NASA Goddard Space Flight Center
Richard Mushotzky
Laboratory for High Energy Astrophysics, Goddard Space Flight Center Greenbelt MD 20771
Abstract
Recent major advances in x-ray imaging and spectroscopy of clusters have allowed the determination of their mass and mass profile out to ~1/2 the virial radius. In rich clusters most of the baryonic mass is in the gas phase and the ratio of mass in gas/stars varies by a factor of 2-4. The baryonic fractions vary by a factor of ~3 from cluster to cluster and almost always exceed 0.09h50-3/2 and thus are in fundamental conflict with the assumption of [Omega]=1 and the results of big bang nucleosynthesis. The derived Fe abundances are 0.2-0.45 solar while the abundances of O and Si for low redshift systems are 0.6-1.0 solar. This distribution is consistent with an origin in pure type II supernova. The amount of light and energy produced by these supernovae is very large, indicating their importance in influencing the formation of clusters and galaxies. The lack of evolution of Fe to a redshift of z~0.4 argues for very early enrichment of the cluster gas. Groups show a wide range of abundances, 0.1-0.5 solar. The results of an x-ray survey indicate that the contribution of groups to the mass density of the universe is likely to be larger than 0.1h50-2. Many of the very poor groups have large x-ray halos and are filled with small galaxies whose velocity dispersion is a good match to the x-ray temperatures.
I. Introduction
A. Observational Status
X-ray observations of groups and clusters of galaxies have matured rapidly in the last 6 years with the advent of good quality imaging with Rosat and moderate quality spectra with ASCA. We now have 100's of high quality x-ray images and ~150 high signal to noise x-ray spectra.
With the present level of data one can reliably determine the abundances of O, Ne, Si, S and Fe in ~20-30 clusters and a few groups, the temperature structure in ~20-30 clusters and a few groups, and the average temperature and Fe abundances for >> 100 clusters and ten's of groups.
"Large" samples (~20-30) of z>0.2 clusters are now available with images, temperatures and Fe abundances. Groups at z~0.2 are being found in deep Rosat fields. Large solid angle surveys, based on Rosat serendipitous surveys are finding numerous cluster candidates in a reliable uniform fashion (1) out to redshifts >0.6.
The luminosity function of rich clusters has been determined at z<0.3 (2) and limits on it at z<0.8 exist (3). The first estimate of the luminosity function of groups at z=0 has also been made (4,5). Progress in the next few years will be rapid as the large ASCA and Rosat archives are analyzed and AXAF, XMM and Astro-E, which have considerably larger collecting area, better angular resolution and improved energy resolution, are launched.
B. Clusters as Cosmological Probes
Clusters are thought to be "fair samples" of the universe-i.e. they represent such a large perturbation (~10 Mpc co-moving volume) that their content should be representative of the universe as a whole. Under this assumption studies of their mass and their baryon fraction should reveal the "gross" properties of the universe as a whole, such as its baryonic fraction and total mass density. Because their dynamical timescales are not much shorter than the age of the universe, clusters should retain an imprint of how they were formed and thus studies of their evolution, temperature and luminosity function should place strong constraints on all theories of large scale structure. Unlike galaxies, which are certainly open systems, rich clusters probably retain all the enriched material that was created in their pre-collapse co-moving volume. Thus studies of their chemical abundances and its evolution should provide fundamental data for the study of the formation of the elements and provide a history of nucleosynthesis in the universe.
II. Mass Distribution and Dark Matter
It has long been known (6) that x-ray imaging spectroscopy of relaxed systems can allow a determination of their total mass. In order to use the data in a straightforward fashion, we make the fundamental assumptions that hydrostatic equilibrium holds and that the only significant source of pressure in the gas is thermal pressure. While this is clearly simplistic, it seems to hold well at roughly the 10-20% level in detailed numerical hydrodynamic simulations. In order to minimize the possible non-equilibrium effects one must consider the dynamical state of the cluster. A fairly large fraction of clusters, 30-70%, appear to be involved in a merger at the present epoch. The indications of this are a highly structured x-ray image, and/or non-azimuthal temperature variations and/or a highly non-Gaussian galaxy velocity field. After rejecting these objects from our sample, we have excluded, at least in projection, those objects for which are simple assumptions may not hold.
