We study the fundamental plane (FP) of field early-type galaxies at intermediate redshift, using Hubble Space Telescope Wide Field Planetary Camera 2 observations and deep Keck spectroscopy. Structural parameters and internal velocity dispersions are measured for 18 galaxies at 0.15 < z < 0.55. Rest-frame M/L-B ratios are determined from the FP and compared to those of cluster early-type galaxies at the same redshifts. The systematic offset between MIL ratios of field and cluster early-type galaxies at intermediate redshift is small and not significant: [ln M/L-B](field) - [ln M/L-B](clus) = -0.18 +/- 0.11. The M/L-B ratio of field early-type galaxies evolves as Delta ln M/L-B = (-1.35 +/- 0.35)z, very similar to cluster early-type galaxies. After correcting for luminosity evolution, the FP of field early-type galaxies has a scatter sigma = 0.09 +/- 0.02 in log r(e), similar to that in local clusters. The scatter appears to be driven by low-mass S0 galaxies; for the elliptical galaxies alone we find a = 0.03(-0.03)(+0.04). There is a hint that the FP has a different slope than in clusters, but more data are needed to confirm this. The similarity of the MIL ratios of cluster and field early-type galaxies provides a constraint on the relative ages of their stars. At (z) = 0.43, held early-type galaxies are younger than cluster early-type galaxies by only 21% +/- 13%, and we infer that the stars in field early-type galaxies probably formed at z greater than or equal to 1.5. Recent semianalytical models for galaxy formation in a Lambda CDM universe predict a systematic difference between held and cluster galaxies of Delta ln M/L-B similar to -0.6, much larger than the observed difference. This result is consistent with the hypothesis that field early-type galaxies formed earlier than predicted by these models.

We present here the final results of the Hubble Space Telescope (HST) Key Project to measure the Hubble constant. We summarize our method, the results, and the uncertainties, tabulate our revised distances, and give the implications of these results for cosmology. Our results are based on a Cepheid calibration of several secondary distance methods applied over the range of about 60-400 Mpc. The analysis presented here benefits from a number of recent improvements and refinements, including (1) a larger LMC Cepheid sample to define the fiducial period-luminosity (PL) relations, (2) a more recent HST Wide Field and Planetary Camera 2 (WFPC2) photometric calibration, (3) a correction for Cepheid metallicity, and (4) a correction for incompleteness bias in the observed Cepheid PL samples. We adopt a distance modulus to the LMC (relative to which the more distant galaxies are measured) of mu (o)(LMC) = 18.50 +/- 0.10 mag, or 50 kpc. New, revised distances are given for the 18 spiral galaxies for which Cepheids have been discovered as part of the Key Project, as well as for 13 additional galaxies with published Cepheid data. The new calibration results in a Cepheid distance to NGC 4258 in better agreement with the maser distance to this galaxy. Based on these revised Cepheid distances, we find values (in km s(-1) Mpc(-1)) of H-o = 71 +/- 2 (random) +/- 6 (systematic) (Type Ia supernovae), H-o = 71 +/- 3 +/- 7 (Tully-Fisher relation), H-o = 70 +/- 5 +/- 6 (surface brightness fluctuations), H-o = 72 +/- 9 +/- 7 (Type II supernovae), and H-o = 82 +/- 6 +/- 9 (fundamental plane). We combine these results for the different methods with three different weighting schemes, and find good agreement and consistency with H-o = 72 +/- 8 km s(-1) Mpc(-1). Finally, we compare these results with other, global methods for measuring H-o.

