Chandra and ALMA Study of X-ray Irradiated
ISM in Circinus Galaxy at 10 pc Resolution(TK et al. to be submitted.)

Taiki Kawamuro (NAOJ)
Collaborators: T. Izumi, M. Imanishi (NAOJ)(red = [S II], green = Hα+[N II], blue = [O III]; Maiolino+94)

Galaxy and Black Hole Co-evolution- Tight correlation between

the massive black hole (MBH) and host gal. properties.
→ the co-evolution
GÜLTEKIN ET AL.

Vol. 6

Black hole mass

204

(Gultekin+09)

stellar dispersion in the bulge

Figure 1. M–σ relation for galaxies with dynamical measurements. The symbol indicates the method of BH mass measurement: stellar dynamical (pentagrams),dynamical (circles), masers (asterisks). Arrows indicate 3σ68 upper limits to BH mass. If the 3σ68 limit is not available, we plot it at three times the 1σ68 or at 1.5 tim
the 2σ68 limits. For clarity, we only plot error boxes for upper limits that are close to or below the best-fit relation. The color of the error ellipse indicates the Hubtype of the host galaxy: elliptical (red), S0 (green), and spiral (blue). The saturation of the colors in the error ellipses or boxes is inversely proportional to the area
8.12

−1 4.24

Galaxy and Black Hole Co-evolution- Tight correlation between

the massive black hole (MBH) and host gal. properties.
→ the co-evolution- AGN may be a key object.

✓ SMBH growth✓ High energy output(i.e., AGN feedback)AGN uniﬁed modelGalaxy and Black Hole Co-evolution- Tight correlation between

the massive black hole (MBH) and host gal. properties.
→ the co-evolution

Esquej et al.
(Esquej+14)

hysical Journal, 780:86 (15pp), 2014 January 1- AGN may be a key object.

✓ SMBH growth✓ High energy output(i.e., AGN feedback)- Starformation rate(SFR) and AGN mass
Comparison
between the SFR relation
on different scales, whereaccretion
implies typical physical scales of ∼0.6 kpc and SFR
isear

nuclearscales. Nondetections
are plotted at a Matsuoka+15)
2σ level. Symbols as in(e.g., Imanishi+11,
e dashed line shows the median value for the nuclear/circumnuclear
r the detections of the nuclear PAH feature (see text and Table 3).
ne indicates a nuclear/circumnuclear ratio of one.
sion of this figure is available in the online journal.)

AGN uniﬁed model
Figure 7. Observed nuclear SFR vs. ṀBH relation. Predictions from Hopkins& Quataert (2010) are shown as dashed lines. We show the ṀBH ≈ 0.1 × SFRrelation, which is expected for r < 100 pc, and the 1:1 relation which, is expected
for the smallest physical scales (r < 10 pc). The solid line represents the fit toour detections of the nuclear 11.3 µm PAH feature (see text for details).
(A color version of this figure is available in the online journal.)

Starformation and AGN accretion power-Suppressed SF in X-ray luminous AGN?
→ AGN may have strong impacts on SF.

Harrison et al.

(Harrison+12)

e n?
iv
at tioeg la
N rrecoX-ray Dominated Region (XDR)
Strong penetrating power of X-rays largely heats the ISM,
so called XDR- X-ray producing photoelectrons dissociates molecules-ξeﬀ = LX/R2nH2N1.1att(Maloney+96)

Atomic/molecular gas vs. SFRn the random observational
andom uncertainties in the0.1 dex; see Fig. 3). Therehis -large scatter. Variations
actor; as a molecular comst peak, then dissipate, andll evolve as well, as the rewe have no reason to expectof gas to stars is a universal
in x 6).
above are likely to bias theus gas surface density law toter that might influence theeasured Schmidt law would
nversion factor X. A fixednalysis. The conversion facy an order of magnitude tod this is unlikely. A multiGarcia-Burillo et al. (1993)
in X between the spiral arm
ule out some possible bias
e suspect that the dispersion
easuring uncertainties (espensities) and physical effects,
associations and clusters andefficiency among the clouds.
the H i and inferred H2 surs dominates most of the gas
he comparison of SFR andrelation- in Figure 4,

Molecular gas seems to be a important parameter for SF.

HIH2,H2(Kennicutt+07)

Fig. 5.— Relation between local SFR density and molecular and atomic hyAGN may suppress
SFbymolecules
drogen surface densitiesthe
separately.
The solid
greendissociatingand open black triangles denote H surface densities (see Fig. 4), with open red circles indicating CO upper! # (3:78 ! 0:09); ð8Þlimits (same symbol notation as for Fig. 4). Blue asterisks show the correspondLet’s confirm
thedissociation!
ing relation between
SFR surface
densities and H i surface densities. The dashedH2rogen surface densities are2line shows the best bivariate least-squares fit to the molecular densities alone. The

CXO and ALMA obs. of Circinus galaxy
Investigation whether AGN has impacts on SF→ Detailed study using a nearby AGN host as a laboratory

Circinus galaxy:- D = 4.2 Mpc (i.e., 0”5 ~ 10 pc)- host of Compton-thick AGN

Chandra & ALMA
(sub-) arcsec resolution- X-ray and submm/mm→ strong penetrating power
to dust/(gas)→ suitable for studying nuclear
dense regions- high S/N data are available-black hole masses.

