CDROM/AJ/V110/P0463 The Shapley Supercluster (Quintana+ 1995) ================================================================================ The Shapley Supercluster. I. Spectroscopic Observations in the Central Region H. Quintana, A. Ramirez, Jorge Melnick, Somak Raychaudhury, & Eric Slezak <1995, AJ, 110, 463> =1995AJ....110..463Q ================================================================================ Abstract: We present a new analysis of the kinematics of the Shapley supercluster based on radial velocities for 1087 galaxies in the clusters A3558 (Shapley 8), A3528 (Klemola 21), A3532 (Klemola 22), A3530, A3556 (SC 1321-314), A3559 (CE 1327-292), A3560, A3562, SC 1329-314 and in the intercluster region of the core of the supercluster, of which 367 are new measurements. We also present accurate positions from APM and MAMA scans of the ESO/SERC Southern Sky Survey photographic plates. We obtain new velocity dispersions and estimate the masses of the member clusters, evaluating dynamical models of the supercluster. The supercluster is found to be significantly flattened. We find that for Omega_0=0.3, H_0=75 km/s/Mpc, the gravitational pull of the supercluster may account for up to 25% of the peculiar velocity of the Local Group required to explain the dipole anisotropy of the Cosmic Microwave Background radiation, in which case the mass of the supercluster would be dominated by intercluster dark matter. This fractional contribution would be considerably higher for combinations of significantly lower values of Omega_0 and higher values of H_0. File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table2.dat 80 497 Galaxy velocities -------------------------------------------------------------------------------- Byte-by-byte Description of file: table2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 7 A7 --- Region *ACO cluster name or cluster area code 8- 9 2X --- --- Blank 10-13 A4 --- ID Observing identifications 14-15 2X --- --- Blank 16-18 I3 --- ESO ESO field 19-20 2X --- --- Blank 21-26 A6 --- Coord *APM, MAMA cat. numbers or other codes 27 1X --- --- Blank 28-30 I3 h RAh []? Right ascension, epoch 1950 31-33 I3 min RAm []? R.A. 34-38 F5.1 s RAs []? R.A. 39 1X --- --- Blank 40 A1 --- DE- Declination sign 41-42 I2 deg DEd []? Declination, epoch 1950 43-45 I3 arcmin DEm []? Dec. 46-48 I3 arcsec DEs []? Dec. 49 A1 --- u_RADE Equatorial coordinate uncertainty flag 50 1X --- --- Blank 51 A1 --- Code *[R:<( ] Codes for following fields 52-56 F5.1 mag m_J []? Ptg. J mag, measured from APM survey 57-63 I7 km/s RadVel Heliocentric velocities 64-67 I4 km/s e_RadVel Heliocentric velocities error 68 1X --- --- Blank 69-73 A5 --- R_nl *R value or number of lines 74-75 2X --- --- Blank 76-80 A5 --- Ref *Code for observer or velocity reference -------------------------------------------------------------------------------- Notes for file: table2.dat -------------------------------------------------------------------------------- Region: Gives either the ACO cluster name, ordered by ascending number, or a code for the area where the cluster is located. These areas denote (1 degree x 5 min) regions (approx 1 square degree) in which we divided the field to program the observations, and are named by the coordinates of the NW corner. If this field is blank, the data in the Code, RadVel, R_nl, and Ref fields are continuations for the previous object. Coord: The APM, MAMA catalogue numbers or other codes used as source for coordinates. Most coordinates are either from digital scans of the SERC IIIa-J atlas, using the APM facility in Cambridge, England or from scans of ESO/SRC R fields done with the MAMA machine at Paris. For galaxies not found in the APM and MAMA scans, positions are quoted from the ESO/Uppsala catalog (Lauberts 1982). Coordinates for galaxies in A3558 were measured with the Optronics machine at ESO, Garching. Code: R = m_J is R magnitude from the MAMA survey. : = m_J is uncertain (saturated image on plate or estimated by eye) < = m_J is an upper limit (the magnitude quoted being the total magnitude of a merged image of which the galaxy is a part) ( = velocities are not used in the mean values of redshifts. R_nl: The R value of the cross-correlation, or the number of lines measured in each spectra, if the line position method was used. The R value is a real value and the number of lines is an integer value. Ref: The code of observer/telescope/date or a reference code if the galaxy also has a velocity reported in the literature. Q1-Q7,M1-M3: observing sessions as in Table 1 of the printed paper. MGS87 Metcalfe et al. 1987, MNRAS, 225, 581 TCG90 Teague et al. 1990, ApJS, 72, 715 Da86 da Costa et al. 1986, AJ, 91, 6 Da87 da Costa et al. 1987, AJ, 93, 1338 DS88 Dressler and Shectman 1998, AJ, 95, 284 D091 Dressler 1991, ApJS, 75, 241 Cr87 Cristiani et al. 1987, A&A, 179, 108 R087 Richter, O.-G. 1987, A&A, 67, 261 Ve90 Vettolani et al. 1990, AJ, 99, 1709 Mo88 Monk et al. 1988, MNRAS, 234, 193 Mo89 Mould et al. 1989, ApJ, 338, 654 PGC Paturel et al. Catalogue of Principal Galaxies, Monographies de la Base de Donnees Extragalactiques, No 1, Lyon: Obs. de Lyon; 1737 ZCAT Catalog, Huchra et al. 1993 -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 06-Oct-1995