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J/A+A/407/31      Heliocentric radial velocities in Abell 376    (Proust+, 2003)

The cluster of galaxies Abell 376. Proust D., Capelato H.V., Hickel G., Sodre Jr. L., Lima Neto G.B., Cuevas H. <Astron. Astrophys. 407, 31 (2003)> =2003A&A...407...31P
ADC_Keywords: Clusters, galaxy ; Radial velocities Keywords: galaxies: distances and redshifts - galaxies: cluster: general - galaxies: clusters: individual: Abell 376 - X-rays: galaxies: clusters Abstract: We present a dynamical analysis of the galaxy cluster Abell 376 based on a set of 73 velocities, most of them measured at Pic du Midi and Haute-Provence observatories and completed with data from the literature. Data on individual galaxies are presented and the accuracy of the determined velocities is discussed as well as some properties of the cluster. We obtained an improved mean redshift value z=0.0478^+0.005-0.006 and velocity dispersion σ=852+120-76km/s. Our analysis indicates that inside a radius of ∼900h70-1kpc (∼15-arcmin) the cluster is well relaxed without any remarkable feature and the X-ray emission traces fairly well the galaxy distribution. A possible substructure is seen at 20-arcmin from the centre towards the Southwest direction, but is not confirmed by the velocity field. This SW clump is, however, kinematically bound to the main structure of Abell 376. A dense condensation of galaxies is detected at 46 arcmin (projected distance 2.6h70-1Mpc) from the centre towards the Northwest and analysis of the apparent luminosity distribution of its galaxies suggests that this clump is part of the large scale structure of Abell 376. X-ray spectroscopic analysis of ASCA data resulted in a temperature kT=4.3±0.4keV and metal abundance Z=0.32±0.08Z_☉. The velocity dispersion corresponding to this temperature using the TX-σ scaling relation is in agreement with the measured galaxies velocities. Description: A total of 71 velocities has been obtained from our observations. Table 1 lists positions and heliocentric velocities for 73 individual galaxies in the cluster including data from Wegner et al. (1999, Cat. J/MNRAS/305/259) and from Postman and Lauer (1995, Cat. J/ApJ/440/28). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 71 78 Heliocentric radial velocities in Abell 376
See also: VII/174 : Morphological type catalog in 55 rich galaxy clusters (Dressler, 1980) J/MNRAS/305/259 : EFAR galaxies redshifts + velocity disp. (Wegner+, 1999) J/ApJ/440/28 : Brightest Cluster Galaxies velocities (Postman+ 1995) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Dressler (1980, Cat. VII/174) number ([D80] ACO 376 NNN in Simbad) 6- 17 A12 --- Name Alternative name LEDA, UGC, GIN or MCG 19- 20 I2 h RAh Right ascension (J2000) 22- 23 I2 min RAm Right ascension (J2000) 25- 28 F4.1 s RAs Right ascension (J2000) 31 A1 --- DE- Declination sign (J2000) 32- 33 I2 deg DEd Declination (J2000) 35- 36 I2 arcmin DEm Declination (J2000) 38- 39 I2 arcsec DEs Declination (J2000) 42- 46 A5 --- MType Morphological type from Dressler's (1980, Cat. VII/174) catalogue 50- 54 I5 km/s HRV ? Heliocentric radial velocity 56- 58 I3 km/s e_HRV ? rms uncertainty on HRV 61- 65 F5.2 --- R ? R cross-correlation parameter derived from Tonry & Davis (1979AJ.....84.1511T) (3) 68- 69 A2 --- Tel Telescope or origin (1) 70 I1 --- Notes [1/4]? Individual notes (2)
Note (1): Telescopes: o: 1.93m OHP telescope + CARELEC spectrograph p: 2.0m Pic du Midi telescope + ISARD l1: from Wegner et al. (1999, Cat. J/MNRAS/305/259) l2: from Postman and Lauer (1995, Cat. J/ApJ/440/28) Note (2): Notes: 1: emission line: OII= 39998 km/s 2: aligned star with a foreground galaxy (V < 10000 km/s) 3: dominant M star 4: dominant star Note (3): R = h/(sqrt(2)*σCCF), where h is the height of the cross-correlation peak and σCCF is the rms noise in the cross-correlation.
Acknowledgements: Dominique Proust
(End) Patricia Bauer [CDS] 27-Jun-2003
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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