The low-redshift universe (z similar to 0.5) is not a dull place. Processes leading to the suppression of star formation and morphological transformation are prevalent: this is particularly evident in the dramatic upturn in the fraction of S0-type galaxies in clusters. However, until now, the process and environment of formation remained unidentified. We present a morphological analysis of galaxies in the optically-selected (spectroscopic friends-of-friends) group and field environments at z similar to 0.4. Groups contain a much higher fraction of S0s at fixed luminosity than the lower density field, with >99.999% confidence. Indeed, the S0 fraction in groups is at least as high as in z similar to 0.4 clusters and X-ray-selected groups, which have more luminous intragroup medium (IGM). An excess of S0s at >= 0.3h(75)(-1) Mpc from the group center with respect to the inner regions, existing with 97% confidence at fixed luminosity, tells us that formation is not restricted to, and possibly even avoids, the group cores. Interactions with a bright X-ray-emitting IGM cannot be important for the formation of the majority of S0s in the universe. In contrast to S0s, the fraction of elliptical galaxies in groups at fixed luminosity is similar to the field, while the brightest ellipticals are strongly enhanced toward the group centers (greater than 99.999% confidence within >= 0.3h(75)(-1) Mpc). Interestingly, while spirals are altogether less common in groups than in the field, there is also an excess of faint, Sc+ type spirals within >= 0.3h(75)(-1) Mpc of the group centers (99.953% confidence). We conclude that the group and subgroup environments must be dominant for the formation of S0 galaxies, and that minor mergers, galaxy harassment, and tidal interactions are the most likely responsible mechanisms. This has implications not only for the inferred preprocessing of cluster galaxies, but also for the global morphological and star formation budget of galaxies: as hierarchical clustering progresses, more galaxies will be subject to these transformations as they enter the group environment.

The low-redshift universe (z similar to 0.5) is not a dull place. Processes leading to the suppression of star formation and morphological transformation are prevalent: this is particularly evident in the dramatic upturn in the fraction of S0-type galaxies in clusters. However, until now, the process and environment of formation remained unidentified. We present a morphological analysis of galaxies in the optically-selected (spectroscopic friends-of-friends) group and field environments at z similar to 0.4. Groups contain a much higher fraction of S0s at fixed luminosity than the lower density field, with >99.999% confidence. Indeed, the S0 fraction in groups is at least as high as in z similar to 0.4 clusters and X-ray-selected groups, which have more luminous intragroup medium (IGM). An excess of S0s at >= 0.3h(75)(-1) Mpc from the group center with respect to the inner regions, existing with 97% confidence at fixed luminosity, tells us that formation is not restricted to, and possibly even avoids, the group cores. Interactions with a bright X-ray-emitting IGM cannot be important for the formation of the majority of S0s in the universe. In contrast to S0s, the fraction of elliptical galaxies in groups at fixed luminosity is similar to the field, while the brightest ellipticals are strongly enhanced toward the group centers (greater than 99.999% confidence within >= 0.3h(75)(-1) Mpc). Interestingly, while spirals are altogether less common in groups than in the field, there is also an excess of faint, Sc+ type spirals within >= 0.3h(75)(-1) Mpc of the group centers (99.953% confidence). We conclude that the group and subgroup environments must be dominant for the formation of S0 galaxies, and that minor mergers, galaxy harassment, and tidal interactions are the most likely responsible mechanisms. This has implications not only for the inferred preprocessing of cluster galaxies, but also for the global morphological and star formation budget of galaxies: as hierarchical clustering progresses, more galaxies will be subject to these transformations as they enter the group environment.

The low-redshift universe (z similar to 0.5) is not a dull place. Processes leading to the suppression of star formation and morphological transformation are prevalent: this is particularly evident in the dramatic upturn in the fraction of S0-type galaxies in clusters. However, until now, the process and environment of formation remained unidentified. We present a morphological analysis of galaxies in the optically-selected (spectroscopic friends-of-friends) group and field environments at z similar to 0.4. Groups contain a much higher fraction of S0s at fixed luminosity than the lower density field, with >99.999% confidence. Indeed, the S0 fraction in groups is at least as high as in z similar to 0.4 clusters and X-ray-selected groups, which have more luminous intragroup medium (IGM). An excess of S0s at >= 0.3h(75)(-1) Mpc from the group center with respect to the inner regions, existing with 97% confidence at fixed luminosity, tells us that formation is not restricted to, and possibly even avoids, the group cores. Interactions with a bright X-ray-emitting IGM cannot be important for the formation of the majority of S0s in the universe. In contrast to S0s, the fraction of elliptical galaxies in groups at fixed luminosity is similar to the field, while the brightest ellipticals are strongly enhanced toward the group centers (greater than 99.999% confidence within >= 0.3h(75)(-1) Mpc). Interestingly, while spirals are altogether less common in groups than in the field, there is also an excess of faint, Sc+ type spirals within >= 0.3h(75)(-1) Mpc of the group centers (99.953% confidence). We conclude that the group and subgroup environments must be dominant for the formation of S0 galaxies, and that minor mergers, galaxy harassment, and tidal interactions are the most likely responsible mechanisms. This has implications not only for the inferred preprocessing of cluster galaxies, but also for the global morphological and star formation budget of galaxies: as hierarchical clustering progresses, more galaxies will be subject to these transformations as they enter the group environment.

