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On the origin of Radio Loudness In AGN Marco Chiaberge STScI , INAF-IRA and JHU

On the origin of Radio Loudness In AGN Marco Chiaberge STScI , INAF-IRA and JHU. RQ. RL. The rise of the RL/RQ dichotomy. Kellerman et al. 1989 114 PG QSO Bimodal distribution ? RL/RQ separation R = F 5GHz / F B = 10. R > 10 is a good definition of radio loudness.

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On the origin of Radio Loudness In AGN Marco Chiaberge STScI , INAF-IRA and JHU

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  1. On the origin of Radio Loudness In AGN Marco Chiaberge STScI, INAF-IRA and JHU

  2. RQ RL The rise of the RL/RQ dichotomy Kellerman et al. 1989 114 PG QSO Bimodal distribution ? RL/RQ separation R = F5GHz / FB = 10 R > 10 is a good definition of radio loudness White et al. 2000, Izevic et al. 2004, Cirasuolo et al 2007, Balokovic et al 2012

  3. SED of radio loud and radio quiet AGNs Radio loud powerful jets Radio quiet weak jets Elvis et al. 1994

  4. THE MOST IMPORTANT QUESTIONS What is the origin of the rl/rq dichotomy? How do Black holes produce jets? What is the role of the environment? Host galaxy: mergers? accretion? Is there any super-unification paradigm?

  5. What is the origin of the observed differences? Spin paradigm(Blandford 1990)‏ jets are powered by spinning BHs LEMl2 B2 MBH2 Radio Loud rapidly spinning BHs Radio quiet slowly spinning BHs Elliptical hosts mergers rapidly spinning BHs Spiral hosts accretion slowly spinning Wilson & Colbert 1995, Modersku & Sikora 1996, Huges & Blandford 2003, Volonteri et al. 2007, 2013

  6. POTENTIAL PROBLEMS: • Broad Fe lines in Radio Quiet AGNs e.g. MCG-6-30-15 Explained as radiation emitted at 6Rg • Bright Radio Quiet QSOs are hosted by massive Elliptical galaxies Dunlop et al. 2003 Fabian et al 2002

  7. Is the radio loudness related to the BH mass? Are the BH masses of RL-QSOs higher than those of RQ-quasars ?‏ Dunlop et al. 2003 McLure & Jarvis 2004 Woo & Urry 2002

  8. Galaxy morphology – radio dichotomy Rapidly rotating (mergers)‏ See e.g. Volonteri et al. 2013 Ellipticals Ellipticals FRI BBLRG RL QSO Rapidly rotating and intermittent at high l SY/LINERS Spirals RQ QSO Ellipticals Slowly rotating at low l Sikora et al. 2007

  9. What can we learn from low luminosity AGN? LINERs d < 19 Mpc from the Palomar sample of nearby galaxies 21/25 have HST images SEYFERT 1Ho & Peng 2001 Palomar sample (dmed = 20 Mpc)‏ CfA sample (dmed = 80 Mpc)‏ 25/32 have HST images FR Iradio galaxies from the 3CR catalog THE LOCAL AGNs ARE WELL REPRESENTED BY THESE 3 SAMPLES Chiab, Capetti, Macchetto 2005

  10. Radio quiet NGC 5033 - HST WFPC2 - V band

  11. Radio loud 3C31 – HST ACS/HRC – F606W

  12. NUCLEAR RADIO LOUDNESS OF LLAGN RQ RL The RQ/RL dividing line is NOT at R=1! Chiab, Capetti, Macchetto 2005 Sikora et al. 2007

  13. Black hole masses of local AGNs On average, Sy1 have lower BH masses than LINERs and FR I

  14. LLAGNs FRIs, Seyfert 1s, LINERS (Chiab, et al. 2005) E+S0 (Capetti & Balmaverde 2005) SDSS DR5 AGN z<0.35 Green & Ho 2007, Rafter et al. 2009 QSOs (Oshlack, Webster & Whiting 2002, Gu Cao & Jiang 2001) High-z QSOs (McIntosh et al. 1999) Chiaberge & Marconi 2011

  15. QSOs (Oshlack, Webster & Whiting 2002, Gu Cao & Jiang 2001, McIntosh et al. 1999) SDSS DR5 AGN z<0.35 Green & Ho 2007, Rafter et al. 2009

  16. Re-calculate BH virial masses using updated formulae MBH/MSun = 106.6 x (FWHM(Hb)/1000)2 x (lLl5100/1044)0.5 + + 107.5 x (lLl5100/1044) Vestergaard & Peterson 2006, Marconi et al. 2008 Radiation pressure correction

  17. QSOs (Oshlack, Webster & Whiting 2002, Gu Cao & Jiang 2001, McIntosh et al. 1999) SDSS DR5 AGN z<0.35 Green & Ho 2007, Rafter et al. 2009 High MBH: RQ and RL exist

  18. SDSSJ151513.58+552504.2 z=0.29

  19. We re-estimated SDSS BH masses using: K-band (2MASS) – MBH relation for red objects u-r >2.2 (Marconi & Hunt 2003) Hb when available (e.g. Shen et al 2011) Removed a few type 2 objects Radiation pressure has no effect on SDSS AGNs

  20. BLACK HOLE MASS VS. RADIO LOUDNESS SPIN RL/jet MCG-6-30-15 MBH < 107 (McHardy et al. 2005) FR I SY 1 LINER Even if the BH is spinning, these objects are RQ BLRG RQ/disk

  21. Core-galaxies vs Power-law galaxies Balmaverde & Capetti 2005, 06, 07 Faber et al. 1997…

  22. CORE GALAXIES : major dry mergers P-L Galaxies: wet mergers (Kormendy et al. 09 and ref therein) HIGH-MASS RAPIDLY SPINNING BH: major mergers (Huges & Blandford 03, Berti & Volonteri 2008) Accretion alone may lead to a~1 only for very large BH masses and if the fueling process is highly anisotropic (Dotti et al. 2013, Volonteri et al 2013) RADIO LOUD Major dry mergers to spin-up the BH and MBH>108 Msun

  23. A REVISED SUPER-UNIFICATION PARADIGM Fundamental parameters MBH Acc. rate/eff. spin (see Blandford 1990) LINERS (RQ) L L L/H LINERS (RL) H L H Seyferts L/H H H/L FR I radiogalaxies H L H FR II radio galaxies H H H Radio QUIET QSO H H L Radio LOUD QSO H H H

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