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The Extension of the Hubble Diagram. II-New Redshifts and Photometry Of THE ASTROPHYSICAL JOURNAL, 221:383-394, 1978 April 15 © 1978. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1978ApJ...221..383K THE EXTENSION OF THE HUBBLE DIAGRAM. IL NEW REDSHIFTS AND PHOTOMETRY OF VERY DISTANT GALAXY CLUSTERS: FIRST INDICATION OF A DEVIATION OF THE HUBBLE DIAGRAM FROM A STRAIGHT LINE JEROME KRISTIAN, ALLAN SANDAGE, AND JAMES A. WESTPHAL Hale Observatories, Carnegie Institution of Washington, California Institute of Technology Received 1977 July 22; accepted 1977 October 31 ABSTRACT Redshifts are given for 50 brightest cluster galaxies, extending as far as z = 0.75; BVR photom­ etry is given for 33 clusters. These data are combined with earlier data of a similar kind in order to investigate several effects. The measured B - V and V - R colors as a function of redshift are well represented by Whitford's standard-galaxy K corrections, as far as these are defined (to · z = 0.28 in B - V and z = 0.48 in V - R). This suggests both that the K corrections are valid over these ranges of z and that no major color change of the galaxies has occurred over the last 4-5 x 109 years. At larger redshifts, the colors, which start out being monotonically redder with z, turn over and become bluer with z. The data at large z seem to follow the prediction based upon ultraviolet photometry of NGC 4486 (M87), which is one extreme of a range of galaxies measured by Code and Welch. Other standard corrections to the measurements are discussed, and formal least-squares values of q0 are computed. To explore the possibility that one might be stalemated by the fact that the value of q0 must, in principle, be known a priori to compute the aperture correction, the data are corrected separately for assumed q0 values of 0 and + 1. The subsequently computed values of q0 differ by only 0.2 between the two cases, which indicates that a simple iterative procedure will converge to produce a self-consistent value of q0• The new data do not significantly change earlier discussions of the corrections for cluster richness and Bautz-Morgan contrast type. If these two corrections are not made, the effect on the present data is to significantly increase the positive curvature of the Hubble diagram, as well as the dispersion in apparent magnitude. To within the limits of the present data, the absolute magnitude of the brightest cluster galaxy does not, in general, depend on whether it is also a bright radio source. The present sample, cut off at z = 0.4 to avoid selection effects and uncertainties in the data, shows the first significant evidence for curvature of the Hubble diagram, with V and R magni­ tudes giving similar results. The formal value of q0 (with galaxy evolution ignored) is + 1.6 ± 0.4. The dispersion in absolute magnitude is less than 0.3 mag, with Mv = -23.28 ± 0.03 and MR= -24.09 ± 0.03. The use of the Hubble diagram in cosmology now depends on a knowledge of brightness changes in galaxies, on the one hand, or of q0 from other evidence, on the other. For example, if it were known with certainty that there has been no significant change in elliptical galaxy luminosities during the last 4 x 109 years, then the present data are nearly good enough for one to say defini­ tively that the universe is closed and finite, with a finite lifetime. At the other extreme, if it were known with certainty from other evidence that the universe was nearly empty (q 0 ::::: 0), then the present data set the constraint that net galaxy luminosities have decreased by .