the kinematics of these clusters and presented evidence for peculiar cd velocities. Observations and analysis of A2107

Transcription

1 THE ASTRONOMICAL JOURNAL, 116:1529È1540, 1998 October ( The American Astronomical Society. All rights reserved. Printed in U.S.A. DYNAMICS OF cd CLUSTERS OF GALAXIES. III. REDSHIFT DATA FOR 11 ABELL CLUSTERS JOHN M. HILL Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ ; jhill=as.arizona.edu AND WILLIAM R. OEGERLE Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD ; oegerle=pha.jhu.edu Received 1998 June 12; revised 1998 June 29 ABSTRACT We present the Ðnal observational data for a spectroscopic study of a sample of cd galaxy clusters. The goal of this program has been to study the dynamics of the clusters, with emphasis on determining the nature and frequency of peculiar-velocity cd galaxies. In this paper we present redshifts for 762 galaxies in the Ðelds of the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. We also present preliminary dynamical properties for these clusters using our measured redshifts. Key words: cosmology: miscellaneous È galaxies: clusters: general È galaxies: distances and redshifts 1. INTRODUCTION Galaxies classiðed as type cd are the most luminous galaxies in the universe. Since they exist only in clusters and groups of galaxies, their existence and evolution are intimately tied to the formation and evolution of the clusters themselves. Although a wealth of data on the properties of cd galaxies exists, it is still unknown whether cdïs are the product of dynamical processes operating in clusters prior to their collapse or after cluster virialization. Clues to the formation of cd galaxies may, then, be found in kinematic studies of cdïs and their parent clusters. The properties of cd galaxies are consistent with the galaxies lying at the bottom of their cluster potential wells. They are located at cluster centers (Matthews, Morgan, & Schmidt 1964) and at the peak of the cluster X-ray emission (Jones et al. 1979). Merritt (1984) has argued that supergiant galaxies can form only at the centers of clusters; otherwise, their envelopes would be tidally truncated by the gravitational Ðeld of the cluster. Galaxies formed at the bottom of the potential well acquire a luminous halo of tidal debris from stripped cluster galaxies. In the galactic cannibalism ÏÏ model (Ostriker & Tremaine 1975; Ostriker & Hausman 1977; Hausman & Ostriker 1978), cd galaxies grow after cluster virialization by merging with galaxies that are dragged into the cluster center by the e ects of dynamical friction. If cd galaxies are born in subclusters that merge with other clusters, we may be able to detect the residual velocity of the cd with respect to the merging clusters. We began a survey of the kinematics of cd clusters to investigate the nature and frequency of peculiar-velocity cd galaxies and their clusters. The advent of multiðber spectrographs has provided the capability to obtain large numbers of galaxy velocities in clusters for such studies. In Paper I (Hill & Oegerle 1993), we presented redshifts for 551 galaxies in the rich Abell clusters A193, A399, A401, A1795, A1809, A2063, and A2124, and we investigated the frequency of emission-line galaxies in these clusters. In a follow-up to that paper, Oegerle & Hill (1994), we studied the kinematics of these clusters and presented evidence for peculiar cd velocities. Observations and analysis of A2107 were reported separately by Oegerle & Hill (1992). The cd velocity and cluster dynamics in A2634 were investigated in Pinkney et al. (1993). A2029 was included in a paper on high velocity dispersion clusters by Oegerle, Hill, & Fitchett (1995). In this paper, we continue the observational study of the sample of clusters deðned in Paper I. Redshifts are presented below for the rich Abell clusters A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666. Detailed analysis of the cluster dynamics and cd galaxy peculiar velocities will be presented in a future paper. 