Transcript Studies of QSO host galaxies

The 10th East Asian Meeting on Astronomy
Studies of QSO host galaxies
Yiping Wang
National Astronomical Observatories of China
[email protected]
2016/09/29 @Seoul
Outline
1) Briefly review the BH growth and the host
galaxy formation
2) Discuss the limit of the current study on
QSO host properties
3) Look forward to 2020s
Motivation
http://en.wikipedia.org
Where comes the fuel to feed
BH?
How to power the central
engine?
http://en.wikipedia.org
Constellation: Virgo : Redshift: 0.158
Type: Blazar, Sy1, Radio source ; Mv: ~ -26
Notable features: optically-brightest quasar;
first spectrum of a quasar
z=7.1,
most
distant
known
qso,
Host galaxy: a giant elliptical galaxy
Discovered by UKIDSS;
Reported in June, 2011
Motivation
Local scaling relation for inactive galaxies and AGNs:
z<0.2 QSOs, Seyferts
Kormendy & Richstone 1995
McLure & Dunlop 2001
Jahnke & Maccio 2011
Wang & Biermann
1998, 2000
These studies all implied that :
------ the broad distribution of the scaling relation could be due to different
velocity dispersion of the accreting gas supplied by different formation
mechanism, and the scaling relation in bright QSOs is probably a limiting case
of black hole evolution by merger enhanced accretion close to Eddington limit
(Wang & Biermann 1998, Wang et al. 2000).
------- only luminous quasars are preferentially triggered by major mergers, as
well as showing that the black hole grows substantially only in a late stage of the
merger and after the peak of star formation (Hopkins & Hernquist 2009 and
Hopkins et al. 2012 ).
------ the creation of the scaling relations can be fully explained by the
hierarchical assembly of BH and stellar mass through galaxy merging from an
initially uncorrelated distribution of BH and stellar masses in the early universe,
provided some physics for the absolute normalization (Jahnke & Maccio 2011).
Interplay between merging, SF and BH growth
Local evidence
The I Zw 1 System
J-band image (ISAAC+VLT)
Foreground star
Scharwachter et al. 2003;
Courtesy: Julia Scharwacher’s ppt
@20 April 2007-Huatulco
1. z=0.06
2. Palomar Green QSO with
a spiral host
3. Possily minor merger
4. Possibly transition stage
5. Narrow-line Seyfert I, probably
young stage of nuclear activity
(Mathur et al. 2000)
6. Black hole mass, small BH,
QSO in formation?
Local evidence
1.
2.
3.
4.
z=0.367
radio source
Mv ~ -25
first solid identification of a quasar
host galaxy
5. possibly two interacting galaxy centers,
as a major merger
“Antennae”-like merger?
Courtesy: Julia
Scharwacher’s
presentation
@20 April
2007-Huatulco
~ 1” to the NE of the QSO nucleus,
possibly two merging nuclei?
Stockton & Ridgway 1991
Merger-driven Evolutionary sequence
from ULIGs to QSO
Sanders et al. 1998
Signs of two galaxy
centers, as a major
meger
Signs of SF
enhanced by tidal
interaction, possibly
a minor meger
ACS’s coronagraph
reveals a spiral plume
wound around the
QSO, a red dust lane,
a blue arc and clump
in the path of the jet
blasted from the QSO.
Challenges from high-z monsters
Courtesy: Rosa Valiante’s presentation
Walter et al.2004;
Peng et al. 2006;
McLure et al. 2006;
Riechers et al/ 2008;
Merloni et al. 2010;
Wang et al. 2010,2012
How to grow quickly
a monster in the early
universe?
---- by super-Eddington
accretion?
---- by merging of BHs?
---- born as giant babies?
Local outliers and labs
In the outer
envelop of M87
Seth et al. Nat.Vol.513,2014
= M_bh / M*
Scaling relation over cosmic time
The circles are the lensed hosts and the triangles are the directly imaged hosts from
Ridgway et al 2001 and Kukula et al. 2001. Points with a vertical line may represent
the low limits.
Peng et al. 2006
MNRAS 429, 2, 2013
Sample design: 17 ~L* quasar at z~1 and z~2
(-24 =< Mv <= -25, RLQ & RQQ (~ fifty-fifty)
Filter selection: rest-frame U&V, avoiding strong galaxy emission lines
Results: 1) rest-frame U-V colors of host galaxies are systematically
bluer than those of comparably massive galaxies at same z
2) mean SFR decreases by a factor of two from z~2 to z~1;
mean SFR for RLQ are about three times of that for RQQ
3) morphology: all bulge-dominated host galaxies
Passive
M*=10^12M_sun
0.01%
0.02%
0.04%
0.08%
0.16%
0.32%
M*=10^11M_sun
0.64%
1.28% 2.56%
5.12% SF
Host galaxies of high-z QSOs,
MBH-Mbulge relation at z~3
Schramm et al. 2013
IRCS+AO observation of UM402 at z~3
5” x 5”, AO corrected FWHM~0.”2
A faint tidal tail?
AO corrected FWHM~0.”13
1) 2”.4 north of the QSO sightline. The candidate is indicated in the image.
2) impact parameter of ~ 19.6 kpc, if at z~2.53.
3) apparent K-magnitude m=21.91+/-0.26, as well as a red color J-K~1.6
Wang et al. 2013, 2015
WFC3/F140W archive images :
2 orients x 2 dithers / single
orbit
Pixel scale 0.13”
Total exposure: 811.736s
AJ152,38L,2016
Simulated images of z~2 QSOs with MICADO@E-ELT in Ks band, assuming a
0.6” seeing, and a very compact and faint host galaxies of Re~0.3”, m(k)~ 23
For those z~2 QSOs
whose host galaxies
are 3-4 magnitudes
fainter than the
nucleus, it’s possible
to determine their
host galaxy
luminosity with an
accuracy better than
10-15%.
Thank you very much !