HELP: star formation as a function of galaxy environment with<i>Herschel</i>

Duivenvoorden, Steven; Oliver, Seb; Buat, V.; Darvish, Behnam; Efstathiou, A.; Farrah, D.; Griffin, Matthew Joseph; Hurley, P. D.; Ibar, E.; Jarvis, Matt J.; Papadopoulos, A.; Sargent, M.; Scott, Douglas; Scudder, Jillian M.; Symeonidis, M.; Vaccari, M.; Viero, Marco P.; Wang, L.

doi:10.1093/mnras/stw1466

Cited by 11 publications

(12 citation statements)

References 91 publications

(107 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Results tend to agree that higher density environments increase the fraction of quiescent (red) galaxies and we do see this in the COSMOS field (see top right panel of Figure 28; Peng et al 2010;McGee et al 2011;Scoville et al 2013;Darvish et al 2014Darvish et al , 2016. Whether or not the normalization of the MS (defined for starforming galaxies) depends on galaxy environment is still under debate, but many studies identify no variations of MS with environments such as clusters and voids, e.g., Tyler et al (2013), Koyama et al (2014), Ricciardelli et al (2014), Tyler et al (2014), Grossi et al (2018), Paulino-Afonso et al (2019), Pharo et al (2020 (although see Duivenvoorden et al 2016 who found a difference at 1.5 < z < 2 in COSMOS). However, at low redshift (z < 0.3), studies have reported a clear dependence of the MS on galaxy environment (e.g., von der Linden et al 2010, Haines et al 2013, Gu et al 2018, Paccagnella et al 2016).…”

Section: Environmental Trendsmentioning

confidence: 56%

“…for all star-forming galaxies) is shown in each redshift bin. Duivenvoorden et al (2016) found that the (IR) SFR decreases (by < 0.2 dex) with local density out to z < 2 in the COSMOS field. However, both our results have large uncertainties and the decreasing trend reported by Duivenvoorden et al (2016) was only significant at 1.5 < z < 2.…”

Section: Morphology Trendsmentioning

confidence: 88%

“…Duivenvoorden et al (2016) found that the (IR) SFR decreases (by < 0.2 dex) with local density out to z < 2 in the COSMOS field. However, both our results have large uncertainties and the decreasing trend reported by Duivenvoorden et al (2016) was only significant at 1.5 < z < 2. The completeness corrected total cosmic SFRD from Duivenvoorden et al (2016) is shown in Figure 8, and is consistent with our SFRD at z ∼ 2.…”

Section: Morphology Trendsmentioning

confidence: 88%

See 2 more Smart Citations

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Leslie

Schinnerer

Liu

et al. 2020

ApJ

120

143

View full text Add to dashboard Cite

We provide a coherent, uniform measurement of the evolution of the logarithmic star formation rate (SFR) -stellar mass (M * ) relation, called the main sequence of star-forming galaxies (MS), for starforming and all galaxies out to z ∼ 5. We measure the MS using mean stacks of 3 GHz radio continuum images to derive average SFRs for ∼ 200,000 mass-selected galaxies at z > 0.3 in the COSMOS field. We describe the MS relation adopting a new model that incorporates a linear relation at low stellar mass (log(M * /M )<10) and a flattening at high stellar mass that becomes more prominent at low redshift (z < 1.5). We find that the SFR density peaks at 1.5 < z < 2 and at each epoch there is a characteristic stellar mass (M * = 1−4×10 10 M ) that contributes the most to the overall SFR density. This characteristic mass increases with redshift, at least to z ∼ 2.5. We find no significant evidence for variations in the MS relation for galaxies in different environments traced by the galaxy number density at 0.3 < z < 3, nor for galaxies in X-ray groups at z ∼ 0.75. We confirm that massive bulgedominated galaxies have lower SFRs than disk-dominated galaxies at a fixed stellar mass at z < 1.2. As a consequence, the increase in bulge-dominated galaxies in the local star-forming population leads to a flattening of the MS at high stellar masses. This indicates that "mass-quenching" is linked with changes in the morphological composition of galaxies at a fixed stellar mass.