2. OBSERVATIONS AND DATA REDUCTION Positions of galaxies with magnitudes brighter than m D 18.5 in the Ðeld of each of the 11 clusters were mea- V sured from digitized Palomar Quick V ÏÏ Survey plates at the Space Telescope Science Institute. Galaxies were identi- Ðed by eye, and the positions were calculated using the Hubble Space Telescope guide star plate solutions. The relative positional accuracies of the coordinates in the tables are 0A.3 rms. All new observations reported here were obtained with the multiðber MX Spectrometer at the Steward Observatory 2.3 m telescope in A detailed description of the design and construction of the MX Spectrometer is given by Hill & Lesser (1986), and it will not be described further here. The detector was a UV-enhanced Loral 1200 ] 800 pixel CCD processed by Lesser (1994). A 400 line mm~1 grating provided wavelength coverage from 3700 to 6950 A at 8 A resolution (2.8 A pixel~1). The use of this detector, with its superior quantum efficiency, Ñat-Ðelding, and charge transfer properties (compared with the Texas Instruments CCD used previously with MX), and the use of a higher efficiency and higher resolution grating resulted in generally higher quality spectra than previously obtained for this project by Hill & Oegerle (1993). The readout noise was 8 electrons pixel~1 rms; however, for several nights during the 1993 observing campaign the dark current in the CCD was abnormally high, yielding an e ective noise of about 16 electrons pixel~1 rmsfora1hrexposure. One-hour exposures were obtained with each Ðber con- Ðguration, followed by exposures of He, Ne, and Ar comparison lamps through all Ðbers for wavelength calibration. 1529

2 1530 HILL & OEGERLE Vol. 116 FIG. 1.È(a) Spectrum of the A779 cd galaxy (No. 201 in Table 2). (b) Spectrum of the A1691 cd galaxy (No. 201 in Table 3). Mg b is redshifted into the [O I] j5577 night-sky line. (c) Spectrum of the A1749 cd galaxy (No. 201 in Table 4). (d) Spectrum of the A1767 cd galaxy (No. 201 in Table 5). Mg b is redshifted into the [O I] j5577 night-sky line. (e) Spectrum of the A1837 cd galaxy (No. 201 in Table 6). ( f ) Spectrum of the A1927 cd galaxy (No. 201 in Table 7). Flat Ðelds were made by illuminating the spectrograph with a quartz lamp through a di user placed below the slit at the beginning and end of the night. Continuum spectra were also taken through the Ðbers without the di user in place to provide Ðber Ñats ÏÏ used to deðne the spectroscopic apertures on the CCD. The data were reduced using IRAF (Tody 1986) and MXPACKAGE, a suite of MX reduction programs and IRAF scripts written by the authors for dealing with MX data. The reduction steps are identical to those described in Hill & Oegerle (1993), and will not be repeated here. Because of the very Ñat CCD with well-behaved charge transfer, the dispersion solutions were exceptionally goodè typical errors obtained from two-piece cubic spline Ðts to the dispersion curves were 0.15 A. The spectra were extracted from each image, wavelength-calibrated, linearized, and then sky-subtracted, as described in Hill & Oegerle (1993) V elocities Radial velocities of galaxies were computed using the IRAF RV package, which is based on the Tonry & Davis (1979) cross-correlation technique. Prior to crosscorrelation, the galaxy spectra were continuum-subtracted, binned in the logarithm of the wavelength, and cleaned of cosmic rays and any emission lines. These steps were performed through the use of several IRAF tasks, so that no modiðcations of the data were performed by potentially biased humans. Cosmic rays were cleaned by rejecting data points more than 3 p above a Ðt to the spectral continuum. Cross-correlations were performed using a library of high signal-to-noise ratio early-type galaxy spectra obtained with MX and the KPNO Hydra multiðber spectrograph. Template galaxies and their adopted heliocentric velocities included NGC 3379 (]922 km s~1), M32 ([200 km s~1), M31 ([297 km s~1), NGC 7331 (]819 km s~1), and the spectra of the central components of two cd galaxies, A779

