Transcript Radio galaxies are

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!