Then for a spherical system the enclosed mass is
M(<r) = kT(r)r/GumH {(dlog [rho]/d log r) +(dlog T/d log r)}
The detailed analysis of cluster mass using the equation of hydrostatic equilibrium has been done for ~10 objects out to ~1/2 of the "virial" radius, by several groups, with rather similar results. Theoretical analysis of this method (7) indicates that the mass derived is unbiased and that the intrinsic spread of the x-ray derived mass to the true mass is <30% (cf. 8, 9 ).
A. General results:
The derived masses are independent of the assumed form of the potential. That is the measured temperature profile has such small statistical errors that all potentials which give the observed temperature profile have the same enclosed mass (10). Of course, these models can disagree in the regime where there are no data. For ASCA with its angular resolution of ~2' and 18' effective field of view there are very few systems in which the mass within 100h50 kpc or beyond 1.5 h50 Mpc are well constrained. The fraction of the mass that is baryonic, fb, (that is the sum of the gas mass and the galaxy mass with an assumed M/Lv~5) ranges from 0.09-0.25 and may be a weak function of the total mass (11), in the sense that most of the low baryonic fraction clusters have relatively low ( <4x1014 M0) total masses. In an encouraging agreement of theory with observation, the derived x-ray masses are in excellent agreement with the scaling relation of Evrard, Metzler and Navarro (7), with a mean ratio of data/theory of 0.87+/-0.14.
Clearly, this high baryonic fraction disagrees with big bang nucleosynthesis and [Omega]=1 and with many simulations of cluster formation and evolution. Analysis of the x-ray derived ratio of baryonic mass to dark matter inside a cluster allows an increase in fb with radius, but at radii less than 1 Mpc this is not required. Recent studies of clusters at larger scales (12) shows than most clusters have a decreasing temperature at radii > 1/4 of the virial radius. While this is not fully understood it arises naturally in low [Omega] simulations and in simulations with large initial injections of thermal energy (reference 7, fig 5).
As first shown by David, Jones and Forman 1994 (11) the "average" M/L derived from x-ray imaging mass estimates is M/L ~150h50 with a fairly wide range. There exists a wide range in the ratio of gas mass to stellar mass as can be seen clearly in Forman and Jones 1994 (13). It is not clear how much of the apparent factor of ~6 range in gas to stellar mass is due to to a lack of published accurate optical photometry for low redshift clusters. Whether this ratio is a monotonic function of mass or has an intrinsic wide scatter is not yet clear, but it seems as if more massive clusters tend to have a higher ratio of gas to stellar mass (11). However, there are some objects, such as a Abell 1060 and Abell 1204, which have the same optical richness and x-ray temperature but a factor 30 difference in x-ray luminosity. This may indicate that much of the observed range in gas to stellar mass is due to "cosmic" scatter rather than a trend.
B. Comparison of results with other methods
i) Optical velocity dispersion:
The x-ray temperature agrees extremely well (on average) with the optical velocity dispersion ([beta]=ump[sigma]2/kT ~1) (14)- however there is a real variance in the distribution (Figure 1a,Figure 1b). This excellent correlation indicates that, to first order, both the gas and the galaxies are in the same potential, that there are not large radial gradients or anisotropies in the galaxies velocity tensor and that the virial theorem is not a strongly biased estimator of the mass (15). However, detailed comparison of viral mass estimates (16) and x-ray mass estimates shows a range of ~2 as expected from the use of the viral theorem (15). In a few clusters with published optical velocity dispersion profiles it is possible to perform a comparison of the predicted velocity dispersion profile with the x-ray determined mass profile, under the assumption of isotropic orbits and the agreement is good.
