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Antonucci, R. R. J.,Baribaud,& Miller, TJ-term monitoring
opticala andnear-response
infrared observations
wavelengths inshowed
delayed
of
the
A. J.
Baribaud, T., Alloin,Barth,D., Glass,ared wavelengths
a delayed
theThe minor
K-bandshowed
light curveafter thatresponseof the V ofband.
conBarth,
A.M
J.
Barth, A. J., Nguyen,
M. L.,and light curveafter thatof theV band.
The
con- flux Barth,tributionof theaccretion
disk
in minorthe K-band
was A.
subBarvainis,
J., Pancoast,A., ThorRution of the tracted
accretion
disk inthe
thevariation
K-band offlux
Barvainis,
R. 1987, Barvainis,
ApJ, 320, R
5
to derive
the wasdust subtorus emission,
andM. C
Barvainis,of
R. 1992, Bentz,
ApJ, 400,
5
ed to derive thethe CCF
variationof thedust
torus toemission,
andmeasurements
analysis
wasappliedobtain 49
Bentz,M. C
CBentz, M.luC., Denney,K. D.,
CCF analysis
wasappliedtoobtain49
measurementsofreverberation
lags
for
the
innermost
dust
torus.
The
optical• |{#mA-!!
Bentz,
M.CC
Bentz, M. C., Denney,K. D.,
rberation lagsminosity
for the innermost
dust
torus.
The
opticalluof the continuum emission from the accretiondisk
2009a,
Bentz,
M.
C.,! Peterson,
B. M.A–ÃÀÆÆ×ÒÀn'Æ×ÒÀn
!
!
!
!
!
The AstrophysicalJournal,788:159 (21pp),
2014
20 from thethe
Koshida et
al.
osity
of the continuum
emissionaccretion
disk and narrow-line
was estimatedbyJunesubtracting
host-galaxy
M. C
2009a, ApJ,
697,Bentz,
160ÃÀÆGr:°²¦«! !We ! found! that! Bentz,!theM.!reestimated byflux
subtracting
the host-galaxy
andfluxes.
narrow-line
contributionsin the V-band
C.,!
Peterson,2006b,
B. M.,A
0.4
ApJ, 644,Bentz,
133 M. C
'«xÖ¡³!
0 dustverberation
lags fluxes.
for theWe
innermosttorus
correcontributionsin theV-bandfound thatthere- strongly2006b,
Boroson,T.
Bentz,M.
C.,
Walsh,
J.
L.,
Bar
with
the opticalluminosity
= −16
to !!
1pc
erationlags lated
for– theinnermost
dust
torus
da6©c! strongly!in the! range!corre! of !MV ! Boroson,! ! T.
Cackett,K.
E.A
0.2
A., & Meyers,−22 (Koshida+14)!
mag. We applied
the regression
new data
d with the opticalluminosity
in the rangeof MV =analysis−16 to to ourCackett,
Clavel,J., W
RE. M., Horne,
K., &
J., W
to obtain
correlationof logto∆tour(days)−2.11–0.2
MVJ.,ormag. 0We applied
the theregression
analysisnew =dataClavel,Reichert,Clavel,
G. A., Allo−1
-1 44
Collier,rin oflog c∆t
(pc)
0.5(L
erg
), assuming
theClavel, J.,
Wamsteker,W., &S.,Gbtain the correlationlog=∆t −0.88(days) +=−2.11–0.2
MV sorV /10
Denney,K.2
0.5 44-0.2−1as that reported in previous
Collier,
S.,&Peterson,
B.
M.
slope
of
∆t
∝
L
to
be
same
studc∆t (pc) = −0.88 + 0.5(LV /10 erg s ), assuming the
Denney,K.P
Denney,K.
D.,
Bentz,
M.
C.,
0.5
The
intrinsic
scatterof theincorrelation
was estimated to bee of ∆t∝ L ies.
to
be
same
as
that
reportedprevious
studDeo, R.
-0.4–
For!most!luminous!quasars!
!
!
!
!
!
!
!
!
!!
Denney,K. D.,
Peterson,B. P.,
M.
0.13 dex, andits estimatedpossibleorigins
were
discussed.
Deo,
R.
P.,
The intrinsic approximately
scatter of the correlation
was
to
be
Deo,! R. P.,
Crenshaw, D. M., K-2 !
(e.g.!Assef+15)
!
!
!
!
!
!
!
!!!!!!!!!!
-2.5
-2
-1.5
-1 !
-0.5
0 !
Thedex,difference
in internal extinction
and the delayedDeo,
response
oximately 0.13
anddiscussed.
dust!torus!
R. P., Richards,Diamond-S
G. T., Nik
log Lbolits/LEddpossible origins wereDietrich,M
BLRr10!pc!(?)!
ofchanges
in
lag
times
to
the
flux
variations
could
have
partlyin
Diamond-Stanic,A.
M.,
Rieke,
inner!radiusdifferenceininternal
extinction
andthedelayedresponse
Figure 12. Residual of the dust lag from the best-fit regression line plotted
Doroshenko
against the Eddington contributed
ratio (obtained by the CCF
analysisassuming α = 0scatter;for
Dietrich,
M.,
Peterson,B. M., Gtotheintrinsic
however,
we
could
not
detect– NGC!4395!(so!called!the! have! !partly! ! ! ! Koshida+14
! !!
hangesin oflagtimes
tothe influx
variations
could
the subtraction
the accretion-disk
component
the K-bandflux).
Y. S. 201
Doroshenko,
V. T., Sergeev, S.
changesinthelag–luminosity
correlation
with
theP., Hu,-3
ributed to thesystematic
intrinsic
scatter;
however,
we
could
not
detectleast!luminous!Seyfert)!
! ! ! 41! !42 ! 43 ! 44Y.! S. 45!2012,! 46MNRAS,!! Du,
47 426, 4
with the model. subclass
The observation
of
an
AGN
with
a
superDullemondoftheSeyferttypetheand the Eddington
63!pc!
ematicchanges
inr thewith the ratio.
log (λLλ(V)[ergP.,
s-1Hu,])
Eddington
mass accretionrate
islag–luminosity
requiredto(Minezaki+06)!
investigate correlation
Du,
C.,
Lu,
K.-X.,
et al.
10
in
Edri,
H.,
R
Furthermore,wecomparedratio.
our results with theradius– C. P., &region
effectanisotropic
illumination
the slim
disk.
Dullemond,
van
Bemm
class
ofof theSeyferttypeofandthe
Eddington
Figure 13. Radii of the innermost dust torus
and the broad emission-line
756, 73log (radius [pc])log∆t - log∆tfit [days]

WTKª{#mA-ν(BLR) plotted against the V-band luminosity. Filled circles (colored red inthe half- engine with a higherdotted
normalized R1/2 in a physical scale. Figure
UV luminosity.
horizontalAlso
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Power-lawfits to R1/2 in pc at
ht radius R1/2 in pc plotted against the same UV luminosity. radii at 2.2 µm normalized by Rin for the s
8.5 and 13 µm as a function of luminosities arehe physical scale, the radius in the mid-IR increases with lu- (Kishimoto et al. 2011), including two ov
nosity much slower than L1/2 . Power-law
at dotted horizontal line indicates radius = Rin! fits to R1/2 in "pc
0.21±0.05
radial structure, this6νLν (5500 Å)
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10 erg/s
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536, A78We(2011) can– Half6light!radii!from!MIR!interferometer!(Kishimoto+11)!
!
"0.01±0.07
simple models. rest frame using R1/
6νLν (5500 Å)d
R1/2 (13 µm) = (1.3 ± 0.3)
pc,We can(5)also tocalculate46
νobs fνobsan(1average+ z)4 /(π10 erg/s!
"0.01±0.07
rest frame using R1/2 as (νLν /4π)/(πR
6νLν (5500 Å)
Figure10 shows thi
13!um
pc,(5)
4
2
2 (13 µm) = (1.3 ± 0.3)
46 erg/s
νobs fνbeing(1 + z) This/(πθ1/2
θ1/2 isc
where we see 10
that
R1/2 at 13 µm is consistentobs
1pc towithcan) where
be directly
Figure 10 shows in
thisa function
constant.
theassame
figure,of
ere we see that
R1/2
at 13areµm
is consistent
being studies
This canofbethe
directlycompared 1with
These
results
contrary
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temperature
at athegi
nstant.
inetthefigure,where
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8.5!um
High!luminous!AGNs
mid-IRsize as a function of luminosity by Tristramal. same(2009)
jects
show
brigh
1
These results
arecontrary
to
those
of
previous
studiesofthetemperature
at
a
given
wavelength.
In
and Tristram & Schartmann (2011), who concluded that the mid- the mid-IR the
brig
Fig. 8. Halfd-IR size as a function of luminosity by Tristram et al. (2009) 1/2
jects
show
the
brightness
temperaturegreen for 13
IR size is consistent with being proportional to L . They used to ∼200 K. Inagainst
theUVnld Tristram & Schartmann (2011), who concluded that the mid- the mid-IR the brightness
temperatur
6 νL (5500 Åa singlewith
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this2.2!um
can lead to a close to the observe
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Kishimoto+11!
than L , ort
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luminosity
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ing their Lthea strong
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configuration,
to brightness
ond andat thirdy-axistemperatures
2.2 and13 R
inner
radiuscase, the simple
size
is quiteinadequate
strong dependence
on the Gaussian
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in this forluminosity
dependen
ondrepresentand third y-axis,
respectively.
We
1/2

