CDROM/AJ/V109/P0853 VLA Survey of Abell Clusters. IV. (Ledlow & Owen 1995) ================================================================================ A 20 cm VLA Survey of Abell Clusters of Galaxies. IV. The Radio Sample and Cluster Properties Michael J. Ledlow & Frazer N. Owen <1995, AJ, 109, 853> =1995AJ....109..853L ================================================================================ Abstract: This is the fourth in a series of papers describing an in depth study of a large statistical sample of radio galaxies in Abell clusters. This sample forms the basis of a detailed optical and radio study of the host galaxy properties, environments, and evolutionary models for radio galaxies as a class of objects. In this paper, we examine the radio detection statistics as a function of cluster morphological type, galaxy richness, and spatial location within the cluster galaxy distribution. These relationships are also parameterized as a function of radio power. The spatial distributions of the radio sources as a function of distance from the cluster center indicate that radio galaxies are preferentially located at small radii from the center of the cluster potential. This is observed as a factor of 2-3 excess over that predicted by a King-model surface-density distribution. The excess is higher in the upper radio power bin. This result is easily explained, however, from the spatial distribution of the brightest galaxies and the relationship between radio and optical luminosity. The sample is divided into richness classes 0, 1, and 2, according to Abell's criterion, and in two radio power ranges. While simple counting shows that richer clusters have more radio galaxies in both radio power bins, when the detections are scaled to the number of galaxies surveyed in each cluster, no significant correlations are found. This result implies that the number of radio galaxies detected simply scales with the number of galaxies surveyed. The higher galaxy density (and presumably higher ICM gas density) in richer clusters does not appear to affect the rate of radio source formation. The clusters are divided into Rood-Sastry and Bautz-Morgan morphological types. While it would appear that the more regular clusters have higher radio detection rates, when the classes are normalized to the number of galaxies, the radio detection rates are found to be identical regardless of cluster morphology. In conclusion, it is the optical properties of the host galaxy which most influence both the radio detection rate and the radio source properties. The cluster properties, galaxy density, and spatial location of the galaxy do not significantly affect the observed radio statistics. File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table1a.dat 137 511 Cluster radio survey (z <= 0.09) table1b.dat 97 231 Cluster radio survey (0.09 < z ~ 0.25) table1a.tex 106 582 AASTeX version of Table 1a table1b.tex 86 270 AASTeX version of Table 1b -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1a.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 A4 --- Abell Abell cluster number 5 1X --- --- Blank 6- 7 A2 --- n_Abell *Abell number note 8- 9 2X --- --- Blank 10-30 A21 --- Redshift *Cluster redshift and reference code 31 A1 --- n_IAU *IAU name note 32 1X --- --- Blank 33-42 A10 --- IAU B1950 IAU name 43-45 I3 h RAh []? Right ascension, B1950 46-48 I3 min RAm []? R.A. 49-54 F6.2 s RAs []? R.A. 55 1X --- --- Blank 56 A1 --- DE- Declination sign, B1950 57-58 I2 deg DEd []? Dec. 59-61 I3 arcmin DEm []? Dec. 62-67 F6.2 arcsec DEs []? Dec. 68-74 I7 mJy Flux []? Measured flux density at 1400 MHz 75-80 F6.2 --- Ac *[]? Distance from cluster center 81-86 F6.2 mag 2E(B-V) []? Extinction at R band for the cluster 87-93 F7.2 mag m10c *[]? Corrected m10 94-101 F8.3 --- z_zest []? Ratio log(z/z_est) based on m10c 102-103 2X --- --- Blank 104-106 A3 --- n_Status *Status note explaining rejection 107 1X --- --- Blank 108-129 A22 --- Status Status of source in statistical sample 130-137 A8 --- Other Other name -------------------------------------------------------------------------------- Notes for file: table1a.dat -------------------------------------------------------------------------------- n_Abell, n_IAU, n_Status: 1 ID's on finder chart in O93 have labeled source A as D and source B as A. 2 ID's on finder chart in O92 have sources A and B switched. 