TABLE 5 - uploaded by I-Non Chiu
Content may be subject to copyright.
Source publication
We present the results of SPT-GMOS, a spectroscopic survey with the Gemini Multi-Object Spectrograph (GMOS) on Gemini South. The targets of SPT-GMOS are galaxy clusters identified in the SPT-SZ survey, a millimeter-wave survey of 2500 squ. deg. of the southern sky using the South Pole Telescope (SPT). Multi-object spectroscopic observations of 62 S...
Context in source publication
Context 1
... the [O II] λ3727 doublet and the H-δ equivalent width data products described above it is straightfor- ward to classify each galaxy with a GMOS spectrum and a spectroscopic redshift using the spectral index criteria described in Table 6 of Dressler et al. (1999). Table 5 lists the specific criteria that we use to classify SPT- GMOS galaxies as one of six types of galaxies; we ap- ply these criteria exclusively to galaxy spectra that have reliable redshift measurements (2243 in total). Briefly, Fig. 11.-These three panels all show the full ensemble of member galaxies from all clusters within SPT-GMOS with each galaxy plotted according to its peculiar velocity relative to the median redshift of its host cluster. ...
Similar publications
We present an optical study of the strong-lensing galaxy cluster MS 0440.5+0204 at z=0.19593, based on CFHT/MegaCam g′, r′ photometry and GMOS/Gemini and CFHT/MOS/SIS spectroscopy in a broader area than previous works. We have determined new spectroscopic redshifts for the most prominent gravitational arcs surrounding the central galaxy in the clus...
Gemini Multi Object Spectrograph medium-resolution spectra and photometric data of 39 objects in the field of the radio galaxy 3C 17 are presented. Based on the new data, a previously uncataloged cluster of galaxies is identified at a mean redshift of z = 0.220 ± 0.003, a projected virial radius of 0.37 Mpc, and a velocity dispersion of σ v = 821 ±...
Citations
... For instance, the Spitzer Adaptation of the Red-sequence Cluster Survey (SpARCS; Muzzin et al. 2009;Wilson et al. 2009) has used red sequence galaxies as tracers of z > 1 clusters. A large number of cluster candidates at z > 1 are identified through the Sunyaev-Zel'dovich effect (Sunyaev & Zeldovich 1972) by the South Pole Telescope (SPT) cluster survey (e.g., Brodwin et al. 2010;Foley et al. 2011;Bayliss et al. 2016). Extended X-ray emissions are also used as signposts of high-redshift clusters/groups (e.g., Pierre et al. 2016;Pacaud et al. 2016;Gozaliasl et al. 2019), although the sample is limited to z ≲ 1.5 due to sensitivity. ...
Galaxy clusters are crucial to understanding role of the environment in galaxy evolution. However, due to their rarity, only a limited number of clusters have been identified at $z\gtrsim2$. In this paper, we report a discovery of seven cluster candidates with massive quiescent galaxies at $z\sim2$ in the $3.5\,\mathrm{deg}^{2}$ area of the XMM-LSS field, roughly doubling the known cluster sample at this frontier redshift if confirmed. We construct a photometric redshift catalog based on deep ($i\sim26$, $K_\mathrm{s}\sim24$) multi-wavelength photometry from $u^*$-band to $K$-band gathered from the Hyper Suprime-Cam Subaru Strategic Program and other collaborative/public surveys. We adopt a Gaussian kernel density estimate with two different spatial scales (10" and 60") to draw a density map of massive ($\log(M_{*}/M_{\odot})>10.5$) and quiescent ($\log(\mathrm{sSFR\, [\mathrm{yr^{-1}}]})<-10$) galaxies at $z\sim2$. Then, We identify seven prominent overdensities. These candidates show clear red sequences in color-magnitude diagrams ($z-H$ vs. $H$). Moreover, one of them shows an extended X-ray emission with $L_\mathrm{X}=(1.46\pm0.35)\times10^{44}$ erg s$^{-1}$, suggesting its virialized nature. There is no clear evidence of enhancement nor suppression of the star formation rate of the main sequence galaxies in the clusters. We find that cluster galaxies have a higher fraction of transition population with $-10.5<\log(\mathrm{sSFR\, [\mathrm{yr^{-1}}]})<-10$ ($12\%$) than the field ($2\%$), which implies the ongoing star formation quenching. The quiescent fraction in the cluster candidates also exceeds that in the field. We confirm that the excess of a quiescent fraction is larger for higher-mass galaxies. This is the first statistical evidence for the mass-dependent environmental quenching at work in clusters even at $z\sim2$.