The <M/L> from the x-ray technique agrees on average with that from virial analysis (12, 16). This is essentially a restatement of the agreement of x-ray temperature and optical velocity dispersion, combined with the roughly isothermal nature of the temperature and velocity dispersion profiles. However, there are clearly outliers (e.g Abell 1689) in which the virial theorm mass is much larger than the x-ray value. This is presumably due to the effects of mergers which can result in "non-virial" galaxy velocities and deviations from hydrostatic equilibrium in the gas .
ii) Comparison with gravitational lensing results:
There is good agreement (better than 30%) in the derived mass from x-ray and strong and weak lensing measurements for ~1/2 of the sample (e.g. PKS 0745 (17), A2390 Bohringer et al 1997 in preparation), but for ~1/2 of the sample the lens mass is significantly greater than the x-ray mass. The sign of the disagreement is consistent with simulations (8, 9) which show that the lensing mass is biased high compared to the true mass because of the spatial correlation of mass and the x-ray estimate is biased slightly low due to incomplete thermalization of shocks and the neglect of turbulence. Specifically, since the lens mass is a measure of the total surface mass density in the line of sight, it necessarily includes the mass of the smaller clusters and groups which lie in the foreground and background of the cluster while the x-ray mass estimate is strongly biased to just the cluster itself. As one goes to smaller mass scales than that of rich clusters, the gravitational lens mass is more biased.
iii) Sunyaev-Zeldovich effect:
As shown in detail by Carlstrom (18) and Myers et al. (19) the Sunyaev-Zeldovich (S-Z) effect measurements derive the same gas surface density (if H0< 70 km/sec/Mpc) as do the x-ray measurements. Since the S-Z data measure, primarily, the path integral of the pressure, while the x-rays measure the projected emission integral and temperature, this consistency indicates that the gas is neither highly clumped nor has an "odd" geometry and that the x-ray gas mass estimates are robust. While these data do not confirm the x-ray total mass estimates, they strongly support the assumptions involved in the analysis.
iv) Possible problems- Other sources of pressure:
While cosmic rays, magnetic fields, and turbulence could potentially, make a major additional contribution to the total pressure, they have not been directly measured. The effects of magnetic fields have been considered in detail by Steigman and Felten (20) and are thought to be rather small. However, it is well known (21), that in the centers of "cooling flow" clusters magnetic fields are important contributors to the total pressure. Turbulence has not been measured in the outer regions of rich clusters, but in the central regions measurements of the velocity field of the optical filaments in cooling flow clusters indicate that turbulence contributes <30% of the total pressure. Theoretical high resolution models of cluster collisions show that after several gigayears the contribution of turbulence to the total pressure should be small (22). Future high resolution x-ray spectroscopy with Astro-E will be able to directly measure the velocity field of the gas and thus determine whether turbulence is a major contributor to the total pressure.
C. Conclusions
Our data are in agreement with the Carlberg et al (16) scenario in which a low [Omega] cosmology can describe the overall cluster data. That is, the cluster determined baryonic fraction is not consistent with a closed universe and the big bang nucleosynthesis determined baryonic fraction, nor is the cluster M/L consistent with closure density. However the variation in baryonic fraction in moderate mass clusters argues that additional physics other than pure gravity should be included in our modeling of cluster formation and evolution. One strong candidate for this additional physics is heating due to cluster winds at an early epoch (23). It is also possible that the variation in baryonic fraction could be due to cluster mergers at high mach number (24), however the occurrence rate for this is a strong function of the cosmological model.
III Abundances and Implications for Origin of Structure
The ASCA spectra for most rich clusters are consistent with a non-solar abundance and ratio for the ratio of (O, Ne and Si) to Fe ( 25, 26, 27 ). The median ratio of Si/Fe is 2.2+/-0.25 solar. and the mean Fe abundance is 0.28 solar. These data are consistent with a "pure" type II supernova origin for all of the heavy elements (23). However, this conclusion is sensitive to stellar models and it is possible that ~1/2 of the Fe was made in type I supernovae (28, 29). What is robust is that most of metals are created in type II supernova even if 50% of the Fe is due to type Is.
