AY202a Galaxies & Dynamics Lecture 17: Galaxy Groups & Clusters continued

1. AY202a Galaxies & DynamicsLecture 17:Galaxy Groups & Clusterscontinued

2. And V = |V1 - V2| < Vlim(V1,V2,m1,m2) with two choices, either fix V or scale it as D. Then select Dlim and Vlim as needed for the sample you have.  RSA Sample

3. 2dF 2PIGS

4. 2MRS Sample (raw)

5. 2MRS Sample (filled)

6. 2MRS Selection Function

7. 2MRS Group Selection Number of groups found f

8. 2MRS Groups

9. / =12 80 3 largest 2MRS Groups Virgo, Fornax/Eridanus, Perseus-Pisces

10. 2MRS Group Mass Function

11. 2MASS Galaxy Groups δρ/ρ = 12 δρ/ρ = 80 ------------------------------------------------------- σP (km/s) 197 183 RPV (Mpc) 1.71 0.97 log MV/LK 1.70 1.53 Log MP/LK 1.90 1.67 ΩM,V 0.14+/-0.02 0.10+/-0.02 ΩM,P 0.23+/-0.03 0.13+/-0.02 -------------------------------------------------------- V=Virial Estimator P = Projected Mass

12. # Density versus redshift for various group surveys:

13. Cluster Classification Just like galaxies, clusters classified morphologically. Overall Compact Medium Compact Open Linear Bautz Morgan classes I, I-II, II, II-III, III based on the ratio between the brightness of 1st and rest I -- single central cD galaxy c.f. A2029 II -- intermediate III -- no dominant cluster galaxy c.f. Hercules

14. Rood-Sastry cD -- like BM I types B -- Binary c.f. Coma L -- Linear C -- Core Compact F -- Flat I -- Irregular Tuning Forks Rood-Sastry cD -- B Struble & Rood I -- F B -- cD L -- F C -- I L C

16. Sky Distribution of Abell Clusters 0.033 < z < 0.83

17. Optical Substructure (Geller & Beers ’82)

18. Cluster Morphology Irregular A1367 A262 Regular A2256 A85 (Jones & Forman ’84)

19. A2029 A2142 Hydra

20. Perrseus A. Fabian

21. Physics of Galaxy Clusters To 0th order, assume spherical, decreasing density from the center. If n(r) is the 3-D number density, the projected density, N(R), is N(R) =  n[(R2+z2)½ ] dz = 2  where z is the coordinate along the l.o.s. and R is the projected radius ∞ -∞ r n(r) dr (r2 – R2) ½ ∞ R

22. Hydrostatic Equilibrium Good basic model for the hot gas is to assume Hydrostatic Equilibrium dPg/dr = - g GM(r)/r2 P =  where g means gas  = + differentiating the gas law  { + } = - g GM(r)/r2  M(r) = { + } kT  mp dPg dg kT g k dT dr dr mp mp dr k T dg g dT mp dr dr - rT d ln g d ln T G mpd ln r d ln r density & temperature gradients

23. You can also treat the galaxies this way, just as a “gas” of much more massive particles = gal P gal = 1/3 <v2> gal = n k Tgal  = and we can compare the gas and galaxy distributions since they are living in the same potential. dPgal GM dr r2 <v2> dPgal kTgas 1 dgas 3gal dr  mp gas dr

24. gas gal 0,gas 0,gal We can write for the relative density relations ( ) = ( ) β where β = = This is known as the Beta Model. If β = 1, gas and galaxies have the same distribution. Generally β 1 IX (r)  [ 1 + (b/rc)2 ]-3β + 1/2  mp <v2>  mp 2los 3 k T kT X-ray surface intensity and rc = optical galaxy core radius

25. Other Dynamical Quantities Crossing Time tcross ~ R/ ~ 2 x 109 yr for R=RA and H=70 Dynamical relaxation (Virialization) takes places on timescales of the crossing time, so (1) clusters are generally relaxed, and the centers of the clusters relax first Two-Body Relaxation time is long in clusters trelax ~ tcross (N / ln N) so cluster galaxies are not in “thermal” equilibrium

26. X-ray Emission Spectrum of x-ray gas is optically thin thermal bremhmmsstrahlung (free-free emission) plus emission lines

27. X-ray emission from Coma. ROSAT (left) and XMM (right). Note structure in the images.

28. 32Z2e6neni 2 3 me c3 3kT me Bremsstrahlung emissivity = ευ = ( )½ e -hυ/kT gff(T,υ) where ne and ni are the number density of electrons and ions, Z is the ion charge and gff is the Gaunt factor. Flat then exponentially decreasing. Typical x-ray temperatures are ~ 50 million degrees or kT = 5 kev For a thermal pasma of solar abundance, bremsstrahlung alone gives eff  3.0 x10-27 (T / 1K) ½ (ne / 1 cm-3)2 erg cm-3 s-1

29. When line emission is included: εtotal  6.2 x10-27 (T / 1K) ½ (ne / 1 cm-3)2 erg cm-3 s-1

30. Use X-ray features to study Chemistry (c.f. Mushotzsky)

31. A Case Study - The Virgo Cluster Assume D = 16 Mpc (HST Key Project) Zw-B(0) magnitudes 6o Core v = 716 km/s rH ~ 0.8 Mpc MP ~ 8 x 1014 M M/LB ~ 750 (M/L) But (1) substructure exists, (2) there is at least one background group contaminating at 2200 km/s (Virgo W), and (3) Spirals avoid the center and appear to be infalling.

32. Markarian’s Chain Virgo Cluster

33. Bohringer et al.

34. X-ray map with contours

35. First problem is to find where the cluster really is: JH85 from CfA survey, luminosity weighted center of all galaxies with v < 3000 km/s, m  14.5 error ~ 3’ --- iterate on sample Isopleths in the Zwicky catalog

36. Virgo Great Wall Background Cl. All known velocities in the 6 degree radius circle.

41. Spirals and Ellipticals are not in the same place in the cluster --- Spirals avoid the center.

42. Virgo Surface Density A hole around M87! How much of this is just due to the Spirals?

43. Velocity Histogram by Type E’s look Gaussian S’s are flat

44. Cluster Infall JH ‘85