... The netw ork w as trained to maximize the PDF peak value for the spectroscopic redshifts ( z spec ) of each galaxy. The spectroscopic information came from a crossmatch between DELVE DR2 and the data available in different large sk y surv e ys (Colless et al. 2001 ;Mortlock, Madgwick & Lahav 2001 ;Wilson et al. 2006 ;Jones et al. 2009 ;Bacon et al. 2010 ;Drinkwater et al. 2010 ;Holwerda, Blyth & Baker 2011 ;Cooper et al. 2012 ;Mao et al. 2012 ;McLure et al. 2012 ;Bradshaw et al. 2013 ;F èvre et al. 2013 ;Newman et al. 2013 ;Baldry et al. 2014 ;Treu et al. 2015 ;Wirth et al. 2015 ;Bayliss et al. 2016 ;Momche v a et al. 2016 ;Nanayakkara et al. 2016 ;Tasca et al. 2017 ;McLure et al. 2018 ;Scodeggio, M. et al. 2018 ;Masters et al. 2019 ;Ahumada et al. 2020 ;Newman et al. 2020 ;Pharo et al. 2020 ;Mao et al. 2021 ;Mercurio et al. 2021 ), which resulted in approximately 4.5 million galaxies with z spec measurements. We also added the z spec 's available from the DECals DR9 Catalogue (Dey et al. 2019 ) also by doing a crossmatch with the DELVE DR2 data. ...
The current and next observation seasons will detect hundreds of gravitational waves (GWs) from compact binary systems coalescence at cosmological distances. When combined with independent electromagnetic measurements, the source redshift will be known, and we will be able to obtain precise measurements of the Hubble constant H0 via the distance-redshift relation. However, most observed mergers are not expected to have electromagnetic counterparts, which prevents a direct redshift measurement. In this scenario, one possibility is to use the dark sirens method that statistically marginalizes over all the potential host galaxies within the GW location volume to provide a probabilistic source redshift. Here we presented H0 measurements using two new dark sirens compared to previous analyses using DECam data, GW190924$\_$021846 and GW200202$\_$154313. The photometric redshifts of the possible host galaxies of these two events are acquired from the DECam Local Volume Exploration Survey (DELVE) carried out on the Blanco telescope at Cerro Tololo. The combination of the H0 posterior from GW190924$\_$021846 and GW200202$\_$154313 together with the bright siren GW170817 leads to $H_{0} = 68.84^{+15.51}_{-7.74}\, \rm {km /s/Mpc}$. Including these two dark sirens improves the 68% confidence interval (CI) by 7% over GW170817 alone. This demonstrates that the addition of well-localized dark sirens in such analysis improves the precision of cosmological measurements. Using a sample containing 10 well-localized dark sirens observed during the third LIGO/Virgo observation run, without the inclusion of GW170817, we determine a measurement of $H_{0} = 76.00^{+17.64}_{-13.45}\, \rm {km /s/Mpc}$.
... For that, we employ a large number of clusters uniformly selected by the Sunyaev-Zel'dovich (SZ) effect (Sunyaev & Zeldovich 1972) from the South Pole Telescope (SPT; Bleem et al. 2015) and Atacama Cosmology Telescope (ACT; Marriage et al. 2011) cluster surveys. We obtain the photometric and spectroscopic information of cluster galaxies from the optical follow-up observations of the SZ clusters (Ruel et al. 2014;Bleem et al. 2015;Bayliss et al. 2016, and references therein). ...
