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THE HST view of z>1 powerful RADIO LOUD AGNs: laboratories for galaxy and black hole mergers Marco Chiaberge Space Telescope Science Institute Johns Hopkins University THE RADIO SKY Cygnus A VLA Image credit NRAO/AUI- Green Bank WV, Condon et al. Radio Loud Active Galactic Nuclei image credit: CXC, Melissa Weiss Accretion disk and BLR NLR Relativistic jets Energy extracted from the BH PERSEUS A : a radio galaxy in the Perseus cluster of galaxies Fabian et al. 2005,06, 11 The MBH - s relation The BH mass and some fundamental properties of their host galaxies (Lbulge, s) are strictly connected Radio-loud AGNs are confined to the high-mass end of the plot High-z RGs are fundamental objects to understand the formation and evolution of the most massive galaxies and clusters of galaxies Spiderweb galaxy z=2.2 Miley et al. 2006 Ferrarese & Merritt 2000 Gebhardt et al. 2000 Tremaine et al. 2002 Gultekin et al. 2009 Graham et al. 2011 Black hole – galaxy co-evolution Galaxy mergers The black hole “awakes” Ultra luminous IR galaxy Galaxy group “Normal” galaxy AGN/Quasar AGN fades Stars evolve “Old” elliptical galaxy Hopkins et al. 2008 MERGERS and AGN activity: still debated Evidence that some AGNs are more common in close (interacting) pairs e.g. Silverman et al. 2011, Satyapal et al. 2014, Ellison et al. 2015 Merger fraction in X-ray AGN increases with NH (~20%) Kocevski et al 2015 Distributions of asymmetry and concentration indices in GOODS show no connection between recent mergers and X-ray selected AGNs Grogin et al 2005, Schawinsky et al. 2011 Powerful reddened QSOs at z~2 Lbol ~ 1048 erg s-1 are mergers Urrutia et al. 2008, Treister et al. 2011, Glikman et al. 2015 Powerful QSO are NOT mergers Mechtley et al.16, Villforth et al. 16 No dependence of AGN merger fraction on luminosity. Less than 40% of the highest luminosity AGNs may be triggered by mergers (CANDELS) Villforth et al. 2014, 2016 ULIRGs are mergers Veilleux et al. 2002 (Most) low – z Radio Galaxies are mergers Heckman 1986, Colina & de Juan 1995, Ramos Almeida et al. 2012, Tadhunter 2016 (review) 1. WHAT TRIGGERS A RADIO-LOUD AGN? 2. 3C 186: a gravitational wave recoiling BH? 3CR HST SNAPSHOT survey Cycle 19 12 Radio galaxies (Type 2) +10 QSOs (Type 1) 1 < z < 2.5 PI M. Chiaberge HST WFC3 UVIS F606W + IR F140W Lbol ~ 1046-47 erg s-1 W.B. Sparks (STScI) G. Miley (Leiden) G. Tremblay (Yale) A. Capetti (INAF-OATO) D. Macchetto (STScI) S. Baum (U.Manitoba) C. O’Dea (U. Manitoba) E. Perlman (FIT) A. Quillen (UofR) B. Hilbert (STScI) JP Kotyla (STScI) C. Stanghellini (INAF-IRA) J. Ely (STScI) C. Norman (JHU/STScI) J. Lotz (STScI) R. Gilli (INAF-OABo) S. Bianchi (U Roma3) A. Marinucci (U Roma3) Hilbert , Chiab et al. (2016) https://hz3c.stsci.edu Adapted form McLure et al 04, Willott et al 2000 POWERFUL RADIO GALAXIES AT z>1 3CR images with HST WFC3/IR F140W Chiaberge , Gilli, Lotz & Norman (2015) MAJOR MERGERS Radio galaxies are compared to matched samples of low and high power AGNs and non-active galaxies Non-merger Possible merger Data from ECDFS Lehmer et al. 2005 4Ms CDFS Xue et al. 2011, CANDELS Grogin et al. 11 Koekemoer et al. 11 3D-HST Brammer et al. 12 Merger MERGER FRACTIONS vs REDSHIFT 3CR Hz3C + HzLPRG 3CR 6CE 7CRS TOOT RADIO LOUD RQTY2AGN Galaxies In agreement with Mechtley 2016 and Villforth 2016 RQ Type 1 QSOs MERGERS Radio-loud AGN CONJECTURE: MBH > 108 M Chiaberge & Marconi 2011 Contopoulos & Kazanas 