1. Does Gas Cool From the Hot Phase? (onto galaxies) The MPA/ESO/MPE/USM 2007 Joint Astronomy Conference Gas Accretion and Star Formation in Galaxies Joel Bregman (Univ. of Michigan) Hot Gas in/around Ellipticals: Lessons Learned Hot Gas Environment of the Milky Way and Local Group: Limits on Accretion Missing Baryons in Galaxies and Galaxy Groups

2. Let’s Look at Galaxies with a lot of Hot Gas that is Cooling Gas masses of 1E8-1E10 Msun T = 3-8 E6 K; Lx ~ 1E41 erg/s Cooling rate of 0.1-1 Msun/yr This is known as Cooling Flows X-ray contours

3. How to Speak “Cooling Flow” Two types of hot gas situations –Hot gas in clusters of galaxies –Hot gas in early-type galaxies Clusters of Galaxies –Most of the baryons are gaseous (not galaxies) –2-10x10 7 K –Cooling: Free-Free (X-Rays) –Last Millennia: cooling rates 100-1000 Msun/yr –This Millennia: cooling rates of 1-30 Msun/yr The last Cooling Flow Meeting

4. Cooling Flow Ellipticals Most Ellipticals are not X-ray bright –Bright ones in groups/clusters (10 41 erg/s) “Lots” of hot gas (~10 9.5 Msun) Gas is bound X-rays mainly due to line emission –X-ray faint galaxies (10 40 erg/s) LMXBs + a little hot gas (~10 8 Msun) Galactic Winds Bright Ellipticals are well-studied

5. Metallicity of the Hot Gas X-Ray Observations (XMM- Newton) Fe is about Solar ([Fe] = 0) [O/Fe] = -0.3 Metallicity like stars Not like Cluster/group [Fe] = -0.5 Gas from Stellar Mass Loss Not dominated by accretion from cluster/group XMM RGS spectrum of NGC 4636 (Xu et al. 2003)

6. Does this Gas Cool? Observe OVIII (hot, ambient; 5E6 K) OVI often detected in X-ray bright galaxies –3E5 K gas; evidence for cooling from hotter gas Far Ultraviolet Spectroscopic Explorer (RIP) OVI is detected in about 40% of galaxies Some cooling gas at 3x10 5 K Cooling rates of 0.1-0.5 Msun/yr In central region; not distributed. Bregman et al. (2005)

7. Where Does The Cooled Gas Go? Es in the RSA Catalog (Hogg et al. 1990; Bregman et al. 1992) 10 4 K gas detected –Same metallicity as stars and hot gas –Not much mass (< 1E5 Msun) HI and H 2 rarely detected –M(HI) < 3E7 Msun for many ellipticals; 5% detection rate –M(H 2 ) < 2E8 Msun; 0% detected –Limits the mass of HI HVC Low levels of star formation, if present –Probably less than 0.1 Msun/yr

8. Lessons Learned From Ellipticals Ellipticals appear to have much more hot gas than Spirals (total ISM mass similar) Cooling flows in Es don’t lead to detectable masses of cooled HI (< 3E7 Msun) Not much evidence for accretion from surrounding group/cluster medium Radially distributed cooling should not occur –Local Thermal Instabilities suppressed in near- hydrostatic situations (Balbus 1995) –Even most non-linear disturbances are suppressed (Reale et al. 1991)

9. Hot Gas Around Spirals and in Galaxy Groups Stellar evolution models for the Galaxy –Need to resolve the G-dwarf problem (Z > 0.2) –Accrete 1-2 M sun /yr of gas with [Fe/H] < -3 L x = 4E40 (M dot /1M sun /yr) (T/3E6 K) erg/s Milky Way has L x ~ 10 39.3 erg/sec Other similar spirals have L x ~ 10 39.5 erg/s No obvious support for accretion with rates exceeding 0.1 M sun /yr

10. NGC 891 in X-rays Chandra ACIS-S; 108 ksec of cleaned data Point sources removed; smoothed Hot gas easily seen to a height of 4.5 kpc from disk (1.6’) Fainter emission goes to a height of 9 kpc (3’) Extent along disk similar to Halpha, FIR