CXO & ALMA archive data

2. List of Archive Data
ChandraTable
datalist

ChandraObs. ID Start Obs. Date (UT) Exp. (ksec) Grating~ 300 ksec (!) archive data
(1)
(2)
(3)
(4)
ALMA356
2000/03/1420NO
365
2000/03/14
1NOcovers
374
2000/06/15
6
YES
multi-species
62877
48
2000/06/16
YES(CO, HCO+, HCN) emission
4770
2004/06/02
48
YES
4771
2004/11/28
52
YESand12823
2010/12/17
147
NO
multi-transition
12824
2010/12/24
38
NO(J=4-3, J=3-2)
Note— Columns: (1) Observation ID. (2) Observation start(3) Exposure after the data reduction. (4) Check on= 5 mol. linesStudy of Circinus Galaxydate.
with Chandra and ALMA
grating observation.

ALMA datalist
Tag

Program Info.

Table 2. List of ALMA Datasets
Obs. DateExp.

Moleculeslines (4)trace the(5) dense gas. The HCO+ (J = 4–3) line isobserved in ** and** data. The former data provides(a) #2015.1.01286.S (PI: F. Costagliola) 2015/12/31 3
HCO+ (J=4–3), HCN(J=4–3), CO(J=3–2)
the high-spatial andhigh-sensitivity data, where as the+(a) #2015.1.01286.S (PI: F. Costagliola) 2015/12/31
HCO(J=3–2),HCN(J=3–2)
latter5 take anadvantage
thatwithin this execuation its+(b) #2016.1.01613.S (PI: T. Izumi)
2016/11/24HCOalong(J=4–3)line is125
observedwith the dense gas tracer of theHCN (J = 4–3).
Note— Columns: (1) Tag of the dataset to indicate that each dataset is used for diﬀetent purposes. (a) ThisThe following subsections describe how we reprocess
(1)

(2)

(3)

dataset is mainly utilized to constrain physical properites of the molecular gas (Sections 3.2 and 2.6.1). (b) This0.01

keV2 (Photons cm−2 s−1 keV−1)

What can we know from X-ray?
10−3

Iron-Kα fluorescent line is very important- τ~1 for log NH ~ 23.9 cm-2
probe of dense gas material- 6.4 keV
6.4emission
keV 輝線: 非熱的放射
high penetrating power
Suitablefor nuclear region study!
光電離
電子衝突
10−410−5(data−model)/error

10−620−2345678678

Energy (keV)

keV2 (Photons cm−2 s−1 keV−1)

0.01

10−310−410−5> 7.1 keV photons(data−model)/error

10−620−2345
Energy (keV)X-ray emission maps
Dec. (J2000)

Chandra provides us with the mostprecise images at X-rays (~ 0.”5)

Dec. (J2000)-3-6 keV

1 sec (20 pc)
6.2-6.5 keV

1 sec (20 pc)
RA (J2000)

X-ray emission maps
Chandra provides us with the mostprecise images at X-rays (~ 0.”5)- Divided image shows dense gas
distribution.
6.2-6.5 keV/3-6 keV-> EW(FeKα)Dec. (J2000)-Dec. (J2000)

preliminary

1 sec (20 pc)

3-6 keV

1 sec (20 pc)
6.2-6.5 keV

1 sec (20 pc)
RA (J2000)

X-ray emission maps
with an enlargement of the central region
which clearly shows that, although thenucleus is much more peaked in K' thanin Hand J, its position does not vary significantly with wavelength (the IR images
are aligned within 0.2//).
The relative positions of the central
peaks in the various lines and continua
are summarized in Figure 9 where wealso include the contours of the [FeXI]
coronal line image (see also 094). Note
that, while the optical line/continua images are aligned within 0.04", the relative position of the IR peak is more uncertain (± 0.2" 30") but sufficient to showa shift between the optical and IR continuum peaks.
A 'true-colour' line image (red = [SII],green = HCY+[NII], blue = [0111]) is shownin Figure 10 where the structure of thecone and of the surrounding galaxy are
best visible.