The mass in metals is correlated with the light in elliptical galaxies (30). However, there is a factor of 4 range in the ratio of light to metal mass, as is seen most clearly in the detailed studies of Abell 1060 and AWM 7 (10). There is also true variation in the metallicity from cluster to cluster of about a factor of 2 (31). While some clusters have abundance gradients or structure (26) they occur in less than 1/3 of rich low redshift clusters and are often confined to the central regions. Figure 3 shows the extremely strong correlation of x-ray luminosity and temperature (32). The highest metallicity is correlated with the "excess" luminosity in the L(x) vs kT correlation (33). In standard theory the temperature determines the mass of the system; this means that the clusters which are the most x-ray luminous for a given total mass have the highest abundances.
With ASCA one can reasonably sample the evolution of the cluster Fe abundance out to z~0.5 (32) (Figure 2). There has been no discernible change in either the mean cluster metallicity, or its variance out to z~0.4. Recently there has been a detection (34) of a cluster at z=0.94 with "normal" Fe metallicity, perhaps extending this result to higher redshift. The lack of evolution of cluster metallicity out to z~0.4 combined with the apparent passive evolution of elliptical galaxies in clusters, indicates that the cluster metals are created at z>1.2 (however the exact epoch depends on the cosmological model ).
The x-ray spectroscopic data essentially count the total grams of silicon in the cluster so one can easily calculate the total energy in metal creation due to type II supernovae (23). The number derived is very large and is typically ~1/4 of the binding energy of the present day clusters (at T~4 keV mass scale). Since in any hierarchical universe the effective potential of a cluster was smaller at larger redshifts, if even a small fraction of this energy is thermalized, it will have a profound effect on the formation of large scale structure and galaxies. The additional heat will delay the infall of gas and change the final configuration of the system by creating a higher entropy core. In fact, recent work on semi-analytic models of galaxy formation (35, 36) have found that they must have a high feedback efficiency of supernova energy into the gas phase to account for the observed metallicity and luminosity of early type galaxies.
The implied luminosity of the early generation of galaxies was also very large (1048/[tau]8 ergs/sec/per galaxy where [tau]8 is the lifetime of the starburst in units of 108 years ). This is a rather robust calculation since it depends only on the total number of massive stars, which is fixed by the total cluster metallicity (23). Since these high luminosity z>1 objects are not seen, in general, in the optical or UV band (37) they must either be "hidden" by dust, and/or be at very high z, and/or exist as galaxy fragments each one of which must have less than 1/100 of the mass of a giant elliptical during the phase in which massive stars are forming. Based on low redshift galaxy samples, in which >>50% of the luminosity of rapidly starforming galaxies appears in the infra-red it seems as if the effects of dust could be important, while the Hubble Deep field data, indicating that high redshift galaxies are rather small, suggest that the galaxy fragment scenario is also important.
The x-ray spectroscopic data indicate that most of the visible metals in clusters ( ~50-80%) are in the hot gas. Since there seems to be little, if any, difference between the fundamental plane of field or cluster galaxies out to z~0.4 (38), the relative amount of metals retained in stars versus those "expelled" into the gas derived from the cluster data should also apply to "field" galaxies. This indicates that the mean metallicity of the universe has been underestimated by 2-4 based on galaxy data alone (a point first noted by Songaila, Cowie and Lilly (40)) and implies much more star formation than estimated by Madau et al. (39) from optical/UV galaxy data. It is amusing to note that the latest calculation of galaxy formation in a hierarchical scenario (35) uses the x-ray cluster metallicity as a fiducial value for the total production of metals and that this produces, in a "natural way", the observed properties of elliptical galaxies with redshift. Given the above scenario, the intergalactic medium (IGM) should be metal enriched at z<3, since the enriched gas expelled from galaxies in a non-cluster environment will not be bound to the system and will enter the IGM.
