The H α star formation main sequence in cluster and field galaxies at <i>z</i> ∼ 1.6

Nantais, Julie; Wilson, Gillian; Muzzin, Adam; Old, Lyndsay; Demarco, R.; Cerulo, P.; Balogh, Michael L.; Rudnick, Gregory; Chan, J.; Cooper, Michael C.; Forrest, Ben; Hayden, Brian; Lidman, C.; Noble, Allison; Perlmutter, S.; Rhea, Carter; Surace, J.; Burg, R. F. J. van der; Kampen, E. van

doi:10.1093/mnras/staa2872

Cited by 13 publications

(14 citation statements)

References 89 publications

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“…As detailed in Section 2.6, we follow the same method explained in Section 6.2 of Whitaker et al (2014) to calculate Hα SFRs from our G141 grism spectroscopy. We also overplot the Hα SFMSs from Figure 8 In general, it can be seen that the cluster star-forming galaxies in our sample are fairly typical, with an Hα SFMS following the field Hα SFMS (as also seen by many other works, e.g., Koyama et al 2013;Nantais et al 2020) from 3D-HST, which forms our comparative field sample.…”

Section: The Star Formation Main Sequence Of the Samplesupporting

confidence: 56%

“…e.g., Koyama et al 2013;Tran et al 2016;Nantais et al 2020), stellar mass functions (SMFs, e.g., , metallicities (e.g., Kacprzak et al 2015;Tran et al 2015), kinematics (Alcorn et al 2016), and sizes and morphologies (Tran et al 2016;Matharu et al 2019) to coeval field star-forming galaxies. Furthermore, most studies in the literature argue for rapid environmental quenching in highredshift galaxy clusters (see Foltz et al 2018 and references therein).…”

Section: Cuts On Hα S/n and F140w Axis Ratiomentioning

confidence: 99%

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HST/WFC3 Grism Observations of z ∼ 1 Clusters: Evidence for Rapid Outside-in Environmental Quenching from Spatially Resolved Hα Maps

Matharu

Muzzin

Brammer

et al. 2021

ApJ

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We present and publicly release (www.gclasshst.com) the first spatially resolved Hα maps of star-forming cluster galaxies at z ∼ 1, made possible with the Wide Field Camera 3 (WFC3) G141 grism on the Hubble Space Telescope (HST). Using a similar but updated method to 3D-HST in the field environment, we stack the Hα maps in bins of stellar mass, measure the half-light radius of the Hα distribution, and compare it to the stellar continuum. The ratio of the Hα to stellar continuum half-light radius, R [ H α / C ] = R eff , H α R eff , Cont , is smaller in the clusters by (6 ± 9)%, but statistically consistent within 1σ uncertainties. A negligible difference in R[Hα/C] with environment is surprising, given the higher quenched fractions in the clusters relative to the field. We postulate that the combination of high quenched fractions and no change in R[Hα/C] with environment can be reconciled if environmental quenching proceeds rapidly. We investigate this hypothesis by performing similar analysis on the spectroscopically confirmed, recently quenched cluster galaxies. 87% have Hα detections, with star formation rates 8 ± 1 times lower than star-forming cluster galaxies of similar stellar mass. Importantly, these galaxies have an R[Hα/C] that is (81 ± 8)% smaller than coeval star-forming field galaxies at fixed stellar mass. This suggests the environmental quenching process occurred outside-in. We conclude that disk truncation due to ram pressure stripping is occurring in cluster galaxies at z ∼ 1, but more rapidly and/or efficiently than in z ≲ 0.5 clusters, such that the effects on R[Hα/C] become observable just after the cluster galaxy has recently quenched.

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Section: The Star Formation Main Sequence Of the Samplesupporting

confidence: 56%

Section: Cuts On Hα S/n and F140w Axis Ratiomentioning

confidence: 99%

HST/WFC3 Grism Observations of z ∼ 1 Clusters: Evidence for Rapid Outside-in Environmental Quenching from Spatially Resolved Hα Maps

Matharu

Muzzin

Brammer

et al. 2021

ApJ

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“…Alternatively, Erfanianfar et al (2016), using data from the COSMOS, AEGIS, ECDFS, and CDFN fields, could not find any difference in the MS between field galaxies and those in structures in the redshift range 0.5 < z < 1.1, but a similar trend to that of Old et al (2020b) in the lowest redshift regime (0.15 < z < 0.5). On the other hand, Nantais et al (2020) could not find any significant difference between field and SpARCS (Muzzin et al 2009) cluster galaxies at a redshift z ∼ 1.6, which they explained either by the fact that galaxies might have been accreted too recently to show signs of quenching, or that the clusters might be not mature enough yet at this redshift to produce measurable environmental effects on these galaxies.…”