... We use observational data sets drawn from the 2500 deg 2 SPT-SZ (Vanderlinde et al. 2010;Reichardt et al. 2013;Ruel et al. 2014;Bleem et al. 2015;Bayliss et al. 2016Bayliss et al. , 2017 and ACT-SZ (Marriage et al. 2011;Hasselfield et al. 2013;Sifón et al. 2013) cluster surveys and the associated optical/near-IR follow-up observations. Due to the redshift independence of the SZ effect, the clusters identified by these surveys are nearly mass-limited with a mass threshold of 3 × 10 14 M e at all redshifts (see, e.g., Figure 6 of Bleem et al. 2015). ...
... The majority of the photometry uses the Sloan Digital Sky Survey (SDSS) i-band filter. For clusters observed with the older Johnson-Cousins photometric BVRI system, the filter transformation of the I band into the SDSS i band is applied in Bayliss et al. (2016; see their Section 5.2). As a result, all of our sample galaxies' L i is measured with respect to the SDSS i-band filter. ...
The environments where galaxies reside crucially shape their star formation histories. We investigate a large sample of 1626 cluster galaxies located within 105 galaxy clusters spanning a large range in redshift (0.26 < z < 1.13). The galaxy clusters are massive ( M 500 ≳ 2 × 10 ¹⁴ M ⊙ ) and uniformly selected from the SPT and ACT Sunyaev–Zel’dovich surveys. With spectra in hand for thousands of cluster members, we use the galaxies’ position in projected phase space as a proxy for their infall times, which provides a more robust measurement of environment than quantities such as projected clustercentric radius. We find clear evidence for a gradual age increase of the galaxy’s mean stellar populations (∼0.71 ± 0.4 Gyr based on a 4000 Å break, D n 4000) with the time spent in the cluster environment. This environmental quenching effect is found regardless of galaxy luminosity (faint or bright) and redshift (low or high- z ), although the exact stellar age of galaxies depends on both parameters at fixed environmental effects. Such a systematic increase of D n 4000 with infall proxy would suggest that galaxies that were accreted into hosts earlier were quenched earlier due to longer exposure to environmental effects such as ram pressure stripping and starvation. Compared to the typical dynamical timescales of 1–3 Gyr of cluster galaxies, the relatively small age increase (∼0.71 ± 0.4 Gyr) found in our sample galaxies seems to suggest that a slow environmental process such as starvation is the dominant quenching pathway. Our results provide new insights into environmental quenching effects spanning a large range in cosmic time (∼5.2 Gyr, z = 0.26–1.13) and demonstrate the power of using a kinematically derived infall time proxy.
... As part of an ongoing follow-up campaign of SZ-selected clusters (e.g., Bayliss et al. 2016;Khullar et al. 2019Khullar et al. , 2022, the SPT collaboration gathered optical spectroscopy of SPT2215 with the LDSS3 instrument on the 6.5 m Magellan telescopes in Chile. Multiobject spectra were obtained on 2019 June 25 using 1 3 slits placed on the BCG and 16 other high-redshift member galaxy candidates. ...
