A Complete Spectroscopic Census of A2029: A Tale of Three Histories

Sohn, Jubee; Geller, Margaret J.; Zahid, H. Jabran; Fabricant, Daniel G.

doi:10.3847/1538-4357/ab0213

Cited by 12 publications

(7 citation statements)

References 137 publications

(265 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…where R is the aperture size. The aperture correction coefficient we use is β = −0.059 ± 0.014 derived from the galaxies with both Portsmouth and Hectospec velocity dispersion measurements (Sohn et al 2019b). This aperture correction is consistent with results from integral field spectroscopy (Cappellari et al 2006).…”

Section: Central Stellar Velocity Dispersionsupporting

confidence: 74%

“…These substructures also appear in both X-ray and weak lensing maps. Sohn et al (2019b) demonstrate that the infalling substructures will be accreted onto the main cluster within 2-3 Gyr timescale. Similarly, the local density peaks we identify in the number density maps of cluster galaxies are potential infalling substructures because they are contained within the caustics.…”

Section: Spatial Distribution Of Large σ Galaxiesmentioning

confidence: 85%

“…Serra & Diaferio (2013) demonstrate that the caustic technique identifies 95% of members within 3R 200 of simulated clusters with ∼ 180 members in fields containing ∼ 1000 galaxies. Several previous observational studies of galaxy clusters use the caustic technique for membership determination (e.g., Rines & Diaferio 2006;Rines et al 2013;Hwang et al 2014;Rines et al 2016Rines et al , 2018Sohn et al 2017aSohn et al , 2019bSohn et al , 2020. Figure 3 shows the relative galaxy velocity difference in the rest frame with respect to the mean cluster redshift for each cluster as a function of projected clustercentric distance (the R-v diagram).…”

Section: Member Identificationmentioning

confidence: 99%

See 2 more Smart Citations

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

Sohn

Zahid

Geller

2017

ApJ

Self Cite

View full text Add to dashboard Cite

We investigate the distribution of central velocity dispersions for quiescent galaxies in the SDSS at 0.03 ≤ z ≤ 0.10. To construct the field velocity dispersion function (VDF), we construct a velocity dispersion complete sample of quiescent galaxies with D n 4000 > 1.5. The sample consists of galaxies with central velocity dispersion larger than the velocity dispersion completeness limit of the SDSS survey. Our VDF measurement is consistent with previous field VDFs for σ > 200 km s −1 . In contrast with previous results, the VDF does not decline significantly for σ < 200 km s −1 . The field and the similarly constructed cluster VDFs are remarkably flat at low velocity dispersion (σ < 250 km s −1 ). The cluster VDF exceeds the field for σ > 250 km s −1 providing a measure of the relatively larger number of massive subhalos in clusters. The VDF is a probe of the dark matter halo distribution because the measured central velocity dispersion may be directly proportional to the dark matter velocity dispersion. Thus the VDF provides a potentially powerful test of simulations for models of structure formation.

show abstract

Section: Central Stellar Velocity Dispersionsupporting

confidence: 74%

Section: Spatial Distribution Of Large σ Galaxiesmentioning

confidence: 85%

Section: Member Identificationmentioning

confidence: 99%

See 1 more Smart Citation

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

Sohn

Zahid

Geller

2017

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

“…The faint end cutoff is not due to photometric completeness but because Connor et al (2017) imposed a hard cut at F814W = 25.5 mag. quence galaxies, e.g., Sohn et al 2019), so we instead use our own data to model an expectation for galaxy metallicities. While a single color is degenerate to mass and metallicity, two colors -particularly an optical and an infrared color -can break this degeneracy.…”

Section: Scatter Around the Red Sequencementioning

confidence: 99%

“…quence galaxies, e.g., Sohn et al 2019), so we instead use our own data to model an expectation for galaxy metallicities. While a single color is degenerate to mass and metallicity, two colors -particularly an optical and an infrared color -can break this degeneracy.…”