46 erg/s
10"0.21±0.05

ν

1/2

1/2

3C 273

IRAS 13349+243

IRAS 09149−6206

I Zw 1

IRAS 05189−2524
H 0557−385

NGC 7469

NGC 1068

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NGC 424NGC 3783
ESO 323−77
NGC 4507

NGC 4151

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Mrk 1239

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NGC 5506

NGC 1365

0.10

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1041

not a statistical error b
r1/2 from the upper lim
servation) and lower li
The magenta and red li
radius as derived empi
outermost radius for 30
by the Barvainis formul
12 µm show a large sc
times larger than at 2 µ
ways a factor of three sm
radius. The statistical emeasurements are smal
therefore not shown. Th
bolometric correction f
text.

10
10
10
10
10
– Half6light!radii!from!MIR!interferometer!(Burtscher+13)!
Mid−infrared luminosity n L (12 µm) [erg/s]• The!12um!size!scale!with!luminosity,!but!with!larger!scaYer!
• Signiﬁcant!contribu[on!of!unresolved!(<5!mas;0.1610pc)!ﬂux!
Fig. 36. (Half-light) ra
42

43

44

45

46

n

Half−light radius [pc]

10.00

1.00

1pc

Circinus

0.10
mid−IR interferometry (type 1 AGNs)
mid−IR interferometry (type 2 AGNs)

Burtscher+13!
type1,!type2

near−IR interferometry (Swain, Kishimoto, Pott, Weigelt)
near−IR reverberation mapping data + fit (Suganuma)

0.01
1042

1043

bands, probing the sas a function of bolo
blue and red circles amates from MIDI obse
type 2 sources respectiv
the near-infrared interand derived ring-fit ra
Kishimoto et al. 2011a
The yellow plus symb
near-infrared reverberat
Suganuma et al. (2006)
the yellow line is a fit
ter in the mid-infrared
larger than in the nearfor NGC 4151 is not anotes the range for r1/(from single-dish obser
from our modeling. The
MIDI size measuremen
symbols and therefore n

1044
1045
1046
Bolometric Luminosity [erg/s]

1047

1048

ET AL.
51, as observed within ourRADOMSKI
N andsured color-corrected FWHM of !
ation
throughout
the nightm andstars
0>58 at18.2 lm basedon aof less thanatwere10.8
n.variations
Short integrationsof ! 5%Gem
t 18.2lm. Absoluteof !
nto NGC
4151 due calibration
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UMa,
andand" Aql,
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563,
A82(2014)
ration
value
and
FWHM
were
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M of less than –6%Inner!wall!of!the!dust!torus!or!the!NLR!dust!?!
throughout theunt
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different
spectralslopenoofe respecations
4151
showedation
throughout
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151,
observed
withinourandendividedinto increments of time
ines
very
00
n
variations
of
less
than
5%
at
10.8
Fig.
1.—N-band
imagesofthecentral'6of NGC 4151. All
asuredcolor-corrected
FWHM
of
!
frequen(60s).
smoothed with a '0>25 Gaussian filter to enhance low-level em
t 18.2calibration of !
wever,
the lm. Absolute
E 18.2 lm based on a
lm
and
0>58
at
onathetelescopewith themodel
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lowest contour representing the 3 % level of the smoothed data (0tedsuchthat north was
and wereeast
cannotbe
djustedforfilterandatmosphericn to NGC
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The next image shows the PSF star ! Gem scaled to the same lev
variations
array.
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value
and
FWHM
were
also
obviously
4151 for comparison.
The 1,next
residua0
PSF.
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ofandseveralstanNo.
2003four images show the MID-IR
70!pc
e‘‘unrotated
’’
!17=4
!22=9
at
4151 after subtraction of the PSF (unresolved component) scale
unt
for ltheUMa,
different
spectral
slope
of
Gem,
and
"
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showedarameters
ctively, to match the position angle
90%, 80%, and 70% of the peak height. In the 80% image, d151,
asobserved
within
our
N
and
ple
is
the
M
of lesspupil,
than
6%projected
throughout
theelescope
asonthedelineate NGC!4151!(type1)!
the edges of the ionization region, as observed by E
−50cefilling
asuredcolor-corrected
FWHM
of
!
ationsofNGC
4151Thisshowednogth
range
by!MIR!direct!
(1993), while
the solid line represents the radio jet axis. With the p
C
4151
was
observed.
isnecesmponentslm
and 0>58into
at 18.2
lm based
to the sameheight as NGC 4151 (100%), the00unresolved compo
endividedincrements
of on
timea
imaging!using!
nt
forof the telescope
ure hasa the rotation
Fig.
1.—N-band
imagesof thedetected
central at'610of
NGC 4151. Alln.
Short
integrationsof ! Gem were 1 pc sents'73%of the total
emission
lm.
−100
h can
be
(60
s).
ground6based!
OSCIR(during an observation orsmoothed with a '0>25 Gaussian filter to enhance low-level em
milar
de-NGC 4151 due to the stability
on
to
dg)
with
large!telescope!
tioon
ofdue
thethetotelescope
scaled logarithmically.
Contours are separated by a factor of 1.
100
50 the Gemini
0 of the
−50
−100
the
alt-azmount
PSF.
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representing the 3 % level of the smoothed data (ntedsuch thatPSF
north
was upandrotaeast
Radomski+03
.erometricInaddition,
imageswere
Circinus!(type2)!by!MIR!inteferometer!
overlaid!on![OIII]
Gem, landshowedFig.UMa,7. False-colour
image"ofAql,
the three-component
model for the
mid-next image showsThethe PSF! Gem
scaledto the same le'0>53–0>58
at 10.8
andstar18.2
lm,
respectively.
array.
In
imagesofgalaxyte.
ccountforpostprocessing,theslighttheinfraredemissionof therotation
nucleus of the of
Circinus(fit 3). The
Tristram+14
4151
comparison.
The
next four
imagesshow '400
the residuaM‘‘ ofless6%throughout
thecoloursthanred, green
and bluecorrespondto the modelat 13.0 µm, 10.5
µm forourshows
N-bandimageofthecentralpc
reunrotated
’’
!17=4
and
!22=9
at
xposure
times
of
NGC
4151.
and
8.0
µm,
respectively.
The
colourscalingislogarithmic
in
order
to
4151
after
subtraction
of
the
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component)
scalations of NGC 4151 showed nooffset δ DEC [mas]WTKª{#mA-RÏ×¾×A-• RÏ×¾×A-!!(individual)!
A&A 563, A82 (2014)

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No. 1, 2003

50

INNER PARSEC OF CIRCINUS AGN

167

N

100

offset δ DEC [mas]e respecervals.
ines veryfrequenwever, theminantlynd differcannot bevariations
obviously– Circinus!galaxy!(Seyfert!type!2)!

