The GOGREEN survey: transition galaxies and the evolution of environmental quenching

McNab, Karen; Balogh, Michael L.; Burg, R. F. J. van der; Forestell, Anya; Webb, Kristi; Vulcani, Benedetta; Rudnick, Gregory; Muzzin, Adam; Cooper, Michael C.; McGee, Sean L.; Biviano, A.; Cerulo, P.; Chan, J.; Lucia, G. De; Demarco, R.; Finoguenov, A.; Forrest, Ben; Golledge, Caelan; Jablonka, P.; Lidman, C.; Nantais, Julie; Old, Lyndsay; Pintos-Castro, Irene; Poggianti, Bianca M.; Reeves, Andrew M. M.; Wilson, Gillian; Yee, H. K. C.; Zaritsky, Dennis

doi:10.1093/mnras/stab2558

Cited by 21 publications

(23 citation statements)

References 97 publications

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“…In other words the GALEX data did not reveal a significant missing component of star-formation from the IR analysis. This is consistent with the high environmental quenching efficiencies of low mass galaxies reported at z < 1.5 (Kawinwanichakij et al 2017;Papovich et al 2018;McNab et al 2021), which as a population must therefore play an important role in setting the evolution of clusters (A21, van der Burg et al 2018). There is tentative evidence for low gas reservoirs and low depletion timescales in log M/M * > 9.5 cluster star-forming galaxies at z ∼ 0.75 (Betti et al 2019), and at z ∼ 1.4 (Alberts et al, submitted) which supports that gas removal is driving a "delayed then rapid" quenching scenario (i.e., Wetzel et al 2013); however, future observations of the gas content in lower mass cluster galaxies are necessary to further test this scenario.…”

Section: Discussionsupporting

confidence: 79%

Measuring the Total Ultraviolet Light from Galaxy Clusters at z=0.5-1.6: The Balance of Obscured and Unobscured Star-Formation

McKinney,

Ramakrishnan,

Lee

et al. 2022

Preprint

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Combined observations from UV to IR wavelengths are necessary to fully account for the star-formation in galaxy clusters. Low mass log M/M * < 10 galaxies are typically not individualy detected, particularly at higher redshifts (z ∼ 1 − 2) where galaxy clusters are undergoing rapid transitions from hosting mostly active, dust-obscured starforming galaxies to quiescent, passive galaxies. To account for these undetected galaxies, we measure the total light emerging from GALEX/N U V stacks of galaxy clusters between z = 0.5 − 1.6. Combined with existing measurements from Spitzer, WISE, and Herschel, we study the average UV through far-infrared (IR) spectral energy distribution (SED) of clusters. From the SEDs, we measure the total stellar mass and amount of dust-obscured and unobscured star-formation arising from all cluster-member galaxies, including the low mass population. The relative fraction of unobscured star-formation we observe in the UV is consistent with what is observed in field galaxies. There is tentative evidence for lower than expected unobscured star-formation at z ∼ 0.5, which may arise from rapid redshift evolution in the low mass quenching efficiency in clusters reported by other studies. Finally, the GALEX data places strong constraints on derived stellar-to-halo mass ratios at z < 1 which anti-correlate with the total halo mass, consistent with trends found from local X-ray observations of clusters. The data exhibit steeper slopes than implementations of the cluster star-formation efficiency in semi-analytical models.

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Section: Discussionsupporting

confidence: 79%

Measuring the Total Ultraviolet Light from Galaxy Clusters at z=0.5-1.6: The Balance of Obscured and Unobscured Star-Formation

McKinney,

Ramakrishnan,

Lee

et al. 2022

Preprint

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“…The behaviour of QFE with M found in our work is similar to the one of QFE derived for high density environments (Balogh et al 2016;van der Burg et al 2020;McNab et al 2021). However, we find relevant differences with respect to cluster environments (McNab et al 2021;van der Burg et al 2020).…”

Section: Fraction Excess Of Quenched Galaxiessupporting

confidence: 88%

“…This difference can be measured by the quenched fraction excess (QFE). Here we adopt the definition given by McNab et al (2021) in their Eq. ( 4):…”

Section: Fraction Excess Of Quenched Galaxiesmentioning

confidence: 99%

“…Kauffmann et al 2004;Blanton & Moustakas 2009;Pasquali et al 2010;Lopes et al 2014;Cappellari 2016). There is strong evidence that the fraction of red galaxies increases with the density field for z < 1 (Woo et al 2013;Nantais et al 2016;Darvish et al 2016;Calvi et al 2018;Moutard et al 2018;Liu et al 2021;McNab et al 2021;Sobral et al 2021), although the quenched fraction is less significant at higher redshift. This result is equivalent to the well-known Bucther-Oemler effect (Butcher & Oemler 1984), which shows that the fraction of blue galaxies in clusters increases with redshift.…”

Section: Introductionmentioning

confidence: 97%

“…Good examples are SDSS (e.g. Yang et al 2007) and MaNGA (Bluck et al 2020) at low-redshift; and zCOSMOS (Peng et al 2012), CANDELS (Liu et al 2021), GOGREEN (Balogh et al 2017;McNab et al 2021), CLASH-VLT (Rosati et al 2014;Mercurio et al 2021) and LEGA-C (Sobral et al 2021) at higher redshifts. In general, multi-wavelength photometry and spectroscopic information are combined to get accurate redshifts and to identify the group and cluster galaxy members.…”