IV Cluster Evolution
As pointed out by N. Bahcall (41) measurement of cluster evolution is a strong test of cosmological models. Recent data from the Rosat all sky survey (2) shows that, contrary to previous reports, there is little or no evolution in the x-ray cluster luminosity function at z <0.3. Recent samples based on deeper Rosat pointed data (1,3) have found little indication of strong cluster luminosity function evolution at z<0.6. Recent analysis of ASCA spectra of high redshift clusters (42) (Figure 1, 2), shows no evidence for evolution in the relationship between x-ray temperature and luminosity or between x-ray temperature and velocity dispersion. The almost total lack of evidence for x-ray cluster evolution argues either for a low [Omega] universe and/or a physical situation in which much of the gas in the cluster core is pre-heated at moderate to high redshifts (43,44).
The overabundance of metals in "over"-luminous clusters (which are also high cooling flow rate objects) can be accounted for in a scenario (33) in which "over"-luminous clusters (the objects to the far right in Figure 3) represent high density perturbations, which collapse early. The high density manifests itself in a high x-ray luminosity and high cooling rate. The lower density perturbations form later and lose metals via winds and thus form clusters which have lower metallicity and low cooling rates. Thus in some sense cluster metallicity might be a signature of relative age.
V Groups
In a major surprise, many poor groups with only 2-4 optically bright members are fairly luminous, L(x)~1042-1043 ergs/sec, extended x-ray sources. (45). The temperature structure and metallicity of ~10 groups has been determined from ASCA and Rosat data and to first order the x-ray bright groups are isothermal out to ~15', which corresponds to 0.1-0.3 of the virial radius. The temperature of these systems cluster around 107 ûK with a rather small dispersion. The abundances vary widely from <0.1->>0.5 solar and some groups show steep abundance gradients. The existence of groups with low total metallicity combined with a low ratio of total metals to optical light argues for the expulsion of metals from the group potential via a wind or some other mechanism. There is strong tendency for the less luminous systems to have low metallicity. The X-ray luminous groups tend to be dominated by luminous (MV > -21.5) elliptical galaxies (46) and very few, if any, spiral dominated groups have luminous x-ray halos.
In a sample of 12 groups, all of the x-ray luminous (L(x)> 4x1041 ergs/sec) systems possess numerous small (MV~-17) galaxies, while the x-ray dim systems do not have such a population (47). The small galaxies have a very extended distribution and often they can be traced out beyond 200h-1 kpc.
For these 12 well measured groups the relationship between x-ray temperature and optical velocity dispersion is similar to that of clusters and thus it is likely that these are relaxed systems.
The x-ray emission from the luminous objects is truly diffuse and not dominated by emission from individual galaxies, however, in some lower luminosity systems emission from individual galaxies is important (46).
The temperature, optical velocity dispersion and x-ray image data from this limited sample, combined with the much larger number of studied objects (45,46) argue that many of the groups are relaxed and that the dark matter distribution for many of the groups is extended over R > 200 kpc. This is confirmed by the dwarf galaxy distribution in the Zadludoff and Mulchaey sample (47).
X-ray luminous groups are very common (~10-2h5/Mpc3 at L(x)~1042 ) in a high surface brightness limited survey (4). Using the scaling relations from numerical work (7) and the independent confirmation of this law from the x-ray data itself, the typical mass inside ~200 kpc is ~2x1013 M0h50-2. Using the Burns et al luminosity function (4), a conversion from luminosity to temperature using the L(x) vs kT relation gives a trivial estimate of the minimum mass in these systems relative to the closure density of [Omega]groups ~ 0.06 Ah2 where A is the correction for mass inside 200kpc to the total mass (A~5). The preliminary all sky survey results, upon which the Burns et al paper is based, certainly miss many massive systems (45) and thus these limits on the mass density of the universe contributed by x-ray emitting groups are conservative.
The mean baryonic fraction in groups is not yet accurately known, but for many of them it is ~10%- with a wide range of M(gas)/M(star). Thus the x-ray luminous groups may contain most of the visible mass in the universe.
