June 6-8, 2018
Galaxy-Evolution Workshop 2018@Ehime Univ.

The Circumnuclear *Multi-phase* Torusin the Circinus Galaxy Revealed by ALMA→ Izumi et al. 2018c, to be submitted

Takuma Izumi(NAOJ Fellow),
K.Wada, R.Fukushige, S.Hamamura (Kagoshima Univ.),
K.Kohno (IoA/Univ. of Tokyo)
1

SMBH obscuration: Torus

2(Strict-) Unified scheme
Type-1

Type-2(e.g., Antonucci 1993, ARA&A, 31, 473)

Type-1HαType-2~a few to 10 pc?
Urry & Padovani 1995, PASP, 107, 803

λ (Å)
Q. Physical origin of the torus??

Big challenge to the paradigm
12μm/VLTI

E4U3-U

8UU2-U 1-U
3 26elo50-U3ngaU1U2-U4NlarNtio

10004-B

2H0-G0A&,A356824)10(2PoFcor [Jy]

v [m]

E0-G0

D0n!

Circinus galaxy

A&A 563, A82 (2014)

3010

1Epcc-Fig. 4. Correlated fluxes of the Circinus galaxye
12 µm for all uv points containing
useful in50
sp s.atterferometric
50colour-coded−data.
Thepointsareer al accordingry -to their correlated flux, F (12 µm),eeh erv using
v aesquare
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ti en as al colours:p cin
Ru [m]vueδmbnibdetio Ci r oi fi st at ow m iﬀ berctsdnpA82ft nss o 563,e e he mhefoisteTristram et al. 2014, A&A,od,od ) c fluxorspectrum
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c cto is r en om
O inw 2007.
appendix)
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tiv publishedrucesht
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f .
s rsre g ﬀe ee The wavelength calibration uof the-50A2oetsff

δtotCED]as[mcor• Polar elongation in MIR continuum of the Circinus galaxy!?
• Statistical confirmation (e.g., Lopez-Gonzaga et al. 2016)

Multi-phase Dynamic Torus model

4

Wada 2012, ApJ, 758, 66

Fountain scheme + Dust rad. transfer

512μm• Indeed, MIR polar elongation
was reproduced• IR SED is well-explained, too.
• Consistent with observations
30 pc
Schartmann et al. 2014,MNRAS, 445, 3878

(morphological/photometricmanner)

6Out Study:
Multi-phase circumnuclear obscuring structures
studied with ALMA

• Atomic vs molecular gas dynamics?

→ geometrically thicker structure in an
atomic disk than a molecular disk?

• Geometrical thickness due to outflows?

ALMA Cycle 4 Observations (Band 7 + 8) 7

. Curran, B. S. Koribalski and I. BainsThe Circinus Galaxy (4.2 Mpc)
HI 21cm

18 kpc• Compton-thick AGN (Arevalo+2014)- NH ~(6-10) × 1024 cm-2- L2-10keV ~ (2-5) × 1042 erg/s• Low SFR (i.e., weak SN-feedback)→ Test the fountain scheme• High resolution CO(3-2) + [CI](1-0) in

ALMA Cycle 4 (PI: T.Izumi)→ molecular + atomic structures and theirdynamical diﬀerences

Curran et al. 2008,MNRAS, 389, 63• θ ~ 5 pc (CO) & ~15 pc (CI)Molecular & Atomic gas distributions

8Izumi et al. 2018c, to be submitted

12CO(3-2)• CND (D ~70 pc) + Spirals• M ~ 3×10 M (CND)

CNDH26sun- c.f., MBH ~ 2×106 Msun

+Spiralarm•

NH2 ~ 5×1023 cm-2 (AGN)- beam-averaged- NH (Xray) ~ 6×1024 cm-2

• CND will be a significant
nuclear obscurer!

Molecular & Atomic gas distributions

9

Izumi et al. 2018c, to be submitted[CI](1-0)• Similar 2D distribution
to the CO(3-2)+• Tracing the samevolume???

• But we don’t know 3Dstructures!

10
Decomposition of Cold Gas Dynamics
T. Izumi et al.

CO(3-2)

Izumi et al. 2018c, to be submitted

(b)

(a)

(d)

• Global motion is dominated by rotation(e)• We decomposed the dynamics with tilted-ring models- Vrot, σ, inclination, P.A.

