SIMBAD references

2013AJ....145...77J - Astron. J., 145, 77 (2013/March-0)

Stellar populations and evolution of early-type cluster galaxies: constraints from optical imaging and spectroscopy of z=0.5-0.9 galaxy clusters.

JORGENSEN I. and CHIBOUCAS K.

Abstract (from CDS):

We present an analysis of stellar populations and evolutionary history of galaxies in three similarly rich galaxy clusters MS0451.6-0305 (z = 0.54), RXJ0152.7-1357 (z = 0.83), and RXJ1226.9+3332 (z = 0.89). Our analysis is based on high signal-to-noise ground-based optical spectroscopy and Hubble Space Telescope imaging for a total of 17-34 members in each cluster. Using the dynamical masses together with the effective radii and the velocity dispersions, we find no indication of evolution of sizes or velocity dispersions with redshift at a given galaxy mass. We establish the Fundamental Plane (FP) and scaling relations between absorption line indices and velocity dispersions. We confirm that the FP is steeper at z ~ 0.86 compared to the low-redshift FP, indicating that under the assumption of passive evolution the formation redshift, zform, depends on the galaxy velocity dispersion (or alternatively mass). At a velocity dispersion of σ = 125 km/s (Mass = 1010.55 M) we find zform= 1.24±0.05, while at σ = 225 km/s (Mass = 1011.36 M) the formation redshift is zform= 1.95+0.3 –0.2, for a Salpeter initial mass function. The three clusters follow similar scaling relations between absorption line indices and velocity dispersions as those found for low-redshift galaxies. The zero point offsets for the Balmer lines depend on cluster redshifts. However, the offsets indicate a slower evolution, and therefore higher formation redshift, than the zero point differences found from the FP, if interpreting the data using a passive evolution model. Specifically, the strength of the higher order Balmer lines Hδ and Hγ implies zform> 2.8. The scaling relations for the metal indices in general show small and in some cases insignificant zero point offsets, favoring high formation redshifts for a passive evolution model. Based on the absorption line indices and recent stellar population models from Thomas et al., we find that MS0451.6-0305 has a mean metallicity [M/H] approximately 0.2 dex below that of the other clusters and our low-redshift sample. We confirm our previous result that RXJ0152.7-1357 has a mean abundance ratio [α/Fe] approximately 0.3 dex higher than that of the other clusters. The differences in [M/H] and [α/Fe] between the high-redshift clusters and the low-redshift sample are inconsistent with a passive evolution scenario for early-type cluster galaxies over the redshift interval studied. Low-level star formation may be able to bring the metallicity of MS0451.6-0305 in agreement with the low-redshift sample, while we speculate whether galaxy mergers can lead to sufficiently large changes in the abundance ratios for the RXJ0152.7-1357 galaxies to allow them to reach the low-redshift sample values in the time available.

Abstract Copyright:

Journal keyword(s): galaxies: clusters: individual (MS0451.6-0305, RXJ0152.7-1357, RXJ1226.9+3332) - galaxies: evolution - galaxies: stellar content

VizieR on-line data: <Available at CDS (J/AJ/145/77): table3.dat table4.dat table5.dat table7.dat table13.dat table14.dat table15.dat table21.dat table22.dat table23.dat table24.dat>

Nomenclature: Fig. 1, Tables 13, 15, 21, 22: [JC2013] MS0451.6-0305 NNNN N=70 among (Nos 12-3906). Fig. 2, Tables 14, 23, 24: [JC2013] RXJ1226.9+3332 NNNN N=119 among (Nos 18-1254).

CDS comments: RXJ0157.2-1357 (Table 1), RXJ0152.7-0152 (p.11), RXJ0152.7-0305 (p.17) and RXJ0152.7-1257 (p.55) are misprints for RXJ0152.7-1357. MS0451.6-0307 (p.15) and MS0451.1-0306 (p.28) are misrpints for MS0451.6-0305. RXJ1226.9+3336 (p.9) and RXJ1226.6+3332 (p.20) are misprints for RXJ1226.9+3332.

Simbad objects: 195

goto Full paper

goto View the reference in ADS

To bookmark this query, right click on this link: simbad:2013AJ....145...77J and select 'bookmark this link' or equivalent in the popup menu


2021.01.28-10:43:40

© Université de Strasbourg/CNRS

    • Contact