We present the discovery of the most distant, dynamically relaxed cool core cluster, SPT-CL J2215−3537 (SPT2215), and its central brightest cluster galaxy (BCG) at z = 1.16. Using new X-ray observations, we demonstrate that SPT2215 harbors a strong cool core with a central cooling time of 200 Myr (at 10 kpc) and a maximal intracluster medium cooling rate of 1900 ± 400 M ⊙ yr ⁻¹ . This prodigious cooling may be responsible for fueling the extended, star-forming filaments observed in Hubble Space Telescope imaging. Based on new spectrophotometric data, we detect bright [O ii ] emission in the BCG, implying an unobscured star formation rate (SFR) of 320 − 140 + 230 M ⊙ yr ⁻¹ . The detection of a weak radio source (2.0 ± 0.8 mJy at 0.8 GHz) suggests ongoing feedback from an active galactic nucleus (AGN), though the implied jet power is less than half the cooling luminosity of the hot gas, consistent with cooling overpowering heating. The extreme cooling and SFR of SPT2215 are rare among known cool core clusters, and it is even more remarkable that we observe these at such high redshift, when most clusters are still dynamically disturbed. The high mass of this cluster, coupled with the fact that it is dynamically relaxed with a highly isolated BCG, suggests that it is an exceptionally rare system that must have formed very rapidly in the early universe. Combined with the high SFR, SPT2215 may be a high- z analog of the Phoenix cluster, potentially providing insight into the limits of AGN feedback and star formation in the most massive galaxies.
... As part of an ongoing follow-up campaign of SZselected clusters (e.g. Bayliss et al. 2016;Khullar et al. 2019Khullar et al. , 2022, the SPT collaboration has gathered optical spectroscopy of SPT2215 with the LDSS3 instrument on the 6.5m Magellan telescopes in Chile. Multi-object spectra were obtained on 25 June 2019 using 1. 3 slits placed on the BCG and 16 other high-redshift member galaxy candidates. ...
We present the discovery of the most distant, dynamically relaxed cool core cluster, SPT-CL J2215-3537 (SPT2215) and its central brightest cluster galaxy (BCG) at z=1.16. Using new X-ray observations, we demonstrate that SPT2215 harbors a strong cool core, with a central cooling time of 200 Myr (at 10 kpc) and a maximal intracluster medium cooling rate of 1900+/-400 Msun/yr. This prodigious cooling may be responsible for fueling extended, star-forming filaments observed in Hubble Space Telescope imaging. Based on new spectrophotometric data, we detect bright [O II] emission in the BCG, implying an unobscured star formation rate (SFR) of 320^{+230}_{-140} Msun/yr. The detection of a weak radio source (2.0+/-0.8 mJy at 0.8 GHz) suggests ongoing feedback from an active galactic nucleus (AGN), though the implied jet power is less than half the cooling luminosity of the hot gas, consistent with cooling overpowering heating. The extreme cooling and SFR of SPT2215 is rare among known cool core clusters, and it is even more remarkable that we observe these at such high redshift, when most clusters are still dynamically disturbed. The high mass of this cluster, coupled with the fact that it is dynamically relaxed with a highly-isolated BCG, suggests that it is an exceptionally rare system that must have formed very rapidly in the early Universe. Combined with the high SFR, SPT2215 may be a high-z analog of the Phoenix cluster, potentially providing insight into the limits of AGN feedback and star formation in the most massive galaxies.
... SPT-CL J0307-6225 is a merger candidate at z = 0.5801 (Bayliss et al. 2016 ), with a mass estimate from SPT data of M 500 = 5 . 06 ± 0 . ...
... 90 × 10 14 h −1 70 M (Bleem et al. 2015 ). SPT-CL J0307-6225 has (1) gri optical data observed with the Megacam instrument on the Magellan Clay telescope (Chiu et al. 2016 ), (2) X-ray data obtained with the Chandra telescope (McDonald et al. 2013 ), and (3) spectroscopic information taken with the Gemini Multi-Object Spectrograph (GMOS; Bayliss et al. 2016 ). Dietrich et al. ( 2019 ) used the Megacam data to measure the weak lensing mass density and, although the cluster was observed under the best seeing conditions in the sample (0.55-0.65 arcsec), the resulting WL mass distribution is of low significance with the reco v ered centre located away from the gas distribution or the galaxies (see their fig. ...
