A compilation of H I line fluxes, systemic velocities and linewidths is presented for 840 detected galaxies, mostly in the vicinities of 30 nearby rich clusters out to a redshift of z~0.04, specifically for use in applications of the Tully-Fisher distance method. New 21 cm H I line profiles have been obtained for ~500 galaxies in 27 Abell clusters visible from Arecibo. Upper limits are also presented for 246 galaxies for which H I emission was not detected. In order to provide a homogeneous linewidth determination optimized for Tully-Fisher studies, these new data are supplemented by the reanalysis of previously published spectra obtained both at Arecibo and Green Bank that are available in a digital archive. Corrections for instrumental broadening, smoothing, signal-to-noise and profile shape are applied, and an estimate of the error on the width is given. When corrected for turbulent broadening and viewing angle, the corrected velocity widths presented here will provide the appropriate line width parameter needed to derive distances via the Tully-Fisher relation.
A photometric and redshift catalog of galaxies in the field of the rich galaxy cluster Abell 2390 (z=0.228) is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. Using five separate fields, the imaging and spectroscopic observations cover a strip of approximately 7.3'x43.2', centered on the cluster. Redshifts for 327 galaxies, primarily ranging in magnitude from r=17 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, geometric, and color selection functions for the redshift sample are discussed and presented.
A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 1621.5+2640 (z=0.4275) and MS 0302.7+1658 (z=0.4245), is presented as part of the Canadian Network for Observation Cosmology (CNOC) Cluster Redshift Survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover strips cantered on each cluster of approximately 23.3'x9.0', and 7.9'x9.0', for MS 1621.5+2640 and MS 0302.7+1658, respectively. Redshifts for 371 galaxies, primarily ranging in magnitude from r=20 to 22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.
Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters, MS 1358.4+6245 (z=0.328) and MS 1008.1-1224 (z=0.306), are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a mosaic of three MOS fields in the north-south direction of a total area of approximately 23.3'x9.0' for MS 1358.4+6245 and a single field of 7.9'x9.0' for MS 1008.1-1224. Redshifts for 361 galaxies, primarily ranging in magnitude from r=20 to r=22, and Gunn r and g photometry for 3015 galaxies to r=24mag were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.
Photometric and redshift catalogs of galaxies in the field of two rich galaxy clusters: MS 1224.7+2007 (z=0.327) and MS 1512.4+3647 (z=0.372) are presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations span three contiguous MOS fields in the east-west direction for MS 1512.4+3647, covering a total area of approximately 8.0'x27.3'. A single field of 7.1'x9.0' was obtained for MS 1224.7+2007. Redshifts for 287 galaxies in the MS 1512.4+3647 fields and 75 galaxies in the MS 1224.7+2007 field (primarily ranging in magnitude from r=18-22) were obtained. The spectroscopic information in this paper is supplemented by photometric information for all galaxies in the fields down to Gunn r=21mag. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.
A photometric and redshift catalog of galaxies in the field of two rich galaxy clusters, MS 0015.9+1609 (z=0.5481) and MS 0451.5-0305 (z=0.5386), is presented as part of the Canadian Network for Observation Cosmology (CNOC) cluster redshift survey carried out at the Canada-France-Hawaii Telescope (CFHT) using the MOS imaging multiobject spectrograph. The imaging and spectroscopic observations cover a single field of approximately 7.6'x9.1', centered on each cluster. Redshifts for 247 galaxies, primarily ranging in magnitude from r=20 to r=22, were obtained. The data set is also presented graphically in several forms. The magnitude, color, and geometric selection functions for the redshift sample are presented and discussed.
