- ID:
- ivo://CDS.VizieR/J/MNRAS/401/1429
- Title:
- WiggleZ dark energy survey (DR1)
- Short Name:
- J/MNRAS/401/1429
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The WiggleZ Dark Energy Survey is a survey of 240000 emission-line galaxies in the distant Universe, measured with the AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope (AAT). The primary aim of the survey is to precisely measure the scale of baryon acoustic oscillations (BAO) imprinted on the spatial distribution of these galaxies at look-back times of 4-8Gyr. The target galaxies are selected using ultraviolet (UV) photometry from the Galaxy Evolution Explorer satellite, with a flux limit of NUV<22.8mag. We also require that the targets are detected at optical wavelengths, specifically in the range 20.0<r<22.5mag. We use the Lyman break method applied to the UV colours, with additional optical colour limits, to select high-redshift galaxies. The galaxies generally have strong emission lines, permitting reliable redshift measurements in relatively short exposure times on the AAT. The median redshift of the galaxies is z_med_=0.6. The redshift range containing 90 per cent of the galaxies is 0.2<z<1.0. The survey will sample a volume of ~1Gpc^3^ over a projected area on the sky of 1000deg^2^, with an average target density of 350deg^-2^.
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Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/474/4151
- Title:
- WiggleZ Dark Energy Survey final DR
- Short Name:
- J/MNRAS/474/4151
- Date:
- 02 Mar 2022 00:09:00
- Publisher:
- CDS
- Description:
- The WiggleZ Dark Energy Survey measured the redshifts of over 200000 ultraviolet (UV)-selected (N_UV_<22.8mag) galaxies on the Anglo-Australian Telescope. The survey detected the baryon acoustic oscillation signal in the large-scale distribution of galaxies over the redshift range 0.2<z<1.0, confirming the acceleration of the expansion of the Universe and measuring the rate of structure growth within it. Here, we present the final data release of the survey: a catalogue of 225415 galaxies and individual files of the galaxy spectra. We analyse the emission-line properties of these UV-luminous Lyman-break galaxies by stacking the spectra in bins of luminosity, redshift, and stellar mass. The most luminous (-25mag<M_FUV_< -22mag) galaxies have very broad H{beta} emission from active nuclei, as well as a broad second component to the [OIII] (495.9nm, 500.7nm) doublet lines that is blueshifted by 100km/s, indicating the presence of gas outflows in these galaxies. The composite spectra allow us to detect and measure the temperature-sensitive [OIII] (436.3nm) line and obtain metallicities using the direct method. The metallicities of intermediate stellar mass (8.8<log(M*/M_{sun}_)<10) WiggleZ galaxies are consistent with normal emission-line galaxies at the same masses. In contrast, the metallicities of high stellar mass (10<log(M*/M_{sun}_)<12) WiggleZ galaxies are significantly lower than for normal emission-line galaxies at the same masses. This is not an effect of evolution as the metallicities do not vary with redshift; it is most likely a property specific to the extremely UV-luminous WiggleZ galaxies.
- ID:
- ivo://CDS.VizieR/J/A+A/633/A104
- Title:
- WINGS cluster galaxies structural parameters
- Short Name:
- J/A+A/633/A104
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a multi-wavelength analysis of the galaxies in nine clusters selected from the WINGS dataset, examining how galaxy structure varies as a function of wavelength and environment using the state of the art software galapagos-2. We simultaneously fit single-Sersic functions on three optical (u, B and V) and two near-infrared (J and K) bands thus creating a wavelength-dependent model of each galaxy. We measure the magnitudes, effective radius (Re), the Sersic index (n), axis ratio, and position angle in each band. The sample contains 790 cluster members (located close to the cluster centre <0.64xR200) and 254 non-member galaxies that we further separate based on their morphology into ellipticals, lenticulars, and spirals. We find that the Sersic index of all galaxies inside clusters remains nearly constant with wavelength while Re decreases as wavelength increases for all morphological types. We do not observe a significant variation on n and Re as a function of projected local density and distance from the clusters centre. Comparing the n and Re of bright cluster galaxies with a subsample of non-member galaxies we find that bright cluster galaxies are more concentrated (display high n values) and are more compact (low Re). Moreover, the light profile (N) and size (R) of bright cluster galaxies does not change as a function of wavelength in the same manner as non-member galaxies.
- ID:
- ivo://CDS.VizieR/J/A+A/637/A54
- Title:
- WINGS cluster survey second u-band extension
- Short Name:
- J/A+A/637/A54
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This is the second u-band extension of the WIde-field Nearby Galaxy-cluster Survey (WINGS), obtained by imaging 39 clusters with the ESO-VLT survey telescope. It follows the first one, realized with several telescopes of the northern hemisphere in the U Cousin-Bessel filter band (Omizzolo et al., 2014A&A...561A.111O, Cat. J/A+A/561/A111), that covered 17 clusters. The u-band data, in combination with those already achieved by the WINGS survey, will permit a detailed multi-wavelength investigation of the properties of the member galaxies from the cluster center out to the periphery. We have derived with SEXT the main properties of the galaxies in the observed fields and measured the u-V colors on circular apertures of increasing radius. The photometric accuracy of the magnitudes has been calibrated with the standard stars and tested by means of comparisons with the u-band data of the Sloan Digital Sky Survey (SDSS). We present the catalogs of the photometric analysis performed by SEXT. Then we provide a brief analysis of the u-V vs V color-magnitude diagram of our clusters, the plots of the color as a function of the cluster-centric distance (for cluster members only) and the correlation of the current star formation rate (SFR) vs the absolute V and u magnitudes for the galaxies in the observed fields.
