銀河進化研究会 2016年 6月 3日 東北大学

AGN key sciences enabled by
TMT/MICHI

市川幸平
JSPS fellow (PD) at NAOJ
1and co-PI of TMT AGN/BH
physics group

What is MICHI (未知)?

mid-IR (MIR) band imaging/spec (+IFU/pol?)One of the TMT 2nd gen. instruments (CfP in 2017?)

co-PIs in US/Japan
C. Packham (UT San Antonio)
M. Honda (Kurume Univ.)

Sght collaboraSon between US and Japan☑ Wavelength: 3-13 (-25um) um : L, M, N, (and Q?)☑ 0.1 mJy @ 10 um imaging w/ 1hr elapsed time
☑ <0.1” @N (~0.03” @ L)
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MICHI science group
7 categories and PIs of each science group

Each group has completed iniSal science cases (2016 May)

Dust, molecules are the key
Great synergies w/ ALMA, JWSTStudies of galaxies are sSll missing

MICHI AGN/BH group16 members (as of May 2016)
A. Alonso-Herrero, P. Gandhi, K. Ichikawa (co-PI), M.
Imanishi (co-PI), H. Inami, T. Izumi, N. Kawakatu, T.
Kawamuro, M. Kishimoto, N. Levenson, E. Lopez-Rodriguez,K. Matsuoka, T. Nagao, N. Oi, C. Packham, M. Shirahata☑ Group w/ IR, ALMA, X-ray, polarimetry, and theory backgrounds☑ We welcome new members anytime!
contact => kohei.ichikawa@nao.ac.jp

11 science cases in total (as of May 2016)
3 science goals☑ Resolving the AGN tori
☑ Peering AGN torus origins/fueling☑ Revealing jet properties of black hole (BH) binaries
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TMT/MICHI
3 2 goals of AGN/BH sciences with MICHI
1. Resolving the AGN tori

2. Peering the torus origins and fueling

3. Jet properSes of Black Hole (BH) binaries(not AGN but *ght connec*on to AGN feedback)6

TMT/MICHI
2 goals of AGN/BH science with MICHI
1. Resolving the AGN tori
2. Peering the torus origins and fueling

3. Jet properSes through Black Hole (BH) binaries (notAGN!)

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AcSve GalacSc Nuclei (AGN)
Rees 84;Antonucci & Miller 85; Urry & Padovani95

Supermassive Black Hole (SMBH)

GalaxyAGN

dusty torus<10 kpc<10 pcAGN Uniﬁed Model☑ op)cal-UV: accre)on disk
☑ X-ray: hot electron corona☑ Infrared (IR): dusty torus(dust/gas provider to SMBH)
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NLR
Co-evoluSon of SMBH and host galaxiesAGNs oTight correlaSon between MBH and Mbulge
torus-s
Magorrian relaSon

MBH [Msun]

AGN<10 pcDetectab

Kormendy & Ho 13

Mbulge [Msun ]Galaxy10 kpcAGN torus bridges SMBH and the host galaxies☑Knowing Torus => Understanding SMBH/galaxies
9Torus: very compact in MIR☑ MIR interferometry constrained torus (emission) size

< 0.1’’ @z>0.005
Tristram+07,14☑ torus size: < 10 pc-scale

Honig+13☑ V ↓ when Baseline (BL) ↑ => sign of resolved torus?
☑ MIR emission is elongated in polar direcSon?
see Tristram+09,+11,+14; Kishimoto+11; Hoenig+12,+13; Lopez-Gonzaga+16a,b10

TMT era with MICHI☑MICHI could directly (parSally) resolve torus @L, M, N band

VLTI

TMT (simulaSon)
Science Case (SC) of Lopez-Rodriguez+

Honig+13

We can obtain
1. dust distribuSon (polar direcSon or not?)+ with the help of (clumpy) torus model,

2. physical parameters (Mdust, inclinaSon)

see SCs of Lopez-Rodriguez, Izumi 11

Polarimetry☑Polarimetry tells dust structure more than total ﬂux image

100 pcGarcia-Burillo+16

10 pc

GTC/CanariCam 8.7 um
Lopez-Rodriguez+16☑Polarimetry could tell the torus morphology(see SCs of Kishimoto, Lopez-Rodriguez)
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TMT/MICHI
2 goals of AGN/BH science with MICHI
1. Resolving the AGN tori
☑ L, M, and N band direct imaging☑ L, M, and N band imaging polarimetry
2. Peering the torus origins and fueling
3. Jet properSes through Black Hole (BH) binaries (notAGN!)

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How does the torus feed SMBH?

