FRINK Linked Data Fragments server

Matches in SemOpenAlex for { <https://semopenalex.org/work/W2029202895> ?p ?o ?g. }

• W2029202895 endingPage "217" @default.
• W2029202895 startingPage "193" @default.
• W2029202895 abstract "We present a detailed (U - V) color-magnitude relation (CMR) analysis for three local (z < 0.06) clusters of galaxies. From square-degree imaging of the Abell clusters A85, A496, and A754, we select 637 galaxies down to L ~ 0.1L with spectroscopic membership, which minimizes uncertain field contamination corrections. To characterize the degree of CMR uniformity among nearby clusters, we use a maximum likelihood technique to quantify the CMR properties of the red galaxies in each cluster. We find that these clusters have similar CMRs with a mean color of (U - V) = 1.40 at MV = -20 + 5 h and narrow limits of intrinsic color scatter [0.047, 0.079] and slope [-0.094, -0.075]. If we restrict our analysis to the core cluster population of red galaxies, the resulting CMRs are in close agreement with that of the Coma Cluster, the only local cluster with a rest-frame (U - V) CMR determination of comparable precision. Therefore, the CMR uniformity of present-day clusters spans a fairly wide range of cluster masses. We test how sensitive the CMR uniformity is to variations in color aperture size and sample selection, and we find at most slightly wider limits of scatter [0.047, 0.112] and slope [-0.104, -0.054]. This upper limit for (U - V) scatter is consistent with the bulk of the stellar populations of red cluster galaxies forming before z = 1.2, with a maximum age spread of 5.2 Gyr. In addition, we note that using colors from apertures containing equal fractions of galactic light does not remove the CMR slope and that none of the slopes exhibit a break as claimed by Metcalf and coworkers. Our findings expand the single Coma data point and provide a much needed z = 0 baseline for comparisons to high-redshift cluster CMRs at the same rest-frame wavelengths. The range in CMR scatter that we find among nearby clusters is consistent with the values reported for clusters at higher redshifts, further suggesting that there has been little evolution in the stellar populations of red-sequence cluster galaxies out to at least z ~ 1. To identify the most recently accreted cluster galaxies, we divide each cluster's membership into three galaxy populations based on (U - V) color relative to the well-defined CMR. Blue and moderately blue galaxies make up 18%-23% by number of each cluster population more luminous than 0.1L*. Our color-magnitude division should represent a rough time since cluster accretion. In testing this hypothesis, we find that blue galaxies are spatially, kinematically, and morphologically distinct from red cluster galaxies. Even in projection, the blue galaxies reside toward the outskirts of the cluster and appear to avoid the inner half-megaparsec, in contrast with the increasing density of red-sequence galaxies toward the cluster center. In addition, the blue galaxies have velocity distributions relative to the cluster rest frame that are flatter, and some have different means, compared to the roughly Gaussian distribution of red member velocities. Members with the bluest colors tend to be disklike or irregular in appearance compared to the red galaxies, which have mostly early-type (E/S0) morphologies. Moderately blue cluster galaxies may be an intermediate mix with a fraction of small bulge-to-disk ratio S0s, yet these require closer scrutiny. The spatial, kinematic, and morphological distinctions between blue and red cluster galaxies provide further evidence that CMR-relative color is related to time since cluster infall and that bluer members are indeed the most recently accreted field spirals as expected in a hierarchical universe." @default.
• W2029202895 created "2016-06-24" @default.
• W2029202895 creator A5061006497 @default.
• W2029202895 creator A5073154205 @default.
• W2029202895 creator A5077018414 @default.