3 No. 4, 1998 DYNAMICS OF cd CLUSTERS. III FIG. 2.È(a) Spectrum of the A2067 cd galaxy (No. 201 in Table 8). (b) Spectrum of the A2079 cd galaxy (No. 201 in Table 9). (c) Spectrum of the A2089 cd galaxy (No. 201 in Table 10). Mg b is redshifted into the [O I] j5577 night-sky line. (d) Spectrum of the A2199 cd galaxy (No. 201 in Table 11). Note the broad Ha emission caused by the cluster cooling Ñow. (e) Spectrum of the A2666 cd galaxy (No. 201 in Table 12). (6868 km s~1) and A2199 (9304 km s~1). Two K giant stars were also used as templates: HD (]94.7 km s~1) and M3 star vz 297 ([142 km s~1). Multiple observations of these standards yielded 26 template spectra. Velocity errors were estimated based on the average Tonry & Davis (1979) R-value ÏÏ of the cross-correlations. We have estimated that the internal velocity error for a single spectrum is given by p \ 280/(1 ] R) km s~1 for R [ 3.0. The minimum allowed MX error from a single spectrum is 20 km s~1 based on wavelength-calibration uncertainties. The reader is referred to Hill & Oegerle (1993) for a more detailed discussion of velocity errors. 3. cd VELOCITIES Spectra of all 11 cd galaxies are plotted in Figures 1 and 2. The spectra have not been Ñux-calibrated. Emission and absorption features have been marked on selected spectra. The plots cover a wavelength range of 3800 to 6500 A. Our velocities for the central cd galaxies are compared with previous observations from the literature in Table 1. Column (1) lists the cluster name and subcomponent of the cd galaxy, where relevant. Column (2) lists our measured heliocentric velocity and errors in km s~1. Column (3) lists the heliocentric velocity and errors reported in the literature. Column (4) lists the velocity di erence, *cz, between our measurements and the literature values in km s~1. Column (5) provides the literature reference. In general, we Ðnd that our velocities agree with those in the literature within the reported errors. 4. CLUSTER SUMMARY AND NOTES Provided below are comments on the clusters in the present sample, comparisons with the literature, and various data reduction notes. A histogram of radial velocities of galaxies in each cluster Ðeld is shown in Figure 3. The histograms include only velocities reported in this paper. Radial velocities and coordinates are reported in Tables 2È12 for A779, A1691, A1749, A1767, A1837, A1927, A2067, A2079, A2089, A2199, and A2666, respectively. In each table, column (1) contains an identifying number; columns (2) and (3) give the sky coordinates (J equinox); the observed heliocentric velocities (cz, inkms~1) are reported in column (4), with errors (dcz, in km s~1) reported in column (5); various notes about the spectra (such as the presence of emission lines) are reported in column (6). An E ÏÏ in column (6) indicates that the velocity comes from measurements of emission lines only, rather than the crosscorrelation of the absorption spectra. We have listed the wavelengths of emission lines that were noted during manual inspection of the spectra. The letter A ÏÏ indicates

