We examine the morphology-density relation for complete mass-limited samples of galaxies from five X-ray luminous clusters from z = 0.023 to z = 0.83. We find no change in the morphology-density relation for our complete sample of 366 galaxies with masses > 10(10.8) M-circle dot (roughly 0.4 M-star at z = 0). In contrast, we find a change in the early-type fraction with redshift that is in good agreement with previous work in a luminosity-selected sample (0.4L(star)) of 478 galaxies from the same parent data. Our results indicate that the galaxies that dominate the morphology-density relation, and its evolution, have masses < 10(10.8) M-circle dot.

Using a magnitude-limited, spectroscopic survey of the X-ray-luminous galaxy cluster MS 1054 - 03, we isolate 153 cluster galaxies and measure MS 1054's redshift and velocity dispersion to be z = 0: 8307 +/- 0: 0004 and sigma(z) = 1156 +/- 82 km s(-1). The absorption-line, poststarburst ('' E+ A ''), and emission-line galaxies, respectively, make up 63% +/- 7%, 15% +/- 4%, and 23% +/- 4% of the cluster population. With photometry from HST ACS, we find that the absorption-line members define an exceptionally tight red sequence over a span of similar to 3.5 mag in i(775): their intrinsic scatter in (V-606 - i(775)) color is only 0: 048 +/- 0: 008, corresponding to a (U - B)(z) scatter of 0.041. Their color scatter is comparable to that of the ellipticals (sigma(Vi) = 0: 055 +/- 0: 008), but measurably smaller than that of the combined E+ S0 sample (sigma(Vi) = 0: 072 +/- 0: 010). The color scatter of MS 1054's absorption-line population is approximately twice that of the ellipticals in Coma; this difference is consistent with passive evolution where most of the absorption-line members (> 75%) formed by z similar to 2, and all of them by z similar to 1: 2. For red members, we find a trend (> 95% confidence) of weakening H delta absorption with redder colors that we conclude is due to age: in MS 1054, the color scatter on the red sequence is driven by differences in mean stellar age of up to similar to 1.5 Gyr. We also generate composite spectra and estimate that the average S0 in MS 1054 is similar to 0.5-1 Gyr younger than the average elliptical; this difference in mean stellar age is mainly due to a number of S0's that are blue (18%) and/or are poststarburst systems (21%).

We examined the morphology-density relations for galaxy samples selected by luminosity and by mass in each of five massive X-ray clusters from z = 0.023 to 0.83 for 674 spectroscopically confirmed members. Rest-frame optical colors and visual morphologies were obtained primarily from Hubble Space Telescope images. The visual morphologies ensure consistency with the extensive published results on galaxy evolution in dense environments. Morphologydensity relations (MDRs) are derived in each cluster from a complete, luminosity-selected sample of 452 galaxies with a magnitude limit M-V < M-V(star) + 1. The change in the early-type fraction with redshift matches previous work for massive clusters of galaxies. We performed a similar analysis, deriving MDRs for complete, mass-selected samples of 441 galaxies with a mass limit of 10(10.6) M-circle dot. Our mass limit includes faint objects, the equivalent of similar or equal to 1 mag below L-star for the red cluster galaxies, and encompasses similar or equal to 70% of the stellar mass in cluster galaxies. The MDRs in the massselected sample at densities of Sigma > 50 galaxies Mpc(-2) are similar to those in the luminosity-selected sample but show larger early-type fractions, with a weak indication of a shallower slope. However, the trend with redshift in the fraction of elliptical and S0 galaxies with masses > 10(10.6) M-circle dot differs significantly between the mass-and luminosityselected samples. The clear trend seen in the early-type fraction from z = 0 to similar or equal to 0.8 is not found in mass-selected samples. The early-type galaxy fraction changes much less and is consistent with being constant at 92% +/- 4% at Sigma > 500 galaxies Mpc(-2) and 83% +/- 3% at 50 galaxies Mpc(-2) < Sigma < 500 galaxies Mpc(-2). Given the mass limit in our sample, this suggests that galaxies of mass lower than > 10(10.6) M-circle dot play a significant role in the evolution of the early-type fraction in luminosity-selected samples; i. e., they are larger contributors to the luminosity-selected samples at higher redshifts than at low redshifts.