E

0

1pc

−50

1 pc

−100
100

50

0
−50
offset δ RA [mas]−100Fig. 7. False-colour image of the three-component model for the midFig. 3.—Superposition of maps for 1997 July and 1998 June. Color indicates velocity, as in Fig. 2. The black scale bar corresponds to 0.2 pc. The blue andred curves
infrared emission of the nucleus of the Circinus galaxy (fit 3).
Theindicate the limb or midline of the putative edge-on warped disk, where the orbital velocity is parallel to the line of sight. The red curve is a secondorder polynomial fitted to the midline. The blue curve is a reflection of the polynomial about the center of the disk. The good agreement between the reflectedcolours red, green and blue correspond to the model at 13.0 µm, 10.5
curve µm
and the blueshifted midline demonstrates how well the data fits an antisymmetric warp model. The lengths of the arcs indicate the range of radii overwhich redshifted maser spots trace a smoothly declining rotation curve (see Fig. 4). The green line represents the innermost orbit, defined by the most highly
and 8.0 µm, respectively. The colour scaling is logarithmic in orderred- andto
blueshifted maser spots. The cross marks the estimated dynamical center of the disk.

Tristram+14!MIR!interferometer

Greenhill+03!H2O!maser!(VLBI)

Til08

6.1

42.1

Til08

6.2

42.6

This work

7.5

Til08

1.7

0.11–0.4

Til08

1.2

0.24–0.80

Kuo11

2.5

∼0.3

tation curves are in boldface. (2) – Distance in Mpc. We adopted the distances used
nsic column density in units of 1023 cm−2 . (4) – References for NH ; Awa09 – Awaki
Cappi et al. (2006); Don03 – Done et al. (2003); Fuk11 – Fukuzawa et al. (2011);
997); Mat99 – Matt et al. (1999); Til08 – Tilak et al. (2008). (5) – Logarithm of them−2 ). For NGC 2273, UGC 3789, NGC 2690 and NGC 6264 we used the observed
ctor of 60 (see Section 5.3) to estimate the intrinsic luminosities (6) – References– Cappi et al. (2006); Gre08 – Greenhill et al. (2008); Til08 – Tilak et al. (2008,
hole mass (in M$ ). (8) – Disc size in pc. (9) – References for columns (8) andal. (2009); Til08 – Tilak et al. (2008, and references therein). (10) – Logarithm ofinosities are taken from Kondratko et al. (2006b, and references therein) for all thesity was derived directly from the spectrum), UGC 3789, NGC 2690 and NGC 6264

wnloaded from http://mnras.oxfordjournals.org/ at University of Tokyo Library on December 16, 201542.5

RÏ×¾×A-• RÏ×¾×A-!!

– Luminosity!dependence!(Tilak+08,!Castangia+13)!
– Blackhole6mass!dependence!(Wardle!&!Yusef6Zardeh+12)!

1pc

Radius (pc)oundThethatAstrophysical Journal Letters, 750:L38 (5pp), 2012 May 10
Wardle & Yusef-Zadeh
ess of theTable 110h the aim
Physical Characteristics of Megamaser Disksn Table 6th VLBI)
SourceBH Mass
Disk Size
7(×10 M" )(pc)
the black1
ity inNGC
the 1194a
6.5 ± 0.3
0.53–1.33
he objects
NGC 2273a
0.75 ± 0.04
0.028–0.084
a
UGC 3789
1.04 ± 0.05
0.084–0.30
galaxies,
a
Rmax
1.16
±
0.05
0.13–0.37NGC29603789 and
0.1
b
NGC 4258
3.7 ± 0.01
0.17–0.29
n recentlya
NGC 4388
0.84 ± 0.02
0.24–0.29
sic X-ray
NGC 6264a
2.91 ± 0.04
0.24–0.80
literaturea
NGC 6323
0.94 ± 0.01
0.13–0.30
0.01
pton-thickc
Sgr A*
0.43 ± 0.02
0.038–0.13
106
107
108
or in caseBlack hole mass (M ), we Notes.
have
Figure 1. Vertical bars indicate the range of radii of the maser distributiona Kuo, as et al. (2011).
L2−10
for published H2 O megamaser disks with well-determined Keplerian rotation
osityb was
Herrnstein etal. (2005).
Figure4. Observed inner radii of the masing discs against AGN bolometriccurves vs. central black hole mass (Kuo et al. 2011; Herrnstein et al. 2005). The
Castangia+13
Wardle&Yusef6Zardeh+12
stellardisk;
Lu foret al.
usedc Compact
thisextent of the compact
stellar disk at the Galactic center (lowest-mass point; Lu
luminosities
the(2009).
sources in Table 6. This figure is an updated version
et
al.
2009)
is
plottedforcomparison. The errors in the black hole masses andilak et al.
of fig. 7 of Tilak et al. (2008). The diamonds mark the position of the discradii are a few percent. The dashed line represents an approximate empiricalmasers already present in the plot of Tilak et al. (2008), while the triangles
6, which

1pc

ÃÀÆA-!§RÏ×¾×A-!
• RÏ×¾×A-!!
– Luminosity!dependence!(Minezaki!unpublished)!
10!N3079radius!(pc)

1pc 1

N1194
Circinus

N4945

N1068
N4388

N4258

0.1

N2273

0.01

dust!reverbera[on!radius!
regression!line!from!Koshida+14
38

39

40

41

42

43

Log![OIV]26um!emission!line!luminosity

44

Centaurus A

Half−l0.10

by the Barvainis formula. The half-light
12 µm show a large scatter, but are abtimes larger than at 2 µm. They are alm
ways a factor of three smaller than the Ba
radius. The statistical errors of the MID
measurements are smaller than the symb
therefore not shown. This plot makes use
bolometric correction factors describedtext.

ÃÀÆA-!§RÏ×¾×A-!
rin (empirical)

0.01
1041

1042
1043
1044
1045
Mid−infrared luminosity n Ln (12 µm) [erg/s]

1046• RÏ×¾×A-!§!MIR!half!light!radii!

– H2O!maser!may!originate!in!the!equatorial!molecular!disk!
Fig. 36. (Half-light) radius at various
bands, probing the structure of the– Comparable!to!or!smaller!than!the!MIR!half!light!radii!
as a function of bolometric luminosit
10

radius!(pc)

1pc 1
0.1

Half−light radius [pc]

10.00

1.00
CircinusN1068

0.10
mid−IR interferometry (type 1 AGNs)
mid−IR interferometry (type 2 AGNs)
near−IR interferometry (Swain, Kishimoto, Pott, Weigelt)
near−IR reverberation mapping data + fit (Suganuma)

0.01

0.01

38

1042

1043

39

40

1044
1045
1046
Bolometric
Luminosity[erg/s]
41
42
43

1047

Log![OIV]26um!emission!line!luminosity

44

1048

blue and red circles are our own siz
mates from MIDI observations of type
type 2 sources respectively. The green st
the near-infrared interferometry observ
and derived ring-fit radii (Swain et al.
Kishimoto et al. 2011a; Weigelt et al.
The yellow plus symbols are the UV/onear-infrared reverberation mapping rad
Suganuma et al. (2006) and references t
the yellow line is a fit to these data. Th
ter in the mid-infrared sizes is signifi
larger than in the near-infrared. The er
for NGC 4151 is not a statistical error bnotes the range for r1/2 from the uppe
(from single-dish observation) and lowe
from our modeling. The statistical errors
MIDI size measurements are smaller thsymbols and therefore not shown.

