A catalog of rich clusters of galaxies

Abell, G. O.; Corwin, H. G.; Olowin, R. P.

doi:10.1086/191333

Cited by 1,392 publications

(1,488 citation statements)

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“…The Swift/UVOT detection in the UVW2 filter proves that the source is at z ≤ 1.7 (we conservatively considered the red limit of the filter). The optical afterglow position lies 8.5 from the center of the rich ACO S 995 cluster of 22 diameter (Abell et al 1989) for which no redshift was found in the literature 5 . The spectra of nine apparent members of this cluster were obtained by Berger et al (2006a) within a redshift range of 0.0843 < z < 0.0877, concluding that the redshift of ACO S 995 is z = 0.0865.…”

Section: Distance Estimatesmentioning

confidence: 79%

A study of the prompt and afterglow emission of the short GRB 061201

Stratta¹,

D’Avanzo

Piranomonte

et al. 2007

A&A

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Context. Our knowledge of the intrinsic properties of short duration Gamma-Ray Bursts has relied, so far, only upon a few cases for which the estimate of the distance and an extended, multiwavelength monitoring of the afterglow have been obtained. Aims. We carried out multiwavelength observations of the short GRB 061201 aimed at estimating its distance and studying its properties. Methods. We performed a spectral and timing analysis of the prompt and afterglow emission and discuss the results in the context of the standard fireball model. Results. A clear temporal break was observed in the X-ray light curve about 40 min after the burst trigger. We find that the spectral and timing behaviour of the X-ray afterglow is consistent with a jet origin of the observed break, although the optical data can not definitively confirm this and other scenarios are possible. No underlying host galaxy down to R ∼ 26 mag was found after fading of the optical afterglow. Thus, no secure redshift could be measured for this burst. The nearest galaxy is at z = 0.111 and shows evidence of star formation activity. We discuss the association of GRB 061201 with this galaxy and with the ACO S 995 galaxy cluster, from which the source is at an angular distance of 17 and 8.5 , respectively. We also test the association with a possible undetected, positionally consistent galaxy at z ∼ 1. In all these cases, in the jet interpretation, we find a jet opening angle of 1-2 degrees.Key words. gamma rays: bursts IntroductionShort duration Gamma-ray Bursts (GRBs) are historically defined as those GRBs with burst duration less than two seconds and hard spectra (Kouveliotou et al. 1993). As the sample of short GRBs increases, in order to take into account all the spectral and temporal properties of the prompt emission, alternative empirical definitions of short GRBs have been introduced (e.g. Norris & Bonnell 2006;Zhang et al. 2007).The expected progenitor for short GRBs is a merging binary system of compact objects. However, our present knowledge of the intrinsic properties of short bursts mainly relies upon a few cases for which the distance could be derived and an extendedThe results reported in this paper are partially based on observations carried out at ESO telescopes under program 078.D-0809.INAF personnel resident at ASDC. multiwavelength monitoring of the afterglow was carried out.From these it appears that short bursts are less energetic and less collimated than long GRBs (e.g. Fox et al. 2005;Burrows et al. 2006;Soderberg et al. 2006). Intrinsic spectral parameters such as the peak energy E p of the EF(E) spectrum of the burst and the equivalent isotropic energy E iso , do not match the E p − E iso correlation for long GRBs (e.g. Amati 2007).The short bursts for which unambiguous hosts have been found are at redshifts between z = 0.10 and z = 0.55. The optical afterglows of seven short bursts and their likely host galaxies have been recently observed with telescopes such as ESO/VLT, Gemini, Magellan and HST, but no firm estimation of...

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Section: Distance Estimatesmentioning

confidence: 79%

A study of the prompt and afterglow emission of the short GRB 061201

Stratta¹,

D’Avanzo

Piranomonte

et al. 2007

A&A

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“…Its properties are listed in Table 1, while the experimental specifications of surveys that have observed RXJ2248 are quoted in Table 2. It was first catalogued by Abell, Corwin & Olowin (1989), who counted 74 galaxies. Thanks to the ROSAT-ESO Flux Limited X-ray (REFLEX) Galaxy Cluster survey, Böhringer et al (2004) measured a spectroscopic redshift z = 0.3475, which has been adopted in the recent literature and has also been confirmed in Gómez et al (2012), who quoted a mean redshift of z = 0.3461 +0.0010 −0.0011 for 81 members.…”

Section: T H E C L U S T E R R X C J 2 2 4 8 7 −4 4mentioning

confidence: 99%

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Palmese

Lahav

Banerji

et al. 2016

Mon. Not. R. Astron. Soc.

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We derive the stellar mass fraction in the galaxy cluster RXC J2248.7−4431 observed with the Dark Energy Survey (DES) during the Science Verification period. We compare the stellar mass results from DES (five filters) with those from the Hubble Space Telescope Cluster Lensing And Supernova Survey (CLASH; 17 filters). When the cluster spectroscopic redshift is assumed, we show that stellar masses from DES can be estimated within 25 per cent of CLASH values. We compute the stellar mass contribution coming from red and blue galaxies, and study the relation between stellar mass and the underlying dark matter using weak lensing studies with DES and CLASH. An analysis of the radial profiles of the DES total and stellar mass yields a stellar-to-total fraction of f = (6.8 ± 1.7) × 10 −3 within a radius of r 200c 2 Mpc. Our analysis also includes a comparison of photometric redshifts and star/galaxy separation efficiency for both data sets. We conclude that space-based small field imaging can be used to calibrate the galaxy properties in DES for the much wider field of view. The technique developed to derive the stellar mass fraction in galaxy clusters can be applied to the ∼100 000 clusters that will be observed within this survey and yield important information about galaxy evolution.

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“…Data relative to X-ray flux and red-shift are from De Grandi et al (1999). Data relative to optical richness and morphology are from Abell et al (1989) …”

Section: Imagingmentioning

confidence: 99%

Luminosity Function of Cluster Galaxies

Molinari

Moretti

Chincarini

et al. 1999

Looking Deep in the Southern Sky

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Abstract. We initiated a large project aimed to estimate the Luminosity Function of galaxies in clusters and to evaluate its relation to cluster morphology. With this paper we deem necessary to outline the general procedures of the data reduction and details of the data analysis. The cluster sample includes the brightest southern ROSAT all-sky survey clusters with z < 0.1. These have been observed in three colours g, r, i, and mapped up to a few core radii using a mosaic of CCD frames. E/S0 galaxies in the cluster core are singled out both by morphology (for the brightest galaxies), and by colour. The details of the data reduction procedure are illustrated via the analysis of the cluster Abell 496, which has been used as a pilot cluster for the whole program. The related photometric catalogue consists of 2355 objects. The limiting magnitudes (the reference Surface Brightness is given in parenthesis) in the various colours are respectively g(25.5) = 24.14, r(25.5) = 24.46, i(25.0) = 23.75. These correspond to the limiting absolute magnitudes −12.28, −11.96 and −12.67 (H 0 = 50 km/s/Mpc).

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A catalog of rich clusters of galaxies

Cited by 1,392 publications

References 0 publications

A study of the prompt and afterglow emission of the short GRB 061201

A study of the prompt and afterglow emission of the short GRB 061201

Comparing Dark Energy Survey andHST–CLASH observations of the galaxy cluster RXC J2248.7−4431: implications for stellar mass versus dark matter

Luminosity Function of Cluster Galaxies

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