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X-ray gas

UV. X-ray gas. Molecular gas. Cool gas. Optical filaments. Star formation. Blue continuum. Carolin Crawford ─ IoA, Cambridge. Central cluster galaxies. Optical emission-line gas. Crawford et al 1999. RXJ1532.9. Z3146. A2204. A1835. Conselice et al 2001.

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X-ray gas

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  1. UV X-ray gas Molecular gas Cool gas Optical filaments Star formation Blue continuum Carolin Crawford ─ IoA, Cambridge Central cluster galaxies

  2. Optical emission-line gas Crawford et al 1999 RXJ1532.9 Z3146 A2204 A1835

  3. Conselice et al 2001 NGC1275/Perseus cluster in Hα in Hα+[NII] Cowie et al 1983

  4. Massive star formation A2597: Koekemoer et al 2002 A1795: McNamara & O’Connell 93

  5. A2204 Z3146 Crawford et al 1999 A1835 A2204

  6. Radius D4000Å Cardiel et al 1999

  7. L(Hα) D4000Å Crawford et al 1999

  8. Line emission found in ~27% of all central cluster galaxies • CCG with line emission lie closer to host cluster X-ray centroid than non-em galaxies • Stronger optical line-emitters show the larger amounts of massive star formation • Intrinsic reddening common E(B─V)~0.3 • molecular gas is seen only if there is optical ionized gas around CCG Cold components are seen only in strong CF cluster cores

  9. the optical-X-ray connection A2052: Blanton et al 02 A1795: Fabian et al 01

  10. Radio+ X-ray U-I B/R light Hα + [NII] [OII] A1795

  11. A1795 3” Hα [NII] Ge & Owen 1993

  12. B/R light Northen lobe A1795 Southern lobe Blob along filament

  13. Hα RXJ0820.9+0752Bayer-Kim et al 03 X-ray V

  14. Perseus: 200ks Chandra Fabian et al 03

  15. Conselice et al 2001

  16. X-ray-Hα filaments in Perseus **see astro-ph today** • Hαfilaments at radii > 30 arcsec with Hαintensity > 2x10-15 erg cm-2s-1arcsec-2 coincide with structures in the soft X-rays • At smaller radii, Hαemissionavoids radio lobes and broad thick X-ray rim to lobes unlike seen in A2052, A2597… • Comparison of X-ray:Hα fluxes  filaments radiate predominantly in the UV/optical (fX/ftot~0.01) • so (local) soft X-rays do not ionize the optical filaments • Filaments ionized by massive blue stars? • But spatial offset observed between brightest Hαgas and blue stars in ‘blue loop’

  17. Summary • Clear connection of X-ray gas to optical emission-line filaments and massive SF • Cause of connection between stars and filaments? • Do stars condense out of the filaments? • Or do we only see nebula if ionized by the stars? • Role of the warm and cold molecular gas? • Revised cooling rates now match the amount of observed star formation and cold gas in inner few tens of kpc (Mdot(stars) ~ 1-100 Mo yr-1) • Balance of heating/cooling has implications for the baryonic mass of the CCG … and by extension to all galaxy formation

  18. UV emission lines Oegerle et al 01

  19. Molecular Gas Edge 01 Edge et al 99 Edge et al 2002

  20. D4000Å Mg2 Crawford et al 1999

  21. Hα RXJ0820.9+0752Bayer-Kim et al 03 X-ray V

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