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

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

Aneta SiemiginowskaCfA

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)

Clusters , Boston July 2011 Aneta Siemiginowska

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.


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Chandra- blue, Gemini -yellow

Cluster Image - CXC Release

X-rays

Optical

http://chandra.harvard.edu/photo/2010/3c186/

October 26, 2010

3C 186

z=1.0671arcsec = 8.2 kpc


3C 186: X-ray Cluster

• Chandra ACIS-S • 200 ksec in 4 exposures• Radial extent ~280 kpc

Radius

qso

cluster

2D Models: circular = 0.48 ±0.17

Rcore = 3.06±0.25 = 25.0±2.5 kpc

Elliptical Models => 28 kpc


Extract spectra from annuli.Fit spectra of annuli with thermal model => use deproject in Sherpa

X-ray Cluster: Physical Parameters

temp

density

entropy


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:

= 0.480.17Rcore = 282 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 LuminosityL(0.5-2 keV)= 4.60.28*1044 erg/s

3C 186 X-ray Cluster

Luminous and Massive Cluster at z~1Fgas typical for low z clusters - (no evolution?)


Density Profile

Cooling time: < 5e8 years Cooling rate: ~ 400190 Msun / year

Heat supply to the cluster?

3C186 Cooling Core Cluster

1.7±0.2*109yr

7.5±2.6*108 yr

Cooling Time Profile

Cluster Core: small Rcore~28 kpc ne ~0.08 cm-3


3C186 Cluster Core: Rcore~30 kpc

Cooling time: < 3e8 years Cooling rate: ~ 460 Msun/year

Heat supply to the cluster?

Cooling Time Profile

Cooling Core Clusters

Russell et al 2010

3C186


3C 186 RL Quasar in the Cluster

• Massive Black Hole:=> 3.2e9 MsunCIV FWHM (Kuraszkiewicz et al 2002)

=> 5.5e9 MsunSDSS (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.

3C186 SED compared to the SED typical

For a radio-loud QSO in Elvis et al 1994

ChandraBBB

CSS

R-L SED


3C 186: Radio Source

2 arcsec

Chandra

2 arcsec

core

VLA 1.5 GHz

VLA 15 GHz

Compact Radio Source CSS Projected Size: 2 arcsec ~16 kpcRadio peaks:

0.3 GHz L(radio) ~1046 erg/s

Young Radio Source! Age: ~5e5 yrs (Murgia et al 1999)

RS size < 30 kpc


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!


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?


Quasar Impact: Non-thermal particles

Sobolewska et al


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


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 is Challenging 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, 3C295 see also poster by Ania Szostek)


Extract spectra from 7 annuli. Check for Quasar ContaminationFit spectra of the annuli with thermal model

=> use deproject in Sherpa

Spectral Modeling


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)

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

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