The Sloan Digital Sky Survey (SDSS) and photometric/ spectroscopic surveys in the GOODS- South field (the Chandra Deep Field-South, CDF- S) are used to construct volume- limited, stellar- mass- selected samples of galaxies at redshifts 0 < z < 1. The CDF- S sample at 0.6 < z < 1.0 contains 207 galaxies complete down to M = 4 x 10(10) M-circle dot (for a "diet'' Salpeter initial mass function), corresponding to a luminosity limit for red galaxies of M-B = -20.1. The SDSS sample at 0: 020 < z < 0: 045 contains 2003 galaxies down to the same mass limit, which corresponds to MB = -19: 3 for red galaxies. Morphologies are determined with an automated method, using the Sersic parameter n and a measure of the residual from the model fits, called "bumpiness,'' to distinguish different morphologies. These classifications are verified with visual classifications. In agreement with previous studies, 65%-70% of the galaxies are located on the red sequence, both at z similar to 0.03 and at z similar to 0.8. Similarly, 65%-70% of the galaxies have n > 2.5. The fraction of E +/- S0 galaxies is 43% +/- 3% at z similar to 0: 03 and 48% +/- 7% at z similar to 0.8; i. e., it has not changed significantly since z similar to 0: 8. When combined with recent results for cluster galaxies in the same redshift range, we find that the morphology- density relation for galaxies more massive than 0.5M* has remained constant since at least z similar to 0.8. This implies that galaxies evolve in mass, morphology, and density such that the morphology- density relation does not change. In particular, the decline of star formation activity and the accompanying increase in the stellar mass density of red galaxies since z similar to 1 must happen without large changes in the early- type galaxy fraction in a given environment.

We present the first detailed study of the properties (temperatures, gravities, and masses) of the NGC 6791 white dwarf population. This unique stellar system is both one of the oldest (8 Gyr) and most metal-rich ([Fe/H] similar to +0.4) open clusters in our Galaxy and has a color-magnitude diagram (CMD) that exhibits both a red giant clump and a much hotter extreme horizontal branch. Fitting the Balmer lines of the white dwarfs in the cluster using Keck/LRIS spectra suggests that most of these stars are undermassive, < M > = 0.43 +/- 0.06 M-circle dot, and therefore could not have formed from canonical stellar evolution involving the helium flash at the tip of the red giant branch. We show that at least 40% of NGC 6791's evolved stars must have lost enough mass on the red giant branch to avoid the flash and therefore did not convert helium into carbon-oxygen in their core. Such increased mass loss in the evolution of the progenitors of these stars is consistent with the presence of the extreme horizontal branch in the CMD. This unique stellar evolutionary channel also naturally explains the recent finding of a very young age (2.4 Gyr) for NGC 6791 from white dwarf cooling theory; helium-core white dwarfs in this cluster will cool similar to 3 times slower than carbon-oxygen-core stars, and therefore the corrected white dwarf cooling age is in fact greater than or similar to 7 Gyr, consistent with the well-measured main-sequence turnoff age. These results provide direct empirical evidence that mass loss is much more efficient in high-metallicity environments and therefore may be critical in interpreting the ultraviolet upturn in elliptical galaxies.

