82 research outputs found

    Color and Morphology of Galaxies in the Region of the 3C 324 Clusters at z \sim 1.2

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    We investigated the color and morphology of optically selected galaxies in the region of clusters at z \sim 1.2 near to the radio galaxy 3C 324 using archived data taken with the Hubble Space Telescope. The faint galaxies selected at the HST F702W band that contribute to the surface-density excess of the region have wide ranges of color, size, and morphology, which are not likely to be due to contamination by foreground galaxies. Namely, the rest-frame ultraviolet emission properties of the galaxies in the clusters are not very homogeneous; various amounts of star-formation activity may occur in a significant fraction of them. Although our analysis is purely statistical, we find that typical star-forming galaxies with blue colors have a relatively late-type morphology compared to the red quiescent population in the systems.Comment: 12 pages, 10 figures, accepted for publication in PAS

    Central Concentration of Asymmetric Features in Post-starburst Galaxies at z0.8z \sim 0.8

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    We present morphological analyses of Post-starburst galaxies (PSBs) at 0.7<z<0.90.7<z<0.9 in the COSMOS field. We fitted ultraviolet to mid-infrared multi-band photometry of objects with i<24i<24 from COSMOS2020 catalogue with population synthesis models assuming non-parametric, piece-wise constant function of star formation history, and selected 94 those galaxies that have high specific star formation rates (SSFRs) of more than 109.510^{-9.5} yr1^{-1} in 321--1000 Myr before observation and an order of magnitude lower SSFRs within recent 321 Myr. We devised a new non-parametric morphological index which quantifies concentration of asymmetric features, CAC_{A}, and measured it as well as concentration CC and asymmetry AA on the Hubble Space Telescope/Advanced Camera for Surveys IF814WI_{\rm F814W}-band images. While relatively high CC and low AA values of PSBs are similar with those of quiescent galaxies rather than star-forming galaxies, we found that PSBs show systematically higher values of CAC_{A} than both quiescent and star-forming galaxies; 36% of PSBs have logCA>0.8\log{C_{A}} > 0.8, while only 16% (2%) of quiescent (star-forming) galaxies show such high CAC_{A} values. Those PSBs with high CAC_{A} have relatively low overall asymmetry of A0.1A \sim 0.1, but show remarkable asymmetric features near the centre. The fraction of those PSBs with high CAC_{A} increases with increasing SSFR in 321--1000 Myr before observation rather than residual on-going star formation. These results and their high surface stellar mass densities suggest that those galaxies experienced a nuclear starburst in the recent past, and processes that cause such starbursts could lead to the quenching of star formation through rapid gas consumption, supernova/AGN feedback, and so on.Comment: 18 pages, 17 figures, accepted for publication in MNRA

    Subaru Weak-Lensing Survey of Dark Matter Subhalos in the Coma Cluster : Subhalo Mass Function and Statistical Properties

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    We present a 4 deg^2 weak gravitational lensing survey of subhalos in the very nearby Coma cluster using the Subaru/Suprime-Cam. The large apparent size of cluster subhalos allows us to measure the mass of 32 subhalos detected in a model-independent manner, down to the order of 10^-3 of the virial mass of the cluster. Weak-lensing mass measurements of these shear-selected subhalos enable us to investigate subhalo properties and the correlation between subhalo masses and galaxy luminosities for the first time. The mean distortion profiles stacked over subhalos show a sharply truncated feature which is well-fitted by a Navarro-Frenk-White (NFW) mass model with the truncation radius, as expected due to tidal destruction by the main cluster. We also found that subhalo masses, truncation radii, and mass-to-light ratios decrease toward the cluster center. The subhalo mass function, dn/dln M_sub, in the range of 2 orders of magnitude in mass, is well described by a single power law or a Schechter function. Best-fit power indices of 1.09_-0.32^+0.42 for the former model and 0.99_-0.23^+0.34 for the latter, are in remarkable agreement with slopes of ~0.9-1.0 predicted by the cold dark matter paradigm. The tangential distortion signals in the radial range of 0.02-2Mpc/h from the cluster center show a complex structure which is well described by a composition of three mass components of subhalos, the NFW mass distribution as a smooth component of the main cluster, and a lensing model from a large scale structure behind the cluster. Although the lensing signals are 1 order of magnitude lower than those for clusters at z~0.2, the total signal-to-noise ratio, S/N=13.3, is comparable to, or higher, because the enormous number of background source galaxies compensates for the low lensing efficiency of the low lensing efficiency of the nearby cluster.Comment: 30 pages, 18 figures, 9 tables, ApJ in press. Full resolution version is available at http://www.asiaa.sinica.edu.tw/~okabe/files/coma_survey.pd

    A Deficit of Faint Red Galaxies in the Possible Large-Scale Structures around the RDCS J1252.9-2927 Cluster at z=1.24

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    (Abridged) We report a discovery of possible large-scale structures around the RDCS J1252.9-2927 cluster at z=1.24 based on photometric redshifts. We carried out multi-band wide-field imaging with Suprime-Cam on the Subaru Telescope and WFCAM on the United Kingdom Infra-Red Telescope (UKIRT). The distribution of photo-z selected galaxies reveals clumpy structures surrounding the central cluster. We compare the observed structure with an X-ray map and find that two of the four plausible clumps show significant X-ray emissions and one with a marginal detection, which strongly suggest that they are dynamically bound systems. Following the discovery of the possible large-scale structure, we carried out deeper SOFI K_s-band imaging with New Technology Telescope on the four plausible clumps. We construct the optical-to-near-infrared colour-magnitude diagrams of the galaxies in the clumps, and find that the colour-magnitude relation (CMR) of the red galaxies in the clumps is sharply truncated below K_s=22. Interestingly, the main cluster shows a clear relation down to K_s=23 (Lidman et al. 2004). We suggest that galaxies follow the 'environment-dependent down-sizing' evolution. Massive galaxies in high density environments first stop forming stars and become red. Less massive galaxies in less dense environments become red at later times. Based on a few assumptions, we predict that the brightest tip of the CMR appears at z~2.5.Comment: 10 pages, 8 figures, accepted for publication in MNRA
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