Hot Gas Around Elliptical Galaxies Mike Anderson (MPA) Joel Bregman (Michigan), Xinyu Dai (Oklahoma), Massimo Gaspari (MPA), Simon White (MPA)
Outline Very brief summary of properties of hot halos! Why do ellipticals have hot halos?! Connecting hot halos in galaxies, groups, and clusters
Hot Halo Basic Properties Total X-ray luminosity Extended emission only Anderson et al. 2013 Ellipticals seem to have higher LX than spirals: because of morphology? M/L ratio? halo mass?
Hot Halo Basic Properties Anderson et al. 2013 Assuming: Z = 0.3 Zsun, kt = 0.2 kev
Hot Gas Baryon Budgets Hot gas surface brightness profile Enclosed Mgas profile bkg NGC 720 AB14 H11 H06 Anderson and Bregman 2014 steepening? Rvir Surface brightness profiles are typically fairly well-behaved But can be difficult to measure at large radii Currently we must rely on large (&uncertain) extrapolations
Temperature Profiles of Hot Halos Competition between heating and cooling T slowly declines with r for galaxies flat-ish for massive galaxies cool core for galaxy groups Diehl and Statler 2008
LX - LK Relation:! Diversity in Hot Gas Properties Mulchaey and Jeltema 2010 effects of feedback? galactic dynamics? environment?
Why do ellipticals have hot gaseous halos? Internal origin theories: ISM converted to hot halo via dynamical heating + SNe (Mathews and Baker 1971; Conroy et al. 2014) *and/or* AGN feedback (Silk and Rees 1998, Springel et al. 2005)! External origin theories: Accretion shocks (White and Rees 1978) *or, for cluster galaxies:* Intracluster medium
Generally internal origin is favored: But low-metallicity accreted gas cannot totally be ruled out: NGC 507 Kim and Fabbiano 2004 Crain et al. 2013 Mike Anderson Quenching and Quiescence 16 July 2014
Rotation seems to matter -> dynamical heating? Salzi et al. 2013 Environment could also be important though Will come back to this later in the talk
A Sample of Locally Brightest Galaxies Anderson et al. 2014 (in prep) N = 259 759
Pressure - Mass relation stacked SZ signal (from Planck) Planck Collaboration et al. 2013
11.9-12.0 1.5 Mpc 11.8-11.9 1.5 Mpc 11.7-11.8 1.25 Mpc 11.6-11.7 1.0 Mpc Anderson et al. 2014 (in prep) log M* = 11.6-11.7 0 0.2 0.4 0.6 0.8 1 0 2 4 6 8 10 10 12 14 16 19 20 21 22 23 24 11 12 13 14 12 18 25 26 0.6 27 15 16 17 0.8 1 1.2 1.4 2 4 6 8 10 12 12 14 16 18 20 18 19 20 21 22 23 24 Mike Anderson 8 9 10 11 1 1.5 14 2 22 25 12 13 14 2 2.5 3 3.5 3 4 5 6 7 8 9 18 19 20 26 14 15 5 21 22 23 16 17 18 19 20 21 7 8 2 3 4 10 24 22 5 9 10 11 6 7 6 7 8 9 18 19 20 21 22 10 11 12 23 12 13 14 15 16 24 25 26 17 4.5 5 5.5 6 6.5 7 27 log M* = 10.8-10.9 28 10.4-10.5 18 19 20 21 10.0-10.1 4 13 10.8-10.9 11 8 11.2-11.3 25 17 23 5 10.1-10.2 6 1 10.5-10.6 15 0 10.9-11.0 17 4 11.3-11.4 10.2-10.3 7 0.5 10.6-10.7 28 17 0 11.0-11.1 10 1.6 11.4-11.5 0.75 Mpc 10.3-10.4 10 0.4 10.7-10.8 18 0.2 11.1-11.2 8 1.2 0 11.5-11.6 1.0 Mpc 7.5 8 8.5 9 Quenching and Quiescence 16 July 2014
LX, 500 - Stellar Mass Relation galaxies groups clusters
LX, 500 - Stellar Mass Relation galaxies groups clusters Low-mass X-ray binaries
Same scatter as LX-LK relation! Intrinsic scatter: comparable to LX - LK relation for galaxies (but these are all centrals!) decreases significantly for groups larger again for clusters (due to steep M*-Mhalo relation)
X-ray Luminosity (0.15-1.0 R500 annulus) Hot halos around (almost) all galaxies with log M* 11.0
LX - M* relation (measured from log M* = 11.0-12.0) Preliminary LX = L0 x (bolo_corr) x (M* /1e11) α
Estimate effective Mhalo for each bin.
fit for LX - M500 relation LX, bol = L0 x bolo_corr x E(z) 7/3 x (M/M0) α Preliminary α log L 0 Self-similar: α = 4/3 Galaxy clusters: α = 1.7-2.0 (due to non-gravitational heating)
fit for LX - M500 relation Preliminary
Conclusions Isolated ellipticals do not seem to have their missing baryons in the hot halo! Elliptical galaxies have diverse temperature profiles and LX! Simple power-law relations hold from clusters to galaxies: M* - Y M* - LX M500 - LX! L-M relations are consistently steeper than self-similar