4 1532 HILL & OEGERLE Vol. 116 TABLE 1 CD VELOCITY COMPARISON cz us cz ref *cz Cluster/cD (km s~1) (km s~1) (km s~1) Reference (1) (2) (3) (4) (5) A779C ^ ^ 80 [ ^ 15 [ ^ 34 ] ^ 20 [1 4 A779 SW ^ ^ 15 [ ^ 15 [24 5 A ^ ^ 15 ]97 6 A ^ ^ 15 ]38 6 A ^ ^ 15 ]110 6 A ^ ^ 30 [ ^ 30 ]11 8 A1927 N ^ A1927 S ^ A ^ ^ 54 [56 9 A ^ ^ 38 ]29 10 A ^ ^ 43 ] A2199C ^ ^ 15 [ ^ 20 ]11 7 A2199 NE ^ ^ 15 ]80 11 A ^ ^ 24 ] ^ 65 ] ^ 16 [ ^ 14 ]7 13 REFERENCES.È(1) MerriÐeld & Kent 1991; (2) Tonry 1985; (3) Huchra et al. 1983; (4) de Vaucouleurs et al. 1991; (5) Zabludo et al. 1990; (6) Hoessel, Gunn, & Thuan 1980; (7) Zabludo et al. 1993; (8) Postman & Lauer 1995; (9) Postman et al. 1988; (10) Postman et al. 1986; (11) Tonry 1984; (12) Hintzen 1980; (13) Smith et al the presence of absorption in the Balmer series. Crossreferences of galaxies to those previously measured by others are also noted in this column. NM ÏÏ indicates a foreground or background galaxy that is not a velocity member of the cluster. cd ÏÏ indicates the central cd galaxy, and is followed by the number of repeated independent observations of the cd redshift. In the discussion below, we report the mean observed velocities and velocity dispersions for these 11 cluster Ðelds. These are computed from the redshifts reported in Tables 2È12, and do not include redshifts from the literature. We used the standard formalism of Danese, DeZotti, & di Tullio (1980). We have also computed biweight ÏÏ estimators of central location, C, and scale, S, for some of the clusters. These quantities are bi robust measures bi of the sample median velocity and dispersion advocated by Beers, Flynn, & Gebhardt (1990), and generally do a much better job of estimating these quantities in the face of non-gaussian distributions or distributions with many velocity outliers.ïï Mean velocities and central locations are reported as observed heliocentric velocities, cz, while velocity dispersions and scales have been computed from these velocities after making corrections for cosmological e ects and measurement errors. In order to determine cluster membership, the Yahil & Vidal (1977) 3p clipping ÏÏ technique is used to eliminate velocity outliers. In some cases, this technique is arguably too aggressive at removing galaxies at the extremes of the distribution. In these cases, the robust measure, S, will provide a more representative value of scale. bi A detailed analysis of the kinematics of these 11 clusters, including additional redshifts from the literature and a summary of the full cd cluster survey, is being prepared by Oegerle & Hill (1998) as Paper IV of this series A779 Redshifts for galaxies in A779 have been published by a number of groups, including Zabludo, Huchra, & Geller (1990) and Ramella et al. (1995). We report here observations of 81 galaxies, yielding 54 new redshifts in the Ðeld. The mean heliocentric velocity of the cluster is 6869 ^ 51 km s~1, and the velocity dispersion corrected for measurement errors is 339 `41 km s~1. The robust scale, S \ 465 ~30 bi km s~1, however, indicates a larger dispersion. We see velocity evidence for two other clusters in the background with mean heliocentric velocities of 14,501 and 17,869 km s~ A1691 Only the redshift of the cd galaxy had previously been observed in this cluster. Of the 80 redshifts we obtained, 69 of the galaxies were cluster members. The mean heliocentric velocity of the cluster is 21,614 ^ 98 km s~1, and the velocity dispersion corrected for measurement errors is 756 `74 km s~1. ~ A1749 Only three redshifts were previously known in A1749. Sixty-seven observations with MX increase the number of known cluster members to 52. The mean heliocentric velocity of the cluster from the MX observations is 17,143 ^ 162 km s~1, and the velocity dispersion corrected for measurement errors is 1050 `126 km s~1. In this case, the biweight estimators do a better ~93 job of rejecting the outliers and give a location of 16,776 km s~1 and a scale corrected for measurement errors of 794 km s~1.

