[CII]輝線で探る銀河相互作用、	  インフロー、アウトフロー	
1. Appleton+13	
  -­‐	
  銀河相互作用	  2. Brisbin+14	
  -­‐	  インフロー（間接的）	
  3. Kreckel+14	
  -­‐アウトフロー	
  [CII]158um微細構造輝線	
• 11.3	
  eV	
  photons	
  to	
  form	  C+	
  – probe	  of	
  the	
  atomic	
  gas	
  heated	
  by	
  the	
  FUV	  (6	  -­‐	  13.6	  eV)	  radiaLon	
  ﬁeld	  from	  massive	  stars	  – indicator	
  of	
  star	  formaLon	
  rate	  • 低励起(91	
  K	
  above	
  ground)	
  	
  – the	
  dominant	
  coolant	
  of	
  the	
  neutral	
  ISM	  	
  • opLcally	
  thin	  – measure	
  of	
  the	
  atomic	
  gas	
  mass	  1.	
  Appleton	
  et	
  al.	  2013,	
  ApJ,	
  777,	
  66	
  
	
  
Shock-­‐enhanced	
  C+	
  Emission	
  and	  the	
  DetecLon	  of	
  H2O	
  from	  the	  Stephan‘s	
  Quintet	
  Group-­‐wide	
  Shock	
  Using	
  Herschel	  	
  銀河相互作用によるショック領域で[CII]が明るくなることがわかった	Stephan's	
  Quintet	

HI:	
  contour	Williams+02	

The Astrophysical Journal, 777:66 (16pp), 2013 November 1

Stephan's	
  Quintet	

(a)Guillard+09	

35	
  x	
  15	
  kpc2	
  shocked	
  	
  intergalacLc	
  ﬁlament	Stephan's	
  Quintet	
(b)

Herschel/PACS	
  Spectroscopic	  	
  ObservaLons	

21	
  kpc	

(b)Log	
  L(C+)/L(sun)=8	(c)Figure 1. (a) The distribution of warm molecular hydrogen (blue) superimpose
on an HSTWFC3 composite color image (red: Hα; green: V-band; pale blu
B-band) of Stephan’s Quintet. The H2 outlines the 0–0 S(1) distribution fro
Cluver et al. (2010), (b) R-band image of Stephan’s Quintet showing the outlinof the three pointings of the 5 × 5 spaxel PACS IFU (blue, green, and magenta
The lettered regions (A–E) show the extraction boxes discussed in the tex
Regions B and E overlap, and were chosen to minimize contamination
the shocked regions by faint star forming emission, (c) SPIRE FTS footprin
superimposed on the R-band image. Blue and red circles show the SSW an
SLW detector beam positions, respectively. Those SSW detectors with lette
inside, denote those detectors in which the pH2 O 111 –000 molecule was detecte(see Tables 1 and 2). Those with a white “X” show non-detections. SSWC3 w
only marginally detected. Upper limits for CO lines at position SLWC3 whic

b Soft X-rays (0.5–2 keV) derived from extractions from the Chanc Assuming D = 94 Mpc.

1.	
  Appleton	
  et	
  al.	  2013,	
  ApJ,	
  777,	
  66	
  
	
  
Shock-­‐enhanced	
  C+	
  Emission	
  and	  the	
  DetecLon	  of	
  H2O	
  from	  the	  Stephan‘s	
  Quintet	
  Group-­‐wide	
  Shock	
  Using	
  Herschel	  	
  銀河相互作用によるショック領域で[CII]が明るくなることがわかった	

2.	
  Brisbin	
  et	
  al.	  2014,	
  arXiv:1411.1332	
  	
  Strong	
  C+	
  emission	
  in	
  galaxies	
  at	
  z~1-­‐2:	
  Evidence	
  for	  cold	  ﬂow	
  accreLon	
  powered	  star	  formaLon	
  in	
  the	
  early	
  Universe	
  high-­‐z	
  ULIRGの1-­‐10kpcにひろがった[CII]輝線領域（星形成起源）はインフ
ローの証拠？	

– 14 –

[CII]158um	
  (CSO/ZEUS)	

[OI]63um	
  (Herschel/PACS)	

IR	  SED	  (MIPS/PACS/SPIRE)	
– 20 –. 3.— The best fit SED model from the library of Dale & Helou (2002) for each of our

AGN	
SB	

AGN	
SB	

We can consider this beam filling factor
in Habingthe formflux,of aparamback
3
G , the– 50 –

0calculation. Wolfire et al. (1990) foundof size
6 D, andG that=F a cloud/1.6⇥10W m 2 lu0

F UVFor LM82/D
if 3wetake D⇠300
phave an average FUV field given by G0 /where
, the mIR
3

(D/pc)⇠0.96(LFG)/G0 or2
IR /L
5: PDRthan
model parameters.
photon, is muchTable
smallerthe cloudextent,D; or
0 / LIR /D

find the spatial extent of star form

models of the physical conditionsof the molecular
ISM in the star fo
SourcePDR parameters

formationis occurring over a larg
3log(n cm )log(G0 )(kpc)
nearby starburst galaxy M82 are remarkably
similarto the size
averagev