Section: Introductionmentioning

confidence: 99%

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The miniJPAS survey

Delgado

Rodríguez‐Martín

Díaz-García

et al. 2022

A&A

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The miniJPAS survey has observed ∼ 1 deg 2 on the AEGIS field with 60 bands (spectral resolution of R ∼ 60) in order to demonstrate the scientific potential of the Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) that will map ∼ 8000 deg 2 of the northern sky during the upcoming years. In particular, this paper shows the potential of J-PAS to detect groups with mass up to 10 13 M and the characterisation of their galaxy populations up to z ∼ 1. The parametric code BaySeAGal is used to derive the stellar population properties by fitting the J-PAS spectral energy distribution (SED) of the galaxy members in 80 groups at z ≤ 0.8 previously detected by the AMICO code, as well as for a galaxy field sample retrieved from the whole miniJPAS down to r < 22.75 (AB). Blue, red, quiescent, and transition (blue quiescent or green valley) galaxy populations are identified through their rest-frame (extinction corrected) (u − r) int colour, galaxy stellar mass (M ), and specific star formation rate (sSFR). We measure the abundance of these galaxies as a function of M and environment to investigate the role that groups play in quenching the star formation. We find: (i) The fraction of red and quiescent galaxies in groups increases with M and it is always higher in groups (28 % on average) than in the field (5 %). (ii) The quenched fraction excess (QFE) in groups shows a strong dependence with M , and increases from a few percent for galaxies with M < 10 10 M , to higher than 60 % for galaxies with M > 3 × 10 11 M . (iii) The abundance excess of transition galaxies in groups shows a modest dependence with M , being 5-10 % for galaxies with M < 10 11 M . (iv) The fading time scale, defined as the time that galaxies in groups spend in the transition phase, is very short (< 1.5 Gyr), indicating that the star formation of galaxies in groups declines very rapidly. (v) The evolution of the galaxy quenching rate in groups shows a modest but significant evolution since z ∼ 0.8. The result is compatible with the expected evolution with constant QFE = 0.4, which has been previously measured for satellites in the nearby Universe, as traced by SDSS. Further, this evolution is consistent with a scenario where the low-mass star-forming galaxies in clusters at z = 1-1.4 are environmentally quenched, as previously reported by other surveys.

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The miniJPAS survey

Rodríguez‐Martín

Delgado

Martínez-Solaeche

et al. 2022

A&A

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The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) is a photometric survey that is poised to scan several thousands of square degrees of the sky. It will use 54 narrow-band filters, combining the benefits of low-resolution spectra and photometry. Its offshoot, miniJPAS, is a 1 deg 2 survey that uses J-PAS filter system with the Pathfinder camera. In this work, we study mJPC2470-1771, the most massive cluster detected in miniJPAS. We survey the stellar population properties of the members, their star formation rates (SFR), star formation histories (SFH), the emission line galaxy (ELG) population, spatial distribution of these properties, and the ensuing effects of the environment. This work shows the power of J-PAS to study the role of environment in galaxy evolution. We used a spectral energy distribution (SED) fitting code to derive the stellar population properties of the galaxy members: stellar mass, extinction, metallicity, (u − r) res and (u − r) int colours, mass-weighted age, the SFH that is parametrised by a delayed-τ model (τ, t 0 ), and SFRs. We used artificial neural networks for the identification of the ELG population via the detection of the Hα, [NII], Hβ, and [OIII] nebular emission. We used the Ew(Hα)-[NII] (WHAN) and [OIII]/Hα-[NII]/Hα (BPT) diagrams to separate them into individual star-forming galaxies and AGNs. We find that the fraction of red galaxies increases with the cluster-centric radius; and at 0.5 R 200 the red and blue fractions are both equal. The redder, more metallic, and more massive galaxies tend to be inside the central part of the cluster, whereas blue, less metallic, and less massive galaxies are mainly located outside of the inner 0.5 R 200 . We selected 49 ELG, with 65.3 % of the them likely to be star-forming galaxies, dominated by blue galaxies, and 24 % likely to have an AGN (Seyfert or LINER galaxies). The rest are difficult to classify and are most likely composite galaxies. These latter galaxies are red, and their abundance decreases with the cluster-centric radius; in contrast, the fraction of star-forming galaxies increases outwards up to R 200 . Our results are compatible with an scenario in which galaxy members were formed roughly at the same epoch, but blue galaxies have had more recent star formation episodes, and they are quenching out from within the cluster centre. The spatial distribution of red galaxies and their properties suggest that they were quenched prior to the cluster accretion or an earlier cluster accretion epoch. AGN feedback or mass might also stand as an obstacle in the quenching of these galaxies.

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The GOGREEN survey: transition galaxies and the evolution of environmental quenching

Cited by 21 publications

References 97 publications

Measuring the Total Ultraviolet Light from Galaxy Clusters at z=0.5-1.6: The Balance of Obscured and Unobscured Star-Formation

Measuring the Total Ultraviolet Light from Galaxy Clusters at z=0.5-1.6: The Balance of Obscured and Unobscured Star-Formation

The miniJPAS survey

The miniJPAS survey

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