... This would be the largest g as-g alaxy offset within the Wittman et al. ( 2018 ) sample of merging galaxy clusters, implying a high potential for SPT-CL J0307-6225 to constrain such models. Using GMOS spectroscopic data, Bayliss et al. ( 2016 ) studied the velocity distribution of the SPT-GMOS sample (62 galaxy clusters), finding SPT-CL J0307-6225 to be one of the nine clusters with a non-Gaussian (i.e. disturbed) velocity distribution (2 σ level). ...
We present MUSE spectroscopy, Megacam imaging, and Chandra X–ray emission for SPT-CL J0307-6225, a z=0.58 major merging galaxy cluster with a large BCG-SZ centroid separation and a highly disturbed X–ray morphology. The galaxy density distribution shows two main overdensities with separations of 0.144 and 0.017 arcmin to their respective BCGs. We characterize the central regions of the two colliding structures, namely 0307-6225N and 0307-6225S, finding velocity derived masses of M200, N = 2.44 ± 1.41 × 1014 M⊙ and M200, S = 3.16 ± 1.88 × 1014 M⊙, with a line-of-sight velocity difference of |Δv| = 342 km s−1. The total dynamically derived mass is consistent with the SZ derived mass of 7.63 h$_{70}^{-1}$ ± 1.36 × 1014 M⊙. We model the merger using the Monte Carlo Merger Analysis Code, estimating a merging angle of 36$^{+14}_{-12}$ degrees with respect to the plane of the sky. Comparing with simulations of a merging system with a mass ratio of 1:3, we find that the best scenario is that of an ongoing merger that began 0.96$^{+0.31}_{-0.18}$ Gyr ago. We also characterize the galaxy population using Hδ and [OII] λ3727 Å lines. We find that most of the emission-line galaxies belong to 0307-6225S, close to the X–ray peak position, with a third of them corresponding to red-cluster sequence galaxies, and the rest to blue galaxies with velocities consistent with recent periods of accretion. Moreover, we suggest that 0307-6225S suffered a previous merger, evidenced through the two equally bright BCGs at the center with a velocity difference of ∼674 km s−1.
... Recent SZ-based galaxy cluster searches from SPT have revealed new samples of galaxy clusters at z > ∼ 1 (Bleem et al. 2015Huang et al. 2020), extending the viability of SZ-cluster studies to redshift as distant as any other sample. These samples are now large enough to be a compelling resource for cluster galaxy evolution studies McDonald et al. 2013;Stalder et al. 2013;Ruel et al. 2014;Bayliss et al. 2016;McDonald et al. 2017;Khullar et al. 2019). ...
Using stellar population synthesis models to infer star formation histories (SFHs), we analyze photometry and spectroscopy of a large sample of quiescent galaxies that are members of Sunyaev–Zel’dovich (SZ)-selected galaxy clusters across a wide range of redshifts. We calculate stellar masses and mass-weighted ages for 837 quiescent cluster members at 0.3 < z < 1.4 using rest-frame optical spectra and the Python-based Prospector framework, from 61 clusters in the SPT-GMOS Spectroscopic Survey (0.3 < z < 0.9) and three clusters in the SPT Hi-z cluster sample (1.25 < z < 1.4). We analyze spectra of subpopulations divided into bins of redshift, stellar mass, cluster mass, and velocity-radius phase-space location, as well as by creating composite spectra of quiescent member galaxies. We find that quiescent galaxies in our data set sample a diversity of SFHs, with a median formation redshift (corresponding to the lookback time from the redshift of observation to when a galaxy forms 50% of its mass, t 50 ) of z = 2.8 ± 0.5, which is similar to or marginally higher than that of massive quiescent field and cluster galaxy studies. We also report median age–stellar mass relations for the full sample (age of the universe at t 50 (Gyr) = 2.52 (±0.04)–1.66 (±0.12) log 10 ( M /10 ¹¹ M ⊙ )) and recover downsizing trends across stellar mass; we find that massive galaxies in our cluster sample form on aggregate ∼0.75 Gyr earlier than lower-mass galaxies. We also find marginally steeper age–mass relations at high redshifts, and report a bigger difference in formation redshifts across stellar mass for fixed environment, relative to formation redshifts across environment for fixed stellar mass.