We report the discovery of a small galaxy system in the vicinity of the Ne VIII absorber at z = 0.20701 toward HE0226 - 4110. The galaxy system consists of two 0.25 L(*) disk galaxies and a 0.05 L(*) galaxy all within Delta v < 300 km s(-1) and rho <= 200 h(-1) physical kpc of the absorber. We consider various scenarios for the origin of the Ne VIII absorption, including photo-ionized gas from an active galactic nucleus, a starburst-driven wind, a hot intragroup medium, hot gas in a galaxy halo, and a conductive front produced by cool clouds moving at high speed through a hot medium. We argue that the conductive front scenario is most likely responsible for producing the Ne VIII feature, because it is consistent with the observed galactic environment around the absorber and because it naturally explains the multi-phase nature of the gas and the kinematic signatures of the absorption profiles. Although our preferred scenario suggests that Ne VIII may not be directly probing the warm-hot intergalactic medium, it does imply the existence of an extended hot confining medium around a disk galaxy that may contain a significant reservoir of baryons in the form of hot gas.

We report the discovery of a small galaxy system in the vicinity of the Ne VIII absorber at z = 0.20701 toward HE0226 - 4110. The galaxy system consists of two 0.25 L(*) disk galaxies and a 0.05 L(*) galaxy all within Delta v < 300 km s(-1) and rho <= 200 h(-1) physical kpc of the absorber. We consider various scenarios for the origin of the Ne VIII absorption, including photo-ionized gas from an active galactic nucleus, a starburst-driven wind, a hot intragroup medium, hot gas in a galaxy halo, and a conductive front produced by cool clouds moving at high speed through a hot medium. We argue that the conductive front scenario is most likely responsible for producing the Ne VIII feature, because it is consistent with the observed galactic environment around the absorber and because it naturally explains the multi-phase nature of the gas and the kinematic signatures of the absorption profiles. Although our preferred scenario suggests that Ne VIII may not be directly probing the warm-hot intergalactic medium, it does imply the existence of an extended hot confining medium around a disk galaxy that may contain a significant reservoir of baryons in the form of hot gas.

We report the discovery of a small galaxy system in the vicinity of the Ne VIII absorber at z = 0.20701 toward HE0226 - 4110. The galaxy system consists of two 0.25 L(*) disk galaxies and a 0.05 L(*) galaxy all within Delta v < 300 km s(-1) and rho <= 200 h(-1) physical kpc of the absorber. We consider various scenarios for the origin of the Ne VIII absorption, including photo-ionized gas from an active galactic nucleus, a starburst-driven wind, a hot intragroup medium, hot gas in a galaxy halo, and a conductive front produced by cool clouds moving at high speed through a hot medium. We argue that the conductive front scenario is most likely responsible for producing the Ne VIII feature, because it is consistent with the observed galactic environment around the absorber and because it naturally explains the multi-phase nature of the gas and the kinematic signatures of the absorption profiles. Although our preferred scenario suggests that Ne VIII may not be directly probing the warm-hot intergalactic medium, it does imply the existence of an extended hot confining medium around a disk galaxy that may contain a significant reservoir of baryons in the form of hot gas.

We report the discovery of a small galaxy system in the vicinity of the Ne VIII absorber at z = 0.20701 toward HE0226 - 4110. The galaxy system consists of two 0.25 L(*) disk galaxies and a 0.05 L(*) galaxy all within Delta v < 300 km s(-1) and rho <= 200 h(-1) physical kpc of the absorber. We consider various scenarios for the origin of the Ne VIII absorption, including photo-ionized gas from an active galactic nucleus, a starburst-driven wind, a hot intragroup medium, hot gas in a galaxy halo, and a conductive front produced by cool clouds moving at high speed through a hot medium. We argue that the conductive front scenario is most likely responsible for producing the Ne VIII feature, because it is consistent with the observed galactic environment around the absorber and because it naturally explains the multi-phase nature of the gas and the kinematic signatures of the absorption profiles. Although our preferred scenario suggests that Ne VIII may not be directly probing the warm-hot intergalactic medium, it does imply the existence of an extended hot confining medium around a disk galaxy that may contain a significant reservoir of baryons in the form of hot gas.

