The catalog gives the redshifts for ~6000 galaxies of the WINGS survey. The given membership has been derived using as cluster velocity dispersion the new determination that takes into account literature as well as this dataset.(http://adsabs.harvard.edu/abs/2009A%26A...495..707C)
We present the results from a comprehensive spectroscopic survey of the WINGS (WIde-field Nearby Galaxy-cluster Survey) clusters, a program called WINGS-SPE. The WINGS-SPE sample consists of 48 clusters, 22 of which are in the southern sky and 26 in the north. The main goals of this spectroscopic survey are: (1) to study the dynamics and kinematics of the WINGS clusters and their constituent galaxies, (2) to explore the link between the spectral properties and the morphological evolution in different density environments and across a wide range of cluster X-ray luminosities and optical properties. We present redshift measurements for 6137 galaxies. The WINGS-SPE has a 30% overlap with previously published data sets, allowing us both to perform a complete comparison with the literature and to extend the catalogs. For each galaxy identifier, equatorial coordinates, redshift, errors, correlation factor and membership are given.
The WIde-field Nearby Galaxy clusters Survey (WINGS) is a project whose primary goal is to study the galaxy populations in clusters in the local universe, and of the influence of environment on their stellar populations. This survey has provided the astronomical community with a high quality set of photometric and spectroscopic data for 77 and 48 nearby galaxy clusters, respectively. We present the catalog containing the properties of galaxies observed by the wings spectroscopic survey, which were derived using stellar populations synthesis modelling approach. We also check the consistency of our results with other data in the literature. Using a spectrophotometric model that reproduces the main features of observed spectra by summing the theoretical spectra of simple stellar populations of different ages, we derive the stellar masses, star formation histories, average age and dust attenuation of galaxies in our sample. ~5300 spectra were analyzed with spectrophotometric techniques, and this allowed to derive the star formation history, stellar masses and ages, and extinction for the wings spectroscopic sample that we present in this paper. The comparison with the total mass values of the same galaxies derived by other authors based on sdss data, confirms the reliability of the adopted methods and data.
The catalog gives the star formation history of WINGS galaxies, i.e. their metallicity (as the best fit metallicity obtained by running our code with 4 different values of global metallocity), the dust extinction (both total and from the youngest component), the star formation rate in four macro bins of age (i.e. 0-2e7; 2e7-6e8; 6e8-5.6e9; 5.6e9-17.8e9), three values of stellar mass (i.e. the mass of stars turned into stars globally, the mass in living stars + remnants and the mass in shining stars) both within the fiber and total. The total mass has been extrapolated from the data by rescaling the V flux to the one that we have from the photometry, i.e. assuming no color gradient from the aperture to the toal photometry. A color correction term has been then calculated using the color at 5 kpc and the calibration by Bell & deJong and is given as weel in the catalog. Finally we list the luminosity weighted age and the mass weighted age of our galaxies. (http://adsabs.harvard.edu/abs/2011A%26A...526A..45F)
This catalog contains the surface brightness measurements of ~42250 galaxies detected in the V images of the WINGS cluster survey. For each galaxy V magnitude, mean surface brightness, effective radius, Sersic index and axial ratio are given, together with their errors. These global parameters were obtained by simultaneously fitting the major and minor axis light growth curves of galaxies with a 2D flattened Sersic-law, convolved by the appropriate, space-varying PSF, which was previously evaluated by the tool itself. (http://adsabs.harvard.edu/abs/2006A%26A...446..373P)
