ASCA observations of massive medium-distant clusters   of galaxies. II.

Matsumoto, Hironori; Pierre, M.; Tsuru, Takeshi Go; Davis, David

doi:10.1051/0004-6361:20010616

Cited by 8 publications

(9 citation statements)

References 13 publications

(23 reference statements)

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“…This is achieved by considering the highest redshift cluster in the control group: Abell 2255. For this cluster, the SDSS limiting 1 We re-affirm the note made by Valtchanov et al (2002) about Abell 1451 (T X = 13.4 keV; Matsumoto et al 2001) possessing a very significant deviation away from the L X -T X scaling relation (e.g., Popesso et al 2005). This cluster merits future follow-up to discern the impact and potential cause of such an extreme temperature.…”

Section: Cluster Sub-structuresupporting

confidence: 64%

How typical is the Coma cluster?

Pimbblet¹,

Davies²

2014

Monthly Notices of the Royal Astronomical Society

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Coma is frequently used as the archetype z ∼ 0 galaxy cluster to compare higher redshift work against. It is not clear, however, how representative the Coma cluster is for galaxy clusters of its mass or X-ray luminosity, and significantly: recent works have suggested that the galaxy population of Coma may be in some ways anomolous. In this work, we present a comparison of Coma to an X-ray selected control sample of clusters. We show that although Coma is typical against the control sample in terms of its internal kinematics (substructure and velocity dispersion profile), it has a significantly high (∼ 3σ) X-ray temperature set against clusters of comparable mass. By de-redshifting our control sample cluster galaxies star-formation rates using a fit to the galaxy main sequence evolution at z < 0.1, we determine that the typical star-formation rate of Coma galaxies as a function of mass is higher than for galaxies in our control sample at a confidence level of > 99 per cent. One way to alleviate this discrepency and bring Coma in-line with the control sample would be to have the distance to Coma to be slightly lower, perhaps through a non-negligible peculiar velocity with respect to the Hubble expansion, but we do not regard this as likely given precision measurements using a variety of approaches. Therefore in summary, we urge caution in using Coma as a z ∼ 0 baseline cluster in galaxy evolution studies.

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Section: Cluster Sub-structuresupporting

confidence: 64%

How typical is the Coma cluster?

Pimbblet¹,

Davies²

2014

Monthly Notices of the Royal Astronomical Society

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“…There is an X-ray emitting star in the south of the cluster whose X-ray emission was deblended. Nine coincident galaxy redshifts leave no doubt about the existence of a cluster at this position (see also the ASCA study of Matsumoto et al 2001). …”

Section: Rxcj00143-6604 A2746 (Also Included In Xbacs)mentioning

confidence: 97%

The ROSAT-ESO Flux Limited X-ray (REFLEX) Galaxy cluster survey

Böhringer¹,

Schuecker²,

Guzzo

et al. 2004

A&A

606

667

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Abstract. We present the catalogue of the REFLEX Cluster Survey providing information on the X-ray properties, redshifts, and some identification details of the clusters in the REFLEX sample. The catalogue describes a statistically complete X-ray flux-limited sample of 447 galaxy clusters above an X-ray flux of 3 × 10 −12 erg s −1 cm −2 (0.1 to 2.4 keV) in an area of 4.24 ster in the southern sky. The cluster candidates were first selected by their X-ray emission in the ROSAT-All Sky Survey and subsequently spectroscopically identified in the frame of an ESO key programme. Previously described tests have shown that the sample is more than 90% complete and there is a conservative upper limit of 9% on the fraction of clusters with a dominant X-ray contamination from AGN. In addition to the cluster catalogue we also describe the complete selection criteria as a function of the sky position and the conversion functions used to analyse the X-ray data. These are essential for the precise statistical analysis of the large-scale cluster distribution. This data set is at present the largest, statistically complete X-ray galaxy cluster sample. Together with these data set we also provide for the first time the full three-dimensional selection function. The sample forms the basis of several cosmological studies, one of the most important applications being the assessment of the statistics of the large-scale structure of the universe and the test of cosmological models. Part of these cosmological results have already been published.