-0.5 mag during the last 5 x 109 years, with a net color change A(B - V) ~ 0.1 mag. It seems possible at present to construct a self-consistent model with q0 ::::: 0 that satisfies the known data, but the case is not yet settled. Subject headings: cosmology- galaxies: clusters of - galaxies: redshifts I. INTRODUCTION the evolution of galaxies and of the universe. We have used SIT television detectors for sky-subtraction This paper is the second in a series reporting meas­ spectroscopy and two-dimensional photometry, in urements ofredshifts and magnitudes of faint galaxies. addition to conventional photomultiplier aperture The overall aim is to obtain these fundamental data photometry. Our strategy has been to start at the for a large sample of galaxies from the former photo­ bright end of the range (z ::::: 0.2) and to work toward graphic cutoff at z = 0.2 to as great a redshift as fainter objects as experience is gained with the new possible, in order to investigate problems relating to detectors. Paper I (Sandage, Kristian, and Westphal 383 © American Astronomical Society • Provided by the NASA Astrophysics Data System TABLE 1 REDSHIFTS DETERMINED FROM 1975 JUNE TO 1976 JUNE WITH THE DIGITAL SKY-SUBTRACTION SPECTROGRAPH WITH SIT DETECTOR (Hale 5 m reflector) GALAXY R BM "(1950) 6 (1950) QUALITY NOTES 1978ApJ...221..383K (1) (2) (3) (4) (5) (7) (8) (9) ABELL CLUSTERS A 15 (Gl) n-m 0012 46.9 -26 19 32 -82 0.121 E A 41 (Gl) 002619.2 +o7 33 22 -55 0.279 G A 46 (Gl) m 00 27 51.5 -13 12 33 -75 0.140 E A 46 (G2) m 0027 54.1 -13 11 33 -75 0.159 p A 180 (Gl) 0119 16.3 +02 44 16 -59 0.135 E A 209 (A) I - Il 012924.8 -13 52 13 -74 0.213 E A 370 n-m 02 37 20.4 -01 47 51 -54 o. 373 F = 0237-01 A 403 (Gl) 025636.7 +o3 17 57 -47 0.107 F A 750 (Gl) n 090610.2 +11 13 56 +35 0.163 E A 777 (Gl) 4 n-m 09 23 27.0 +78 30 28 +34 0.224 F A 868 (Gl) n 09 42 58.l -08 2517 +32 0.154 E A 873 (GA) n 094836.6 +71 32 29 +39 0.182 E A 1246 (Gl) n-m 11 21 21. 0 +21 45 15 +69 o. 216 G A 1278(G3) m 11 27 33.4 +20 47 52 +70 0.129 E A 1571 (Gl) n 12 32 09.1 +83 40 35 +34 0.208 E A 1759 (Gl) m 13 31 40.3 +20 30 53 +78 0.168 E A 1942 (Gl) 14 35 48.3 +03 51 24 +55 0.224 G 10 A 1942 (G2) 14 35 51.4 +03 53 15 +55 0.224 E A 2218 (Gl) 4 I -Il 16 35 38.6 +66 18 35 +38 0.171 F 3, 10 A 2218 (G2) 4 I -Il 16 36 00.9 +66 20 03 +38 0.170 E A 2218 (FG) 4 1-Il 16 :i6 05.3 +66 20 23 +38 0.023 E Foreground A 2240 (Gl) m 16 53 38.4 +66 50 05 +36 0.137 E A 2283 (A) 174448.8 +69 42 18 +31 0.182 E A 2283 (B) 17 4512.7 +69 41 39 +31 o.036 F Foreground A 2320 (Gl) 1916 49.0 +70 50 41 +24 0.170 G 10 A 2397 (Gl) m 21 53 35.3 +01 09 10 -39 0.222 E 10 A 2443 22 23 43.2 +170603 -33 0.107 E 10 A 2554 (cD) 23 09 40. 7 -21 46 32 -67 0.106 E 10 A 2645 (Gl) 4 n 23 38 42.5 -09 18 14 -65 0.246 G SPECjAL SURVEY CLUSTERS 0340 - 06 (HS) 1-Il 03 40 21 -06 30 01 -44 0. 226 G 0819 + 54 (3a.J) 08 19 53.1 +54 18 40 +35 0.307 E 10 0822 + 67 (3aJ) 08 22 20.6 +67 56 53 +34 0.384 E 0905 + 64 (3a.J) m 09 05 15 +64 12 21 +39 0. 215 E 10 1351 + 51 (3aJ) 13 51 21 +51 31 33 +63 o. 220 E 10 1(101+29 (3a.T) 160138.0 +29 05 36 +48 0.280 E 10 2223 + 13 (127) 22 23 31.5 +13 44 32 -36 o. 374 p 10 2244 - 02 (127) 22 44 38.3 -02 21 30 -51 0.328 G 10 RADIO GALAXIES 3C 19 OQ 38 13.8 +32 53 42 -30 0.482 F 4, 11 3C 111 04 14 54.9 +37 53 34 -9 0. 050 E 9, 10 3C 123 043355.2 +29 34 13 -12 0.218: F 5, 12, 13 3C 268.3 12 03 50.3 +64 30 59 +52 0.371 E 9, 10, 11 3C 330 COMPANION 16 09 11.3 +66 03 27 +41 0.532 E 6. 11, 12 3C 343.l 16 37 55.2 +62 40 35 +39 o. 750 E 3C 401 19 39 38. 8 +60 34 31 +18 0.200 E 5, 10: CLUSTER 3C 424 20 45 44.4 +o6 50 10 -22 0.222 F 7, 10 3C 424 (FG) (WEST) 20 45 42.7 +06 49 53 -22 0.125 E 3C 424 (FG) (EAST) -22 0.123 E 3C 434 21 20 54.4 +15 35 12 -24 0.323 E 4, 5, 10, 12 3C 438 21 53 45.5 +37 46 15 -13 o. 292 G 4, 5, 12 3C 460 231859.8 +23 30 22 -35 0.268 E 8, 11, 12 © American Astronomical Society • Provided by the NASA Astrophysics Data System EXTENSION OF HUBBLE DIAGRAM 385 NOTES TO TABLE 1 1.
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