ÃÀÆÆ×ÒÀª• ÃÀÆÆ×ÒÀª!covering!factor!
– Covering!factor!0.7!→!half!opening!angle!45°!(!hr!)!
– $6¦!covering!factor,!obscured!frac[on!«Y/!
– Receding!torus!model!(Lawrence!91)!
Maiolino+07ÃÀÆÆ×ÒÀª• ÃÀÆÆ×ÒÀª!covering!factor!
– $6¦!covering!factor,!obscured!frac[on!«Y/!
– Receding!torus!model!(Lawrence!91)!
Low!L

High!L• h!constant!
• rin!!L1/2!
• →!half!opening!angle!L61/2ÃÀÆÆ×ÒÀª
AA53CH10-Netzer

ARI

16 July 201512:38

• ÃÀÆÆ×ÒÀª!covering!factor!
– $6¦!covering!factor!«Y/Ü ! ! ! ! ! !
eg¯>U©°¤¥^¨³lJ;!redshim!dependency?!
ab

Optical classification

X-ray classification
0.3 < z < 0.8
0.8 < z < 1.1
1.1 < z < 1.5
1.5 < z < 2.1
2.1 < z < 3.5

Obscured AGN fraction (%)

d from www.annualreviews.org
itaka on 12/17/15. For personal use only.

100

80

60

40

20

0

43.0

43.5

44.5

44.0
–1

log LX (erg s )Figure 8

45.0

43.0

43.5

44.0

44.5

45.0

–1

log LX (erg s )Figure!from!Netzer!15,!originally!presented!by!Merloni+14

The fraction of obscured and unobscured AGNs at various redshifts and L(2–10 keV). (a) Fractions obtainedby optical classification. (b) Fractions obtained by a classification based on column densities derived from

H8==ª• hx(106100pc)!

– PAH!11.3!um!feature ! ! ! !
ﬂux!peak!at!the!nucleus!
– ;106100pc!¦®H8= 2774
! ! A. !Alonso-Herrero! ! !et al. ! ! !! !!
W ! ! ! ! ! ! ! ! ! ! ! ! ! !!
2770
A. Alonso-Herrero et al.
(e.g.!Alonso6Herrero+14)!

67!pc

Downloaded from http://mMrk1066!(type!2)

Figure 1. Mrk 1066. The top panel is the GTC/CanariCam Si-2
(λc = 8.7 µm) image on a colour linear scale as plotted on the right-handside. Orientation is north up, east to the left. The image was smoothed with aGaussian function with σ = 0.6 pixels. The contours are also in a linear scalewith the lowest contour corresponding to the local background value plus 1.5
standard deviations measured in the image before rotating and smoothing
the images. The hatched circle represents the angular resolution of the image (FWHM) approximated as a Gaussian function. The dotted lines show
the approximate width and orientation of the slit. The middle panel shows
the partially reduced GTC/CanariCam 2D spectrum in a square-root colour
scale and smoothed with a Gaussian function. On the y-axis positive offsets
indicate north-west and negative offsets south-east. The bottom panel compares the GTC/CanariCam nuclear and 0.52 arcsec × 2 arcsec spectra with
the Spitzer/IRS SL spectrum extracted as a point source. We smoothed the
GTC/CanariCam spectra by averaging together three pixels in the spectral
direction.
Figure6. Lower panel: GTC/CanariCam spatial profiles of Mrk 1066 as afunction of the projected distance from the AGN dAGN . We show the profiles

Figure 2. M
GTC/Canari
σ = 0.6 pixe
correspondin
measured indle panel is
y-axis positi
The bottom
in Fig. 1, bot
0.52 arcsec ×
of 1.8 to mat

calibration
10–15 per c
For those8–13 µm spectra to investigate the nature of this extended emission
and its relation to the active nucleus.

star α Cen was obtained between the exposures of Circdifferent PAs. Wavelength calibration is with respect t
etary nebula NGC 6302, which has a rich emission-lin(see Casassus, Roche & Barlow 2000, for the spectrum a
2 O B S E RVAT I O N S
wavelengths).
The spectra were straightened, registered in the disperLong-slit spectra between 8 and 13 µm were obtained at thetionwith reference to the sharp structure in the absorptio
8-m Gemini South Telescope in clearing skies with the facility MIR
to atmospheric ozone at 9.6 microns, and the dispersi
imager/spectrometer, T-ReCS (Telesco et al. 1998), in 2004 May untion from NGC 6302 was applied. The T-ReCS detect
der the programme GS-2004A-C-2. Acquisition images at 12 µm
cross-talk across the different readout amplifiers as is cshowed structure similar to that presented by Packham et al. (2005),
this kind of detector (e.g. Sako et al. 2003), resulting iand slit position angles (PAs) of 100◦ and 10◦ (north through east),ofthe spectrum in the spectral direction. The detectorThalalong and orthogonal to the extended emission, were selected forfrom periodic electronic pick-up noise which manifested
Circinus PA 10 South
Ci
along the detector rows. To provide partial compensatio
effects, the detector signal in theunexposed region lon
centrecenterthe filter cut-off was extracted and applied to1000
the expos
1000
section. The spectra were correctedforatmosphericabs
0.27 S
20!pc
straightening and growing the α Cen spectrum along theing it into the Circinus spectra and multiplying by a blac
10pc!oﬀset
temperature of 5770 K (Cohen et0.54al.S 1996). The bright co100
100
nus is compact and so the slit losses for the galaxy
anstar are probably similar. None 0.80
theSless, the calibration
is likely to be significant and we estimate ∼15 per centK. R. W. Tristram et al.: The dusty torus in the Circinus galaxy
MIR flux calibration from the ground. In fact, the flux
1.07 S10
10
along
the slit is within 10 per centof that measured
in a-0.2 dex
frequency ν [Hz]aperture by Roche et al. (1991), confirming the compac
1012
1011
1010
the nuclear source.
Blue!line:!MIDI!total!ﬂux
1.6 Sbinning three rows toSpectra have been extracted by5-0.5 dex
in spatial increments of 0.27 arcsec, close to thediffra1
1
A&A 563, A82 (2014)
at 8 microns) out to the radii of 1.6 arcsec and eight row
4
directly estimated from the bootstrap distribution of the respec2.1 S
The spectra are presented for thePA 10◦ and 100◦ slitNtive parameter and mark the 68.3% (1σ) confidence intervals.
100-1.0 dex
Our model can fit the data on the shortest baselines veryin Figs 2 and 3, respectively. The noise in the spectr
Fig. 10. Nuclear SED of the Circinus
well, which means that it reproduces the low spatial frequen3
cies of the source adequately. On longer baselines, however, theEdata is not well reproduced by our model. This is predominantly
between 9 and 10 µm because of low atmospheric transm
galaxy. Blue dots are high resolution50
due to small scale variations of the correlated fluxes and differ0.1
0.1
ential phases at longer baselines (cf. Fig. 4), which cannot be
to absorption by ozone in the upper atmosphere,
while tphotometry compiled by Prieto et al.
reproducedbyoursmoothmodel.
We
interpretthesevariations2
as signatures for small scale structures that our model obviously0
thesewavelengths
aredecreasedbysilicateabsorptionin(2010)
plus
anadditional
measurement
cannot replicate.
−4
Finally, a few remarks on degeneracies: several parameters
effects
becomeincreasingly
apparent
in the spatiawith ALMA at λ = 9.3 × 10 m (321 GHz) 8 These
9
10
11
12
13
14
8
of our model are not independent. The clearest example is the1−50
degeneracy between the temperature T and the surface filling
furthestfromthenucleus.
Spatial
cuts
along
the
spectrby Hagiwara et al. (2013). The measurefactor f . Because we are fitting a narrow wavelength range(8 µm < λ < 13 µm), the temperatures of our dust components
been extracted for the two PAs by binning in the spectral
1pc
ment in the J-band,
which is only
an2.upper
are not well constrained. A small change in temperature has a
FigureThe spectra obtained at PA 10◦ . The spectra on the south and north sides of the nucleus
1 pc
−100
direct influence on the brightness of the source, which can beover= offset
0.5 µm.
These
haveandeffective
waveleng
7
8
9
10the surface
11 filling 12
13 de- 14
there is a change in the"λspatialat 1.07arcseccuts
separationthat the on-nucleus
limit, is marked with an arrow. Note
Alsothatshowncompensatedby changing
factor. Similar-6 the axis ratio of thegeneracies arewavelength
present between the
and
100
50
0
−50
−100
−20
−2
λsize
[10
m]
the spectra(bluerepresents the fits
described
in the12.5
text. Flux
is in units
of 10
W cm
.
10.2,
11.3 andmicrons,
respectively,
and µmare−1show
offset δ RA[mas]source, which all change the emitted flux density. Depending on
are low
resolution
IRAS photometry
how well these parameters are constrained by the interferometricFig. 7. False-colour image of the three-component model for the midalong with similar cuts for the reference star α Cen. For αmeasurements, these parameters can become degenerate.
a MIDI
flux spectrum
infrared emission ofcrosses),
the nucleus of the Circinus
galaxy (fit correlated3). Thecolours red, green and blue correspond to the model at 13.0 µm, 10.5 µm
levelstructure seen on the right-hand side of the cuts c
and 8.0 µm, respectively.
The colour
scaling is logarithmicin order to(cyanline),
the averaged
MIDI total flux

