========================================================================== IX/49 XXL Survey: First results (Pierre+, 2016) The following files can be converted to FITS (extension .fit or fit.gz) xxlpoint.dat xxl100gc.dat xxl1000a.dat xxl_vla.dat list.dat xxl_atca.dat xxlaaoz.dat xxl100bc.dat ========================================================================== Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=IX/49 ==========================================================================
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Beginning of ReadMe : IX/49 XXL Survey: First results (Pierre+, 2016) ================================================================================ The XXL Survey: First results. Pierre M., Pacaud F., Adami C., Alis S., Altieri B., Baran B., Benoist C., Birkinshaw M., Bongiorno A., Bremer M.N., Brusa M., Butler A., Ciliegi P., Chiappetti L., Clerc N., Corasaniti P.S., Coupon J., De Breuck C., Democles J., Desai S., Delhaize J., Devriendt J., Dubois Y., Eckert D., Elyiv A., Ettori S., Evrard A., Faccioli L., Farahi A., Ferrari C., Finet F., Fotopoulou S., Fourmanoit N., Gandhi P., Gastaldello F., Gastaud R., Georgantopoulos I., P.Giles, Guennou L., Guglielmo V., Horellou C., Husband K., Huynh M., Iovino A., Kilbinger M., Koulouridis E., Lavoie S., Le Brun A.M.C., LeFevre J.P., Lidman C., Lieu M., Lin C.A., Mantz A., Maughan B.J., Maurogordato S., McCarthy I.G., McGee S., Melin J.B., Melnyk O., Menanteau F., Novak M., Paltani S., Plionis M., Poggianti B.M., Pomarede D., Pompei E., Ponman T.J., Ramos-Ceja M.E., Ranalli P., Rapetti D., Raychaudury S., Reiprich T.H., Rottgering H., Rozo E., Ryko E., Sadibekova T., Santos J., Sauvageot J.L., Schimd C., Sereno M., Smith G.P., Smolcic V., Snowden S., Spergel D., Stanford S., Surdej J., Valageas P., Valotti A., Valtchanov I., Vignali C., Willis J., Ziparo F. <Astron. Astrophys. 592, A1-A12 (2016)> =2016yCat.9049....0P =2016A&A...592A...1P +2016A&A...592A...2P +2016A&A...592A...3G +2016A&A...592A...4L +2016A&A...592A...5F +2016A&A...592A...6P +2016A&A...592A...7A +2016A&A...592A...8B +2016A&A...592A...9Z +2016A&A...592A..10S +2016A&A...592A..11K +2016A&A...592A..12E +2016PASA...33....1L +2016MNRAS.462.4141L ================================================================================ ADC_Keywords: Surveys ; X-ray sources ; Space observations ; Observatory log ; Clusters, galaxy ; Radio sources ; QSOs ; Redshifts Keywords: surveys - X-rays: general - X-rays: galaxies: clusters - X-rays: diffuse background - large-scale structure of Universe - cosmological parameters - galaxies: active - photometry - galaxies: groups: general - radio continuum: galaxies - radio continuum: general - radiation mechanisms: general - galaxies: quasars: general Abstract: The quest for the cosmological parameters that describe our universe continues to motivate the scientific community to undertake very large survey initiatives across the electromagnetic spectrum. Over the past two decades, the Chandra and XMM-Newton observatories have sup- ported numerous studies of X-ray-selected clusters of galaxies, active galactic nuclei (AGNs), and the X-ray background. The present paper is the first in a series reporting results of the XXL-XMM survey; it comes at a time when the Planck mission results are being finalised. We present the XXL Survey, the largest XMM programme totaling some 6.9Ms to date and involving an international consortium of roughly 100 members. The XXL Survey covers two extragalactic areas of 25deg^2^ each at a point-source sensitivity of 5x10^-15^erg/s/cm^2^ in the [0.5-2]keV band (completeness limit). The survey's main goals are to provide constraints on the dark energy equation of state from the space-time distribution of clusters of galaxies and to serve as a pathfinder for future, wide-area X-ray missions. We review science objectives, including cluster studies, AGN evolution, and large-scale structure, that are being conducted with the support of approximately 30 follow-up programmes. List of XXL papers: I. Scientific motivations - XMM-Newton observing plan - Follow-up observations and simulation programme. II. The bright cluster sample: catalogue and luminosity function. III. Luminosity-temperature relation of the bright cluster sample. IV. Mass-temperature relation of the bright cluster sample. VI. The 1000 brightest X-ray point sources. VII. A supercluster of galaxies at z = 0.43. VIII. MUSE characterisation of intracluster light in a z 0.53 cluster of galaxies. IX. Optical overdensity and radio continuum analysis of a supercluster at z=0.43. X. K-band luminosity - weak-lensing mass relation for groups and clusters of galaxies. XI. ATCA 2.1 GHz continuum observations. XII. Optical spectroscopy of X-ray-selected clusters and the frequency of AGN in superclusters. XIII. Baryon content of the bright cluster sample. XIV. AAOmega redshifts for the southern XXL field. Description: Paper I. Scientific motivations - XMM-Newton observing plan. Follow-up observations and simulation programme. The table xxlpoint.dat is a list of all XMM survey-type observations (<=AO-10) in the XXL fields, providing the match between the internal naming and the