Approaching the origin of thesuper-massive black holes with TMT
review of the science cases from TMT-AGN science WG in Japan

Masayukiki Akiyamaki((Tohokuh k U.))
Chair: Tohru Nagao (Ehime)
K.Aoki (NAOJ), M.Imanishi (NAOJ), S.Ozaki(NAOJ), N.Kawakatsu (Tsukuba), T.Kawaguchi(Tsukuba), H.Sugai (Kyoto), A.Tanikawa((Tsukuba),
su uba), Y.Terashimae asa ((Ehime),e), T.Misawasa a(Shinsyu), T.Minezaki (Tokyo)
2011 03 28
2011.03.28

“Origin of the super-massive black hole (SMBHs)”
What do we want to know in general ?
1. Seeds of the SMBHs

Intermediate ? Massive ?

2. Growth history of the SMBHs

Accretion ? Merging ?
Accretion: Eddington-limited ? Super-Eddington ?
AAccretion:i
Ob
Obscuredd?N
Non-obscured
bd?

3 IInterplay
3.
tl b
betweent
growthth off SMBH
SMBHs andd galaxies
l i
Feedback processes ?
Feeding processes ?

Three major areas with TMT
A. SMBHs in the local universe with nearby galaxies.
= statisticali i l constraints
ion theh seeds
d off theh SSMBHs

B Central 100pc around SMBHs with nearby AGNs
B.
AGNs.
= understanding on the feeding and feedback processes= obscuration in AGNs

C. Cosmological evolution of SMBHs with AGNs atdistant universe.

= quantitative understanding on the growth history of SMBHs= “co-evolution” of SMBHs and galaxies= feeding and feedback in the “violent” epoch, during the eraof significant growth

A. SMBHs in the local universe
A-1:
A
1: Pushing stellar/gas dynamics SMBH mass estimate tomore distant galaxies (<1000Mpc), establish connection
between stellar/gas dynamics and reverberation mapping
studies (currently only 2 cross calibration available)
available).
Stellar/Gas Dynamics
yBaseline for local SMBHs

8m to 30m
Black hole mass constraint
limit estimated withthe size of “sphere ofinfluence”
influence

Reverberationmapping:

Baseline for distant SMBHs

A. SMBHs in the local universe
A-2:
A
2: Pushing stellar/gas dynamics SMBH mass estimate tolower black hole mass range with dwarf galaxies toexamine the low mass end of the mass function of SMBHs
which can constrain the mass of the seed black holes
holes.

Stellar/Gas
Dynamics

8m to 30m

Barth et al. 2005

ReverberationmappingiA. SMBHs in the local universe
A-3:A
3: Intermediate mass black hole can provide us direct
constraints on the seed black hole.
Are intermediate mass black holes associated withglobular clusters ?
Use change of radial velocity of stars in the central
region instead of velocity dispersion etc.
Expected velocity change due to Keplarian motion
aroundd 3000M
3000Msolarl blblackkhholel iis 200-300m/s/yr
200 300 / / att
1500AU from the black hole.
Intermediate mass black holes identified with ultraluminous X-ray sources ?
D t ti
Detecting
opticalti l counterparts
tt off ULXs
ULX
systematically.
Detailed studies on the opticalp
counterparts,p, i.e.
SEDs and line diagnostics.

B. Central 100pc around SMBHs
B-1: Mid-IR observation of dusty
y torus = structure of dusty
yobscuration and large-scale feeding to the SMBHs
Simulations on the structureof molecular gas torus
torus.
MIR diffraction limited
imaging (Q-band0.12”=20pc@z=0.01) toexamine the structure inthe lower temperature
dust component
64 64
64x64pc
iregionSStructureevolution
l iaroundd 100pc100region
iWada & Norman 2002
64x64pc region

High mass-accretion rate
Star-formation in gas-disk

Kawakatsu & Wada 2008
LLow
mass-accretion
tiratetB. Central 100pc around SMBHs
B-2: Energeticgin the heavily-obscured
yAGNs,, i.e. ULIRGs
MIR high-spatial-resolution
high spatial resolution
spectroscopy and imaging
are necessary toquantitatively evaluate
th energetic
theti ini thethULIRGs.
MIR imaging can constrain
the contribution from SF
based on limits on thesurface density
y of SF.
Imanishi et al 2006, 2007

