Herschel-ATLAS/GAMA: How does the far-IR luminosity function depend on galaxy group properties?

Guo, Qi; Lacey, Cedric G.; Norberg, Peder; Cole, Shaun; Baugh, C. M.; Frenk, Carlos S.; Cooray, Asantha; Dye, S.; Bourne, Nicholas; Dunne, L.; Eales, Stephen Anthony; Ivison, R. J.; Maddox, S.; Alpasan, M.; Baldry, I. K.; Bland-Hawthorn, Joss; Driver, Simon P.; Robotham, Aaron S. G.

doi:10.1093/mnras/stu962

Cited by 8 publications

(27 citation statements)

References 98 publications

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“…Our IR LFs do not sample the z < 0.1 redshift range. For this we use the lowest redshift determination of the IR LF of the Robotham et al (2011) groups by Guo et al (2014). This LF is based on the 250 μm luminosity (L ν (250 μm)) of the H-ATLAS SPIRE survey of a 135 deg 2 region.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

“…This LF is based on the 250 μm luminosity (L ν (250 μm)) of the H-ATLAS SPIRE survey of a 135 deg 2 region. In addition, we use also the LFs derived by Guo et al (2014) in the other redshift bins A105, page 6 of 14 Fig. 4.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

“…Error bars are 1σ. The IR LF in groups in the lowest redshift bin at z < 0.1 (blue points) is obtained by averaging the IR LF in groups obtained in three different group halo mass bins by Guo et al (2014). The solid (resp.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

“…For a meaningful comparison, we average the LFs obtained by Guo et al (2014) in several group mass bins from 10 12.5 to 10 13 M . We use as error bars the dispersion of the LF in any L ν (250 μm) luminosity bin.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

“…As a last step we use Eq. (2) of Guo et al (2014) to transform the group L ν (250 μm) LF into the IR LF in groups.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

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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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Section: The Composite Lf: Resultsmentioning

confidence: 99%

Section: The Composite Lf: Resultsmentioning

confidence: 99%

Section: The Composite Lf: Resultsmentioning

confidence: 99%

Section: The Composite Lf: Resultsmentioning

confidence: 99%

“…As a last step we use Eq. (2) of Guo et al (2014) to transform the group L ν (250 μm) LF into the IR LF in groups.…”

Section: The Composite Lf: Resultsmentioning

confidence: 99%

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The evolution of galaxy star formation activity in massive haloes

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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The role of massive halos in the star formation history of the Universe

Popesso

Biviano

Finoguenov

et al. 2015

A&A

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Context. The most striking feature of the cosmic star formation history (CSFH) of the Universe is a dramatic drop in the star formation (SF) activity after z ∼ 1. Aims. In this work we investigate whether the very same process of assembly and growth of structures is one of the major drivers of the observed decline in the Universe's SF activity. Methods. We study the contribution to the CSFH of galaxies in halos of different masses. This is done by studying the total SF ratehalo mass-redshift plane from redshift 0 to redshift ∼1.6 in a sample of 57 groups and clusters by using the deepest available midand far-infrared surveys conducted with Spitzer MIPS and Herschel PACS and SPIRE, on blank (ECDFS, CDFN, and the COSMOS) and cluster fields. Results. Our results show that low mass groups (M halo ∼ 6 × 10 12 −6 × 10 13 M ) provide a 60−80% contribution to the CSFH at z ∼ 1. This contribution has declined faster than the CSFH in the past 8 billion years to less than 10% at z < 0.3, where the overall SF activity is sustained by lower mass halos. More massive systems (M halo > 6 × 10 13 M ) provide only a marginal contribution (<10%) at any epoch. A simplified abundance-matching method shows that the large contribution of low mass groups at z ∼ 1 is due to a large fraction (>50%) of very massive, highly star-forming main sequence galaxies. Below z ∼ 1 a quenching process must take place in massive halos to cause the observed faster suppression of their SF activity. Such a process must be a slow one, though, since most of the models implementing a rapid quenching of the SF activity in accreting satellites significantly underpredict the observed SF level in massive halos at any redshift. This would rule out short time-scale mechanisms such as ram pressure stripping. Instead, starvation or the satellite's transition from cold to hot accretion would provide a quenching timescale of 1 to few Gyr that is more consistent with the observations. Conclusions. Our results suggest a scenario in which, owing to the structure formation process, more and more galaxies experience the group environment and the associated quenching process in the past 8 billion years. This leads to the progressive suppression of their SF activity so that it shapes the CSFH below z ∼ 1.

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Galaxy and mass assembly: luminosity and stellar mass functions in GAMA groups

Vázquez-Mata

Loveday

Riggs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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How do galaxy properties (such as stellar mass, luminosity, star formation rate, and morphology) and their evolution depend on the mass of their host dark matter halo? Using the Galaxy and Mass Assembly (GAMA) group catalogue, we address this question by exploring the dependence on host halo mass of the luminosity function (LF) and stellar mass function (SMF) for grouped galaxies subdivided by colour, morphology and central/satellite. We find that spheroidal galaxies in particular dominate the bright and massive ends of the LF and SMF, respectively. More massive haloes host more massive and more luminous central galaxies. The satellite LF and SMF respectively show a systematic brightening of characteristic magnitude, and increase in characteristic mass, with increasing halo mass. In contrast to some previous results, the faint-end and low-mass slopes show little systematic dependence on halo mass. Semi-analytic models and simulations show similar or enhanced dependence of central mass and luminosity on halo mass. Faint and low-mass simulated satellite galaxies are remarkably independent of halo mass, but the most massive satellites are more common in more massive groups. In the first investigation of low-redshift LF and SMF evolution in group environments, we find that the red/blue ratio of galaxies in groups has increased since redshift z ≈ 0.3 relative to the field population. This observation strongly suggests that quenching of star formation in galaxies as they are accreted into galaxy groups is a significant and ongoing process.

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Herschel-ATLAS/GAMA: How does the far-IR luminosity function depend on galaxy group properties?

Cited by 8 publications

References 98 publications

The evolution of galaxy star formation activity in massive haloes

The evolution of galaxy star formation activity in massive haloes

The role of massive halos in the star formation history of the Universe

Galaxy and mass assembly: luminosity and stellar mass functions in GAMA groups

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