ESA XXM log,the coordinates and useful exposure times of the XMM pointings, their quality and ancillary information. Paper II. The bright cluster sample: catalogue and luminosity function. Paper III. Luminosity-temperature relation of the bright cluster sample. Paper IV. Mass-temperature relation of the bright cluster sample. This article presents the XXL bright cluster sample, a subsample of 100 galaxy clusters selected from the full XXL catalogue by setting a lower limit of 3*10^-14^erg/cm^2^/s on the source flux within a 1' aperture. The selection function was estimated using a mixture of Monte Carlo simulations and analytical recipes that closely reproduce the source selection process. An extensive spectroscopic follow-up provided redshifts for 97 of the 100 clusters. We derived accurate X-ray parameters for all the sources. Scaling relations were self-consistently derived from the same sample in other publications of the series. On this basis, we study the number density, luminosity function, and spatial distribution of the sample. The bright cluster sample consists of systems with masses between M_500_=7*10^+14^ and 3*10^+14^M_sun_, mostly located between z=0.1 and 0.5. The observed sky density of clusters is slightly below the predictions from the WMAP9 model, and significantly below the prediction from the Planck 2015 cosmology. In general, within the current uncertainties of the cluster mass calibration, models with higher values of sigma_8_ and/or Omega_M_ appear more difficult to accommodate. We provide tight constraints on the cluster differential luminosity function and find no hint of evolution out to z 1. We also find strong evidence for the presence of large-scale structures in the XXL bright cluster sample and identify five new superclusters. We provide the XXL-100-GC catalogue (xxl100gc.dat), the master catalogue of the 100 brightest galaxy clusters from the XXL Survey. This catalogue summarizes all the information published on this sample by the XXL collaboration, which were initially distributed over several articles. It contains the sources positions, redshifts, fluxes and mass estimates published in Appendix D of paper II, combined with luminosities and temperatures from Table 1 of paper III, as well as gas masses from Table A.1 of paper XIII. Paper VI. The 1000 brightest X-ray point sources. We provide the XXL_1000_AGN catalogue (xxl1000a.dat), the first catalogue release of the XXL point source catalog, detected in the 2-10keV energy band. The catalogue contains the 1000 brightest sources, at the flux limit of F[2-10 keV]=4.8 10^-14^erg/s/cm^2^. We provide derived X-ray spectral parameters, and counterpart properties including four optical magnitudes, photometric and spectroscopic redshift estimates. We also provide the best photometric redshift class based on machine learning classification and the probability for a source to be a star or a photometric redshift outlier. Paper IX. Optical overdensity and radio continuum analysis of a supercluster at z=0.43. The table xxl_vla.dat contains the full source catalogue of all 155 radio sources detected with S/N>=6 in the Very Large Array 3GHz continuum survey of the XXL-North field. The observations covered the 0.7x0.7 square degrees subarea of the 25 square degree XXL-North field. The radio data has an angular resolution of 3.2x1.9 square arcsec and a mean rms of 20uJy per beam. There are 25 resolved sources, of which 8 are multicomponent objects. Paper XI. ATCA 2.1 GHz continuum observations. The table xxl_atca.dat contains the full source catalogue of all 1389 radio sources detected with S/N>=5 in the Australia Telescope Compact Array 2.1GHz continuum pilot survey of the XXL-South field. The observations covered the inner 6.5 square degrees of the 25 square degree XXL-South field. The radio data has an angular resolution of 4.7x4.2 square arcsec and a median rms of 50uJy per beam. There are 305 resolved sources, of which 77 are multicomponent objects. The table contains various observed parameters of the radio sources, such as position, peak flux density and signal-to-noise ratio. Paper XIV. AAOmega redshifts for the southern XXL field. We present a catalogue (xxlaaoz.dat) containing the redshifts of 3660 X-ray selected targets in the XXL southern field. The redshifts were obtained with the AAOmega spectrograph and 2dF fibre positioner on the Anglo-Australian Telescope. The catalogue contains 1515 broad line AGN, 528 stars, and redshifts for 41 out of the 49 brightest X-ray selected clusters in the XXL southern field. Paper XV. Evidence for dry merger driven BCG growth in XXL-100-GC X-ray clusters Given the availability of good quality multiband photometry together with photometric and spectroscopic redshifts to z<1, a simple set of criteria can be used to identify BCGs. For the present work, we define a BCG as: - the brightest galaxy in z-band, - within 0.5xr500 of the cluster X-ray centroid, - with a redshift that is consistent with that of the cluster as determined from all the redshifts available around the X-ray centroid. Our final sample (xxl100bc.dat) consists of 85 clusters, 45 of which are in the Northern field and 40 in the Southern field.