3C 186 A Luminous Quasar in the Center of a Strong Cooling Core Cluster at z>1

1. 3C 186 A Luminous Quasar in the Center of a Strong Cooling Core Cluster at z>1 Aneta Siemiginowska CfA Tom Aldcroft (CfA) Steve Allen (Stanford) Jill Bechtold (Arizona) Doug Burke (CfA) Tracy Clarke (NRL) Teddy Cheung (NRL) Giulia Migliori (CfA) Malgorzata Sobolewska (CfA) Diana Worrall (Bristol)

2. Outline • 3C 186 X-ray Cluster • 3C 186 Radio-Loud Quasar • Quasar - Cluster Interactions • Papers: * 2010, ApJ, 722, 102 - “High-redshift X-ray Cooling-core Cluster Associated with the Luminous Radio-loud Quasar 3C 186”, Siemiginowska, Burke, Aldcroft, Worrall, Allen, Bechtold, Clarke, Cheung * 2005 ApJ, 632, 110, Siemiginowska et al. Aneta Siemiginowska

3. Chandra- blue, Gemini -yellow Cluster Image - CXC Release October 26, 2010 3C 186 X-rays Optical z=1.067 1arcsec = 8.2 kpc http://chandra.harvard.edu/photo/2010/3c186/ Aneta Siemiginowska

4. 3C 186: X-ray Cluster • Chandra ACIS-S • 200 ksec in 4 exposures • Radial extent ~280 kpc qso cluster Radius 2D Models: circular  = 0.48 ±0.17 Rcore = 3.06±0.25 = 25.0±2.5 kpc Elliptical Models => 28 kpc Aneta Siemiginowska

5. X-ray Cluster: Physical Parameters temp density entropy Extract spectra from annuli. Fit spectra of annuli with thermal model => use deproject in Sherpa Aneta Siemiginowska

6. 3C 186 X-ray Cluster NFW model parameters: concentration => c1=7.4 (+2.8/-2.3) scale => rs=120 (+70/-40) kpc velocity dispersion c=780 (+90/-60) km/s r2500 = 283 (+18/-13) kpc Surface Brightness fitting results:  = 0.480.17 Rcore = 282 kpc Central density = 0.08 cm-3 Cluster Mass M(r2500) = 1.02(+0.21/-0.14) * 1014 Msun Gas mass fraction =0.129 (+0.015/-0.016) Cluster Luminosity L(0.5-2 keV)= 4.60.28*1044 erg/s Luminous and Massive Cluster at z~1 Fgas typical for low z clusters - (no evolution?) Aneta Siemiginowska

7. 3C186 Cooling Core Cluster Density Profile Cooling Time Profile 1.7±0.2*109yr 7.5±2.6*108 yr Cluster Core: small Rcore~28 kpc ne ~0.08 cm-3 Cooling time: < 5e8 years Cooling rate: ~ 400190 Msun / year Heat supply to the cluster? Aneta Siemiginowska

8. 3C186     Cooling Core Clusters Cooling Time Profile Cluster Core: Rcore~30 kpc Cooling time: < 3e8 years Cooling rate: ~ 460 Msun/year Heat supply to the cluster? 3C186 Russell et al 2010 Aneta Siemiginowska

9. R-L SED BBB Chandra CSS 3C 186 RL Quasar in the Cluster 3C186 SED compared to the SED typical For a radio-loud QSO in Elvis et al 1994 • Massive Black Hole: => 3.2e9 Msun CIV FWHM (Kuraszkiewicz et al 2002) => 5.5e9 Msun SDSS(Shen et al 2011) • Strong UV Big Blue Bump LBBB = 5.7x1046 erg/s • Luminous in X-rays LX(2-10 keV) ~ 1.2x1045 erg/s • Accretion Rate: L/LEdd ~ 0.25 • Requires 10 Msun/year This is a small fraction (< 3%) of the total cooling rate of the cluster. Aneta Siemiginowska

10. 2 arcsec core 2 arcsec VLA 1.5 GHz VLA 15 GHz 3C 186: Radio Source RS size < 30 kpc Chandra Compact Radio Source CSS Projected Size: 2 arcsec ~16 kpc Radio peaks: 0.3 GHz L(radio) ~1046 erg/s Young Radio Source! Age: ~5e5 yrs (Murgia et al 1999) Aneta Siemiginowska

11. 2 arcsec Quasar Impact • Jet and Radio Source Power? • Pressure in Radio Lobes => 10-8 erg/cm3 • Pressure of thermal gas => 10-10 erg/cm3 • Overpressured expansion - strong shock • Instantenous jet power: pdV ~ 1058 ergs (under-estimated) RS age 5x105 years =>Ljet = 1.7x1045 erg/s • Jet Power using Sradio(151 MHz) = 6x10-24 erg/s/cm2/Hz and based on Willot et al (1999) => Ljet = 1046 erg/s • Modeling of the jet SED (see Giulia Migliori poster) => Ljet > 1047 erg/s • Quasar Radiation Power => Lrad = 6x1046 erg/s RS Compact! Aneta Siemiginowska

12. Cluster Heating? • M (Rcore=45 kpc) = 3x1011 Msun • Eheat (core) ~ (1keV/1GeV) Mcorec2 => 6x1059 erg • Core Cooling time => 7x108 years => Needs a supply of E~ 2.7x1043 erg/s =>Only a fraction of QSO energy to heat the cluster • Quasar Lbol ~1047 erg/s • Jet Power ~ 1046 erg/s => enough to heat the gas in 5e5 year • Ljet (1046-47 erg) ~ Lradiation (1047)erg • Quasar role? Aneta Siemiginowska

13. Quasar Impact: Non-thermal particles Sobolewska et al Aneta Siemiginowska

14. Summary • X-ray Luminous massive cluster at high redshift. • Luminous Quasar located in a center of this massive X-ray cluster. • Cluster exhibits a strong cooling flow • Ljet ~ Lradiation • Quasar mode could be important for this cluster heating Aneta Siemiginowska

15. Quasars in Clusters • Powerful RL quasars in Rich Environments Ellingson & Yee ‘90; Ellingson, Green & Yee ‘90, Smith & Heckman’90 • Search for X-ray clusters by ROSAT Worrall et al ‘94 Hall et al ‘95, ‘97, Crawford et al ‘99 • Diffuse X-ray emission can also be associated with CMB from radio lobes, relic, jets Cellotti & Fabian 04, Crawford & Fabian ‘03, Croston et al ‘05, Worrall et al ‘04 • Detecting X-ray emission from thermal cluster gas isChallenging and requires Chandra! • Majority of nearby clusters host a low power FRI radio source. • But there are examples of X-ray clusters associated with powerful radio sources at lower redshift (e.g. Cygnus A, 3C295see also poster by Ania Szostek) Aneta Siemiginowska

16. Spectral Modeling Extract spectra from 7 annuli. Check for Quasar Contamination Fit spectra of the annuli with thermal model => use deproject in Sherpa Aneta Siemiginowska

17. Quasar Contamination? • Simulate PSF - assumed • quasar spectrum of =1.9 • Fit the simulated PSF spectra • for the same regions • Include a non-deprojected • component in the spectral • model for each cluster region • - simple in Sherpa • Innermost annulus most affected • fit indicates lower temperatures • kT=2.54 (+1.02/-0.57) Aneta Siemiginowska