3 ID's on finder chart in O93 have labeled source A as B and source B as C. 4 ID in O93 is labeled D on finder chart. 5 Only A is listed in O92, and is a background source. 6 ID's on finder in O92 have labeled sources A as C, B as A, and C as B. 7 Rejected because abs(log(z/z_est)) > 0.24. 8 Rejected because source is greater than 0.3 A_c from cluster center. 9 Rejected because galactic absorption is greater than 0.1 magnitudes. 10 Cluster was rejected because redshift is too low to have surveyed 0.5 A_c field. 11 Measured velocity was too different from mean cluster velocity Redshift: Number in parentheses following reference code is the number of galaxies used to compute the redshift. Reference codes are: (ACO) Abell, G.O., Corwin, H.G., and Olowin, R.P. 1989, ApJS, 70, 1 (H) Huchra, J.P. 1989, private communication (L) Lebedev, V.S. and Lebedeva, I.A. 1986, Astron. Tsirk, #1469, 4 (OH) Oegerle, W. and Hill, J. M. 1992, AJ, 104, 278 (O92) Owen, F.N., White, R.A., and Burns, J.O. 1992, ApJS, 80, 501 (O93) Owen, F.N., White, R.A., and Ge, J.-P. 1993, ApJS, 87, 135 (P) Postman, M., Huchra, J.P., and Geller, M.J. 1992, ApJ, 384, 404 (SGH) Schneider, D.P., Gunn, J.E., and Hoessel, J. 1983, ApJ, 264, 337 (S) Struble, M.F. and Rood, H.J. 1991, ApJS, 77, 363 Ac: The distance of the galaxy from the cluster center positions of Abell [1958, ApJS, 3, 211] expressed in units of a fraction of an Abell radius. m10c: The magnitude of the tenth brightest cluster galaxy corrected for the Scott effect and K-dimming -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1b.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 A4 --- Abell Abell cluster number 5 1X --- --- Blank 6 A1 --- n_Abell *Abell number note 7 1X --- --- Blank 8-19 A12 --- Redshift *Cluster redshift and reference code 20 1X --- --- Blank 21-30 A10 --- IAU B1950 IAU name 31-33 I3 h RAh []? Right ascension, B1950 34-36 I3 min RAm []? R.A. 37-42 F6.2 s RAs []? R.A. 43 1X --- --- Blank 44 A1 --- DE- Declination sign, B1950 45-46 I2 deg DEd []? Dec. 47-49 I3 arcmin DEm []? Dec. 50-54 F5.1 arcsec DEs []? Dec. 55-60 I6 mJy Flux []? Measured flux density at 1400 MHz 61-66 F6.2 --- Ac *[]? Distance from cluster center 67-72 F6.2 mag 2E(B-V) []? Extinction at R band for the cluster 73 1X --- --- Blank 74-76 A3 --- n_Status *Status note explaining rejection 77 1X --- --- Blank 78-97 A20 --- Status Status of Source in statistical sample -------------------------------------------------------------------------------- Notes for file: table1b.dat -------------------------------------------------------------------------------- n_Abell, n_Status: 1 Cluster has High R-Extinction, but kept because source is FR2 2 Cluster found to have z<0.09. Left in sample, but not included analysis 3 Radio flux slightly below 200 mJy cutoff, but left in sample 4 ID's on finder chart in O92 have sources A as B and B listed as C 5 Rejected because source is > 0.5 A_c from cluster center 6 Rejected because galactic absortption is > 0.1 magnitudes Redshift: Number in parentheses following reference code is the number of galaxies used to compute the redshift. Reference codes are: (H) Huchra, J.P. 1989, private communication (L) Lebedev, V.S. and Lebedeva, I.A. 1986, Astron. Tsirk., #1469, 4 (O92) Owen, F.N., White, R.A., and Burns, J.O. 1992, ApJS, 80, 501 (OLK) Owen, F.N., Ledlow, M.J., and Keel, W. 1995, AJ, ??,??? (OWT) Owen, F.N., White, R.A., and Thronson, H.A. 1987, AJ, 95, 1 (P) Postman, M., Huchra, J.P., and Geller, M.J. 1992 ApJ, 384, 404 (S) Struble, M.F. and Rood, H.J. 1991, ApJS,77, 363 Ac: The distance of the galaxy from the cluster center positions of Abell [1958, ApJS, 3, 211] expressed in units of a fraction of an Abell radius. -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 02-May-1995