We present an imaging and spectroscopic survey of galaxies in fields around QSOs HE 0226-4110, PKS 0405-123, and PG 1216+069. The fields are selected to have ultraviolet echelle spectra available, which uncover 195 Ly alpha absorbers and 13 O VI absorbers along the three sightlines. We obtain robust redshifts for 1104 galaxies of rest-frame absolute magnitude M-R - 5 log h less than or similar to - 16 and at projected physical distances. rho less than or similar to 4 h(-1) Mpc from the QSOs. Hubble Space Telescope (HST)/WFPC2 images of the fields around PKS 0405-123 and PG 1216+069 are available for studying the optical morphologies of absorbing galaxies. Combining the absorber and galaxy data, we perform a cross-correlation study to understand the physical origin of Lya and O VI absorbers and to constrain the properties of extended gas around galaxies. The results of our study are: (1) both strong Ly alpha absorbers of log N(H I) >= 14 and O VI absorbers exhibit a comparable clustering amplitude as emission-line-dominated galaxies and a factor of approximate to 6 weaker amplitude than absorption-line-dominated galaxies on comoving projected distance scales of r(p) < 3 h(-1) Mpc; (2) weak Ly alpha absorbers of log N(H I) < 13.5 appear to cluster very weakly around galaxies; (3) none of the absorption-line-dominated galaxies at r(p) <= 250 h(-1) kpc has a corresponding O VI absorber to a sensitive upper limit of W(1031) less than or similar to 0.03 angstrom, while the covering fraction of O VI absorbing gas around emission-line-dominated galaxies is found to be kappa approximate to 64%; and (4) high-resolution images of five O VI absorbing galaxies show that these galaxies exhibit disk-like morphologies with mildly disturbed features on the edge. Together, the data indicate that O VI absorbers arise preferentially in gas-rich galaxies. In addition, tidal debris in groups/galaxy pairs may be principally responsible for the observed O VI absorbers, particularly those of W(1031) > 70 m angstrom.

We present an imaging and spectroscopic survey of galaxies in fields around QSOs HE 0226-4110, PKS 0405-123, and PG 1216+069. The fields are selected to have ultraviolet echelle spectra available, which uncover 195 Ly alpha absorbers and 13 O VI absorbers along the three sightlines. We obtain robust redshifts for 1104 galaxies of rest-frame absolute magnitude M-R - 5 log h less than or similar to - 16 and at projected physical distances. rho less than or similar to 4 h(-1) Mpc from the QSOs. Hubble Space Telescope (HST)/WFPC2 images of the fields around PKS 0405-123 and PG 1216+069 are available for studying the optical morphologies of absorbing galaxies. Combining the absorber and galaxy data, we perform a cross-correlation study to understand the physical origin of Lya and O VI absorbers and to constrain the properties of extended gas around galaxies. The results of our study are: (1) both strong Ly alpha absorbers of log N(H I) >= 14 and O VI absorbers exhibit a comparable clustering amplitude as emission-line-dominated galaxies and a factor of approximate to 6 weaker amplitude than absorption-line-dominated galaxies on comoving projected distance scales of r(p) < 3 h(-1) Mpc; (2) weak Ly alpha absorbers of log N(H I) < 13.5 appear to cluster very weakly around galaxies; (3) none of the absorption-line-dominated galaxies at r(p) <= 250 h(-1) kpc has a corresponding O VI absorber to a sensitive upper limit of W(1031) less than or similar to 0.03 angstrom, while the covering fraction of O VI absorbing gas around emission-line-dominated galaxies is found to be kappa approximate to 64%; and (4) high-resolution images of five O VI absorbing galaxies show that these galaxies exhibit disk-like morphologies with mildly disturbed features on the edge. Together, the data indicate that O VI absorbers arise preferentially in gas-rich galaxies. In addition, tidal debris in groups/galaxy pairs may be principally responsible for the observed O VI absorbers, particularly those of W(1031) > 70 m angstrom.

We present an imaging and spectroscopic survey of galaxies in fields around QSOs HE 0226-4110, PKS 0405-123, and PG 1216+069. The fields are selected to have ultraviolet echelle spectra available, which uncover 195 Ly alpha absorbers and 13 O VI absorbers along the three sightlines. We obtain robust redshifts for 1104 galaxies of rest-frame absolute magnitude M-R - 5 log h less than or similar to - 16 and at projected physical distances. rho less than or similar to 4 h(-1) Mpc from the QSOs. Hubble Space Telescope (HST)/WFPC2 images of the fields around PKS 0405-123 and PG 1216+069 are available for studying the optical morphologies of absorbing galaxies. Combining the absorber and galaxy data, we perform a cross-correlation study to understand the physical origin of Lya and O VI absorbers and to constrain the properties of extended gas around galaxies. The results of our study are: (1) both strong Ly alpha absorbers of log N(H I) >= 14 and O VI absorbers exhibit a comparable clustering amplitude as emission-line-dominated galaxies and a factor of approximate to 6 weaker amplitude than absorption-line-dominated galaxies on comoving projected distance scales of r(p) < 3 h(-1) Mpc; (2) weak Ly alpha absorbers of log N(H I) < 13.5 appear to cluster very weakly around galaxies; (3) none of the absorption-line-dominated galaxies at r(p) <= 250 h(-1) kpc has a corresponding O VI absorber to a sensitive upper limit of W(1031) less than or similar to 0.03 angstrom, while the covering fraction of O VI absorbing gas around emission-line-dominated galaxies is found to be kappa approximate to 64%; and (4) high-resolution images of five O VI absorbing galaxies show that these galaxies exhibit disk-like morphologies with mildly disturbed features on the edge. Together, the data indicate that O VI absorbers arise preferentially in gas-rich galaxies. In addition, tidal debris in groups/galaxy pairs may be principally responsible for the observed O VI absorbers, particularly those of W(1031) > 70 m angstrom.