Star-Forming Galaxy Evolution in Nearby Rich Clusters

Tyler, K. D.; Rieke, G. H.; Bai, Lei

doi:10.1088/0004-637x/773/2/86

Cited by 22 publications

(44 citation statements)

References 122 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We checked recent redshift surveys, and found significant (> 90) numbers of new redshifts for Abell clusters: A2029 from Tyler et al (2013), A2142 from Owers et al (2011), A2255 from Tyler et al (2014), and A2256 from Rines et al (2016). For 2A 0335+96, NED now offers more redshifts from Huchra et al (2012), resulting in 14 galaxies between 8400 and 13200 km/s, with a velocity dispersion of about 720 km/s.…”

Section: Optical Data and Analysismentioning

confidence: 95%

HIFLUGCS: X-ray luminosity-dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys

Zhang

Reiprich

Schneider

et al. 2017

A&A

View full text Add to dashboard Cite

Abstract. We present the X-ray luminosity versus dynamical mass relation for 63 nearby clusters of galaxies in a flux-limited sample, the HIFLUGCS (consisting of 64 clusters). The luminosity measurements are obtained based on ∼ 1.3 Ms of clean XMM-Newton data and ROSAT pointed observations. The masses are estimated using optical spectroscopic redshifts of 13647 cluster galaxies in total. We classify clusters into disturbed and undisturbed ones, based on a combination of the X-ray luminosity concentration and the offset between the brightest cluster galaxy and X-ray flux-weighted center. Given sufficient numbers (i.e. ≥45) of member galaxies in computing the dynamical masses, the luminosity versus mass relations agree between the disturbed and undisturbed clusters. The cool-core clusters still dominate the scatter in the luminosity versus mass relation even when a core corrected X-ray luminosity is used, which indicates that the scatter of this scaling relation mainly reflects the structure formation history of the clusters. As shown by the clusters with a small number of spectroscopically confirmed members, the dynamical masses can be underestimated and thus lead to a biased scaling relation. To investigate the potential of spectroscopic surveys to follow up high-redshift galaxy clusters/groups observed in X-ray surveys for the identifications and mass calibrations, we carried out Monte-Carlo re-sampling of the cluster galaxy redshifts and calibrated the uncertainties of the redshift and dynamical mass estimates when only reduced numbers of galaxy redshifts per cluster are available. The re-sampling considers the SPIDERS and 4MOST configurations, designed for the follow-up of the eROSITA clusters, and was carried out for each cluster in the sample at the actual cluster redshift as well as at the assigned input cluster redshifts of 0.2, 0.4, 0.6, and 0.8. For following up very distant cluster/groups, we also carried out the mass calibration based on the re-sampling with only ten redshifts per cluster, and redshift calibration based on the re-sampling with only five and ten redshifts per cluster, respectively. Our results demonstrate the power of combining upcoming X-ray and optical spectroscopic surveys for mass calibration of clusters. The scatter in the dynamical mass estimates for the clusters with at least ten members is within 50%.

show abstract

Section: Optical Data and Analysismentioning

confidence: 95%

HIFLUGCS: X-ray luminosity-dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys

Zhang

Reiprich

Schneider

et al. 2017

A&A

View full text Add to dashboard Cite

show abstract

“…Hopkins (Sohn et al 2015). Tyler et al (2013) previously conducted a redshift survey for A2029 using the MMT/ Hectospec with the 270 line mm −1 grating. They obtained 1164 spectra and identified cluster members to investigate the infrared properties of A2029 galaxies.…”

Section: Spectroscopymentioning

confidence: 99%

“…For each Hectospec field, we obtained three sequential exposures of 1200 s each. Tyler et al (2013) used the same integration times for their Hectospec observations; thus we include their spectra and measurements without any correction.…”

Section: Hectomentioning

confidence: 99%

“…The median uncertainty of velocity dispersion measurement from SDSS spectroscopy is -7 km s 1 . We measure velocity dispersions for all of the galaxies with Hectospec spectroscopy, (our targets and the targets of Tyler et al 2013) using the University of Lyon Spectroscopic analysis Software (ULySS, Koleva et al 2009). ULySS compares the Hectospec spectra with stellar population templates calculated with the PEGASE-HR code (Le Borgne et al 2004) and the MILES stellar library.…”