5 No. 4, 1998 DYNAMICS OF cd CLUSTERS. III FIG. 3.ÈHistograms of radial velocities for galaxies in the Ðelds of each cluster. The bin size is 250 km s~1. These histograms include only the velocities reported in this paper A1767 Hintzen et al. (1982) have published 17 redshifts in the region of A1767. Our observations of 61 galaxies repeat all but one of these, and include 58 cluster members. The mean heliocentric velocity of the cluster is 21,069 ^ 121 km s~1, and the velocity dispersion corrected for measurement errors is 849 `92 km s~1. A1767 has a striking lack of emission-line galaxies, ~70 compared with the other clusters A1837 Zabludo et al. (1993) have published 26 redshifts in the region of A1837. Our observations repeat nine of these and add 38 new redshifts. The mean heliocentric velocity of the cluster from the MX data is 20,933 ^ 124 km s~1, and the velocity dispersion corrected for measurement errors is 624 `101 km s~1. The 3p clipping ÏÏ has removed several ~68 galaxies at the extremes of the velocity distribution. The biweight estimators give a location of 20,908 km s~1 and a scale corrected for measurement errors of 780 km s~1. A1837 has another cluster in the foreground, referred to as A1837A by Zabludo et al. (1993), with a mean heliocentric velocity of 11,046 km s~ A1927 Only half a dozen redshifts in the vicinity of A1927 were previously available in the literature. All but one of our 65 observations represent new velocities. The mean heliocentric velocity of the cluster is 28,385 ^ 95 km s~1, and the velocity dispersion corrected for measurement errors is 563 `72 km s~1. The biweight estimators give a location of ~52 28,391 km s~1 and a scale of 705 km s~1. A1927 has another cluster, AWM3, in the near foreground with a

6 TABLE 2 A779 REDSHIFT DATA ] cd; n \ 3; NGC ] ] MK ] ] E; j3727, Ha, j ] E; Hb, j5007, Ha, j ] j3727; NM ] E; j3727, j5007; NM ] ] ] ] ] NGC ] ] ] ] NM ] NM ] NM ] E; j3727, Hb, j5007, Ha, j6583, j ] ] NGC ] ] ] ] ] NGC ] NGC ] NGC ] E; j3727,ha ] NM ] ] NGC ] NM ] ] j3727, Ha, j6583, j ] Ha, j ] ] ] ] ] ] NGC ] NGC ] NGC ] ] NM ] ] E; Ha ] E; j3727, Ha ] ] ] ] ] ] ] NM ] NM ] NM ] ] NM ] ] ] ] NM ] NM ] NM ] NM ] NM ] NM ] E; j3727, j5007, Ha; background ] ] j3727, Ha, j6583; NM ] ] NM ] ] ] Ha, j ] A; j3727, Hb, j4959, j5007, Ha, j6583, j6717; NGC ] ] NM NOTE.ÈUnits of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds. TABLE 3 A1691 REDSHIFT DATA ] cd; n \ ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] j ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] E; j3727; NM ] NM ] ] ] j3727, Ha, j6583; NM ] Ha, j6583; NM ] ] ] ] ] NM ] ] NM ] ] ] j3727, Hb; NM ] ] ] ] E; j3727, Hb, j ] ] NM ] ] NM ] ] ] NM ] ] NM ] ] ] ] ] ] ] ] ] ] ]

