Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Damjanov, Ivana; Zahid, H. Jabran; Geller, Margaret J.; Utsumi, Yousuke; Sohn, Jubee; Souchereau, Harrison

doi:10.3847/1538-4357/aaf97d

Cited by 37 publications

(82 citation statements)

References 115 publications

(153 reference statements)

Supporting

Mentioning

Contrasting

Order By: Relevance

“…At a fixed stellar mass, quiescent galaxies in the local universe with older stellar populations are smaller and have larger stellar velocity dispersions. Similar trends are also observed at earlier times (Wu et al 2018;Damjanov et al 2019). The relation between stellar mass, size and stellar velocity dispersion for local quiescent galaxies is consistent with virial equilibrium expectations if the non-homologous galaxy structure is taken into account (Zahid & Geller 2017).…”

Section: Introductionsupporting

confidence: 86%

“…Figure 11 shows the mass dependent evolution of galaxy half-light radii as a function of redshift for the projected SDSS sample and direct measurements from SHELS. Our growth model reproduces the mass dependent evolutionary trends reported by Damjanov et al (2019).…”

Section: Test Of Consistencysupporting

confidence: 75%

“…Half-light radii of SHELS galaxies and details of the procedure are published in Damjanov et al (2019). Here we provide a brief summary.…”

Section: Galaxy Radiusmentioning

confidence: 99%

“…The two samples are now consistent. Damjanov et al (2019) analyze the half-light radius evolution of quiescent galaxies as a function of redshift and stellar mass. They report differential evolution in galaxy half-light radii with respect to stellar mass; all quiescent galaxies grow but less massive objects grow more.…”

Section: Test Of Consistencymentioning

confidence: 99%

“…Observations reveal that galaxies are significantly smaller at early times (Daddi et al 2005;Zirm et al 2007;Buitrago et al 2008;van Dokkum et al 2008;Damjanov et al 2011;van der Wel et al 2014;Belli et al 2017;Damjanov et al 2019).…”

Section: Introductionmentioning

confidence: 99%

See 4 more Smart Citations

The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

Zahid

Geller

Damjanov

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

We investigate the growth of massive quiescent galaxies at z < 0.6 based on the Sloan Digital Sky Survey and the Smithsonian Hectospec Lensing Survey-two magnitude limited spectroscopic surveys of high data quality and completeness. Our three parameter model links quiescent galaxies across cosmic time by self-consistently evolving stellar mass, stellar population age sensitive D n 4000 index, half-light radius and stellar velocity dispersion. Stellar velocity dispersion is a robust proxy of dark matter halo mass; we use it to connect galaxies and dark matter halos and thus empirically constrain their coevolution. The typical rate of stellar mass growth is ∼ 10 M ⊙ yr −1 and dark matter growth rates from our empirical model are remarkably consistent with N-body simulations. Massive quiescent galaxies grow by minor mergers with dark matter halos of mass 10 10 M ⊙ M DM 10 12 M ⊙ and evolve parallel to the stellar mass-halo mass relation based on N-body simulations. Thus, the stellar mass-halo mass relation of massive galaxies apparently results primarily from dry minor merging.

show abstract

Section: Introductionsupporting

confidence: 86%

Section: Test Of Consistencysupporting

confidence: 75%

“…Half-light radii of SHELS galaxies and details of the procedure are published in Damjanov et al (2019). Here we provide a brief summary.…”

Section: Galaxy Radiusmentioning

confidence: 99%

Section: Test Of Consistencymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 3 more Smart Citations