VI Conclusion
The lack of evolution in cluster properties (abundance, luminosity function, L vs T) combined with the type II SN origin of the metals argues for the very strong influence of non-gravitational processes in structure formation and/or a low value of [Omega]. The high baryon fraction in clusters alone is the strongest argument for a low [Omega]. The "low" M/L for clusters (~150) and the observed number density of clusters also argues for a low [Omega]. However, the evidence for the importance of heat in the early universe indicates that most simulations have not included important physics for cluster and galaxy formation.
The quality of the x-ray data will improve markedly in the next few years with the next generation of instruments on AXAF,XMM and ASTRO-E. I anticipate that the next NAS meeting on this subject will be equally exciting.
Acknowledgments : I would like to thank my collaborators at GSFC and on the ASCA team, especially Michael Loewenstein, Caleb Scharf, Keith Arnaud, John Mulchaey, Dave Davis, Yasuo Tanaka and Una Hwang, whose hard work have contributed to the results presented in this paper.
References
1. Scharf, C, Jones, L., Ebeling, H., Perlman, E., Malkan,M. and Wegner, G. 1997 ApJ. 477 79-92
2. Ebeling, H., Edge, A., Fabian, A., Allen, S., Crawford, C and Boehringer, H. 1997 ApJ Lett 479 L 101-104
3. Collins, C., Burke, D., Romer, A,.K., Sharples, R., Nichol, R. 1997 ApJ Lett in press
4. Burns, J., Ledlow, M., Loken, C., Klypin, A., Voges,W., Bryan, G., Norman, N. and White, R. 1997 Ap.J. Lett. 467 49-52
5. Henry, J.P., Gioia,I., Huchra,J., Burg, R., McLean,B., Bohringer,H., Bower, R., Briel, U., Voges, W., MacGillivray, H. and Cruddace, R. 1995 Ap.J. 449,422-430
6. Fabricant, D., Lecar, M and Gorenstein, P. 1980 ApJ. 241,552-560
7. Evrard, G., Metzler, C. and Navarro, J. 1996 ApJ. 469 494-507
8. Bartelmann, M. and Steinmetz, M. 1996 MNRAS 283 431-446
9. Cen, R. 1997 ApJ in press
10. Loewenstein, M. and Mushotzky, R. 1996 ApJ Lett. 471 83-86
11. David, L., Jones, C. and Forman, W. 1995 ApJ 473, 692-706
12. Markevitch, M. 1996 ApJ Lett 465 1-4
13. Forman, W. and Jones, C., 1994 in "Cosmological Aspect of X-ray Clusters of Galaxies" ed. W.C. Seitter pg 38
14. Bahcall, N. and Lubin, L. 1994 ApJ 426, 513-515
15. Heiseler, J., Tremaine, S. and Bahcall, J. 1985 ApJ 298 8-17
16. Carlberg, R., Yee, H., Ellingson, E., Abraham, R., Gravel,P. Morris, S. and Pritchet, C. 1996 ApJ 462, 32- 49
17. Allen, S., Fabian, A. and Kneib, J 1996 MNRAS 279, 615-635
18. Carlstrom, J. 1997 these proceedings
19. Myers, S., Baker,J., Readhead, A., Leithch,E. and Herbig,T. 1997 ApJ in press
20. Steigman, G. and Felten, J. 1995 SSR 74 245-258
21. Ge, J and Owen, F. 1994 AJ 108, 1523-1533
22. Roettiger, K., Stone, J. and Mushotzky, R. 1997 ApJ in press
23. Loewenstein, M. and Mushotzky, R. 1996 ApJ 466, 695-703
24. Cen, R. and Ostriker, J. 1994 Ap.J,. 429 4-21
25. Mushotzky, R., Loewenstein, M., Arnaud, K., Tamura, T. Fukazawa,Y., Matsushita, K., Kikuchi,K. and Hatsukade, I. 1996 ApJ 466 686-694
26. Fukazawa,Y. Tamura, T., Ezawa, H., Makishima, K., Kikuchi, K., Ohashi, T., Ikebe, Y. and Tsuru,T. 1997 in X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas pg 101-102 ed F. Makino, K Mitsuda. Universal Academy Press Tokyo
27. Hatsukade, I., Kawabata,K. Takenaka, K. and Ishisaka, J. 1997 in X-ray Imaging and Spectroscopy of Cosmic Hot Plasmas pg 105-106 ed F. Makino, K Mitsuda. Universal Academy Press Tokyo