H8==ª• hx(1610!pc);!PAH!11.3!um!feature!
Roche+06

– Circinus!
b?@!
4Xy!

offset δ DEC [mas]flux νFν [1014 Jy⋅Hz]

Tristram+14

ii

H8==ª• {#mA-ª=x!
The Astrophysical Journal, 785:154 (22pp), 2014 April 20

Leipski et al.

– {#mA-→!H8==Ú!intrinsic!AGN!dust!torus!!
– many!studies!with!diﬀerent ! ! ! ! ! ! ! !!
samples!and!methods!
– !large!diversity!
The AstrophysicalJournal, 785:154 (22pp), 2014 April 20
Leipski et al.
ν Fν [erg s−1 cm−2]

10−12

10−12

total fit
UV/opt power law

NIR blackbody
torus model1450Å
z−bandFIR mod. BB

y−bandJ, H, K

Spitzer
Herschel

literature data(λrest > 10 µm)

10−12
10−13
10−14

10−13

10

−15

J0338+0021
z = 5.00

J0756+4104
z = 5.09

10−13

NIR blackbody
10−14
torus model

0.1

ν Fν [erg s−1 cm−2]

total fit
UV/opt power law

1450Å
z−bandFIR mod. BB

1
10rest wavelength (µm)

10−12100

10−15

Figure 2. Schematic representation of the components used for SED
fitting. As
10−13
an example, we use the observed photometry of the z = 5.03 QSO J1204−0021.
(A color version of this figure is available in the online journal.)

10−13

10−14

y−bandSpitzer
10−14
J, H, K J0927+2001
Herschel

J0338+0021
z = 5.00

z = 5.77

literature data(λrestJ1044−0125> 10 µm)z = 5.78

10−13
10−14
10−15

J1148+5251
z = 6.43

J0756+4104
z = 5.09

J1202+3235
z = 5.31

The rest frame UV/optical and infrared SEDsof these
10−15
10 objects can be fitted well with a combination of these 4
10−13components. The best fitting model combinations are shown−13
in Figure 3 and Table 6 summarizes some basic10properties
10−14
J1204−0021
J1340+2813
determined from the fitting. Using these fits we also determinez = 5.03
z = 5.34
the relative contributions of the different components to−14
the total
10−15
10infrared SED. For this we combine the dust component in the
J0927+2001
J1044−0125
NIR and the torus model, both of which are likely to be powered
10−14
10−13
z = 5.77
z = 5.78−15 to theby the AGN. We compare this AGN related emission
10
0.1
1
10
100
additional FIR component and show their relative contributions
10−14
rest wavelength(µm)
to the total
infrared emission as a function of wavelength in
J1602+4228
J1626+2751
z = 6.07
z = 5.30−13
Figure 4. We
seeforthatSEDin thepresenceof luminous FIRemission10
10−15
Figure 2. Schematic representation of the components
usedfitting.
As
13
10 L# ), this component dominates the total infrared
0.1
1
10
100
1
10
100
an example, we use the observed photometry(L
ofFIR
the∼
z=
5.03 QSO J1204−0021.
SED at rest frame wavelengths above ∼50 µm for all 10 objects.
rest wavelength (µm)
rest wavelength (µm)−14
(A color version of this figure is available inThis
the online
10
meansjournal.)that in such cases of strong FIR/submillimeter
Figure 3. SEDs of the 10 quasars detected in at least four Herschel bands. The
J1148+5251
J1202+3235
emission, rest frame wavelengths !50 µm isolate the additionalplots shows νFν in units of erg s−1 cm−2 over the rest frame wavelength. Thez=
6.43z = 5.31−15
coloredlines
indicatetheresults of a multi-component SED fit as described
FIR component without the need for full SED fits
(at
least
10

A!schema[c!ﬁgure;!Leipski+14

Leipski+14!!
z=566!quasars

with SEDs with lower values of α1 falling more rapidly at FIR
NETZER ET AL.

0.0 and 0.4, respectively. This relative difference between the

H8==ªVol. 666• {#mA-ª=x!
NETZER ET AL.– Intrinsic!AGN!SED!in!FIR!

Vol. 666

1.0
1.0

νLν

νLν

0.1

0.1
Netzer+07!PG!quasars!“weak!FIR”!sample

p curve) and weak FIR QSOs (right, top curve). The adjacent red SED curves show ‘‘intrinsic’’ AGN SEDs
) spectrum (shown in black) from the mean SEDs. (See text for explanation.) [See the electronic edition

Mullaney+11!Seyfert!galaxies

Figure 7. Left: the mean-average and range of intrinsic AGN infrared SEDs from this study plotted against the observed infrared SEDs of Mrk 231 and N

H8==ª• Recent!results!with!ALMA!

5

10

15

20

25

– Circinus!(1!arcsec!=!20!pc)!
K. R. W. Tristram et al.: The dusty torus in the Circinus galaxy-65 20 19.0

frequency ν [Hz]1014

flux νFν [Jy⋅Hz]

1011

1010

19.5

A&A 563, A82 (2014)

14

1012

5. Discussion
5.1. Morphology

1010

The direct analysis of the data (Sect. 3) and our modelling(Sect. 4) confirm that the mid-infrared emission in the nucleusof the Circinus galaxy comes from at least two distinct components: a highly elongated, compact “disk-like” component anda moderately elongated, extended component. To some degree,
the distinction between the two components is suggested by thetwo different regimes of the correlated fluxes as a function of
the projected baseline length (see Sect. 3.1). Primarily, however, the distinction is suggested by the different orientations of
the two components: the two components are elongated roughly
perpendicular to one another. Two clearly separated emission
components have also been found in NGC 1068 and NGC 3783
(Raban et al. 2009; Hönig et al. 2013), and a two-component
morphology in the infrared appears to be common to a large
number of AGN (Kishimoto et al. 2011b; Burtscher et al. 2013).
We interpret the mid-infrared emission as emission fromwarm dust in the context of the hydrodynamic models of dusty
tori in AGN by Schartmann et al. (2009), Wada et al. (2009) andWada-5 (2012). These models find a relatively-4 cold, geometricallythin and very turbulent disk in the mid-plane of the torus, surrounded by a filamentary structure. The latter consists of longradial filaments with a hot tenuous medium in between. We associate the central, highly elongated component in the Circinus
nucleus with the dense disk in these simulations, and we interpret the extended mid-infrared emission in the context of the filamentary torus structure seen in these models.
A false-colour image of our best fitting model (fit 3) isshown in Fig. 7, with the model images at 13.0 µm, 10.5 µm
and 8.0 µm mapped to the red, green and blue channels of theimage, respectively.
When interpreting our observations, we have to take into account that the emission is dominated by the warmest dust at a
certain location, which normally comes from the dust clouds directly illuminated by the central UV source. There are probably
also considerable amounts of cooler dust. However, the cooler

4

DECLINATION (J2000)

5

directly estimated from the bootstrap distribution of the respective parameter and mark the 68.3% (1σ) confidence intervals.
Our model can fit the data on the shortest baselines very
well, which means that it reproduces the low spatial frequencies ofSpitzer
the IRS
source adequately. On longer baselines, however, thedata is not well reproduced by our model. This is predominantly
due to small scale variations of the correlated fluxes and differential phases at longer baselines (cf. Fig. 4), which cannot be
reproduced by our smooth model. We interpret these variations
as signatures for small scale structures that our model obviously
cannot replicate.
Finally, a few remarks on degeneracies: several parametersof our model are not independent. The clearest example is thedegeneracy between the temperature T i and the surface filling
factor fi . Because we are fitting a narrow wavelength range(8 µm < λ < 13 µm), the temperatures of our dust components
are not well constrained. A small change in temperature has adirect influence on the brightness of the source, which can becompensated by changing the surface filling factor. Similar degeneracies are present between the size and the axis ratio of thesource, which all change the emitted flux density. Depending on
how well these parameters are constrained by the interferometricmeasurements, these parameters can become degenerate.