Section: Scatter Around the Red Sequencementioning

confidence: 99%

On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters

Connor

Kelson

Donahue

et al. 2019

ApJ

View full text Add to dashboard Cite

In clusters of galaxies, the red sequence is believed to be a consequence of a correlation between stellar mass and chemical abundances, with more massive galaxies being more metal-rich and, as a consequence, redder. However, there is a color scatter around the red sequence that holds even with precision photometry, implying that the galaxy population is more complicated than as described by a mass-metallicity relation. We use precision photometry from the Cluster Lensing and Supernova survey with Hubble (CLASH) to investigate what drives this scatter. In four CLASH clusters at z = 0.355 ± 0.007, we find that the optical-IR galaxy colors confirm the previously known trend of metallicity along the red sequence but also show a strong connection between stellar age and red sequence offset, with ages ranging from 3 to 8 Gyr. Starting with fixed-age color-magnitude relations motivated by the mass-metallicity correlations of CLASH cluster galaxies, and by adjusting galaxy colors through stellar population models to put them all at the age of our red sequence, we are able to reduce the, e.g., F625W − F814W scatter from 0.051 mag to 0.026 mag with median photometric errors of 0.029 mag. While we will extend this analysis to the full CLASH sample, in four clusters our technique already provides a color precision in near-total-light apertures to resolve the spread in stellar population formation ages that drives the scatter in the red sequence.

show abstract

In pursuit of giants

Donevski,

Damjanov,

Nanni

et al. 2023

A&A

View full text Add to dashboard Cite

The physical mechanisms that link the termination of star formation in quiescent galaxies and the evolution of their baryonic components, stars, and the interstellar medium (ISM; dust, gas, and metals) are poorly constrained beyond the local Universe. In this work, we characterise the evolution of the dust content in 545 quiescent galaxies observed at 0.1 < z < 0.6 as part of the hCOSMOS spectroscopic redshift survey. This is, to date, the largest sample of quiescent galaxies at intermediate redshifts for which the dust, stellar, and metal abundances are consistently estimated. We analyse how the crucial markers of a galaxy dust life cycle, such as specific dust mass (Mdust/M⋆), evolve with different physical parameters, namely gas-phase metallicity (Zgas), time since quenching (tquench), stellar mass (M⋆), and stellar population age. We find morphology to be an important factor in the large scatter in Mdust/M⋆ (∼2 orders of magnitude). Quiescent spirals exhibit strong evolutionary trends of specific dust mass with M⋆, stellar age, and galaxy size, in contrast to the little to no evolution experienced by ellipticals. When transitioning from solar to super-solar metallicities (8.7 ≲ 12 + log(O/H)≲9.1), quiescent spirals undergo a reversal in Mdust/M⋆, indicative of a change in dust production efficiency. By modelling the star formation histories of our objects, we unveil a broad dynamical range of post-quenching timescales (60 Myr < tquench < 3.2 Gyr). We show that Mdust/M⋆ is highest in recently quenched systems (tquench < 500 Myr), but its further evolution is non-monotonic, as a consequence of different pathways for dust formation, growth, or removal on various timescales. Our data are best described by simulations that include dust growth in the ISM. While this process is prevalent in the majority of galaxies, for ∼15% of objects we find evidence of additional dust content acquired externally, most likely via minor mergers. Altogether, our results strongly suggest that prolonged dust production on a timescale of 0.5 − 1 Gyr since quenching may be common in dusty quiescent galaxies at intermediate redshifts, even if their gas reservoirs are heavily exhausted (i.e. cold gas fraction < 1 − 5%).

show abstract

A Complete Spectroscopic Census of A2029: A Tale of Three Histories

Cited by 12 publications

References 137 publications

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

On the Origin of the Scatter in the Red Sequence: An Analysis of Four CLASH Clusters

In pursuit of giants

Contact Info

Product

Resources

About