1995 Laor et al. 2000 Dunlop et al. 2003 Best et al. 2005 Chiaberge et al 2006 Calderone et al. 2013 Bagchi et al. 2014 Singh et al. 2015 Mao et al. 2015 + BH SPIN jets are powered by spinning BHs LEM l2 B2 M2BH Blanford & Znajek 1977 Hawley et al. 2007 Tchekhovskoy et al. 2011 Ghisellini et al. 2014 Major galaxy mergers AND major BH-BH mergers In some cases, BH-BH mergers lead to BH spin-up Wilson & Colbert 1995 Chiaberge , Gilli, Lotz & Norman (2015) (e.g. Schnittman 2013) When galaxies merge, their black holes merge too… (?) When galaxies merge, their black holes merge too… (?) Chiab et al., submitted arXiv 1611.05501 3C 186 z = 1.07 WFC3-IR F140W image smoothed image ~ 1” (10kpc) projected offset between the galaxy photo-center and the QSO Tidal arcs or shells – merger remnant ~1-2Gyr old SDSS SPECTRUM Isolated low-ionization narrow lines Systemic redshift of the NRL (host galaxy) z=1.0685 Broad lines: Mg II concave shape, offset v~2100 km/s CIII] offset v~2100 km/s HST/FOS UV spectrum of 3C 186 (1991) Ly a C IV Narrow absorption at the systemic redshift z=1.0685 Broad line offsets v ~ 2100 km/s 3C 186 HST images: spatial offset between the QSO and the host photocenter SDSS and HST/FOS UV SPECTRA Broad emission lines (Lya, CIV, MgII, CIII],…) are blue-shifted with respect to narrow emission lines velocity offset v = -2140 ± 390 km/s a. The BLR (accretion disk and BH) is moving with respect to the NLR (i.e. the host galaxy) b. The QSO is a foreground object (with no NLR?) UV narrow absorption lines (CIV and Lya) and optical narrow emission lines [OII] and [NeIII] are at the same systemic redshift The QSO cannot be a foreground object Gravitational wave recoiling black hole! The merged BH may get a kick from anisotropic 1962, Bekenstein 1973 emission of gravitational waves Peres Campanelli et al 2007, Lousto et al 08,11, 12 Loeb 2007, Volonteri & Madau 08 Gravitational waves detected by LIGO Abbott et al. 2016 We know that stellar mass BHs mergers happen Do SMBH merge? Final parsec problem (Milosavljevic & Merrit 2003) Prospect for GW detections with LISA and PTA GW recoiling black hole candidates SDSS 0927 z=0.7 Komossa et al. 2008 CID-42 z=0.36 NGC 3718 z=0.003 Markakis et al. 2015 SDSS 0956 z=0.7 Civano et al. 2010 MBH=6x108 M ? MBH=106 M Dual AGN? MBH=108 M Merger. No v offset? Steinhardt et al. 2012 MBH=4x108 M Eccentric disk? SDSS 1133 z=0.008 Koss et al. 2014 MBH=106 M SBS 1421 z=0.28 Sun et al 2016 MBH=2x107 M Bipolar outflow? 3c186 z=1.07 Chiab et al. submitted LBV star + SN MBH=5x109 M Lbol ~1047 erg s-1 A GW RECOILING BH IN A RADIO-LOUD AGN VERY IMPORTANT!!! Galaxy merger timescale (roughly) known from simulations: 1-2 Gyr Time since the GW “kick” (from the velocity and the QSO offset): ~5 Myr We know the age of the AGN from radio observations: ~1 x105 years (Murgia et al. 1999) Direct comparison with theory/simulations SUMMARY Close environment of (type 2) RLAGN: Mergers! Radio galaxies are ~3x more likely to be in a merger than Radio Quiet AGN or non-AGN (but that is from ~30% to ~100%!!!) This fits in a scenario where RL AGNs are linked to major mergers of galaxies with >108 Msun black holes and the BH is spun-up by the BH-BH merger With JWST we will be able to learn much more on the merger timescale, BH feeding mechanism, and extend the study to z>2 (and to Type 1 too!) Gravitational wave recoiling BH in 3C 186 Additional evidence for BH mergers in RLAGN Supermassive BHs may merge. Good news for LISA and PTA!