☑ Hydro+radia)ve transfer simula)ons suggest
inﬂow/ou\low into the SMBH (fountain model)
Schartmann & Wada 14 based on Wada 12’s radia)ve code

Kawakatu+08: inﬂow induced by nuclear SB (and SN)

1. nuclear inﬂow/ouqlow
2. nuclear SB
are the keys of AGN fuelingCO high-J absorpSon: inﬂow/ouqlow tracer☑ CO 4.7um absorp)on: ro-vibra)onal line with J=0->1
Shirahata+13☑ Good to know density, temperature, and velocity!
☑ It is available from the ground☑ high spec. resolu)on is necessary (R>5000@M band)☑ 50 mJy => 10 mJy @M band w/ TMT (see SC of Ichikawa, Shirahata+)

Ionized nuclear ouqlow: [SIV]10.5um☑ ionized line [SIV]10.5um (and/or [NeII]12.8um)☑ good tracer of nuclear ou\low (high energy poten)al)☑ strong against ex)nc)on
Not achievable w/ ALMA bands, op)cal, but IR!
(Mason+06)
IRAS F00183

N band IFU will reveal nuclear gas kinema)cs(to check fountain model)(see SC of Izumi, Nagao)(Spoon+09)

LAGN vs LSF : 100 pc => 10 pc scale☑MICHI can resolve nuclear SB w/ 10 pc scale☑PAH 3.3 and/or 11.3 um: pure SB tracer☑L or N band conSnuum : AGN torus dust tracer(Vaisanen+12)(Esquej+14)☑ L and N band IFU are crucial for this study!
(see SCs of Imanishi, Oi for L band, andAlonso-Herrero, Kawakatu for N band)Summary: Instrument Requests

2 goals of AGN/BH science with MICHI
1. Resolving the AGN tori (II: compelling)☑ L, M, and N band direct imaging☑ L, M, and N band imaging polarimetry
2. Peering the torus origins and fueling (III: excellent)☑ L, N band IFU☑ M band high spec. resoluSon

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Summary: Instrument Requests

2 goals of AGN/BH science with MICHI
1. Resolving the AGN tori
☑ direct check of the polar elongated emission☑ direct check of the torus models
2. Peering the torus origins and fueling☑ tracing 10 pc scale SB, inﬂow/ouqlow
MICHI will be…

the MICHI (道; path) to the MICHI (未知; unknown)
Contact:
chris.packham@utsa.edu, hondamt1977@gmail.com 19

Appendix

Synergy with ALMA
☑MICHI can resolve torus in MIR☑ ALMA reveal molecular gas/cold dust structure (CND)
Garcia-Burillo+16

CombinaSon of MICHI and ALMA will reveal
whole dust/gas structure in the central 100 pc of AGN(see SC of Izumi)

TMT/MICHI
3 goals of AGN/BH science with MICHI
1. Resolving the AGN tori
2. Peering the torus origins and fueling

3. Jet properSes through Black Hole (BH) binaries (notAGN!)

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Jet properSes of BH binary w/ MICHI
When outburst occurs in BH binary, synchrotron peak (vbreak) appears in MIR
Very few follow-ups (Gandhi+11; Russell+13) due to the limited sensiSvity

LocaSng Jet break vbreakvbreak changes w/ 10 sec scale

Gandhi+11

B (magneSc ﬁeld )R (the size of the jet base)changes rapidly
Requirement:
1. prompt follow-up (< 1 week) once outburst occurs (>10 events/yr)
2. covering wide IR coverage (quasi-)simultaneously to locate break
3. PolarizaSon monitor is also good to trace synchrotron acSviSes 23

instrument
summary24

SensiSvity: imaging

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SensiSvity: spectroscopy (R=600)
N band26

SensiSvity: spectroscopy (R=600)
Q band27

SensiSvity: spectroscopy (R=120,000)
N band28

SpaSal resoluSon of TMT/IRIS, MICHISensiSvity vs. PWVWhat does “outburst” in Gandhi+11 mean?
outburst means the bright epoch in “X-ray”
But the state must be “low-hard” state, not high-so{ state

Cajole Bel+11 (2010 outburst of GX 339-4) Corbet+13 (Lx vs Lradio | Lcorona+disk vs. Ljet)

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TMT/MICHI w/ high R>5000☑ Using 4.7um CO abs.,
Shirahata+13 detected threevelocity components from ULIRG

1. blue (v=-160km/s) w/ 270K-> ouqlow from the accreSon disk?
2. red (v=+100km/s) w/ 700 K-> inﬂow to the accreSon disk
3. v=0km/s w/ 20K☑ Good support of clumpy torus☑ ﬁrst robust inﬂow/ou\lowdetec)on in buried AGN
Shirahata+13

Candidates: AKARI CO detected BAT AGN☑ AKARI discovered CO detected(?) candidates of type-2 AGN(Shirahata+14; Castro+14)

CO?
☑ NH > 1023 cm: one criterion? (e.g., Meijerink+05)☑ ~10 candidates from AKARI observed BAT/AGN sourcesTorus models on the marketType-1☑ torus is clumpy! (clumpy model; Krolik & Begelman 86, Nenkova+02)
radia)ve code (e.g., CLUMPY) enable us to✓ Get torus geometry from the observa)ons
Ichikawa
et al.
(see Ramos Almeida+11;
Alonso-Herrero+11;
Ichikawa+15 )clumpy model
Type-1
NHBLR

HBLR

HBLR

Ichikawa+15
Ramos Almeida+11

But, the model is staSc (no-inﬂow/ouqlow)
model does not tell us the torus origin (and SMBH growth)

How and when does the torus feed SMBH?

Herschel study of CO high-J lines☑ CO high J (J>10) lines is a good AGN indicator

Mashian+14☑ Good to know density, mass, and temperature☑ spa)al resolu)on is limited (due to Herschel)☑ Not available currently