6.2-6.5 keV/3-6 keV-> EW(FeKα)EDec. (J2000)

Chandra provides us with the mostprecise images at X-rays (~ 0.”5)- Divided image shows dense gas
distribution.
-The nucleus

East-limb In the continuum at 5100 A (Fig. 1) theConeemission is dominated by late B stars
associated with an old starburst and extends over several arcsec with two spatially resolved peaks which are separated by 2// N-S but connected by afainter bridge. The southern peak is coincident with the much more prominent
7000 A nucleus (Fig. 2 ) which is single
and unresolved. In the infrared (Fig. 8)
the nucleus also shows only a single
peak whose position is coincident at J, H
and K' but which is more sharply peaked
at K'. This infrared peak is also shiftedby 0.25// relative to the southern visible
peak in the direction away from the ionization cone (Fig. 9). We therefore assume that the 'true' nucleus is at or close

South-limb

1 sec (20 pc)

Dec. (J2000)

preliminary

3-6 keVN

1 sec (20 pc)

W

6.2-6.5 keVS

Figure 10: A 'true colour' image of the Circinus galaxy with red = [SIIJ, green = Ho:+[NIIJ andblue = [0111]. This representation clearly shows the ionization cone, the extended circumnuclear
starburst and the chain of supernova remnants to the S.

1 sec (20 pc)

Within the cone there are highexcitation [FeXI] (see 094 for moredetails of the coronal line emission) and [0111] clumps with observed

detailed spectroscopic study of the extended NLR of NGC1 068 (Bergeron et al.
1989). One possibility is that the [SII] knot
is a photodissociating (or photoevapo-

RA (J2000)

Iron-Kα and Mol. gas emission lines
HCO+(4-3)→ Molecular gas→ high critical dens.
= dense gas tracer- Iron-Kα line
→ gas irrespectiveof atomic/mol. phases

Dec. (J2000)-preliminary

1 sec (20 pc)

RA (J2000)

Figure 2. Each of figures show the same

Iron-Kα and Mol. gas emission lines
HCO+(4-3)→ Molecular gas→ high critical dens.
= dense gas tracer- Iron-Kα line
→ gas irrespectiveof atomic/mol. phases-Clear atomic-to-mol.
transition boundaries-Mol. dissociation ?

Dec. (J2000)-preliminary

1 sec (20 pc)

atomic-to-mol. gastransition boundary

RA (J2000)

Figure 2. Each of figures show the same

Iron-Kα and Mol. gas emission lines
HCO+(4-3)→ Molecular gas→ high critical dens.
= dense gas tracer- Iron-Kα line
→ gas irrespectiveof atomic/mol. phases--

Clear atomic-to-mol.
transition boundaries

Dec. (J2000)-Mol. dissociation ?
→ NEXT
Quantitative
discussion w/ XDR model

East-limb

preliminarynucleus

ConeSouth-limb

1 sec (20 pc)

atomic-to-mol. gastransition boundary

1.1attRA (J2000)
ξeﬀ = LX/R2nH2
N
Figure 2. Each of figures show the same

Mol. line ratios ﬁtting by RADEX non-LTE code
5 molecular lines → 10 line ratios- 4 free par. = NH2, n(H2), Tk, [HCN]/[HCO+]-NucleusCone

East_Limb

South_Limb

log NH2[cm-2]

24.0[23.0-25.0]

25.0[20–25.0]

23.5

22.0
[21.5-22.0]

log nH2[cm-3][HCN]/[HCO+]

5.5[4.5-5.5]
380[100–400]
2
[2-4]

3.0
[3.0-5.0]
390[110-390]
2
[2-3]

4.5
[3.5-5.5]
40[30-60]
3
[3-4]

6.0
[6.0]
30
[20-30]
3[-]

chi2

1.15

0.24

0.58

3.33

Tk
[K]

[20.0-21.0,22.5–23.5]

X-ray dominant region (XDR)
ξeﬀ = LX/R2nH2Nαatt
LX ~ 1.3e+43 (1–100 keV)
(NuSTAR estimate by Arevalo+14)

R ~ 60 pc(spatial resolved map)

nH2 ~ 3.0-6.0 cm-3
(mol. line ratios fit by RADEX)Natt ~ 1e+23.9 cm-2
(τ~1 for the neutral iron)

Nucleuslog ξeﬀ -4.0~-5.0

Cone

East_Limb

South_Limb-2.5~-4.5-3.0~-5.0-5.5

X-ray dominant region (XDR)
ξeﬀ = LX/R2nH2Nαatt
LX ~ 1.3e+43 (1–100 keV)
(NuSTAR estimate by Arevalo+14)

R ~ 60 pc(spatial resolved map)

nH2 ~ 3.0-6.0 cm-3
(mol. line ratios fit by RADEX)Natt ~ 1e+23.9 cm-2

(τ~1 forthe neutraliron) that the X-ray radiation from the AGN canOurresultsupports
dissociate the molecule(, and the SF may be suppressed therein.)

Nucleuslog ξeﬀ -4.0~-5.0

Cone

East_Limb

South_Limb-2.5~-4.5-3.0~-5.0-5.5

Summary-

Science BG: Physical connection between SF and AGN-CXO & ALMA obs. of Circinus gal. at 10 pc resolution→ Study of X-ray heating eﬀects on ISM--Anti-spatial correlation b/w the dense molecular gasand iron line distribution.

-From ξeﬀ, we examined the XDR model to interpret themol. deficit.

-AGN X-ray can form the XDR and destructs molecule.

AGN may suppress the SF, if the molecular formation iscritical for forming stars.