7 DYNAMICS OF cd CLUSTERS. III TABLE 4 A1749 REDSHIFT DATA ] cd; n \ ] j3727, Hb, Ha ] ] NM ] ] ] ] NM ] j3727, Hb; NM ] ] NM ] NM ] E; j3727, Hb, j ] ] ] ] j3727, Hb ] j3727, Hb, j ] j3727, Hb, j ] ] ] ] E; j3727, Hb ] ] ] E; j3727, j ] ] ] ] ] j3727, Hb ] j3727; NM ] ] ] ] ] ] E; j3727; NM ] ] ] ] ] NM ] j3727, j ] Hb; NM ] ] ] NM ] ] ] NM ] ] ] Ha ] ] NM ] E; j3727, Hb, j ] ] ] NM ] NM ] ] NM ] E; j3727, Hb, j5007; NM ] ] ] TABLE 5 A1767 REDSHIFT DATA R.A. Decl ] cd; n \ ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] NM ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] ] NM ] ] ] ] ] ] ] ] ] ] ] ] ] NM ] ] ] ] ] ] ] ] ] ] ] ] ] A mean heliocentric velocity of 4423 km s~1. Now that we have a reliable mean velocity for A1927, it turns out to be slightly beyond the redshift limit of our original cluster sample deðned by Hill & Oegerle (1993) A2067 In their survey of the Corona Borealis region, Postman, Huchra, & Geller (1986) and Postman, Geller, & Huchra (1988) observed a few dozen galaxies in the area around A2067 and A2061. Our 85 observations in A2067/A2061 repeat all but 16 of those, bringing the total number of measured redshifts to 101 (of which 70 are members of A2067 or A2061). The mean heliocentric velocity of the combined clusters in our Ðeld based on the MX observations is 23,056 ^ 119 km s~1, and the velocity dispersion corrected for measurement errors is 853 `89 km s~1. Our ~68

8 1536 HILL & OEGERLE TABLE 6 A1837 REDSHIFT DATA a [ cd; n \ 3; ZHGV [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ [ j [ ZHGV [ [ [ ZHGV [ [ ZHGV [ E; j3727, j4959, j5007; ZHGV [ [ [ [ [ [ [ E; Ha, j6583; ZHGV 1AIZ [ ZHGV [ ZHGV [ [ Ha, j6583, j [ [ [ [ [ [ [ ZHGV [ a (ZHGV) Zabludo et al table of velocities certainly does include many galaxies from A2061. The velocity dispersion of A2067 alone appears to be signiðcantly smaller than for the combined clusters. This Ðeld also contains a foreground group at 9360 km s~1 and a background cluster, A2067B, with 22 members at central location 33,980 km s~1 with a scale of 716 km s~ A2079 Our 75 redshift measurements in A2079 double the number of redshifts from the Corona Borealis survey by Postman et al. (1986), and we repeat all but one of their measurements. We Ðnd 62 cluster members in the MX data, with a mean heliocentric velocity of 19,832 ^ 94 km s~1 and a velocity dispersion corrected for measurement errors of 680 `71 km s~1. ~ A2089 Our 61 redshift measurements repeat all but two of the 10 galaxies observed in A2089 by Postman et al. (1986). We TABLE 7 A1927 REDSHIFT DATA ] cd; n \ ] ] ] ] NM ] ] ] ] ] ] ] ] ] ] NM ] NM ] ] ] j3727, Hb, j4959, j5007, Ha, j6583; NM ] ] ] Ha, j6583; NM ] ] ] NM ] ] ] ] ] ] j3727, Hb, j4959, j5007, Ha, j6583; NM ] NM ] NM ] ] E; j3727, Hb ] ] j3727, Hb ] ] NM ] ] NM ] ] NM ] ] j3727, j ] j3727, j4959, j ] j3727, j ] ] ] j ] NM ] ] j3727, j4959, j ] ] ] ] ] NM ] Ha; NM ] ] NM ] ] ] ] Ðnd that 45 of our measured galaxies are cluster members. The mean heliocentric velocity of the cluster is 22,066 ^ 79 km s~1, and the velocity dispersion corrected for measurement errors is 485 `61 km s~1. The biweight estimator of scale, S \ 630 km ~45 s~1, indicates a larger dispersion. There bi may be a slight overlap with the outer parts of A2079, which lies 1.3 away.