N

100

E

50
offset δ DEC [mas]

10

1012

flux νFν [1014 Jy⋅Hz]

10

1013

16

3

0

2

−50

1

1 pc

−100

7

100

50

0
−50
offset δ RA [mas]

8

9
10
11
12
wavelength λ [10 m]−100

Fig. 7. False-colour image of the three-component model for the midinfrared emission of the nucleus of the Circinus galaxy (fit
-6 3). The
colours red, green and blue correspond to the model at 13.0 µm, 10.5 µm
and 8.0 µm, respectively. The colour scaling is logarithmic in order toshow both bright and faint features. Clearly the colour gradient of theextended component due to the increase in the silicate depth towards
the south-east is visible. This colour gradient leads to a chromatic photocentre shift towards the north-west. Despite the lower surface brightness, 80% of the emission comes from the extended component. Also
plotted is the trace of the water maser disk: the blue and red parts trace
the approaching and receding sides of the maser disk respectively. Notethat the relative offset of the mid-infrared emission with respect to themaser disk is not known (see text for details).

13

14

ALMA

Prieto+ 2010 & Hagiwara+ 2013
Roche et al. 2006
material only contributes insignificantly to the infrared emission
MIDI total & corr. flux spectra (see also Sect. 5.3).
5.1.1. The disk-like component
three-component model
The disk-like component is highly elongated and has a major
800 K "hot dust" (NIR fit)axis FWHM of ∆ ∼ 1.1 pc. Due to the strong position angle

108
10-6

10

10
10
wavelength λ [m]

10

20.5

Fig. 10. Nuclear
SED of the Circinus
21.0
galaxy. Blue dots are high resolution
photometry21.5compiled by Prieto et al.
(2010) plus an additional measurementwith ALMA22.0
at λ = 9.3 × 10−4 m (321 GHz)
by Hagiwara et al. (2013). The measurement in the 22.5
J-band, which is only an upper
limit, is marked with an arrow. Also shown
23.0
are low resolution IRAS photometry (bluecrosses), a 14MIDI
flux spectrum
13 10.3 correlated
10.2
10.1
10.0
09.9
09.8
09.7
09.6
(cyan line), the averaged MIDIRIGHT
total
flux (J2000)
ASCENSION
scale
flux range=
2.7 - 30.0
mJy / beam
spectrum (blueGrey
line)
and
high
resoluCont
peakflux =the
1.3517E+01
Jy / beam
Levs =Roche
1.352E+00(-3,(2006,-2, 2, 3, 4,grey
5, 6, 7, 8, 9)
tion spectrum fromet *al.
line).Fig.The
SED
of
our
best
fittingmodel
4.— Integrated intensity image (contours) of the 321 GHz His
O maser overlaid the 321 GHz continuum
image (gray scale) observed with the ALMA. The peak integrated intensity of the H O maser and the peakplottedinred. A possible compactbeam
hot dust
flux density of the continuum are 13.6 Jy km s
and 40.6 mJy beam , respectively. Contour
levels and grayfitted
scales (scales
2.7 mJydata(∼3σ) tomarked
30 mJy) are denoted in the image. The synthesizedcomponent,
to arethefromSED
beam (FWHM) is plotted in the left bottom corner.
by the dark red boxes, is shown by the dotted, dark red line. A zoom on the10N-band
region with linear scaling of the axes isshown as an inset. See text for further details.
2

Hagiwara+13!
321GHz!con[nuum!
(gray!scale)!
Flux!within!φ!26!pc
2

−1

2

dependency of the correlated fluxes for the longest baselines,
the position angle of the major axis is very well constrained:
ψ2 = 46 ± 3°. The strong elongation of this component with anaxis ratio of-3more than 6 : 1 at first suggests an-2interpretation
as a highly inclined disk, as in Tristram et al. (2007). This interpretation is supported by the close agreement in orientationand size of this component with the warped maser disk fromGreenhill et al. (2003). The masers were modelled by a thin disk
extending from rin ∼ 0.1 pc to rout ∼ 0.4 pc. The maser disk iswarped with the position angle changing from 29° ± 3° at rin
to 56° ± 6° at rout . With a position angle of ψ2 ∼ 46°, our disklike component now matches this orientation much better thanpreviously. The larger size of the mid-infrared disk as comparedto the maser disk could be evidence of the disk extending out
to larger radii than is probed by the maser emission. We emphasise that the agreement is only in orientation and size, not in
the absolute position. With MIDI alone, no absolute astrometry
is possible because the absolute phase signal is destroyed by theatmosphere (see Sect. 2.2). By consequence, the relative position
between the maser disk and our disk-like component cannot be

20.0

10-1

−1

Tristram+14;!the!SED!model!based!on!the!MIR!IF!data!
Does!NOT!need!addi[onal!cool!dust!for!the!ALMA!ﬂux!
in generalshow a steep decrease in the torus SED towards longer NGC 1068 (Jaffe et al. 2004; Raban et al. 2008; López-Gonzaga
wavelengths.
Towards shorter wavelengths, the model SED rapidly deA82, page 12 of 30

et al. 2014). NGC 1068 is similarly well resolved (both in termsof visibility and scales of the supposed sublimation radius) as−1

S. García-Burillo et al.: Molecular line emission in NGC 1068

the overall SED
the galaxy. The e
conversion facto
in Sect. 6 to deriregion.
The SED w
model to deriveand emissivity imeasured fluxes⌫ ⇥ B⌫ (T dust )/D
as ⇠352 GHz ⇥ ((a value rounded
Klaas et al. 200
the distance. Prio
were corrected fo
S. García-Burillo et al.: Molecular line emission in NGC 1068 imaged with ALMA. I.
the central 100 ap
The best MBB
the overall SED of the dust emission in the central r = 400
pc of
T dust = 46 ± 3 K
the galaxy. The estimate of Mgas based on this fit and the implied
rameters of the ficonversion factor for CO (XCO ), discussed in Sect. 5.4, are
used
range
of missing
and
3.2.
in Sect. 6 to derive the mass load of the outflow identified in this
The value ofregion.
tral gas mass bud
The SED was fit using a modified black-body scaling(MBB)ratio ofmodel to derive the dust temperature (T dust ), dust mass 2013)(Mdustto)the gastral2
kpc
and emissivity index ( ) in this region. In this approach, the of NG
2004, 2007),
whi
measured fluxes, S ⌫ , can be expressed as S ⌫ = M
dust ⇥
estimatethatthe⌫ ⇥ B⌫ (T dust )/D2 , where the emissivity of dust, ⌫ ,turescalesis Mgas = (52as ⇠352 GHz ⇥ (⌫[GHz]/352) , with 352 GHz = 0.09 mthe
kg 1
molecularga
2
1 in the disk of NG(a value rounded up from 352 GHz = 0.0865 m kg used bya bright
Klaas et al. 2001), B (T ) is the Planck function, andD isring betw

H8==ª• Recent!results!with!ALMA!

– NGC!1068!(1!arcsec!=!70!pc)!