The initial-final mass relation represents a mapping between the mass of a white dwarf remnant and the mass that the hydrogen-burning main-sequence star that created it once had. The empirical relation thus far has been constrained using a sample of similar to 40 stars in young open clusters, ranging in initial mass from similar to 2.75 to 7 M-circle dot, and shows a general trend that connects higher mass main-sequence stars with higher mass white dwarfs. In this paper, we present CFHT CFH12K photometric and Keck LRIS multiobject spectroscopic observations of a sample of 22 white dwarfs in two older open clusters, NGC 7789 (t = 1.4 Gyr) and NGC 6819 (t = 2.5 Gyr). We measure masses for the highest signal-to-noise ratio spectra by fitting the Balmer lines to atmosphere models and place the first direct constraints on the low-mass end of the initial-final mass relation. Our results indicate that the observed general trend at higher masses continues down to low masses, with M-initial = 1.6 M-circle dot main-sequence stars forming M-final = 0.54 M-circle dot white dwarfs. When added to our new data from the very old cluster NGC 6791, the relation is extended down to M-initial = 1.16 M-circle dot (corresponding to M-final = 0.53 M-circle dot). This extension of the relation represents a fourfold increase in the total number of hydrogen-burning stars for which the integrated mass loss can now be calculated from empirical data, assuming a Salpeter initial mass function. The new leverage at the low-mass end is used to derive a purely empirical initial-final mass relation. The sample of white dwarfs in these clusters also shows several interesting systems that we discuss further: a DB (helium) white dwarf, a magnetic white dwarf, a DAB (mixed hydrogen/helium atmosphere or a double degenerate DA+DB) white dwarf(s), and two possible equal-mass DA double degenerate binary systems.

To determine the relative contributions of galactic and intracluster stars to the enrichment of the intracluster medium (ICM), we present X-ray surface brightness, temperature, and Fe abundance profiles for a set of 12 galaxy clusters(4) for which we have extensive optical photometry. Assuming a standard initial mass function and simple chemical evolution model scaled to match the present-day cluster early-type SN Ia rate, the stars in the brightest cluster galaxy (BCG) plus the intracluster stars (ICS) generate 31(-9)(+11)%, on average, of the observed ICM Fe within r(500) (similar to 0.6 times r(200), the virial radius). An alternate, two-component SN Ia model (including both prompt and delayed detonations) produces a similar BCG+ ICS contribution of 22(-9)(+9)%. Because the ICS typically contribute 80% of the BCG+ ICS Fe, we conclude that the ICS are significant, yet often neglected, contributors to the ICM Fe within r(500). However, the BCG+ICS fall short of producing all the Fe, so metal loss from stars in other cluster galaxies must also contribute. By combining the enrichment from intracluster and galactic stars, we can account for all the observed Fe. These models require a galactic metalloss fraction (0.84+(+0.11)(-0.14)) that, while large, is consistent with the metal mass not retained by galactic stars. The SN Ia rates, especially as a function of galaxy environment and redshift, remain a significant source of uncertainty in further constraining the metal-loss fraction. For example, increasing the SN Ia rate by a factor of 1.8-to just within the 2 sigma uncertainty for present-day cluster early-type galaxies-allows the combined BCG + ICS + cluster galaxy model to generate all the ICM Fe with a much lower galactic metal-loss fraction (similar to 0.35).

We have compiled a sample of early-type cluster galaxies from 0 < z < 1.3 and measured the evolution of their ellipticity distributions. Our sample contains 487 galaxies in 17 z > 0.3 clusters with high-quality space-based imaging and a comparable sample of 210 galaxies in 10 clusters at z < 0.05. We select early-type galaxies (elliptical and S0 galaxies) that fall within the cluster R-200, and which lie on the red-sequence in the magnitude range -19.3 > M-B > -21, after correcting for luminosity evolution as measured by the fundamental plane. Our ellipticity measurements are made in a consistent manner over our whole sample. We perform extensive simulations to quantify the systematic and statistical errors, and find that it is crucial to use point-spread function (PSF)-corrected model fits; determinations of the ellipticity from Hubble Space Telescope image data that do not account for the PSF "blurring" are systematically and significantly biased to rounder ellipticities at redshifts z > 0.3. We find that neither the median ellipticity, nor the shape of the ellipticity distribution of cluster early-type galaxies evolves with redshift from z similar to 0 to z > 1 (i.e., over the last similar to 8 Gyr). The median ellipticity at z > 0.3 is statistically identical with that at z < 0.05, being higher by only 0.01 +/- 0.02 or 3 +/- 6%, while the distribution of ellipticities at z > 0.3 agrees with the shape of the z < 0.05 distribution at the 1-2% level (i.e., the probability that they are drawn from the same distribution is 98-99%). These results are strongly suggestive of an unchanging overall bulge-to-disk ratio distribution for cluster early-type galaxies over the last similar to 8 Gyr from z similar to 1 to z similar to 0. This result contrasts with that from visual classifications which show that the fraction of morphologically-selected disk-dominated early-type galaxies, or S0s, is significantly lower at z > 0.4 than at z similar to 0. We find that the median disk-dominated early-type, or S0, galaxy has a somewhat higher ellipticity at z > 0.3, suggesting that rounder S0s are being assigned as ellipticals. Taking the ellipticity measurements and assuming, as in all previous studies, that the intrinsic ellipticity distribution of both elliptical and S0 galaxies remains constant, then we conclude from the lack of evolution in the observed early-type ellipticity distribution that the relative fractions of ellipticals and S0s do not evolve from z similar to 1 to z = 0 for a red-sequence selected samples of galaxies in the cores of clusters of galaxies.