9 TABLE 8 A2067/A2061 REDSHIFT DATA a ] cd; n \ 6; PGH ] PGH ] j3727; PGH ] PGH ] ] PGH ] ] NM; PGH ] NM ] NM ] ] PGH ] ] NM ] NM ] ] j ] ] PGH ] j3727; NM; PGH ] NM ] NM ] A; NM ] Hb, j ] ] NM ] ] ] NM ] ] j3727, Hb, j ] PHG N ] NM; PHG N ] ] ] PHG N ] ] ] NM ] ] ] NM ] A; j3727, Hb; NM ] ] PGH ] PGH ] ] PGH ] ] ] NM; PHG N ] NM; PHG N ] j3727, Hb, j5007; NM ] NM; PGH ] NM ] ] ] ] ] PHG N ] ] PHG N ] ] ] PHG N ] NM; PHG N ] ] ] NM ] ] ] PHG S ] PHG S ] PHG S ] PHG S ] NM ] ] ] ] ] ] ] ] ] TABLE 9 A2079 REDSHIFT DATA a ] cd; n \ 5; PHG ] PHG ] PHG ] ] ] PHG ] A; PHG ] PHG ] E; j3727, Hb ] ] ] PHG ] NM; PHG ] PHG ] ] ] ] PHG ] ] ] NM; IC 4547, PHG ] PHG ] ] PGH ] ] ] ] ] j3727, j ] ] j3727, j5007; PHG ] PHG ] ] PHG ] PHG ] PHG ] NM; PHG ] ] NM ] PHG ] Hb, Ha, j6583; NM; IC 4546, PHG ] PHG ] PHG ] NM ] ] PHG ] NM ] ] PHG ] ] PHG ] j3727, Hb ] ] ] NM ] NM; PHG ] j3727, Hb, j4958, j ] ] NM ] ] PHG ] ] ] PHG ] PHG ] PHG ] ] PHG ] ] PHG ] ] NM ] j3727, Hb, j ] NM ] a (PHG) Huchra, & Geller (PGH) Geller, & Postman, 1986; Postman, Huchra a (PGH) Postman, Geller, & Huchra 1988; (PHG) Postman, Huchra, & Geller 1986.

10 1538 HILL & OEGERLE Vol. 116 TABLE 10 A2089 REDSHIFT DATA a ] cd; n \ 5; PHG ] ] ] PGH ] ] ] ] PGH ] ] PHG ] PGH ] PGH ] PHG ] NM ] ] NM ] NM ] PGH ] ] PGH ] PGH ] PGH ] E; j3727, Ha; NM ] E; j3727, Hb, j ] PHG ] ] PHG ] ] NM ] ] Ha; NM; PHG ] ] ] ] PGH ] ] PGH ] ] NM; PGH ] PHG ] ] ] ] ] NM ] j ] NM ] NM ] PHG ] ] ] NM ] ] PHG ] ] NM ] ] ] ] ] NM a (PHG) Postman, Huchra, & Geller 1986; (PGH) Postman, Geller, & Huchra A2199 Minkowski (1961), Ti t (1974), and Gregory & Thompson (1984) have published 136 redshifts in the region of A2199 and A2197. Where those observations overlap with our own, the Rood-Sastry identiðcation numbers are included in Table 10. As discussed by Gregory & Thompson (1984), A2197 lies 1.3 north of A2199. Our 98 MX observations in the area traditionally deðned as A2199 bring the total number of redshifts in that cluster to 210, of TABLE 11 A2199 REDSHIFT DATA ] cd; n \ 3; j3727, Hb, j5007, Ha, j6583; NGC 6166, RS ] NGC 6166 NE ] ] ] ] ] ] Ha, j ] ] ] j3727, Hb, j5007, Ha, j6583; RS ] ] RS ] ] ] ] j3727, Ha, j6583; IR ] j3727, Ha, j ] ] j3727, Hb, j4959, j5007, Ha, j6583, j6717; RS ] ] RS ] RS ] ] RS ] ] NM ] RS ] E; j3727, Hb, j5007, Ha, j ] RS ] ] RS ] ] RS ] RS ] RS ] NM ] RS ] RS ] ] RS ] ] ] RS ] RS ] RS ] Ha, j6583; NGC 6166B, RS ] RS ] ] ] ] ] ] RS ] ] ] RS ] ] ] M ] ] ] NM ] ] ] ] j6583?; RS ] ] NM ] NM ] ]