Garcia6Burillo+14

15!pc

⌫dust

3. Upper panel:SEDof fluxes
the dust continuum
emission
theFig.
distance.
Priorthetonuclear
the fit,thein the two
ALMA bands
in NGC 1068 derived using NIR and MIR continuum and spectroscopy
5. MolecularlÃÀÆÆ×ÒÀÐÅÓ!(CLUMPY!Nenkova+08)!Ê·ÄÆ©°³Æ×ÒÀ#:!
werefortheAlonso-Herrerocontamination
by non-thermal
emissionindata corrected(blue squares)fromet al. (2011),
and the ALMA00
thedatacentralapertureat theAGN,
as wasestimated
Sect.In 4.1.1.
points in1Bands
7 and 9 (redstars).
The SEDderived in inaperthis section w
+1
00
5
tures
centered
at
the
AGN
that
range
from
0.
2
(⇠14
pc)
for
NIR
data
The
best
MBB
fit
is
found
for
M
=
(8
±
2)
⇥
10
M ,the mor
compare• NIR+MIR!only!(Alonso6Herrero+11)!!6 !62!topc!
dust
0.00 5 (⇠35 pc) for MIR and Band-7 ALMA data. The best CLUMPY
T dust= fit46
K and (curve)= 1.7and±the0.2.
errorbars
model
to ±
the3observations
1 The
uncertainty
range ofon the pa• !+!ALMA!(Garcia6Burillo+14)!!!!!!!!!!!!!20+6610!
pc!!
the fit (grayregion)are superposed
onto the datadue
points.
rameters
ofshaded
the fitreflectthe uncertainties
toLowerthe estimated
5.1. CO maps
panel:aclose-up
view
of
the
dust
continuum
emissioninBand
9.
Levelsrange of missing flux in the ALMA
bands, derived in Sects. 3.1
 dust!cloud!number!density!ª:3©7(;!clouds!«;!
and markers are as in Fig. 1. The (0.00 4 ⇥ 0.00 2)-aperture used to extract Figure 4 shows
and3.2.
intensity maps
the flux at the position of the AGN is plotted as an ellipse.
¢®¢®!band9!image!ª!AGN! o©!point!source!u¨CO neumaps reveal
The value of Mdust can be used to predict the associatedNGC
1068 withtralIncidentally,gas massthebudgetin thisregion.
the linear dust/gas
NIR data
pointsare alsoApplying
above the CLUMPY
ties: 600 and 2
scalingratiofit.ofThe
Draineet al.
(2007)(see also
Sandstrom
et al.
torus model
extra flux
at thesewavelengths
might
come
tively. As for the

!

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TREMBLAY ET AL.

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4"

Vol. 666
TREMBLAY ET AL.

3C31

3C321

2"

600pc

2!kpc

600pc
4"

2"

3C 465

3C 264
3C 264N

Vol. 666

3C 465

NGC 4261
N

Fig. 2.— Examples of a circumnuclear dusty disk and a dust lane, respectively. (a) A 1.6 "m /0.702 "m absorption map of the nuclear disk of 3C 31, made from dividing
HST NICMOS and HST WFPC2 images. The disk exhibits more absorption on its southwestern edge, and previous studies of the axial ratio (b/a) for the disk haveestimated the southwestern edge to be nearer the observer than the northeastern edge, with arccos(b/a) $ 41% with respect to the plane of the sky ( Fraix-Burnet et al. 1991;
de Koff et al. 2000). (b) A 1.6 "m /0.702 "m absorption map of the !6.5 kpc dust lane in 3C 321. Note that, while we include 3C 321 in this figure because it best illustrates
what we define as a dust lane, we do not include it in our 84 object sample as its H-band isophotes are very highly distorted by a foreground object.

3C465

NGC 4261

3C449

N

hundreds of pc in diameter. We find 13 such dusty disks, clearlydisks, and the projected extent of a lane is always far greater thanresolvable either in optical WFPC2 data or with an H /R-banda disk diameter. For these reasons, it is not likely that we arecolor map. Our color maps have been normalized such that amisidentifying edge-on disks as lanes. In Figure 3 we present themeasured difference in pixel values between two regions corredistribution of linear sizes for all of the disks and lanes in ourNNN
sponds to a difference in a proportional number of R-band magsample. Lanes are associated with a swath of extinction (greater
nitudes. This allows for quick extinction estimates.
than 1 R-band magnitude) spanning more than !4 kpc, while the
In Figure 2a we present our color map for 3C 31, which
disks in our sample have diameters smaller than !2.5 kpc.
contains an excellent example of a dusty disk. Although theSome objects in our sample (e.g., 3C 317, 3C 338) contain thinlargest in our sample (at !2.5 kpc in diameter), this disk shares
tendrils and wisps of dust, which we do not consider lanes. Whilesimilar properties with the 12 others we observe. Based on theirlanes are typically associated with more than 1 R-band magnicommon traits, we define a dusty disk as a round nuclear feature
tude of extinction, far less massive and cohesive features, such as
seen in absorption, qualitatively appearing continuous (from its
the one in 3C 338, are far more optically thin at R band and areouter boundaries to the nucleus), flat, and sufficiently resolvablebetter described as wispy tendrils or clumps rather than full lanes.
so as to allow for a confident estimate of b/a (the ratio of theWe also note that 3C 236 is unique in that its inner dusty disk is
disk’s minor axis b to its major axis a). Assuming a circular, flat
connected to a large surrounding filamentary structure. We do
disk, this axis ratio can be projected into an estimate for the disk’s
not classify this outer feature as a lane, as it appears to be coninclination i with respect to the plane of the sky by i ¼ arccos(b/a).
nected to the inner disk by a thin tendril. Nevertheless, we mea1"
2"2"
These disks are typically associated with more than 1 R-band magsure the inclination of the dust feature in 3C 236 with respect456789 :; -./U>VWXT 3,'24A32&4 0/2."% '7 KX KC5 RYX FZ[T5 KX TNM5 KX MN[ 2&4 RYX MTNC: J-" 2,,'(% 0&4012#" &',#-5 (-0+" #-" %-',# 42%-"% /2,< #-"nitudeof extinction.
In manywe
instances,
was necessary
first HSTtoNICMOS2
the inner nuclear
disk.
We discuss
236withfurtherin x 6. See',0"&#2#0'& '7 #-" /20& ,240' 9"#:Fig. 8.— Examples of some of the unique dust featuresin oursample, which
discussit directlyin x 5.toTop:
1.6 !mimageof 3C3C236
highlighted
producean H /R-bandcolor (seemap soas toconfirm that
dust feaTable
1 for!ma qualitativeof dustthe averaging
regionx 3)
boundedby thedashedlines, anda 1.6/0.7 !mclassification
color map of
the morphology
dusty disk (wherein theisophotal contours, its associated a4 /a radial profile with*+2&" '7 #-" %<85 #-" ,240' 9"#% 2)0% %-'$+4 #-","7'," 2**"2,turewasindeedcontinuous
from
its
outer
edge
to
the
unresolved
applicable)
for
every
objectinoursample.
" # $ % $ &0/2."%'" ( ) *'7+ #KX( , KC5- $ "RYX. $ $ FZ[T5* / ( + KX
0 ' TNM5* / KX MN[ 2&4 RYX MTNC: J-" 2,,'(%
of2&4
3C*2,2++"+
236,
made
division
HST NICMOS2
and WFPC2 data. This object is unique in that it is one of the largest galaxies in the universe, and its nucleus
456789 :; -./U>VWXT !3,'24A32&4
0&4012#"&',#-5%-',#of42%-"%/2,< #-"*",*"&401$+2, #' #-" ?2**2,"&#@ nucleus/29', 2)0%#' (-0+"#-" via #-"nucleus. Many of the dusty disks in our sample possess small
1 $ " ) % ( $ * "'" ( ) * +Hostspiral
GalaxyIsophotal
Properties
contains both a dusty disk and a dust lane. Middle: Sameasymmetries,
as the top row,
but for
3C 465. The
disk
3Cgiving
465 isrise
lopsided, with two4.2.
sharpfeaturesto thenorth and south.
',0"&#2#0'& '7 #-" /20& ,240'
9"#:/0&', 2)0% '7 #-" 40%1:
includinglopsidedness(e.g.,
3C in
465,
Bottom:as 7,'/
the toprow, but for 3C 449. The dustytodisk
in uncertainty
this objectinis its
uniquein that see
it isFig.
a clearoutlier to the observed
but perhaps
not real) jet/disk
orthogonality;& ',4", #' #"%# #-0% -8*'#-"%0%5(" -26"Same4",06"45-0.-A!"# $% &'( ")*+'," #-" ."'/"#,012+ ,"+2#0'&%-0* 3"#(""& 40%1 2&4
added
b/a estimate;8), nonplanar
Here we (examine
the sample-wide
distributionsof the isowe calculated
warps(e.g., NGC
3C 449,8; Ferrarese
photal parameters(a4 /a)orthogonality,"%'+$#0'& ,240' /2*% *$3+0%-"4 0&#-" +0#",2#$,"?B',.2&#0"# 2+:,240' 2)"% 2&45 0& *2,#01$+2,5 (-"#-", 2&4 2# (-2# +"6"+ '7 211$,218
trend,
which wediscuss
in x 1. The disk in 3C 449 has beenmodeledby6251,
Tremblayet Fig.
al. (2006)
with&a Fordlarge1999;
warp, accounting
for jet/disk
on smaller(!50usingpc)
ave and !ave , which#-"I %<85#-"CDDKG
,240'
9"#%
2)0%
%-'$+4 #-","7'," 2**"2,
thestrategy
discussed
in
x
3.
The
histograms
for
these
distribuTremblay
etal.
2006),
spiralfeatures(e.g.,
3C
31,
Fig.
2a),
and
CDEFG*+2&"
B',.2&#05'7
H0++""&
J24-$&#",
!2,2
"#
2+:
CDDF@5#-"#-" 40%1 ',0"&#2#0'& 12& 3" 1'&%04","4 2& 0&4012#', '7 #-" 9"#scales.
! " # $ % $ & '" 40,"1#0'&:()*+#(, -$".$$* /(+0 '*/tions are plotted in Figures 4a and 4b, respectively. The shaded
wispy filamentary structures (e.g., 3C 66B). As our study is con*'%0#0'&2&.+"% '7 #-" ,240' 9"#%#-" =6",240' .2+2)0"%: /29',
J-"," 2," 2)0% 2&4 *2,2++"+ #' #-"*",*"&401$+2,#'7',#-"?2**2,"&#@
regions of both histograms mark the 13 objects in which we
cerned with the orientations of disks as measured with respect to
1 $ " ) % ( $ * "'" (;&)#-"* +%0/*+"%# %1"&2,0'5 ,240' 9"#% 2," "9"1#"4 2+'&. #-"&' %0.&0=12&# 4077","&1"% 3"#(""& #-" 40,"1#0'&% '7 *2,%"1 2&4
/0&',
2)0%
'7I #-"
40%1:
observe dusty disks, the morphologies of which we describe in
their outer edges, we are generally not concerned with these small<0+'*2,%"19"#% ?":.:
L'&"%>"-,+"
CDDF@: ;& J23+" K (" ,"*',# #-",'#2#0'& 2)0% '7 #-" 1"&#,2+ 3+21< -'+"5 (-01- 2+%' 4"=&"% #-"x 4.1. mechanisms capable of creating and /orscale features.
Anotherexampleof dustserving
illustrateconnections
study discussed physical,"+2#06" #'#' #-"
3,0.-#",,240'
9"#:',0"&#2#0'&'7 #-" 0&&",211,"#0'& 40%1: ;7#-" ")#"&4"4&$1+"2,;& ',4",#"%##-0%-8*'#-"%0%5(" -26"
4",06"457,'/to-0.-A!"# $% &'( ")*+'," #-"."'/"#,012+,"+2#0'&%-0*
3"#(""&
40%1
2&4 *'%0#0'& 2&.+"%
From the (a /a) distribution in Figure 4a, it is clear that our
In Figure 2b is a color map of the highly disturbed dust feature