We use extensive new observations of the very rich z similar to 0.4 cluster of galaxies A851 to examine the nature and origin of starburst galaxies in intermediate-redshift clusters. New HST observations, 24 mu m Spitzer photometry and ground-based spectroscopy cover most of a region of the cluster about 10' across, corresponding to a cluster-centric radial distance of about 1.6 Mpc. This spatial coverage allows us to confirm the existence of a morphology-density relation within this cluster, and to identify several large, presumably infalling, subsystems. We confirm our previous conclusion that a very large fraction of the star-forming galaxies in A851 has recently undergone starbursts. We argue that starbursts are mostly confined to two kinds of sites: infalling groups and the cluster center. At the cluster center, it appears that infalling galaxies are undergoing major mergers, resulting in starbursts whose optical-emission lines are completely buried beneath dust. The aftermath of this process appears to be proto-S0 galaxies devoid of star formation. In contrast, major mergers do not appear to be the cause of most of the starbursts in infalling groups, and fewer of these events result in the transformation of the galaxy into an S0. Some recent theoretical work provides possible explanations for these two distinct processes, but it is not clear whether they can operate with the very high efficiency needed to account for the very large starburst rate observed.

We present the first results from the largest spectroscopic survey to date of an intermediate redshift galaxy cluster, the z = 0.834 cluster RX J0152.7-1357. We use the colors of galaxies, assembled from a D similar to 12 Mpc region centered on the cluster, to investigate the properties of the red sequence as a function of density and clustercentric radius. Our wide-field multislit survey with a low-dispersion prism in the Inamori Magellan Areal Camera and Spectrograph at the 6.5 m Baade telescope allowed us to identify 475 new members of the cluster and its surrounding large-scale structure with a redshift accuracy of sigma(z)/(1 + z) approximate to 1% and a contamination rate of similar to 2% for galaxies with i' < 23.75 mag. We combine these new members with the 279 previously known spectroscopic members to give a total of 754 galaxies from which we obtain a mass-limited sample of 300 galaxies with stellar masses M > 4 x 10(10) M-circle dot (log M/M-circle dot > 10.6). We find that the red galaxy fraction is 93 +/- 3% in the two merging cores of the cluster and declines to a level of 64 +/- 3% at projected clustercentric radii R greater than or similar to 3 Mpc. At these large projected distances, the correlation between clustercentric radius and local density is nonexistent. This allows an assessment of the influence of the local environment on galaxy evolution, as opposed to mechanisms that operate on cluster scales (e.g., harassment, ram-pressure stripping). Even beyond R > 3 Mpc we find an increasing fraction of red galaxies with increasing local density. The red galaxy fraction at the highest local densities in two large groups at R > 3 Mpc matches the red galaxy fraction found in the two cores. Strikingly, galaxies at intermediate densities at R > 3 Mpc, that are not obvious members of groups, also show signs of an enhanced red galaxy fraction. Our results point to such intermediate-density regions and the groups in the outskirts of the cluster, as sites where the local environment influences the transition of galaxies onto the red sequence.