The aim of this paper is to introduce the WIRCam Ultra Deep Survey (WUDS), a near-IR photometric survey carried out at the CFH Telescope in the field of the CFHTLS-D3 field (Groth Strip). WUDS includes four near-IR bands (Y, J, H and Ks) over a field of view of ~400arcmin^2^. The typical depth of WUDS data reaches between ~26.8 in Y and J, and ~26 in H and Ks (AB, 3{sigma} in 1.3" aperture), whereas the corresponding depth of the CFHTLS-D3 images in this region ranges between 28.6 and 29 in ugr, 28.2 in i and 27.1 in z (same S/N and aperture). The area and depth of this survey were specifically tailored to set strong constraints on the cosmic star formation rate and the luminosity function brighter or around L* in the z~6-10 redshift domain, although these data are also useful for a variety of extragalactic projects. This first paper is intended to present the properties of the public WUDS survey in details: catalog building, completeness and depth, number counts, photometric redshifts, and global properties of the galaxy population. We have also concentrated on the selection and characterization of galaxy samples at z~[4.5-7] in this field. For these purposes, we include an adjacent shallower area of ~1260arcmin^2^ in this region, extracted from the WIRCam Deep Survey (WIRDS), and observed in J, H and Ks bands. UV luminosity functions were derived at z~5 and z~6 taking advantage from the fact that WUDS covers a particularly interesting regime at intermediate luminosities, which allows a combined determination of M* and {PHI}* with increased accuracy. Our results on the luminosity function are consistent with a small evolution of both M* and {PHI}* between z=5 and z=6, irrespective of the method used to derive them, either photometric redshifts applied to blindly-selected dropout samples or the classical Lyman Break Galaxy color-preselected samples. Our results lend support to higher {PHI}* determinations at z=6 than usually reported. The selection and combined analysis of different galaxy samples at z>=7 will be presented in a forthcoming paper, as well as the evolution of the UV luminosity function between z~4.5 and 9. WUDS is intended to provide a robust database in the near-IR for the selection of targets for detailed spectroscopic studies, in particular for the EMIR/GTC GOYA Survey.
Spectra from the Univsity of Wisconsin Pine Bluff Observatory
in the 3,200 - 7,750 Å range, resolution ~ 80, V_max ~ 15, ~ 2800 observations
of ~ 400 targets, 1989-1998. Note spectropolarimetry data is also included.
Observations complement those obtained from the ASTRO WUPPE project.
The catalog contains all-sky survey of the soft X-ray diffuse background and the count-rate data from which the maps were made for the ten flights included in the survey. It contains 40 files in the machine-readable version and includes documentation and utility subroutines. The data files contain different band maps (B, C, M, M1, M2, I, J, 2-6 keV) in a 0 degree-centered Aitoff projection, in a 180-degree-centered Aitoff projection, in a north polar projection, and in a south polar projection. Lookup tables in the form of FITS images are provided for conversion between pixel coordinates and Galactic coordinates for the various projections. The bands are: B = 130-188eV C = 160-284eV M1 = 440-930eV M2 = 600-1100eV I = 770-1500eV J = 1100-2200eV 2-6keV = 1800-6300eV
The Wisconsin Ultraviolet Photo-Polarimeter Experiment WUPPE was one of three ultraviolet telescopes on the ASTRO-1 mission flown on the space shuttle Columbia during 2-10 December, 1990. 98 observations of 75 targets were obtained. The same three instruments were later flown on the space shuttle Endeavour from 3-17 March, 1995, as part of the ASTRO-2 mission. During the longer ASTRO-2 mission, 369 observations of 254 targets were obtained.
![To the extent possible under law, the publisher has waived all copyright and related or neighboring rights to GAVO's ADQL course. For details, see the `Creative Commons CC0 1.0 Public Domain dedication <http://creativecommons.org/publicdomain/zero/1.0/>`_. Of course, you should still give proper credit when using this data as required by good scientific practice. .. image:: /static/img/cc0.png :alt: [CC0]](/registry-search/?f%5Brights_facet%5D%5B%5D=To+the+extent+possible+under+law%2C+the+publisher+has+waived+all+copyright+and+related+or+neighboring+rights+to+GAVO%27s+ADQL+course.++For+details%2C+see+the+%60Creative+Commons+CC0+1.0+Public+Domain+dedication+%3Chttp%3A%2F%2Fcreativecommons.org%2Fpublicdomain%2Fzero%2F1.0%2F%3E%60_.++Of+course%2C+you+should+still+give+proper+credit+when+using+this+data+as+required+by+good+scientific+practice.%0A%0A..+image%3A%3A+%2Fstatic%2Fimg%2Fcc0.png%0A+++%3Aalt%3A+%5BCC0%5D%0A%0A&f%5Btype_facet%5D%5B%5D=%0A++++++++++++){kind=link}