The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

Zahid

Geller

Damjanov

et al. 2019

ApJ

Self Cite

View full text Add to dashboard Cite

show abstract

Stellar populations of galaxies in the ALHAMBRA survey up to z ∼ 1

Díaz-García

Cenarro

López-Sanjuan

et al. 2019

A&A

View full text Add to dashboard Cite

Aims. We perform a comprehensive study of the stellar population properties (formation epoch, age, metallicity, and extinction) of quiescent galaxies as a function of size and stellar mass to constrain the physical mechanism governing the stellar mass assembly and the likely evolutive scenarios that explain their growth in size. Methods. After selecting all the quiescent galaxies from the ALHAMBRA survey by the dust-corrected stellar mass–colour diagram, we built a shared sample of ∼850 quiescent galaxies with reliable measurements of sizes from the HST. This sample is complete in stellar mass and luminosity, I ≤ 23. The stellar population properties were retrieved using the fitting code for spectral energy distributions called MUlti-Filter FITting for stellar population diagnostics (MUFFIT) with various sets of composite stellar population models. Age, formation epoch, metallicity, and extinction were studied on the stellar mass–size plane as function of size through a Monte Carlo approach. This accounted for uncertainties and degeneracy effects amongst stellar population properties. Results. The stellar population properties of quiescent galaxies and their stellar mass and size since z ∼ 1 are correlated. At fixed stellar mass, the more compact the quiescent galaxy, the older and richer in metals it is (1 Gyr and 0.1 dex, respectively). In addition, more compact galaxies may present slight lower extinctions than their more extended counterparts at the same stellar mass (< 0.1 mag). By means of studying constant regions of stellar population properties across the stellar mass–size plane, we obtained empirical relations to constrain the physical mechanism that governs the stellar mass assembly of the form M⋆ ∝ rcα, where α amounts to 0.50–0.55 ± 0.09. There are indications that support the idea that the velocity dispersion is tightly correlated with the stellar content of galaxies. The mechanisms driving the evolution of stellar populations can therefore be partly linked to the dynamical properties of galaxies, along with their gravitational potential.

show abstract

The dark matter halo masses of elliptical galaxies as a function of observationally robust quantities

Sonnenfeld

Tortora

Hoekstra

et al. 2022

A&A

View full text Add to dashboard Cite

Context. The assembly history of the stellar component of a massive elliptical galaxy is closely related to that of its dark matter halo. Measuring how the properties of galaxies correlate with their halo mass can therefore help to understand their evolution. Aims. We investigate how the dark matter halo mass of elliptical galaxies varies as a function of their properties, using weak gravitational lensing observations. To minimise the chances of biases, we focus on the following galaxy properties that can be determined robustly: the surface brightness profile and the colour. Methods. We selected 2409 central massive elliptical galaxies (log M*/M⊙ ≳ 11.4) from the Sloan Digital Sky Survey spectroscopic sample. We first measured their surface brightness profile and colours by fitting Sérsic models to photometric data from the Kilo-Degree Survey (KiDS). We fitted their halo mass distribution as a function of redshift, rest-frame r-band luminosity, half-light radius, and rest-frame u − g colour, using KiDS weak lensing measurements and a Bayesian hierarchical approach. For the sake of robustness with respect to assumptions on the large-radii behaviour of the surface brightness, we repeated the analysis replacing the total luminosity and half-light radius with the luminosity within a 10 kpc aperture, Lr, 10, and the light-weighted surface brightness slope, Γ10. Results. We did not detect any correlation between the halo mass and either the half-light radius or colour at fixed redshift and luminosity. Using the robust surface brightness parameterisation, we found that the halo mass correlates weakly with Lr, 10 and anti-correlates with Γ10. At fixed redshift, Lr, 10 and Γ10, the difference in the average halo mass between galaxies at the 84th percentile and 16th percentile of the colour distribution is 0.00 ± 0.11 dex. Conclusion. Our results indicate that the average star formation efficiency of massive elliptical galaxies has little dependence on their final size or colour. This suggests that the origin of the diversity in the size and colour distribution of these objects lies with properties other than the halo mass.

show abstract

Quiescent Galaxy Size and Spectroscopic Evolution: Combining HSC Imaging and Hectospec Spectroscopy

Cited by 37 publications

References 115 publications

The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

The Coevolution of Massive Quiescent Galaxies and Their Dark Matter Halos over the Last 6 Billion Years

Stellar populations of galaxies in the ALHAMBRA survey up to z ∼ 1

The dark matter halo masses of elliptical galaxies as a function of observationally robust quantities

Contact Info

Product

Resources

About