show abstract

Section: Environmental Trendsmentioning

confidence: 56%

Section: Morphology Trendsmentioning

confidence: 88%

Section: Morphology Trendsmentioning

confidence: 88%

See 1 more Smart Citation

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Leslie

Schinnerer

Liu

et al. 2020

ApJ

120

143

View full text Add to dashboard Cite

show abstract

“…Chuter et al (2011) and Quadri et al (2012) find that the relation holds up to z ∼ 2 in UDS data. Duivenvoorden et al (2016) find in the Herschel Extragalactic Legacy Survey (HELP) that their data is consistent with no environmental dependence at z > 2. Conversely, Elbaz et al (2007) and Welikala et al (2015), find the relation reversing in the Great Observatories Origins Deep Survey and South Pole Telescope data (with some simulations reporting similar results e.g.…”

Section: Quenching Over Cosmic Timementioning

confidence: 89%

Environmental quenching and galactic conformity in the galaxy cross-correlation signal

Hatfield

Jarvis

2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

It has long been known that environment has a large effect on star formation in galaxies. There are several known plausible mechanisms to remove the cool gas needed for star formation, such as strangulation, harassment and ram-pressure stripping. It is unclear which process is dominant, and over what range of stellar mass. In this paper, we find evidence for suppression of the cross-correlation function between massive galaxies and less massive star-forming galaxies, giving a measure of how less likely a galaxy is to be star-forming in the vicinity of a more massive galaxy. We develop a formalism for modelling environmental quenching mechanisms within the Halo Occupation Distribution scheme. We find that at z ∼ 2 environment is not a significant factor in determining quenching of star-forming galaxies, and that galaxies are quenched with similar probabilities when they are satellites in sub-group environments, as they are globally. However, by z ∼ 0.5 galaxies are much less likely to be star forming when in a high density (group or low-mass cluster) environment than when not. This increased probability of being quenched does not appear to have significant radial dependence within the halo at lower redshifts, supportive of the quenching being caused by the halting of fresh inflows of pristine gas, as opposed to by tidal stripping. Furthermore, by separating the massive sample into passive and star-forming, we see that this effect is further enhanced when the central galaxy is passive, a manifestation of galactic conformity.All magnitudes are given in the AB system (Oke & Gunn 1983) and all calculations are in the concordance cosmology ΩΛ = 0.7, Ωm = 0.3 and H0 = 70 km s −1 Mpc −1 unless otherwise stated.

show abstract

“…Daddi et al 2007;Elbaz et al 2007;Whitaker et al 2012;Speagle et al 2014), while there is very little environmental dependence at fixed redshift (e.g. Peng et al 2010;McGee et al 2011;Koyama et al 2013;Lin et al 2014;Koyama et al 2014;Darvish et al 2016;Duivenvoorden et al 2016;Wagner et al 2017). Koyama et al (2013) compared the SFR-M⋆ relation for Hα-selected galaxies in clusters and fields at z=0.4-2.2, and conclude that the environmental variation of the SF main sequence is always small over the last ∼10-Gyrs (with ∼0.2-dex at maximum).…”

Section: Introductionmentioning

confidence: 99%

The nature of H α-selected galaxies along the large-scale structure at z = 0.4 revealed by Subaru Hyper Suprime-Cam survey

Koyama

Hayashi

Tanaka

et al. 2017

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

We present the environmental dependence of colour, stellar mass, and star formation (SF) activity in Hα-selected galaxies along the large-scale structure at z=0.4 hosting twin clusters in DEEP2-3 field, discovered by Subaru Strategic Programme of Hyper Suprime-Cam (HSC SSP). By combining photo-z selected galaxies and Hα emitters selected with broad-band and narrow-band (NB) data of the recent data release of HSC SSP (DR1), we confirm that galaxies in higher-density environments or galaxies in the cluster central regions show redder colours. We find that there still remains a possible colour-density and colour-radius correlation even if we restrict the sample to Hα-selected galaxies, likely due to the presence of massive Hα emitters in denser regions. We also find a hint of increased star formation rates (SFR) amongst Hα emitters towards the highest-density environment, again primarily driven by the excess of red/massive Hα emitters in high-density environment, while their specific SFR does not significantly change with environment. This work demonstrates the power of the HSC SSP NB

show abstract

HELP: star formation as a function of galaxy environment withHerschel

Cited by 11 publications

References 91 publications

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

The VLA-COSMOS 3 GHz Large Project: Evolution of Specific Star Formation Rates out to z ∼ 5

Environmental quenching and galactic conformity in the galaxy cross-correlation signal

The nature of H α-selected galaxies along the large-scale structure at z = 0.4 revealed by Subaru Hyper Suprime-Cam survey

Contact Info

Product

Resources

About