18

CI vs CO: Multi-phase Torus Dynamics

11T. Izumi et al.

Izumi et al. 2018c, to be submitted(a)

Velocity (km/s)

160 Blue = CO(3-2)
Red = [CI](1-0)

12080Dispersion

400(b)

σ/Vrot (~H/R)

Rotation

0200.5

4060

Radius (pc)

80 100•0.40.3• Geometrically thicker atomic disk than

0.2

the densediskr < 10 pc!Gaussian fit toTable 6.mol.
Resultsof theatthree-component[C I](1–0) spectrum→ Multi-phase geometrical structures!

0.100

Figure 18.
Line profile of the [C I](1–0) measure
the AGN position (with the single 0′′ .71 × 0′′ .66 beam
the Circinus galaxy. Three-component Gaussian fit wasformed: eachthincomponent
the black-da
Geometricallymol. is& indicatedatomicbydisks
atlines, and the total model is shown by the red-solid line
derived line
are summarizer > 20spectively.
pc (c.f.,Thelow-SFRin propertiesCircinus)
Table 6.

204060Radius (pc)

80Central

Peak(mJy beam−1 )1107.9 ± 1.6

Centroid(km s−1 )453.7 ± 5.6

FWHM(km s−197.7 ± 0T. Izumithe
et al.
Then, what makes
geometrical thickness?

Flux density (mJy/beam)

1200
1000

12Nuclear-scale (15 pc) spectrum(b)[CI](1-0)
FWHM ~ 320
km/s[CI](1-0)

FWHM ~ 240 km/s

800
600
400200CO(3-2)•0Nuclearshowsa18.
Line[CI](1-0)
profile ofspectrum
the [C I](1–0)
measuredat
250 300 350 400 450 500 550 600Figure650′′′′the AGNlarger
position(withthesingle0.71
×0FWHM than CO(3-2). .66 beam) ofthe Circinus galaxy. Three-component Gaussian fit was pergure 11. Line profiles of the [C I](1–0) and theCO(3–2)
formed:each component is indicatedbythe black-dashed′′′′Multi-Gaussians
yieldedabetterfit
asured at (a) the inner 10 × 10 box and (b) the AGN
lines, and the total model is shown by the red-solid line, re′′′′ation (with the single 0 .71 × 0 .66 beam) of the Circinus→ The
Almostsymmetric
emergenceof theinspectively.
derivedline properties
are summarized
axy. The uv-range and the beam size of the CO(3–2) data
Table 6. additional blue- and red-components
matched to those of the [C I](1–0) data. The multiple

Velocity (km/s)••

n-line profile in (a) is due to the spiral arms. Results ofCoherent motion like outflows??
gle Gaussian fits to the CO(3–2) and [C I](1–0) spectra
the AGN position (indicated by the dashed lineand dotTable
6.-Resultsof the three-component
Gaussian
fit to theconsistentwith the fountainmodel
hed line, respectively) are summarized in Table[C 5.
I](1–0) spectrum- will fall back to the disk (failed wind)Quantitative comparison with our modelCO(3-2): TB

13[CI](1-0): TB(inclination = 75°)
Izumi et al. 2018c, to be submitted• M , Eddington ratio, CND-scale M : Circinus-like values• Hydrodynamic simulation + XDR chemistry (Wada+16) + rad. transfer• CO(3-2) → mid-plane of the CND/torus• [CI](1-0) → mid-plane + puﬀed-up component due to outflows
BHgas

Quantitative comparison with our model

14

Izumi et al. 2018c, to be submitted• Indeed, we found diﬀerent line profiles for the simulated CO(3-2) and [CI](1-0)• Triple-Gaussians can well fit the profile → outflow components stand out• Good consistency between ALMA obs. and our simulation→ Support the fountain scheme, where atomic outflows play the key role indetermining the “torus” geometry.

Summary• Now we are testing the multi-phase dynamic torus model with

ALMA: ~5-15 pc resolution CO(3-2) and [CI](1-0) data are in hand.

• Gas (and dust) distributions = CND/torus + spiral arms.
• The CND can provide a significant nuclear obscuration (as a torus).
• CI (atom) gas is in a geometrically thicker volume than the CO(molecule) gas at r < 10 pc.
→ multi-phase gas dynamics in the torus!

• The thickness of the atomic disk would be due to nuclear atomic
outflows, as expected in our fountain model→ Physical origin of the torus!?

15