We have obtained deep, long-slit spectroscopy along the major axis of NGC 6166, the cD galaxy in the cluster A2199, in order to measure the kinematics of intracluster stars at large radii. The velocity dispersion initially decreases from the central value of 300 to 200 km s(-1) within a few kiloparsecs and then steadily rises to 660 km s(-1) at a radius of 60 kpc (H-0 = 75 km s(-1) Mpc(-1), Omega(m) = 0.3, Omega(Lambda) = 0.7), nearly reaching the velocity dispersion of the cluster (sigma(A2199) = 775 +/- 50 km s(-1)). These data suggest that the stars in the halo of the cD galaxy trace the potential of the cluster and that the kinematics of these intracluster stars can be used to constrain the mass pro le of the cluster. In addition, we find evidence for systematic rotation (V/sigma approximate to 0.3) in the intracluster stars beyond 20 kpc. Such rotation is not seen in the kinematics of the cluster members. The surface brightness and velocity dispersion profiles can be fitted using a single-component mass model only by making unphysical assumptions about the level of anisotropy for both the stars in the cD galaxy and the kinematics of the galaxies in the cluster. Two-component mass models for the cD galaxy and its halo are subsequently explored using the kinematics of known cluster members as an additional constraint on the total enclosed mass beyond the extent of the stellar kinematics. Under the assumption of isotropy, the observed major-axis kinematics can be reproduced only if the halo, parameterized by a generalized Navarro-Frenk-White (NFW) profile, has a soft core, i.e., alpha < 1 ( a generalized NFW halo with alpha = 1 is excluded because of low implied stellar mass-to-light ratios). This result is inconsistent with the predictions of current N-body simulations for dark matter halos. To test the consistency of our halo profiles with those derived from strong lensing measurements in intermediate-redshift clusters, we calculate the critical radii for tangential arcs, assuming that our best-fit mass models for A2199 were placed at cosmological redshifts between 0.2 <= z <= 0.5. The calculated critical radii for our best-fit two-component isotropic models range from 5" to 40", depending on the assumed source redshift, consistent with the radii for gravitational arcs observed in intermediate-redshift clusters. We also present the results of Monte Carlo simulations testing the general reliability of velocity dispersion measurements in the regime of low signal-to-noise ratio and large intrinsic Doppler broadening.

In two-dimensional spectrographs, the optical distortions in the spatial and dispersion directions produce variations in the subpixel sampling of the background spectrum. Using knowledge of the camera distortions and the curvature of the spectral features, one can recover information regarding the background spectrum on wavelength scales much smaller than a pixel. As a result, one can propagate this better sampled background spectrum through inverses of the distortion and rectification transformations and accurately model the background spectrum in two-dimensional spectra for which the distortions have not been removed (i.e., the data have not been rebinned/rectified). The procedure, as outlined in this paper, is extremely insensitive to cosmic rays, hot pixels, etc. Because of this insensitivity to discrepant pixels, sky modeling and subtraction need not be performed as one of the later steps in a reduction pipeline. Sky subtraction can now be performed as one of the earliest tasks, perhaps just after dividing by a flat field. Because subtraction of the background can be performed without having to "clean" cosmic rays, such bad pixel values can be trivially identified after removal of the two-dimensional sky background.

Combining Hubble Space Telescope WFPC2 mosaics with extensive ground-based spectroscopy, we study the nature of E+A galaxies in three intermediate-redshift clusters (z = 0.33, 0.58, and 0.83). From a sample of similar to500 confirmed cluster members, we isolate 46 E+A candidates to determine the E+A fraction and study their physical properties. Spectral types are assigned using Balmer (Hdelta, Hgamma, Hbeta) and [O II] lambda3727 equivalent widths. For all members, we have galaxy colors, luminosities, Hubble types, and quantitative structural parameters. We also include measured internal velocity dispersions for 120 cluster members and estimate velocity dispersions for the rest of the cluster sample using the fundamental plane. We find that E+A galaxies comprise a nonnegligible component (similar to7%-13%) of the cluster population at these redshifts, and their diverse nature indicates a heterogeneous parent population. While cluster E+A's are predominantly disk-dominated systems, they span the range in Hubble type and bulge-to-total fraction to include even early-type members. Cluster E+A's also cover a wide range in luminosity [L-B similar to (0.2-2.5)L-B*], internal velocity dispersion (sigma similar to30-220 km s(-1)), and half-light radius [r(1/2) similar to (0.4-4.3)h(-1) kpc]. From their velocity dispersions and half-light radii, we infer that the descendants of E+A's in our highest redshift cluster are massive early-type galaxies. In contrast to the wide range of luminosity and internal velocity dispersion spanned by E+A's at higher redshift, only low-mass E+A's are found in nearby clusters, e. g., Coma. The observed decrease in the characteristic E+A mass is similar to the decrease in the luminosity of rapidly star-forming field galaxies since z similar to 1, i.e., galaxy "downsizing." In addition, we argue that our statistics imply that greater than or similar to30% of the E-S0 members have undergone an E+A phase; the true fraction could be 100% if the effects of E+A downsizing, an increasing E+A fraction with redshift, and the conversion of spiral galaxies into early type galaxies are also considered. Thus, the E+A phase may indeed be an important stage in the transformation of star-forming galaxies into early-type members.

