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Evolution of a Powerful Radio Loud Quasar 3C186 and its Impact on the Cluster Environment at z=1. Aneta Siemiginowska Harvard-Smithsonian Center for Astrophysics. With: - PowerPoint PPT Presentation
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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