• W2029202895 creator A5082738705 @default.
• W2029202895 date "2005-01-20" @default.
• W2029202895 modified "2023-09-26" @default.
• W2029202895 title "Testing the Universality of the (<i>U</i>−<i>V</i>) Color‐Magnitude Relations for Nearby Clusters of Galaxies" @default.
• W2029202895 cites W1963899544 @default.
• W2029202895 cites W1964055719 @default.
• W2029202895 cites W1964338087 @default.
• W2029202895 cites W1967681399 @default.
• W2029202895 cites W1968547533 @default.
• W2029202895 cites W1969160776 @default.
• W2029202895 cites W1971146348 @default.
• W2029202895 cites W1973007101 @default.
• W2029202895 cites W1973518746 @default.
• W2029202895 cites W1974098844 @default.
• W2029202895 cites W1974772481 @default.
• W2029202895 cites W1975485972 @default.
• W2029202895 cites W1978090530 @default.
• W2029202895 cites W1980118658 @default.
• W2029202895 cites W1982051859 @default.
• W2029202895 cites W1986936588 @default.
• W2029202895 cites W1988371023 @default.
• W2029202895 cites W1992898138 @default.
• W2029202895 cites W1993080318 @default.
• W2029202895 cites W1994671833 @default.
• W2029202895 cites W1999367759 @default.
• W2029202895 cites W2002573945 @default.
• W2029202895 cites W2007325934 @default.
• W2029202895 cites W2013171719 @default.
• W2029202895 cites W2019783281 @default.
• W2029202895 cites W2021008553 @default.
• W2029202895 cites W2021918512 @default.
• W2029202895 cites W2022441827 @default.
• W2029202895 cites W2024765452 @default.
• W2029202895 cites W2025097755 @default.
• W2029202895 cites W2029130923 @default.
• W2029202895 cites W2030154533 @default.
• W2029202895 cites W2037853609 @default.
• W2029202895 cites W2038434077 @default.
• W2029202895 cites W2039414721 @default.
• W2029202895 cites W2041335483 @default.
• W2029202895 cites W2048758550 @default.
• W2029202895 cites W2049531400 @default.
• W2029202895 cites W2051313615 @default.
• W2029202895 cites W2052755662 @default.
• W2029202895 cites W2053254002 @default.
• W2029202895 cites W2053837851 @default.
• W2029202895 cites W2055327934 @default.
• W2029202895 cites W2058889425 @default.
• W2029202895 cites W2061510346 @default.
• W2029202895 cites W2062557349 @default.
• W2029202895 cites W2064094999 @default.
• W2029202895 cites W2065121054 @default.
• W2029202895 cites W2070304421 @default.
• W2029202895 cites W2072016033 @default.
• W2029202895 cites W2076577536 @default.
• W2029202895 cites W2078590813 @default.
• W2029202895 cites W2079120125 @default.
• W2029202895 cites W2080660497 @default.
• W2029202895 cites W2083006690 @default.
• W2029202895 cites W2083116240 @default.
• W2029202895 cites W2084091264 @default.
• W2029202895 cites W2085911494 @default.
• W2029202895 cites W2088863566 @default.
• W2029202895 cites W2092316045 @default.
• W2029202895 cites W2092916207 @default.
• W2029202895 cites W2094710844 @default.
• W2029202895 cites W2111817932 @default.
• W2029202895 cites W2125884793 @default.
• W2029202895 cites W2139208191 @default.
• W2029202895 cites W2142238829 @default.
• W2029202895 cites W2145510903 @default.
• W2029202895 cites W2156479091 @default.
• W2029202895 cites W2156546445 @default.
• W2029202895 cites W2158932364 @default.
• W2029202895 cites W2159354593 @default.
• W2029202895 cites W2171327366 @default.
• W2029202895 cites W2171494255 @default.
• W2029202895 cites W2569367783 @default.
• W2029202895 cites W3100569743 @default.
• W2029202895 cites W3100711035 @default.
• W2029202895 cites W3101826679 @default.
• W2029202895 cites W3102951400 @default.
• W2029202895 cites W3104518655 @default.
• W2029202895 cites W3104578891 @default.
• W2029202895 cites W3105149290 @default.
• W2029202895 cites W3105386670 @default.
• W2029202895 cites W3105828359 @default.
• W2029202895 cites W3106151161 @default.
• W2029202895 cites W3106442446 @default.
• W2029202895 cites W3125941288 @default.
• W2029202895 cites W3181935618 @default.
• W2029202895 cites W4229934221 @default.
• W2029202895 cites W4245147268 @default.

• next