We select E+A candidates from a spectroscopic data set of similar to800 field galaxies and measure the E+A fraction at 0.3 < z < 1 to be 2.7% +/- 1.1%, a value lower than that in galaxy clusters at comparable redshifts (11% +/- 3%). HST WFPC2 imaging for five of our six E+A's shows that they have a heterogeneous parent population: these E+A's span a range in half-light radius (0.8 h(-1) kpc < r(1/2) < 8 h(-1) kpc) and estimated internal velocity dispersion (50 km s(-1) less than or similar to sigma(est) less than or similar to 220 km s(-1)), and they include luminous systems (-21.6 less than or equal to M-Bz - 5 log h less than or equal to - 19.2). Despite their diversity in some aspects, the E+A's share several common characteristics that indicate that the E+A phase is an important link in the evolution of star-forming galaxies into passive systems: the E+A's are uniformly redder than the blue, star-forming galaxies that make up the majority of the field, they are more likely to be bulge-dominated than the average field galaxy, and they tend to be morphologically irregular. We find that E+A's make up similar to9% of the absorption-line systems in this redshift range and estimate that greater than or similar to25% of passive galaxies in the local field had an E+A phase at z less than or similar to 1.

Using wide-field Hubble Space Telescope WFPC2 imaging and extensive Keck LRIS spectroscopy, we present a detailed study of the galaxy populations in MS 2053-04, a massive, X-ray-luminous cluster at z = 0.5866 +/- 0.0011. Analysis of 149 confirmed cluster members shows that MS 2053 is composed of two structures that are gravitationally bound to each other; their respective velocity dispersions are 865 +/- 71 km s(-1) (113 members) and 282 +/- 51 km s(-1) (36 members). MS 2053's total dynamical mass is 1.2 x 10(15) M.. MS 2053 is a classic Butcher-Oemler cluster with a high fraction of blue members (24% +/- 5%) and an even higher fraction of star-forming members (44% +/- 7%), as determined from their [O II] lambda3727 emission. The number fraction of blue/star-forming galaxies is much higher in the infalling structure than in the main cluster. This result is the most direct evidence to date that the Butcher-Oemler effect is linked to galaxy infall. In terms of their colors, luminosities, estimated internal velocity dispersions, and [O II] lambda3727 equivalent widths, the infalling galaxies are indistinguishable from the field population. MS 2053's deficit of S0 galaxies combined with its overabundance of blue spirals implies that many of these late-type galaxies will evolve into S0 members. The properties of the blue cluster members in both the main cluster and infalling structure indicate that they will evolve into low-mass, L < L-* galaxies with extended star formation histories like that of low-mass S0 galaxies in Coma. Our observations show that most of MS 2053's blue cluster members, and ultimately most of its low-mass S0 galaxies, originate in the field. Finally, we measure the redshift of the giant arc in MS 2053 to be z = 3.1462; this object is one in only a small set of known strongly lensed galaxies at z > 3.

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.