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“…Properties of the two clusters. References: Abell (1958), Abell et al (1989) for the coordinates and richness; Bautz & Morgan (1970) for classification for Abell 1451; coordinates for RXJ1314−25 are from RASS (Voges et al 1999); T X and L X in the 2-10 keV band are from Matsumoto et al (2001); redshift and σ v are from this paper; the apparent magnitude of an L * galaxy was calculated using M * (B j ) = −21.8, obtained by adjusting the Lumsden et al (1997) was equipped with EFOSC1 (ESO Faint Object Spectrograph and Camera), Tektronix 512 × 512 CCD (pixel size 27 µm and 0.61 /pixel) and Grism B300, covering the range 3740-6950 Å, with central wavelength 5250 Å and dispersion of 6.2 Å/pixel. The observations in 1999 were performed with EFOSC2, CCD #40 2048 × 2048 (pixel size 15 µm, 0.157 /pixel) and Grism O300 which covers 3860-8070 Å with central wavelength 5000 Å and dispersion 2.06 Å/pixel.…”

Section: Observations and Reductionmentioning

confidence: 99%

“…By means of EXSAS (Zimmermann et al 1994), the observed count-rate is then used to normalize the spectral modela Raymond & Smith (1977) thermal plasma emission, convolved by the ROSAT/HRI response function, with temperature and metallicity from ASCA data (Matsumoto et al 2001) and line-of-sight Galactic absorption by H I from Dickey & Lockman (1990). The spectrum is then integrated to derive the flux and cluster rest frame luminosity in the "standard" X-ray bands [0.5-2] and [2-10] keV.…”

Section: X-ray Propertiesmentioning

confidence: 99%

“…N H is taken from Dickey & Lockman (1990). ASCA data for T X and L X in the [2 − 10] keV band (Matsumoto et al 2001) Count-rate C(r < r lim ) (cts s 0.25 0.27 † ASCA/GIS luminosity out to 4 , including the contribution from the QSO ∼ 1 30 south of the centre. ‡ ASCA/GIS luminosity out to 4 , including the contribution from the Sy1 galaxy ∼3 15 south-east of the centre.…”

Section: Parametermentioning

confidence: 99%

See 1 more Smart Citation

Abell 1451 and 1RXS J131423.6-251521: A multi-wavelength study of two dynamically perturbed clusters of galaxies

Valtchanov

Murphy

Pierre

et al. 2002

A&A

Self Cite

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Abstract. We present results from optical, X-ray and radio observations of two X-ray bright (L X ∼ 10 45 erg s −1 ) galaxy clusters. Abell 1451 is at redshift z = 0.1989 and has line-of-sight velocity dispersion σ v = 1330 km s −1 as measured from 57 cluster galaxies. It has regular X-ray emission without signs of substructure, a Gaussian velocity distribution, lack of a cooling flow region and significant deviations from the observed scaling laws between luminosity, temperature and velocity dispersion, indicating a possible merging shock. There is only one spectroscopically confirmed cluster radio galaxy, which is close to the X-ray peak. 1RXS J131423.6−251521 (for short RXJ1314−25) has z = 0.2474 and σ v = 1100 km s −1 from 37 galaxies. There are two distinct galaxy groups with a projected separation of ≈700 kpc. The velocity histogram is bi-modal with a redshift-space separation of ∼1700 km s −1 , and the X-ray emission is double peaked. Although there are no spectroscopically confirmed cluster radio galaxies, we have identified a plausible relic source candidate.

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ASCA observations of massive medium-distant clusters of galaxies. II.

Cited by 8 publications

References 13 publications

How typical is the Coma cluster?

How typical is the Coma cluster?

The ROSAT-ESO Flux Limited X-ray (REFLEX) Galaxy cluster survey

Abell 1451 and 1RXS J131423.6-251521: A multi-wavelength study of two dynamically perturbed clusters of galaxies

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