Large area catalogs of galaxy clusters constructed from ROSAT All Sky Survey provide the base for our knowledge on the population of clusters thanks to the long-term multiwavelength efforts to follow-up observations of these clusters.. Advent of large area photometric surveys superseding in depth previous all-sky data allows us to revisit the construction of X-ray cluster catalogs, extending the study to lower cluster masses and to higher redshifts and to provide the modelling of the selection function. We perform a wavelet detection of X-ray sources and make extensive simulations of the detection of clusters in the RASS data. We assign an optical richness to each of the 24,788 detected X-ray sources in the 10,382 square degrees of SDSS BOSS area, using redMaPPer version 5.2 run on Sloan Digital Sky Survey photometry. We name this survey COnstrain Dark Energy with X-ray (CODEX) clusters. We show that there is no obvious separation of sources on galaxy clusters and AGN, based on distribution of systems on their richness. This is a combination of increasing number of galaxy groups and their selection as identification of an X-ray sources either by chance or due to groups hosting an AGN. To clean the sample, we use a cut on the optical richness at the level corresponding to the 10% completeness of the survey and include it into the modelling of cluster selection function. We present the X-ray catalog extending to a redshift of 0.6. CODEX is the first large area X-ray selected catalog of Northern clusters reaching the fluxes of 10^-13^ergs/s/cm^2^. We provide the modelling of the sample selection and discuss the redshift evolution of the high end of the X-ray luminosity function (XLF). Our results on z<0.3 XLF are in agreement with previous studies, while we provide new constraints on the 0.3<z<0.6 XLF. We find a lack of strong redshift evolution of the XLF, provide exact modeling of the effect of low number statistics and AGN contamination and present the resulting constraints on the flat {LAMBDA}CDM.
The results of a CO line survey in central cluster galaxies with cooling flows are presented. Cold molecular gas is detected with the IRAM 30m telescope, through CO(1-0) and CO(2-1) emission lines in 6-10 among 32 galaxies. The corresponding gas masses are between 3x10^8^ and 4x10^10^M_{sun}. These results are in agreement with recent CO detections by Edge (2001MNRAS.328..762E). A strong correlation between the CO emission and the H{alpha} luminosity is also confirmed. Cold gas exists in the center of cooling flow clusters and these detections may be interpreted as evidence of the long searched for very cold residual of the hot cooling gas.
Galaxies in Hickson Compact Groups (HCGs) are believed to experience morphological transformations from blue, star-forming galaxies to red, early-type galaxies. Galaxies with a high ratio between the luminosities of the warm H_2_ to the 7.7micron PAH emission (so-called Molecular Hydrogen Emission Galaxies, MOHEGs) are predominantly in an intermediate phase, the green valley. Their enhanced H_2_ emission suggests that the molecular gas is affected in the transition. We study the properties of the molecular gas traced by CO in galaxies in HCGs with measured warm H_2_ emission in order to look for evidence of the perturbations affecting the warm H_2_ in the kinematics, morphology and mass of the molecular gas. We observed the CO(1-0) emission of 20 galaxies in HCGs and complemented our sample with 11 CO(1-0) spectra from the literature. Most of the galaxies have measured} warm H_2_ emission, and 14 of them are classified as MOHEGs. We mapped some of these galaxies in order to search for extra-galactic CO emission. We analyzed the molecular gas mass derived from CO(1-0), MH_2_, and its kinematics, and then compared it to the mass of the warm molecular gas, the stellar mass and star formation rate (SFR). Our results are the following. (i) The mass ratio between the CO-derived and the warm H_2_ molecular gas is in the same range as found for field galaxies. (ii) Some of the galaxies, mostly MOHEGs, have very broad CO linewidths of up to 1000km/s in the central pointing. The line shapes are irregular and show various components. (iii) In the mapped objects we found asymmetric distributions of the cold molecular gas. (iv) The star formation efficiency (=SFR/MH_2_) of galaxies in HCGs is very similar to isolated galaxies. No significant difference between MOHEGs and non-MOHEGs or between early-type and spiral galaxies has been found. In a few objects the SFE is significantly lower, indicating the presence of molecular gas that is not actively forming stars. (v) The molecular gas masses, MH_2_, and ratios MH_2_/Lk are lower in MOHEGs (predominantly early-types) than in non-MOHEGs (predominantly spirals). This trend remains when comparing MOHEGs and non-MOHEGs of the same morphological type. We found differences in the molecular gas properties of MOHEGs that support the view that they have suffered (or are presently suffering) perturbations of the molecular gas, as well as a decrease in the molecular gas content and associated SFR. Higher resolution observations of the molecular gas are needed to shed light on the nature of these perturbations and their cause.
In this paper, we present a set of photometric observations in 15 colors of stars in the Landolt SA95 field with the BATC (Beijing-Arizona-Taipei-Connecticut) system. The wavelengths covered by the system range from 300nm to 1000nm. Visual magnitudes of the stars studied in the field are from the 10th to 20th mag. The observational methodology and the data reduction procedures are described. The relationships between the BATC intermediate-band system and the Landolt UBVRI broad band system are obtained. A catalogue of the photometry has been produced which contains the spectral energy distributions (SEDs) of 3613 stars.
