IR luminosity functions from different evolutionary models (i.e. Valiante et al 2009;Franceschini et al 2010;Gruppioni et al 2011) into line luminosity functions and to derive the numbers of objects detectable by SPICA at different redshifts and luminosities. This approach -purely empirical -could be taken as an upper limit for the SPICA detections, since it applies the relations found for a sample of AGNs to all the AGN populations considered in the models, regardless of the AGN contribution to LIR, while -thanks to Herschel -we now know that LIR in IR detected AGNs is typically composed by both AGN and starburst contributions (Hatziminaoglou et al 2010) in different proportions (in large fractions of objects the AGN contributes to LIR for <10%; see Delvecchio et al 2014).…”

Section: Line Luminosity Functions and Number Countsmentioning

confidence: 99%

“…Their calculations were based on the phenomenological evolutionary models by Franceschini et al (2010), Gruppioni et al (2011) and Valiante et al (2009). The Franceschini et al (2010) and the Gruppioni et al (2011) models, like most classical backward evolution models, evolve the star forming galaxies and the AGNs independently. This class of models have been quite successful in reproducing far-IR to sub-millimeter source counts but are clearly unable to predict the composite line spectra of galaxies in which star formation and AGN activity co-exist.…”

Section: Introductionmentioning

confidence: 99%

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Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

Bonato

Negrello

Cai

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present new estimates of redshift-dependent luminosity functions of IR lines detectable by SPICA/SAFARI and excited both by star formation and by AGN activity. The new estimates improve over previous work by using updated evolutionary models and dealing in a self consistent way with emission of galaxies as a whole, including both the starburst and the AGN component. New relationships between line and AGN bolometric luminosity have been derived and those between line and IR luminosities of the starburst component have been updated. These ingredients were used to work out predictions for the source counts in 11 mid/far-IR emission lines partially or entirely excited by AGN activity. We find that the statistics of the emission line detection of galaxies as a whole is mainly determined by the star formation rate, because of the rarity of bright AGNs. We also find that the slope of the line integral number counts is flatter than 2 implying that the number of detections at fixed observing time increases more by extending the survey area than by going deeper. We thus propose a wide spectroscopic survey of 1 hour integration per field-of-view over an area of 5 deg 2 to detect (at 5σ) ∼760 AGNs in [OIV]25.89µm − the brightest AGN mid-infrared line − out to z ∼ 2. Pointed observations of strongly lensed or hyper-luminous galaxies previously detected by large area surveys such as those by Herschel and by the SPT can provide key information on the galaxy-AGN co-evolution out to higher redshifts.

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Section: Line Luminosity Functions and Number Countsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

Bonato

Negrello

Cai

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…To extend the Σ(SFR)/Mz relation to the field regime, i.e. to dark matter halo masses typical of field galaxies, we use published global SFR densities at different redshifts (Madau et al 1998;Gruppioni et al 2011;Magnelli et al 2011). …”

Section: In the Localmentioning

confidence: 99%

The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

Popesso¹,

Biviano²,

Rodighiero³

et al. 2012

A&A

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102

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Aims. Star formation in massive galaxies is quenched at some point during hierarchical mass assembly. To understand where and when the quenching processes takes place, we study the evolution of the total star formation rate per unit total halo mass (Σ(SFR)/M) in three different mass scales: low mass halos (field galaxies), groups, and clusters, up to a redshift z ≈ 1.6. Methods. We use deep far-infrared PACS data at 100 and 160 µm to accurately estimate the total star formation rate of the Luminous Infrared Galaxy population of 9 clusters with mass ∼ 10 15 M ⊙ , and 9 groups/poor clusters with mass ∼ 5 × 10 13 M ⊙ . Estimates of the field Σ(SFR)/M are derived from the literature, by dividing the star formation rate density by the mean comoving matter density of the universe.Results. The field Σ(SFR)/M increases with redshift up to z ∼ 1 and it is constant thereafter. The evolution of the Σ(SFR)/M-z relation in galaxy systems is much faster than in the field. Up to redshift z ∼ 0.2, the field has a higher Σ(SFR)/M than galaxy groups and galaxy clusters. At higher redshifts, galaxy groups and the field have similar Σ(SFR)/M, while massive clusters have significantly lower Σ(SFR)/M than both groups and the field. There is a hint of a reversal of the SFR activity vs. environment at z ∼ 1.6, where the group Σ(SFR)/M lies above the field Σ(SFR)/M -z relation. We discuss possible interpretations of our results in terms of the processes of downsizing, and star-formation quenching.

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“…For this reason, we study the evolution of the IR LF of galaxies in groups, and compare it to that of more isolated field galaxies. While the IR LF of field galaxies and its evolution are relatively well known up to z ∼ 2.5−3 (Caputi et al 2007;Magnelli et al 2009;Gruppioni et al 2011Gruppioni et al , 2013Reddy et al 2008), the IR LF of galaxies in groups and clusters is still poorly known.…”

Section: Introductionmentioning

confidence: 99%

The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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Context. There is now a large consensus that the current epoch of the cosmic star formation history (CSFH) is dominated by low mass galaxies while the most active phase, between redshifts 1 and 2, is dominated by more massive galaxies, which evolve more quickly. Aims. Massive galaxies tend to inhabit very massive haloes, such as galaxy groups and clusters. We aim to understand whether the observed "galaxy downsizing" could be interpreted as a "halo downsizing", whereas the most massive haloes, and their galaxy populations, evolve more rapidly than the haloes with lower mass. Methods. We studied the contribution to the CSFH of galaxies inhabiting group-sized haloes. This is done through the study of the evolution of the infra-red (IR) luminosity function of group galaxies from redshift 0 to redshift ∼1.6. We used a sample of 39 X-rayselected groups in the Extended Chandra Deep Field South (ECDFS), the Chandra Deep Field North (CDFN), and the COSMOS field, where the deepest available mid-and far-IR surveys have been conducted with Spitzer MIPS and with the Photodetector Array Camera and Spectrometer (PACS) on board the Herschel satellite. Results. Groups at low redshift lack the brightest, rarest, and most star forming IR-emitting galaxies observed in the field. Their IR-emitting galaxies contribute ≤10% of the comoving volume density of the whole IR galaxy population in the local Universe. At redshift 1, the most IR-luminous galaxies (LIRGs and ULIRGs) are mainly located in groups, and this is consistent with a reversal of the star formation rate (SFR) vs. density anti-correlation observed in the nearby Universe. At these redshifts, group galaxies contribute 60-80% of the CSFH, i.e. much more than at lower redshifts. Below z ∼ 1, the comoving number and SFR densities of IR-emitting galaxies in groups decline significantly faster than those of all IR-emitting galaxies. Conclusions. Our results are consistent with a "halo downsizing" scenario and highlight the significant role of "environment" quenching in shaping the CSFH.

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Modelling galaxy and AGN evolution in the infrared: black hole accretion versus star formation activity

Cited by 40 publications

References 109 publications

Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

Exploring the relationship between black hole accretion and star formation with blind mid-/far-infrared spectroscopic surveys

The evolution of the star formation activity per halo mass up to redshift ~1.6 as seen byHerschel

The evolution of galaxy star formation activity in massive haloes

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