... Ongoing and forthcoming wide extra-galactic surveys, from the lowest to the highest frequencies, will provide complete and pure galaxy cluster samples up to high redshifts and down to low masses. Among them are the Kilo Degree Survey 1 (KiDS, de Jong et al. 2017;Kuijken et al. 2019), the Dark Energy Survey 2 (The Dark Energy Survey Collaboration 2005; Abbott et al. 2021), the Vera C. Rubin Observatory LSST 3 (LSST Dark Energy Science Collaboration 2012, 2021), and Euclid 4 (Amendola et al. 2018;Euclid Collaboration et al. 2019Scaramella et al. 2021) in optical and nearinfrared, the South Pole Telescope 5 (Bayliss et al. 2016;Chown et al. 2018), the Atacama Cosmology Telescope 6 (Naess et al. 2020;Orlowski-Scherer et al. 2021), and the Simons Observatory 7 (Ade et al. 2019;Xu et al. 2021) surveys at high-radio frequencies, as well as eROSITA 8 (Brunner et al. 2021;Liu et al. 2021) in X-rays. ...
We analysed the clustering of a photometric sample of galaxy clusters selected from the Third Data Release of the Kilo-Degree Survey, focusing on the redshift-space two-point correlation function (2PCF). We compared our measurements to theoretical predictions of the standard $\Lambda$ cold dark matter ($\Lambda$CDM) cosmological model. We measured the 2PCF of the sample in the cluster centric radial range $r\in[5,80]$ $h^{-1}$Mpc, considering 4934 galaxy clusters with richness $\lambda^*\geq15$ in the redshift range $z\in[0.1,0.6]$. A Markov chain Monte Carlo analysis has been performed to constrain the cosmological parameters $\Omega_{\rm m}$, $\sigma_8$, and $S_8 \equiv \sigma_8(\Omega_{\rm m}/0.3)^{0.5}$, assuming Gaussian priors on the mass-richness relation given by the posteriors obtained from a joint analysis of cluster counts and weak lensing. In addition, we constrained the normalisation of the mass-richness relation, $\alpha$, with fixed cosmological parameters. We obtained $\Omega_{\rm m}=0.28^{+0.05}_{-0.04}$, $\sigma_8=0.82^{+0.14}_{-0.12}$, and $S_8=0.80^{+0.08}_{-0.08}$. The constraint on $S_8$ is consistent within 1$\sigma$ with the results from WMAP and Planck. Furthermore, by fixing the cosmological parameters to those provided by Planck, we obtained $\alpha=0.12^{+0.06}_{-0.06}$, which is fully consistent with the result obtained from the joint analysis of cluster counts and weak lensing performed for this sample.
... We complemented MUSE galaxy redshifts with Gemini/GMOS data published by Bayliss et al. (2016). Bayliss galaxy redshift sample consists in 35 cluster galaxies redshifts, with 8 not present in our MUSE data. ...
... Bayliss galaxy redshift sample consists in 35 cluster galaxies redshifts, with 8 not present in our MUSE data. The spectroscopic data from their sample can be found online at the V R C S (Ochsenbein et al. 2000), with the details on the data reduction described in Bayliss et al. (2016) and Bayliss et al. (2017). For SPT-CLJ 0307-6225, they used 2 spectroscopic masks with an exposure time of 1 hour each. ...
... In addition, we supplement this data with 35 GMOS archival spectroscopic reduced data (Bayliss et al. 2016). Unfortunately, the header of these spectroscopic data did not have the information regarding the wavelength calibration, so we estimate that manually and then use to estimate redshifts. ...