Section: Introductionmentioning

confidence: 86%

Scaling relations of z~0.25-1.5 galaxies in various environments from the morpho-kinematic analysis of the MAGIC sample

Mercier,

Epinat,

Contini

et al. 2022

Preprint

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Context. The evolution of galaxies is influenced by many physical processes which may vary depending on their environment. Aims. We combine Hubble Space Telescope (HST) and Multi-Unit Spectroscopic Explorer (MUSE) data of galaxies at 0.25 z 1.5 to probe the impact of environment on the size-mass relation, the Main Sequence (MS) and the Tully-Fisher relation (TFR). Methods. We perform a morpho-kinematic modelling of 593 [O ii] emitters in various environments in the COSMOS area from the MUSE-gAlaxy Groups In Cosmos (MAGIC) survey. The HST F814W images are modelled with a bulge-disk decomposition to estimate their bulge-disk ratio, effective radius, and disk inclination. We use the [O ii]λλ3727, 3729 doublet to extract the galaxies ionised gas kinematic maps from the MUSE cubes, and we model those maps for a sample of 146 [O ii] emitters, including bulge and disk components constrained from morphology and a dark matter halo. Results. We find an offset of 0.03 dex (1σ significant) on the size-mass relation zero point between the field and the large structure subsamples, with a richness threshold of N = 10 to separate between small and large structures, and of 0.06 dex (2σ) with N = 20. Similarly, we find a 0.1 dex (2σ) difference on the MS with N = 10 and 0.15 dex (3σ) with N = 20. These results suggest that galaxies in massive structures are smaller by 14% and have star formation rates reduced by a factor of 1.3 − 1.5 with respect to field galaxies at z ≈ 0.7. Finally, we do not find any impact of the environment on the TFR, except when using N = 20 with an offset of 0.04 dex (1σ). We discard the effect of quenching for the largest structures that would lead to an offset in the opposite direction. We find that, at z ≈ 0.7, if quenching impacts the mass budget of galaxies in structures, these galaxies would have been affected quite recently, for roughly 0.7 − 1.5 Gyr. This result holds when including the gas mass, but vanishes once we include the asymmetric drift correction.

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“…One of the ways to study galaxy evolution is to analyse the relation between SFR and stellar mass to check their location in comparison to the MS of star-forming galaxies (e.g., Elbaz et al 2007;Whitaker et al 2012;Davies et al 2016;Leslie et al 2016;Pović et al 2016;Elbaz et al 2018;Popesso et al 2019;Nantais et al 2020). The details on SFR and stellar mass measurements are explained briefly in Section 2, with more details given in Mahoro et al (2017).…”

Section: Main Sequence Of Star Formationmentioning

confidence: 99%

Stellar populations of a sample of far-IR AGN and non-AGN green valley galaxies

Mahoro,

Pović,

Väisänen

et al. 2022

Preprint

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We present a study on the stellar populations and stellar ages of a sub-sample of farinfrared AGN and non-AGN green valley galaxies analysed in Mahoro et al. (2017Mahoro et al. ( , 2019 at 0.6 < z < 1.0 using the data from the COSMOS field. We used long-slit spectroscopy and derived stellar populations and stellar ages using the stellar population synthesis code "STARLIGHT" and analysed the available Lick/IDS indices, such as Dn4000 and Hδ A . We find that both FIR AGN and non-AGN green valley galaxies are dominated by intermediate stellar populations 67% and 53%, respectively. The median stellar ages for AGN and non-AGN are log t = 8.5 [yr] and log t = 8.4 [yr], respectively. We found that majority of our sources (62% of AGN and 66% of non-AGN) could have experienced bursts and continuous star formation. In addition, most of our FIR AGN (38%) compared to FIR non-AGN (27%) might have experienced a burst of SF more than 0.1 Gyr ago. We also found that our FIR AGN and non-AGN green valley galaxies have similar quenching time-scales of ∼ 70 Myr. Therefore, the results obtained here are in line with our previous results where we do not find that our sample of FIR AGN in the green valley shows signs of negative AGN feedback, as has been suggested previously in optical studies.

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The H α star formation main sequence in cluster and field galaxies at z ∼ 1.6

Cited by 13 publications

References 89 publications

HST/WFC3 Grism Observations of z ∼ 1 Clusters: Evidence for Rapid Outside-in Environmental Quenching from Spatially Resolved Hα Maps

HST/WFC3 Grism Observations of z ∼ 1 Clusters: Evidence for Rapid Outside-in Environmental Quenching from Spatially Resolved Hα Maps

Scaling relations of z~0.25-1.5 galaxies in various environments from the morpho-kinematic analysis of the MAGIC sample

Stellar populations of a sample of far-IR AGN and non-AGN green valley galaxies

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