11. Oosterloo et al. 2007; NGC 891 HI Chandra 0.3 keV gas; 8’ box Thermal emission; 4E39 erg/s M dot = 0.1 M sun /yr

12. Give Up The Idea Of Accreting Pristine Gas Onto MW Every Galaxy Group with good X-ray data –0.0 > [Fe/H] > -0.7 Sightlines out of the MW show OVII and OVIII in absorption (metals are present) Need to adopt a different approach to solving the G-dwarf problem –pollute the gas with metals before accretion (Binney and Merrifield; Galactic Astronomy)

13. A Census of 10 6 -10 7 K Gas in the Milky Way and Local Group Z = 0.1 Solar N = 10 19 cm -2 OVII, OVIII have X-ray resonance lines; best sensitivity Detect Hot Gas by X-ray Absorption Lines

14. Galactic Halo Model : distribution largely spherical around the MW column densities similar in all directions might see evidence for the shape of the Galaxy Local Group Model Local Group is elongated along the MW-M31 axis columns greater along this axis and especially toward M31 (the long way through the LG) Concern: M31 may have its own extended halo Discriminating Between a Galactic Halo and Local Group Model

15. Group simulation like the Local Group (Moore) shows elongation of matter. Column enhancement along major axis ~2-3x perpendicular to axis

16. 26 Target AGNs; mean EW = 22 mÅ; 17 with rms < 10 mÅ These are the 4 best. Bregman and Lloyd-Davies (2007; arXiv:0707.1699 ) Toward Bulge

17. An AGN toward M31 (long axis of Local Group) One of the smallest columns, not one of the largest Local Group Model Prediction

18. The OVII data don’t fit a Local Group Model Prediction of Local Group Model

19. A Galactic (Halo) Model Works Better Central Line Velocities close to MW

20. Correlation with Galactic ¾ keV X-Ray Background Supports a Galatic Halo Origin (10-100 kpc) Gas Mass of 10 8 – 10 10 M sun Compare to NGC 5746 (Rasmussen & Ponman 2004) : 10 9 M sun for similar metallicity

21. Other Evidence for Hot Gas In Local Group Nearby LG dwarfs have no gas but distant ones have gas (Blitz & Robishaw 2000; Grcevich et al. 2007) –Ram pressure stripping –n = 2.5E-5 cm -3 at d = 200 kpc (less than column inferred from OVII line by 4x) –1E10 M sun of gas –Cooling time longer than Hubble time

22. X-Ray Shadowing: CHVC and a Magellanic Stream Cloud This would reveal the fraction of X-ray emission beyond these clouds Help determine the hot gas component of the Local Group JNB, Birgit Otte, J. Irwin, M. Putman, E. Lloyd-Davies, C. Breuns (2007) We see a brightening, not a shadow toward both clouds. Clouds are interacting with a hot medium within 100 kpc of the MW. Density/Temp of the hot medium is model-dependent.

23. Mini-Summary There is hot gas around the Milky Way and in the Local Group –Masses are not large (0.1-10E9 M sun ) –Cooling times are long (3E8-1E10 yr) Observed Lx is consistent with only 0.05 M sun /yr of accretion onto MW (and other spirals) HVC probably not dominated by condensations from the dilute hot gas

24. When the Demons Visit at Night Where did the Baryons go? –Cosmological value is 17% –Rich Clusters have not lost their baryons –Spirals (like MW) are missing 2/3 of baryons –Galaxy groups (T < 1 keV) also missing most of their baryons within r 1000 Good News – Bad News –Lots of gas available for accretion –… but it’s nowhere in sight (unbound)

25. Make the galaxy, then blow out the baryons in a “superwind” (this must occur, but when?) –Pollutes the surroundings –Need to drive the gas way away from galaxy (to the outer parts of the groups) Other Possibility: The Gas Never Fell In –Entropy floor (preheating is 0.4 keV; 5E6K) Need about 1 SNe per 500 M sun of gas –Enrich the metals by distributed SNe (Pop III) 0.2 Solar metals is also 1 SNe per 500 M sun of gas –Naturally solves the G-dwarf problem (accrete enriched gas to make the disk) –Need to form some parts of galaxy before preheating (halo stars; dwarf galaxies) –Predict that this SNe heating occurs at z > 2 (Pop III ?) Disk is 10 Gyr old –Has a significant effect on modeling (e.g., Davé): gas supply is hot

26. How are galaxies so smart? –Tight relationship as more baryons are lost –Clever feedback/formation scheme? 5E6 K Poor Groups