We present VLT/MUSE spectroscopy, along with archival Gemini/GMOS spectroscopy, Magellan/Megacam imaging, and Chandra X-ray emission for SPT-CLJ0305-6225, a z=0.58 galaxy cluster. A large BCG-SZ centroid separation and a highly disturbed X-ray morphology classifies SPT-CLJ0307-6225 as a major merging cluster. Furthermore, the galaxy density distribution shows two main overdensities with separations of 0.144' and 0.017' to their respective BCGs. We characterize the central regions of the two colliding structures, namely 0307-6225N and 0307-6225S. We find velocity derived masses of $M_{200,N}=$ 2.42 $\pm$ 1.40 $\times10^{14}$ M$_\odot$ and $M_{200,S}=$ 3.13 $\pm$ 1.87 $\times10^{14}$ M$_\odot$, with a line-of-sight velocity difference between the two structures of $|\Delta v| = 342$ km s$^{-1}$. The total dynamically derived mass is consistent with the SZ derived mass of 7.63 h$_{70}^{-1}$ $\pm$ 1.36 $\times10^{14}$ M$_\odot$. We model the merger using the Monte Carlo Merger Analysis Code, estimating a merging angle of 36$^{+14}_{-12}$ degrees with respect to the plane of the sky. Comparing with simulations of a merging system with a mass ratio of 1:3, we find that the best scenario is that of an ongoing merger that began 0.96$^{+0.31}_{-0.18}$ Gyr ago, which could be close to turnaround. We also characterize the galaxy population using the H$\delta$ and [OII] $\lambda 3727$ \AA \ lines. We find that most of the emission-line galaxies belong to 0307-6225S, close to the X-ray peak position, with a third of them corresponding to red-cluster sequence galaxies, and the rest to blue galaxies with velocities consistent with recent periods of accretion. Moreover, we suggest that 0307-6225S suffered a previous merger, evidenced through the two equally bright BCGs at the center with a velocity difference of $\sim$674 km s$^{-1}$.
... Recent SZbased galaxy cluster searches from SPT have revealed new samples of galaxy clusters at z>∼1 (Bleem et al. 2015Huang et al. 2020), extending the viability of SZ-cluster studies to redshift as distant as any other sample. These samples are now large enough to be a compelling resource for cluster galaxy evolution studies Stalder et al. 2013;McDonald et al. 2013;Ruel et al. 2014;Bayliss et al. 2016;McDonald et al. 2017;Khullar et al. 2019). ...
Using stellar population synthesis models to infer star formation histories (SFHs), we analyse photometry and spectroscopy of a large sample of quiescent galaxies which are members of Sunyaev-Zel'dovich (SZ)-selected galaxy clusters across a wide range of redshifts. We calculate stellar masses and mass-weighted ages for 837 quiescent cluster members at 0.3 < z < 1.4 using rest-frame optical spectra and the Python-based Prospector framework, from 61 clusters in the SPT-GMOS Spectroscopic Survey (0.3 < z < 0.9) and 3 clusters in the SPT Hi-z cluster sample (1.25 < z < 1.4). We analyse spectra of subpopulations divided into bins of redshift, stellar mass, cluster mass, and velocity-radius phase-space location, as well as by creating composite spectra of quiescent member galaxies. We find that quiescent galaxies in our dataset sample a diversity of SFHs, with a median formation redshift (corresponding to the lookback time from the redshift of observation to when a galaxy forms 50% of its mass, t$_{50}$) of $z=2.8\pm0.5$, which is similar to or marginally higher than that of massive quiescent field and cluster galaxy studies. We also report median age-stellar mass relations for the full sample (age of the Universe at $t_{50}$ (Gyr) = $2.52 (\pm0.04) - 1.66 (\pm0.11)$ log$_{10}(M/10^{11} M\odot))$ and recover downsizing trends across stellar mass; we find that massive galaxies in our cluster sample form on aggregate $\sim0.75$ Gyr earlier than lower mass galaxies. We also find marginally steeper age-mass relations at high redshifts, and report a bigger difference in formation redshifts across stellar mass for fixed environment, relative to formation redshifts across environment for fixed stellar mass.