28. Gibson, B., Loewenstein, M. and Mushotzky, R. 1997 MNRAS submitted
29. Ishimaru, Y. and Arimoto, N 1997 PASJ 49 1-8
30 Arnaud, M. Rothenflug, R., Boulade, O. Vigroux, L. and Bangioni-Flan, E.
A&A 254,49-64
31. Fabian,A., Crawford,C. Edge,A. and Mushotzky, R.1994 MNRAS 267 779-784
32. Mushotzky, R. and Loewenstein, M. 1997 Ap.J. Lett in press
33. Scharf, C. and Mushotzky, R. 1997 ApJ. submitted
34. Hattori, M. Ikeve, Y., Asaoi,A.,I., Takeshima,T. Bohringer, H. Mihara,T. Neumann, D. Schindler, S., Tsuru, T. and Tamura,, T. 1997 Nature submitted
35. Kauffmann, G. and Charlot, S. 1997 MNRAS in press
36 Baugh, C.M., Cole, S. Frenk, C. 1996 MNRAS 283, 1361-1378
37. Steidel, C. 1997 these proceedings
38. Schade, D. Carlberg,R. Yee,H., Lopez-Cruz, O. and Ellingson,.E. 1996 ApJ Lett. 464 63-66
39. Madau, P., Ferguson, H., Dickinson, M., Giavalisco, M., Steidel, C. and Fruchter, A. 1997 MNRAS 283 1388-1404
40. Songaila,A., Cowie, L. and Lilly, S. 1990 ApJ 348, 371-377
41. Bahcall, N. 1997 these proceedings
42. Mushotzky, R. and Scharf, C. 1997 Ap.J. Lett in press
43. Kaiser, N. 1991 ApJ 383,104-111
44. Bower, R. 1997 MNRAS in press
45. Mulchaey,J., Davis,D. Mushotzky,R. and Burstein,D. 1996 ApJ 456, 80-97
46. Ponman, T., Bourner,P. Ebeling, H. and Bohringer, H. 1996 MNRAS 690-708
47. Zabludoff, A. and Mulchaey, J. 1997 ApJ submitted
1a) Optical velocity dispersion compared to emission weighted average x-ray temperature for a large sample of low and high (z.>0.14) redshift clusters. The solid line is not a fit to the data but the expectation if the x-ray temperature and the cluster galaxy velocity dispersion were equal. Note the scatter and the appearance of a few objects with much higher velocity dispersion than expected from the x-ray temperature. These 2 clusters are also objects with strong gravitational arcs.
1b). The distribution of [beta]=ump[sigma]2/kT for a large sample of well measured clusters. The mean value =1 and the variance is real. This indicates that, while on average the cluster gas and galaxies have the same "temperature" there is a real variation due presumably to cluster mergers, non-virialization temperature and velocity dispersion gradients and foreground/background projection effects.
2) Average iron abundance vs redshift for the entire sample of published objects in the literature. There is no evidence for variation in the Fe abundance with redshift but there is real variation from object to object. The errors bars are 90% confidence. The low redshift data were obtained by the Ginga satellites non-imaging proportional counters while the high redshift data were obtained by ASCA (reference 32)
3) Correlation of the x-ray bolometric luminosity and x-ray temperature. The very strong correlation, of the form kT~L0.3, does not evolve with redshift, but has an intrinsic dispersion of ~3 in luminosity at a fixed temperature.
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