Evolution of a Powerful Radio Loud Quasar 3C186 and its Impact on the Cluster Environment at z=1

Aneta SiemiginowskaHarvard-Smithsonian Center for

Astrophysics

With: Tom Aldcroft (CfA), Jill Bechtold (Steward), Doug Burke(CfA), Teddy Cheung (Stanford), Stephanie LaMassa (JHU), Diana Worrall (Bristol)

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186 RL Quasar in X-ray Cluster

Outline:• Quasar• Cluster• Interactions

Smoothed Chandra X-ray Image

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

Questions• Are there any Quasars in X-ray Clusters?

=> Radio loud Quasars reside in rich optical environment, outskirts, only marginal detection of the X-ray emission associated with optically bright quasars, thermal/non-thermal X-ray emission at high z

• Is 3C 186, the radio-loud quasar Unique?• What are the properties of the X-ray

Cluster at z>1? • What can we learn about the early stage

interactions between the jet and the cluster environment?

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: Radio Morphology

Compact Radio Source: Size: 2 arsec ~ 16 kpc Radio peaks: 0.3 GHz L(radio) ~1046 erg s-1

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

2 arcsec

core

VLA 1.5 GHz

VLA 15 GHz

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: RL Quasar SED

• Strong Big Blue Bump (BBB)LBBB = 5.7e46 erg/s

LBBBLedd

=> MassBH = 4.5e8 Msun

CIV FWHM (Kuraszkiewicz et al 2002)

=> 3.2e9 Msun • Accretion Rate:

Requires 10 Msun/year

• Radio loudness: Log(F5GHz/B) = 4.3 higher than for a typical radio-loud QSO

• Weaker X-rays, but luminousLX(2-10 keV) ~ 1.2x1045 erg/s

3C186 SED compared to the SED typicalFor a radio-loud QSO in Elvis et al

1994 ChandraBBB

CSS

R-L SED

Broad Emission Lines

Ly- CIV

Kuraszkiewicz et al 2002

HST/FOS

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

CSS/GPS Radio Loudness

Radio Loudness

CSSRL

RQ

Sikora et al 2007R

adi

o

B-luminosity

RL QSO

RQ QSO

CSS/GPS

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: X-ray Cluster

• Chandra ACIS-S 33 ksec• QSO (r=1.5”):

1968.7(+/-44.3) cts

• Diffuse Emission: 741.5 (+/-40.3) cts

• Radial extent ~ 120 kpc

Radial Profile

Diffuse

PSF

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: X-ray Cluster

Cluster Parameters:

kT = 5.2 (+1.2/-0.9) keV

L(0.5-2 keV) = 6e44 erg s-1

R(core) = 45 (+12/-10) kpc

ne = 0.044(+/-0.006) cm-3

M(gas) (r< 1Mpc) ~2e13 Msun

M(grav) ~ 2.6e14 Msun

M(gas) ~ 10% M(grav)

kT = 5.2 (+1.2/-0.9) keV

Thermal Model Fit to Total Spectrum

Fe-linez=1.1

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: X-ray Cluster

3C 186

Vikhlinin et al 2002

3C 186

Low z

Mass vs. Temperature

Luminosity

Tem

pera

ture

Temperature

Mass

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: Optical Cluster ?

X-ray emission traces the gas while optical emission shows structures.

X-ray image is smaller than the optical field of view.

> 50 arcsec offset between the quasar and the centroid of the galaxy distribution in Sanchez & Gonzales-Serrano K-band data

3C186

K-band emission

Opt Peak

Sanchez & Gonzalez-Serrano 2002

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: Optical Cluster ?

Gemini North - GMOS redobserved on Feb 20, 2007

Sanchez centroid

X-ray contours

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

Quasar - Cluster Interaction

2 arcsec

Spencer et al1.6 GHz• Jet/HS within

unresolved X-ray core• 2 arcsec = 16 kpc• HS Outside the galaxy

• Jet Confinement• Jet progress• Cluster heating• Relic?

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

Jet Confinement and Jet Progress

Pressure:

radio HS ~ 10-8 dyn cm -2

hot cluster gas ~ 5 x 10-11 dyn cm -2

Radio components highly overpressured !

Density - clumpy medium?

NH limit from X-ray spectrum of the core < 9e20 cm -2

Required 1-30 cm -3 of a clumpy medium stopping/slowing jet (Carvahlo 1985, De Young 1991, 1993,

Bicknell 1997)

A total thickness of the clumpy medium=> 10-100pc

=> Jet is not frustrated

Bicknell etal 1997

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

Quasar - Cluster Interaction

• Large scale radio structure? • Initial VLA radio data show

a Bubble? • Structure towards the lower

X-ray emission: • Bubble deficit in X-ray only

of -13.9 counts (1.5 sigma)

• More VLA observations in June 2007 to confirm and

get numbers!

Difference in X-ray and radio elongation

Chandra X-rays imageVLA C - Radio contours Radio Bubble?

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

What did we learn so far?

• Ljet = 1046 ergs/s• Lacc = 6x1046 ergs/s• tage = 5x105 yrs• pV work => 1056 ergs• Expansion of the radio source with 0.1c

=> average expansion with power 6x1043 ergs/s

In 107 yrs => 1058 ergs totalIf Mdot = 10 Msun/yr

= > 108Msun if continuous supply

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

Conclusions• Powerful RL quasar in cluster• Lack of Confinement of CSS source - Jet is not

frustrated• The source is at the early stage of expansion • A possible relic activity reflected in the X-ray

and radio emission - future radio and X-ray observations to confirm this

• Optical spectroscopy will determine the cluster galaxies and potential offsets between optical and X-ray centroids

• Searching for more quasars in clusters

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: X-ray Cluster

Radial Profile

Diffuse

PSF

Beta Model Fit

Aneta Siemiginowska Extragalactic Jets, Alaska May 2007

3C 186: X-ray Cluster

Diffuse Emission is Non-Symmetric

It is elongated in NE-SW direction.

Hard emission towards NE

Structure orthogonal to the radio jet

HardSoft