Hot Gas Around Elliptical Galaxies Mike Anderson (MPA) Joel Bregman - - PowerPoint PPT Presentation

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Hot Gas Around Elliptical Galaxies Mike Anderson (MPA) Joel Bregman - - PowerPoint PPT Presentation

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Hot Gas Around Elliptical Galaxies Mike Anderson (MPA) Joel Bregman (Michigan), Xinyu Dai (Oklahoma), Massimo Gaspari (MPA), Simon White (MPA) Mike Anderson Quenching and Quiescence 16 July 2014 Outline Very brief summary of properties of

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Hot Gas Around Elliptical Galaxies

Mike Anderson (MPA) Joel Bregman (Michigan), Xinyu Dai (Oklahoma), Massimo Gaspari (MPA), Simon White (MPA)

Mike Anderson Quenching and Quiescence 16 July 2014

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SLIDE 2

Outline

Very brief summary of properties of hot halos

  • Why do ellipticals have hot halos?
  • Connecting hot halos in galaxies, groups, and clusters

Mike Anderson Quenching and Quiescence 16 July 2014

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Total X-ray luminosity Extended emission only

Hot Halo Basic Properties

Ellipticals seem to have higher LX than spirals: because of morphology? M/L ratio? halo mass?

Anderson et al. 2013

Mike Anderson Quenching and Quiescence 16 July 2014

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Assuming: Z = 0.3 Zsun, kT = 0.2 keV

Hot Halo Basic Properties

Anderson et al. 2013

Mike Anderson Quenching and Quiescence 16 July 2014

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Hot gas surface brightness profile

Hot Gas Baryon Budgets

Anderson and Bregman 2014

Enclosed Mgas profile

H11 H06 AB14

bkg Rvir

NGC 720

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

steepening?

Mike Anderson Quenching and Quiescence 16 July 2014

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Diehl and Statler 2008

  • T slowly declines with r for galaxies
  • flat-ish for massive galaxies
  • cool core for galaxy groups

Temperature Profiles of Hot Halos

Competition between heating and cooling

Mike Anderson Quenching and Quiescence 16 July 2014

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LX - LK Relation:

Diversity in Hot Gas Properties

Mulchaey and Jeltema 2010

effects of feedback? galactic dynamics? environment?

Mike Anderson Quenching and Quiescence 16 July 2014

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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

Mike Anderson Quenching and Quiescence 16 July 2014

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Kim and Fabbiano 2004

NGC 507 Generally internal origin is favored: But low-metallicity accreted gas cannot totally be ruled out:

Crain et al. 2013

Mike Anderson Quenching and Quiescence 16 July 2014

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Salzi et al. 2013

Rotation seems to matter -> dynamical heating? Environment could also be important though… Will come back to this later in the talk

Mike Anderson Quenching and Quiescence 16 July 2014

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A Sample of Locally Brightest Galaxies

N = 259 759

Anderson et al. 2014 (in prep)

Mike Anderson Quenching and Quiescence 16 July 2014

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stacked SZ signal (from Planck)

Planck Collaboration et al. 2013

Pressure - Mass relation

Mike Anderson Quenching and Quiescence 16 July 2014

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SLIDE 13 4 4.5 5 5.5 6 6.5 7 7.5 8 8.5 9 10.0-10.1 0.5 Mpc 5 6 7 8 9 10 11 10.1-10.2 0.5 Mpc 7 8 9 10 11 12 13 14 15 10.2-10.3 0.5 Mpc 10 11 12 13 14 15 16 17 10.3-10.4 0.5 Mpc 11 12 13 14 15 16 17 18 19 20 21 10.4-10.5 0.5 Mpc 14 15 16 17 18 19 20 21 22 23 10.5-10.6 0.5 Mpc 17 18 19 20 21 22 23 24 25 26 10.6-10.7 0.5 Mpc 18 19 20 21 22 23 24 25 26 27 28 10.7-10.8 0.5 Mpc 17 18 19 20 21 22 23 24 25 26 27 28 10.8-10.9 0.5 Mpc 17 18 19 20 21 22 23 24 25 10.9-11.0 0.5 Mpc 10 12 14 16 18 20 22 11.0-11.1 0.5 Mpc 8 10 12 14 16 18 11.1-11.2 0.5 Mpc 5 6 7 8 9 10 11 12 13 11.2-11.3 0.5 Mpc 2 3 4 5 6 7 8 9 10 11.3-11.4 0.5 Mpc 2 4 6 8 10 12 14 11.4-11.5 0.75 Mpc 2 4 6 8 10 12 11.5-11.6 1.0 Mpc 1 2 3 4 5 6 7 8 11.6-11.7 1.0 Mpc 0.5 1 1.5 2 2.5 3 3.5 4 11.7-11.8 1.25 Mpc 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 11.8-11.9 1.5 Mpc 0.2 0.4 0.6 0.8 1 1.2 11.9-12.0 1.5 Mpc

log M* = 11.6-11.7 log M* = 10.8-10.9

Anderson et al. 2014 (in prep)

Mike Anderson Quenching and Quiescence 16 July 2014

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clusters

groups

galaxies

LX, 500 - Stellar Mass Relation

Mike Anderson Quenching and Quiescence 16 July 2014

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clusters

groups

galaxies

LX, 500 - Stellar Mass Relation

Low-mass X-ray binaries

Mike Anderson Quenching and Quiescence 16 July 2014

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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)

Same scatter as LX-LK relation!

Mike Anderson Quenching and Quiescence 16 July 2014

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Hot halos around (almost) all galaxies with log M* ≈ 11.0

X-ray Luminosity (0.15-1.0 R500 annulus)

Mike Anderson Quenching and Quiescence 16 July 2014

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LX - M* relation

(measured from log M* = 11.0 - 12.0) LX = L0 x (bolo_corr) x (M* /1e11)α Preliminary

Mike Anderson Quenching and Quiescence 16 July 2014

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Estimate effective Mhalo for each bin….

Mike Anderson Quenching and Quiescence 16 July 2014

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… fit for LX - M500 relation

LX, bol = L0 x bolo_corr x E(z)7/3 x (M/M0)α Self-similar: α = 4/3 Galaxy clusters: α = 1.7-2.0 (due to non-gravitational heating)

Mike Anderson Quenching and Quiescence 16 July 2014

Preliminary

log L0 α

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… fit for LX - M500 relation

Mike Anderson Quenching and Quiescence 16 July 2014

Preliminary

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Conclusions

Mike Anderson Quenching and Quiescence 16 July 2014

  • 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