300!pc

1"

2"

2"

HST/WFPC2!images!(Capez!&!Celoz!99)

600pc

350pc

1.6um/0.7um!color!map!by!HST!
Tremblay+07ÃÀÆYÎÄÉÕ¼
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Nuclear astrometry in type 2 galaxies
NGC4594

35pc

37!pc

22!pc

Figure maps
8. Extinctionof ESO
428-G14, MCG-05-23-016,
NGC
1068
andderived
NGC 1386
using
same
for aseachobject as in theExtinctionof ESO maps
428-G14,
MCG-05-23-016,
NGC 1068 andNGC
1386
using derived
the samedustthemaps
fordusteachmaps
objectin thecorresponding
individual
Figs
1–4.
The
reference
level
is
taken
from
a
dust-free
region
away
from
the
filamentary
structures
andwithinakpc
radius from theding individual Figs 1–4. The reference level is taken from a dust-free region away from the filamentary structures and within a kpc radius from theuptheandleft.
east is to the left.
orth iscentre.
up andNorth
east isis to

Dust!ex[nc[on!map!based!on!the!NIR/OPT!color!image!
Prieto+14

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NGC1386

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foundfully visible.
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structuretheneededtorus –toisexplain
neededthe
to explain theof strongemissionthe opticalimages,may obscuring– thetorus –– isstrongtion
emissionlines
in the lines
opticalin images,
which
may whichfurther
lack ofemission
broad-line
and the morphology
of gas.
the ionized gas.
In the casebluestcolours,
optical–IR
colours,
AV . oflackofof broad-line
andemission
the morphologyof the ionized
the case
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hence,
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In where
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where well-defined
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NGC
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the ex- and theクホールの系統的質量測定ËÒÄ»Í×Óªj
• “Sphere!of!Inﬂuence”!

The Astrophysical Journal, 764:151 (19pp), 2013 February 20

surements of supermassive black holes
M6σ*!rela[on!from!
Graham&ScoY!13

• w~!

Graham & Scott !ALMA|AGN!workshop!
BH重力圏/銀河回転境界で降着物質の相・
2011/06/11!ÀÒ¸Ç°²

BH重力圏

100!pc
10!pc

クホールの質量は、十分に高い角度分解能にて銀河中心部の星あるいはガスの速度場

1!pc析することによって力学的に求められている。周囲の星・ガスの速度場にたいしてブきくなる範囲 sphere of influence はブラックホール質量と銀河中心付近の星の速度分を与えることができる。

Figure 2. Black hole scaling relations involving (a) central velocity dispersion σ , (b) Ks -band host spheroid magnitude, and (c) B-band host spheroid magnitude. The
red dots represent the (luminous) core-Sérsic galaxies and the blue
8 circles represent the (intermediate-luminosity) Sérsic galaxies and bulges, while the open crosses
BH
BH"given in Table 3 are shown here, except for panel (a) which shows the OLS(σ |Mbh ) regression
designate those which are barred. The symmetrical bisector regressions
h (dotted blue)
for the 21 barred−1 2 along with the symmetrical bisector regression for the 24 core-Sérsic galaxies. The faint2 and 27 non-barred (solid blue) Sérsic galaxies,
dot-dashed gray line at the∗bottom of panel (a) corresponds
to a black hole’s sphere of influence of 0.!! 1 at a distance of 1.3 Mpc. With such a limiting spatial resolution∗!!
of 0. 1, black holes residing below this line cannot be reliably detected. Using the LKs –σr and–σ relations
for the Sérsic galaxies, constructed using both a bisector< 1LBpc: BH重力圏
regression and an OLS(L|σ ) regression, this gray line has been mapped into panels (b) and (c). The leftmost core-Sérsic galaxy in panels (b) and (c) is NGC 3998.
(A color version of this figure is available in the online journal.)r > 10 pc : 銀河回転

r =

GM
σ

≈ 10

(M /10 M )pc(σ /200 km s )

(1.1)

•
遠鏡や補償光学を駆使した地上
rh!~!1!–!100!pc10m クラス望遠鏡によって研究が行われてきたが、こ•測装置によっても角度分解能の制限のため、中心巨大ブラックホールの存在を確認でGiven that the 27 non-barred Sérsic galaxies define an Mbh –σgalaxy type) Mbh –σ relation gives slopes of 5.21 ± 0.27, 5.61 ±kµ²©
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