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

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:

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

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

  2. 3C 186 RL Quasar in X-ray Cluster Smoothed Chandra X-ray Image • Outline: • Quasar • Cluster • Interactions Extragalactic Jets, Alaska May 2007

  3. 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? Extragalactic Jets, Alaska May 2007

  4. 3C 186: Radio Morphology 2 arcsec Compact Radio Source: Size: 2 arsec ~ 16 kpc Radio peaks: 0.3 GHzL(radio) ~1046 erg s-1 Young Radio Source! Age: ~5e5 yrs (Murgia et al 1999) core VLA 1.5 GHz VLA 15 GHz Extragalactic Jets, Alaska May 2007

  5. R-L SED BBB Chandra Broad Emission Lines CSS CIV Ly- 3C 186: RL Quasar SED 3C186 SED compared to the SED typical For a radio-loud QSO in Elvis et al 1994 • Strong Big Blue Bump (BBB) LBBB = 5.7e46 erg/s LBBBLedd => MassBH = 4.5e8 Msun CIV FWHM (Kuraszkiewicz et al 2002) => 3.2e9 Msun • Accretion Rate: Requires 10 Msun/year • Radio loudness: Log(F5GHz/B) = 4.3higher than for a typical radio-loud QSO • Weaker X-rays, but luminous LX(2-10 keV) ~ 1.2x1045 erg/s HST/FOS Kuraszkiewicz et al 2002 Extragalactic Jets, Alaska May 2007

  6. Radio RL QSO RQ QSO B-luminosity CSS/GPS Radio Loudness CSS/GPS RQ CSS RL Radio Loudness Sikora et al 2007 Extragalactic Jets, Alaska May 2007

  7. 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 Extragalactic Jets, Alaska May 2007

  8. kT = 5.2 (+1.2/-0.9) keV 3C 186: X-ray Cluster Thermal Model Fit to Total Spectrum 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) Fe-line z=1.1 Extragalactic Jets, Alaska May 2007

  9. Mass vs. Temperature Low z 3C 186 3C 186 Vikhlinin et al 2002 3C 186: X-ray Cluster Mass Temperature Luminosity Temperature Extragalactic Jets, Alaska May 2007

  10. 3C 186: Optical Cluster ? K-band emission Opt Peak • 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 Sanchez & Gonzalez-Serrano 2002 Extragalactic Jets, Alaska May 2007

  11. 3C 186: Optical Cluster ? Gemini North - GMOS red observed on Feb 20, 2007 Sanchez centroid X-ray contours Extragalactic Jets, Alaska May 2007

  12. Spencer et al 1.6 GHz 2 arcsec Quasar - Cluster Interaction • Jet/HS within unresolved X-ray core • 2 arcsec = 16 kpc • HS Outside the galaxy • Hot spot - pressure • Outside the galaxy • Dynamics/Mach numbers • Bullet-like => cluster does not stop/slow down the jet • Hot spots - give jet power ? • Bfield? • How the energy is transfer to the cluster? • Jet Confinement • Jet progress • Cluster heating • Relic? Extragalactic Jets, Alaska May 2007

  13. Bicknell etal1997 Jet Confinement and Jet Progress Pressure: radio HS ~ 10-8 dyn cm -2 hot cluster gas ~ 5 x10-11 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 Extragalactic Jets, Alaska May 2007

  14. Quasar - Cluster Interaction Chandra X-rays image VLA C - Radio contours Radio Bubble? • 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 Extragalactic Jets, Alaska May 2007

  15. 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 total If Mdot = 10 Msun/yr = > 108Msun if continuous supply Extragalactic Jets, Alaska May 2007

  16. 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 Extragalactic Jets, Alaska May 2007

  17. 3C 186: X-ray Cluster Beta Model Fit Radial Profile Diffuse PSF Extragalactic Jets, Alaska May 2007

  18. 3C 186: X-ray Cluster Soft • Diffuse Emission is Non-Symmetric • It is elongated in NE-SW direction. • Hard emission towards NE • Structure orthogonal to the radio jet Hard Extragalactic Jets, Alaska May 2007

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