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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.

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Presentation on theme: "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."— Presentation transcript:

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 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186 RL Quasar in X-ray Cluster Outline: Quasar Cluster Interactions Smoothed Chandra X-ray Image

3 Aneta SiemiginowskaExtragalactic 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?

4 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186: Radio Morphology Compact Radio Source: Size: 2 arsec ~ 16 kpc Radio peaks: 0.3 GHz L(radio) ~10 46 erg s -1 Young Radio Source! Age: ~5e5 yrs ( Murgia et al 1999) 2 arcsec core VLA 1.5 GHz VLA 15 GHz

5 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186: RL Quasar SED Strong Big Blue Bump (BBB) L BBB = 5.7e46 erg/s L BBB  L edd => Mass BH = 4.5e8 M sun CIV FWHM (Kuraszkiewicz et al 2002) => 3.2e9 M sun Accretion Rate: Requires 10 Msun/year Radio loudness: Log(F 5GHz /B) = 4.3 higher than for a typical radio-loud QSO Weaker X-rays, but luminous L X (2-10 keV) ~ 1.2x10 45 erg/s 3C186 SED compared to the SED typical For a radio-loud QSO in Elvis et al 1994 Chandra BBB CSS R-L SED Broad Emission Lines Ly-  CIV Kuraszkiewicz et al 2002 HST/FOS

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

7 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186: X-ray Cluster Chandra ACIS-S 33 ksec QSO (r=1.5”): (+/-44.3) cts Diffuse Emission: (+/-40.3) cts Radial extent ~ 120 kpc Radial Profile Diffuse PSF

8 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 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 n e = 0.044(+/-0.006) cm -3 M(gas) (r< 1Mpc) ~2e13 M sun M(grav) ~ 2.6e14 M sun M(gas) ~ 10% M(grav) kT = 5.2 (+1.2/-0.9) keV Thermal Model Fit to Total Spectrum Fe-line z=1.1

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

10 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 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

11 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186: Optical Cluster ? Gemini North - GMOS red o bserved on Feb 20, 2007 Sanchez centroid X-ray contours

12 Aneta SiemiginowskaExtragalactic Jets, Alaska May 2007 Quasar - Cluster Interaction 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? 2 arcsec Spencer et al 1.6 GHz Jet/HS within unresolved X-ray core 2 arcsec = 16 kpc HS Outside the galaxy Jet Confinement Jet progress Cluster heating Relic?

13 Aneta SiemiginowskaExtragalactic Jets, Alaska May 2007 Jet Confinement and Jet Progress Pressure: radio HS ~ dyn cm -2 hot cluster gas ~ 5 x 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=> pc => Jet is not frustrated Bicknell etal 1997

14 Aneta SiemiginowskaExtragalactic 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 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 image VLA C - Radio contours Radio Bubble?

15 Aneta SiemiginowskaExtragalactic Jets, Alaska May 2007 What did we learn so far? L jet = ergs/s L acc = 6x10 46 ergs/s t age = 5x10 5 yrs pV work => ergs Expansion of the radio source with 0.1c => average expansion with power 6x10 43 ergs/s In 10 7 yrs => ergs total If Mdot = 10 Msun/yr = > 10 8 Msun if continuous supply

16 Aneta SiemiginowskaExtragalactic 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

17 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 186: X-ray Cluster Radial Profile Diffuse PSF Beta Model Fit

18 Aneta SiemiginowskaExtragalactic Jets, Alaska May C 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 Hard Soft


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