- ID:
- ivo://CDS.VizieR/J/A+A/497/667
- Title:
- WINGS: Deep optical phot. of 77 nearby clusters
- Short Name:
- J/A+A/497/667
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This is the second paper of a series devoted to the WIde Field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long term project which is gathering wide-field, multi-band imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04<z<0.07) located far from the galactic plane (|b|>200deg). The main goal of this project is to establish a local reference for evolutionary studies of galaxies and galaxy clusters. This paper presents the optical (B,V) photometric catalogs of the WINGS sample and describes the procedures followed to construct them. We have paid special care to correctly treat the large extended galaxies (which includes the brightest cluster galaxies) and the reduction of the influence of the bright halos of very bright stars. We have constructed photometric catalogs based on wide-field images in B and V bands using SExtractor. Photometry has been performed on images in which large galaxies and halos of bright stars were removed after modeling them with elliptical isophotes. We publish deep optical photometric catalogs (90% complete at V21.7, which translates to ~ MV* + 6 at mean redshift), giving positions, geometrical parameters, and several total and aperture magnitudes for all the objects detected. For each field we have produced three catalogs containing galaxies, stars and objects of "unknown" classification (~16%). From simulations we found that the uncertainty of our photometry is quite dependent of the light profile of the objects with stars having the most robust photometry and de Vaucouleurs profiles showing higher uncertainties and also an additional bias of ~-0.2m. The star/galaxy classification of the bright objects (V<20) was checked visually making negligible the fraction of misclassified objects. For fainter objects, we found that simulations do not provide reliable estimates of the possible misclassification and therefore we have compared our data with that from deep counts of galaxies and star counts from models of our Galaxy. Both sets turned out to be consistent with our data within ~5% (in the ratio galaxies/total) up to V~24. Finally, we remark that the application of our special procedure to remove large halos improves the photometry of the large galaxies in our sample with respect to the use of blind automatic procedures and increases (~16%) the detection rate of objects projected onto them.
- ID:
- ivo://CDS.VizieR/J/A+A/572/A87
- Title:
- WINGS galaxies surface photometry with GASPHOT
- Short Name:
- J/A+A/572/A87
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the B, V, and K band surface photometry catalogs obtained by running the automatic software GASPHOT on galaxies from the WINGS cluster survey with isophotal areas larger than 200 pixels. The luminosity growth curves of stars and galaxies in a given catalog relative to a given cluster image were obtained simultaneously by slicing the image with a fixed surface brightness step in several SExtractor runs. Then, using a single Sersic law convolved with a space-varying point spread function (PSF), GASPHOT performed a simultaneous {chi}^2^ best-fit of the major- and minor-axis luminosity growth curves of galaxies. We outline the GASPHOT performances and compare our surface photometry with that obtained by SExtractor, GALFIT, and GIM2D. This analysis is aimed at providing statistical information about the accuracy that is generally achieved by the softwares for automatic surface photometry of galaxies.
- ID:
- ivo://CDS.VizieR/J/A+A/501/851
- Title:
- WINGS JK photometry of 28 galaxy clusters
- Short Name:
- J/A+A/501/851
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This is the third paper in a series devoted to the WIde-field Nearby Galaxy-cluster Survey (WINGS). WINGS is a long-term project aimed at gathering wide-field, multiband imaging and spectroscopy of galaxies in a complete sample of 77 X-ray selected, nearby clusters (0.04<z<0.07) located far from the galactic plane (|b|>=20{deg}). The main goal of this project is to establish a local reference sample for evolutionary studies of galaxies and galaxy clusters. This paper presents the near-infrared (J,K) photometric catalogs of 28 clusters of the WINGS sample and describes the procedures followed to construct them.
- ID:
- ivo://CDS.VizieR/J/A+A/581/A11
- Title:
- 72 WINGS nearby clusters luminosity functions
- Short Name:
- J/A+A/581/A11
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using V band photometry of the WINGS survey, we derive galaxy luminosity functions (LF) in nearby clusters. This sample is complete down to M_V_=-15.15, and it is homogeneous, thus facilitating the study of an unbiased sample of clusters with different characteristics. We constructed the photometric LF for 72 out of the original 76 WINGS clusters, excluding only those without a velocity dispersion estimate. For each cluster we obtained the LF for galaxies in a region of radius=0.5xr_200_, and fitted them with single and double Schechter's functions. We also derive the composite LF for the entire sample, and those pertaining to different morphological classes. Finally, we derive the spectroscopic cumulative LF for 2009 galaxies that are cluster members. The double Schechter fit parameters are correlated neither with the cluster velocity dispersion nor with the X-ray luminosity. Our median values of the Schechter's fit slope are, on average, in agreement with measurements of nearby clusters, but are less steep that those derived from large surveys, such as the SDSS. Early-type galaxies out number late-types at all magnitudes, but both early and late types contribute equally to the faint end of the LF. Finally, the spectroscopic LF is in excellent agreement with the one derived for A2199, A85 and Virgo, and with the photometric LF at the bright magnitudes (where both are available). There is a large spread in the LF of different clusters, however, this spread is not caused by correlation of the LF shape with cluster characteristics such as X-ray luminosity or velocity dispersions. The faint end is flatter than previously derived ({alpha}_f_=-1.7), which is at odds with that predicted from numerical simulations.
8169. WINGS-SPE II catalog
- ID:
- ivo://CDS.VizieR/J/A+A/526/A45
- Title:
- WINGS-SPE II catalog
- Short Name:
- J/A+A/526/A45
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 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.
- ID:
- ivo://CDS.VizieR/J/A+A/620/A51
- Title:
- WIRCam Ultra Deep Survey photometric catalogs
- Short Name:
- J/A+A/620/A51
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 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.