Section: Velocity Dispersionsmentioning

confidence: 99%

“…Furthermore, stellar mass is not directly observable. The Tyler et al (2013) and "MMT" from the MMT/Hectospec observation for this study.…”

Section: Stellar Mass Functionmentioning

confidence: 99%

See 2 more Smart Citations

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Sohn¹,

Geller²,

Zahid³

et al. 2017

ApJS

107

View full text Add to dashboard Cite

Based on an extensive redshift survey for galaxy clusters Abell 2029 and Coma, we measure the luminosity functions (LFs) and stellar mass functions (SMFs) for the entire cluster member galaxies. Most importantly, we measure the velocity dispersion functions (VDFs) for quiescent members. The MMT/Hectospec redshift survey for galaxies in A2029 identifies 982 spectroscopic members; for 838 members, we derive the central velocity dispersion from the spectroscopy. Coma is the only other cluster surveyed as densely. The LFs, SMFs, and VDFs for A2029 and Coma are essentially identical. The SMFs of the clusters are consistent with simulations. The A2029 and Coma VDFs for quiescent galaxies have a significantly steeper slope than those of field galaxies for velocity dispersion  -100 km s 1 . The cluster VDFs also exceed the field at velocity dispersion  -250 km s 1 . The differences between cluster and field VDFs are potentially important tests of simulations and of the formation of structure in the universe.

show abstract

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Boselli

Fossati

Roediger

et al. 2023

A&A

View full text Add to dashboard Cite

Using a compilation of Hα fluxes for 384 star-forming galaxies detected during the Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE), we study several important scaling relations linking the star formation rate, specific star formation rate, stellar mass, stellar mass surface density, and atomic gas depletion timescale for a complete sample of galaxies in a rich environment. The extraordinary sensitivity of the narrow-band imaging data allows us to sample the whole dynamic range of the Hα luminosity function, from massive galaxies (M star 10 11 M ) to dwarf systems (M star 10 6 M ), where the ionised gas emission is due to the emission of single O-early B stars. This extends previous works to a dynamic range in stellar mass and star formation rate (10 −4 S FR 10 M yr −1 ) that has never been explored so far. The main-sequence relation derived for all star-forming galaxies within one virial radius of the Virgo cluster has a slope comparable to that observed in other nearby samples of isolated objects, but its dispersion is about three times larger (∼ 1 dex). The dispersion is tightly connected to the available amount of HI gas, with gas-poor systems located far below objects of similar stellar mass, but with a normal HI content. When measured on unperturbed galaxies with a normal HI gas content (HI − de f ≤ 0.4), the relation has a slope a=0.92±0.06, an intercept b = -1.57±0.06 (at a pivot point of log M star = 8.451 M ), and a scatter σ 0.40, and it has a constant slope in the stellar mass range 10 6 M star 3 × 10 11 M . The specific star formation rate of HI-poor galaxies is significantly lower than that of HI-rich systems of similar stellar mass, while their atomic gas consumption timescale τ HI is fairly similar, in particular, for objects of stellar mass 10 7 M star 10 9 M . We compare these observational results to the prediction of models expressly tuned to reproduce the effects induced by the interaction of galaxies with their surrounding environment. The observed scatter in the main-sequence relation can be reproduced only after a violent and active stripping process such as ram-pressure stripping that removes gas from the disc (outer parts first) and quenches star formation on short (< 1 Gyr) timescales. This rules out milder processes such as starvation. This interpretation is also consistent with the position of galaxies of different star formation activity and gas content within the phase-space diagram. We also show that the star-forming regions that formed in the stripped material outside perturbed galaxies are located well above the main-sequence relation drawn by unperturbed systems. These extraplanar HII regions, which might be at the origin of ultra-compact dwarf galaxies (UCDs) and other compact sources typical in rich environments, are living a starburst phase lasting only 50 Myr. They later become quiescent systems.

show abstract

Star-Forming Galaxy Evolution in Nearby Rich Clusters

Cited by 22 publications

References 122 publications

HIFLUGCS: X-ray luminosity-dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys

HIFLUGCS: X-ray luminosity-dynamical mass relation and its implications for mass calibrations with the SPIDERS and 4MOST surveys

The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

Contact Info

Product

Resources

About