AGNSF

Imanishi et al 2010

B. Central 100pc around SMBHs
B-3: Feedback pprocesses examined with NLR structure(associated narrow-absorption lines of QSOs and NLRs of
distant AGNs at high-redshifts)
Dynamical structure ofnarrow-line region canprovide us information on
feedback processes.
Feedback processes can beevaluatedl t d with
ith associatedi t dnarrow-absorption linesof QSOs and NLR
dynamics of AGNs athigh-redshifts

0.4 arcsec-resolution 3D-spectrograph data of NGC1052
102km/sk / velocityld
difference
ffSugai et al. 2005

C. Cosmological evolution of SMBHs
C-1: Spectroscopic identification of obscured AGNs at high redshifts are
crucial for quantitative understanding of SMBHs accretion growth
Spectroscopic-z
po opsample
a pPhotometric-z
oosamplea p

K=22.5
Narrow-line AGNs

Broad-line AGNs

Gal-SEDs
GalSEDs

QSO SEDs
QSO-SEDs

Photometric redshift estimations of X-ray sources found in Subaru XMM-Newton
Deep Survey field suggest that there are large number of obscured AGNs atredshift
d hift >1
1 among ththe sample
l beyondbd opticalti l spectroscopytlimits
li it off 88-10m
10class telescope (Akiyama et al. 2011).

C. Cosmological evolution of SMBHs
C-1: Spectroscopic identification of obscured AGNs at high redshifts are
crucial for quantitative understanding of SMBHs accretion growth
Z>1.5 X-ray sources (zspec or zphot) in GOODS-North(Akiyama et al.
al 2011)

K=22.5

V=24

Black dots: optical spec IDs
Red filled: MOIRCS spec IDs
Red open: MOIRCS spec cont. detection
Red cross: MOIRCS no-detection

Even with deep (3-5hours)
NIR spectroscopic
observation cannot
identify these objects.
There are large numberof X-ray sources beyond
optical / NIR spectroscopy
limit of 8-10m classtelescopes.
Considering the X-ray to[OIII] etc line flux ratio,
2-32
3 hours integration withTMT is necessary todetect rest-frame opticalemission lines of X-ray
AGN foundAGNs
fd iin thehdeepest Chandra fields.

C. Cosmological evolution of SMBHs
C-2: Properties
pof host ggalaxies are important
pto understandco-evolution of SMBHs and galaxies
Black hole mass with broad-line width

Stellar mass of host galaxies

Detailed studies onlypossible
ibl with
ith 3030m

Ratio
i betweenbblblackkhholel massand stellar mass of hostgalaxies is examined withground-based
d bd AO
AO-imaging
iiup to redshift ~3 so far (ex.
Falomo et al. 2008).
HHowever,th
the uncertaintyt i t withith
the current dataset is large(see next slide), and 30m
diffraction limited studies
are necessary to obtainsolid constraints on theredshift dependence of theratio.

C. Cosmological evolution of SMBHs
C-2: Properties
pof host ggalaxies are important
pto understandco-evolution of SMBHs and galaxies
8m to 30m
K-bandHb dH-band
QSOimg

PSF
subtracted

Suabru AO188+IRCS imaging of z~3 QSOs (Schramn et al. 2011). Diffraction limited
imaging with 30m telescope is critical to detect faint host galaxies around QSOs.

C. Cosmological evolution of SMBHs
C-3: Metalicities of high-redshiftgQSOs can pQ
provide theinformation on the chemical evolution of the central regionsof galaxies

Juarez et al. 2009
including Nagao et al. 2006

Summary and instruments required
A SMBHA.
SMBHs ini theth localll universei
A-1: more distant SMBHs = IRIS+NFIRAOS
A-2:
A
2: lower mass SMBHs = IRIS+NFIRAOS,
IRIS+NFIRAOS highhigh-dispersion
dispersion NIR
spectrograph+NFIRAOS
A-3: intermediate mass black holes = IRIS+NFIRAOS, highdi
dispersioni
NIR spectrograph+NFIRAOS
th NFIRAOS
B. Central 100pc around SMBHs
B-1:
B
1: dusty torus,torus feeding = IRIS+NFIRAOS,
IRIS+NFIRAOS MIR
MIR-imager+MIRAO
imager+MIRAO,
high-dispersion NIR spectrograph+NFIRAOS
B-2: energetic in ULIRGs = MIR-imager+MIRAO
B-3: feedback processes = IRIS+NFIRAOS, WFOS+3D, highdispersion Opt/NIR spectrographs
C Cosmological evolution of SMBHs
C.
C-1: AGN surveys = WFOS, IRMS, wider-field IRMS
C-2: host galaxies = IRIS+NFIRAOS
C-3: metalicity evolution = IRIS, WFOS