We present follow-up spectroscopy of the galaxy cluster MS 1054 03 (z = 0.83) confirming that at least six of the nine merging galaxy pairs identified by van Dokkum et al. in 1999 are indeed bound systems: they have projected separations of R-s < 10h(-1) kpc and relative line-of-sight velocities of Delta nu < 165 kms(-1). For the remaining three pairs, we were unable to obtain redshifts of both constituent galaxies. To identify a more objective sample of merging systems, we select bound red galaxy pairs (R-s <= 30 h(-1) kpc,Delta nu <= 300 km s(-1)) from our sample of 121 confirmed cluster members: galaxies in bound red pairs make up 15.7% +/- 3.6% of the cluster population. The color-magnitude diagram shows that the pair galaxies are as red as the E/S0 members and have a s homogeneous stellar population. The red pair galaxies span a large range in luminosity and internal velocity dispersion, to include some of the brightest, most massive members (L > L*,sigma(1D) > 200 km s(-1)); these bound 1D galaxy pairs must evolve into E/S0 members by z similar to 0.7. These results, combined with MS 1054' s high merger fraction and reservoir of likely future mergers, indicates that most, if not all, of its early-type members evolved from (passive) galaxy- galaxy mergers at. z <= 1.

We examine the distribution of stellar masses of galaxies in MS 1054.4 - 0321 and Cl 0152.7 - 1357, two X-ray-selected clusters of galaxies at z = 0.83. Our stellar mass estimates, from spectral energy distribution fitting, reproduce the dynamical masses as measured from velocity dispersions and half-light radii with a scatter of 0.2 dex in the mass for early-type galaxies. When we restrict our sample of members to high stellar masses, those over 10(11.1) M-circle dot (M* in the Schechter mass function for cluster galaxies), we find that the fraction of early-type galaxies is 79% +/- 6% at z = 0.83 and 87% +/- 6% at z = 0.023 for the Coma Cluster, consistent with no evolution. Previous work with luminosity-selected samples has found that the early-type fraction in rich clusters declines from similar or equal to 80% at z = 0 to similar or equal to 60% at z = 0.8. The observed evolution in the early-type fraction from luminosity-selected samples must predominantly occur among sub-M* galaxies. As M* for field and group galaxies, especially late types, is below M* for cluster galaxies, infall could explain most of the recent growth in the early-type fraction. Future surveys could determine the morphological distributions of lower mass systems, which would confirm or refute this explanation.

In this paper we analyze previously published spectra with high signal-to-noise ratios of E/S0s in the rich cluster CL 1358+62 at z = 0.33. Introducing techniques for fitting stellar population models to the data, we focus on the 19 Es and SOS with a homogeneous set of eight blue Lick indices. We explore the galaxy properties using six-parameter stellar population models from the literature and describe an approach for fitting the models differentially, such that the largest systematic errors are avoided. The results of the model fitting are accurate relative measures of the stellar population parameters. We find (1) no difference between the best-fit stellar population parameters of Es and S0s at fixed or; (2) the stars in Es and S0s are uniformly old, consistent with previously published results using the fundamental plane; (3) a correlation of [Z/H] with sigma, in a manner consistent with the observed B-V colors of the galaxies; (4) no strong correlation of [alpha/Fe] with sigma, discrepant with the correlation inferred from data on nearby galaxies at the < 3 sigma or level; and (5) a significant anticorrelation of [alpha/N] with sigma, which we interpret as a correlation of the abundance of secondary nitrogen with mean metallicity. While the differences between our conclusions and the current view of stellar populations may point to serious deficiencies, our deduced correlation of mean metallicity with velocity dispersion does reproduce the observed colors of the galaxies and the slope of the local Mg-sigma relation. More specifically, our data conclusively show that cluster S0s did not form their stars at significantly later epochs than cluster elliptical galaxies of the same mass, and the presence of secondary nitrogen indicates that both Es and S0s formed from self-enriching progenitors, presumably with extended star formation histories.

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).