4sources, namely, n⇠10 cm

3

0.25
0.25
MIPS 22530 field
3.75±
2.25±
0.25
intensity,
G00.25⇠100.252.9-9.1, which
3 0.5
0.25
and G⇠10
(Lord
et
al.
1996),
sothat w
SWIRE
3-9
3.5±
2.5±
2.2-6.3
0.5
0.25

comparing[CII] and
[OI] (see Fig
0.25
0.25

SWIRE 3-14
3.5±0.5
2.75±0.25
by which we scale our redshift
1-2 sample.
Note thatstrictly1.4-3.0
this com

0.25
SWIRE 3-18 larger
3-5 which is
2.0±
2.3-6.5
0.5 reasonable,notsothat the relative distribution ofstar(extendedvs2.6-8.0
nuclear)
SMM
J03 formation
3.25±0.25
2.25±0.25
0.25
0.25
SWIRE 4-5

by Dı́az-Santos
et0.5al. (2014) of a
0.25
4.25±

1.25±

3.1-10.0

0.5
0.5
M82 and our sources. Without resolved observationsof our sample i
0.25
0.25

SWIRE 4-15 correlation
4.25±0.52.25±0.75 the 2.3-6.4
between
FUV int

0.25
0.25
this is the case, so we proceedSDSS
with
expectation
our2.6-7.6
findings
J12 the3.5±2.25±that
0.25
0.25

galaxy-wide scale on average, G0

orderof magnitude
only.
green	
  [OI]/[CII],	
  cyan	
  ([OI]+[CII])/IR,	
  blue	  [the
CII]/IR,	  orange	  [OI]/CO(3→2)	
  	

our estimates of the emitting size

12.— PDR diagnostic plots. Color shaded contours show constraints on n and G0

Our finding
kpcformation
scale powerestarNote. — The size scale represents the summed
areal extentof
of staron the following ratios: green [OI]/[CII], cyan ([OI]+[CII])/IR, blue
[CII]/IR,orangerepresentative value only and its range is based on the most likely G0 value under the sepa
spatially resolved CO in high redlarge mean free photon paths relative to cloud size as outlined in section 5 (andCO(3!2). Solid lines note ratio values and shaded areas representof small±1 andregions.
We
for the uncertainty on G0 or the uncertainty in the fraction of [CII] from PDRs). Represe
Ivison et al. 2011; Riechers et alvaluesgive the bestred
PDRlinesolution assuming 70% of observed [CII] is due to PDRs. Error
ute 70% of observed [CII] to the classic PDR model. Also overlaid asa dashed
spatialdistribution
molecularthat 68.27% of the power in the marginalized
probability
distribution ofof eachparameter is cregion containing 68.27% of the volume in the two dimensional probability distribution
star formation, but instead is ve
nd G0 . For source SWIRE 4-5, which has a tentative [OI] detection, we additionallywhich are not individually resolvea purple dashed region indicating the 68.27% region that would result if we take theSchmidt-Kennicutt law.
etection as an upper limit instead. Note that in this source the UV field is constrained
As shown in Table 5, the com

2.	
  Brisbin	
  et	
  al.	  2014,	
  arXiv:1411.1332	
  	
  Strong	
  C+	
  emission	
  in	
  galaxies	
  at	
  z~1-­‐2:	
  Evidence	
  for	  cold	  ﬂow	
  accreLon	
  powered	  star	  formaLon	
  in	
  the	
  early	
  Universe	
  high-­‐z	
  ULIRGの1-­‐10kpcにひろがった[CII]輝線領域（星形成起源）はインフ
ローの証拠？	

3.	
  Kreckel	
  et	
  al.	  2014,	
  ApJ,	
  790,	
  26	
  
	
  
A	
  Far-­‐IR	
  View	
  of	
  the	
  Starburst-­‐driven	  Superwind	
  in	
  NGC	  2146	  	
  空間分解した[CII]速度分散マップ
からアウトフローが同定出来る	

A. Taramopoulos et al.: HI observations of the starburst galaxy NGC 2146
0

NGC2146	

1

2

365
3

Jy * km/s

HI:	
  contour	

78 50

R

L/2

LIR=1.2e11	
  Lsun	  (LIRG)	
  M*=2e10	
  Msun	  SFR=8	
  Msun/yr	

40

φ abs

DECLINATION (B1950)

30

20

10

200	
  kpc	  HI	  tail	00

Fig. 6. Schematic diagram of the H I absorption layer in
NGC 2146

77 50

The Astrophysical Journal, 790:26 (15pp), 2014 July 20

05

Taramopoulos+01	

Fig. 7. The total integrated H I flux density of NGC 2146.
Contours are drawn at −0.5, −0.2, −0.1, 0.1, 0.2, 0.5, 1, 2, 4
and 5 Jy km s−1 . The peak flux is 5.8 Jy km s−1
0

78 26

24

DECLINATION (B1950)

The integrated H I flux density map is shown in Figs. 7(large scale) and 8 (small scale). We estimate the total mass for the cloud to be about 6.2 109 M⊙ (H0 =75 km s−1 Mpc−1 ) of which 1.6 109 M⊙ come from thebright region around the galaxy itself, and 4.6 109 M⊙
from the extended component. Furthermore, the extended distribution is not symmetric with respect to theamount of gas in the south (3.1 109 M⊙ ) and the north(1.5 109 M⊙ ). For the above calculations a velocity component of 223 km s−1 of our Sun towards NGC 2146’s
direction has been assumed, in order to refer the redshift
velocity to the center of mass of the Local Group.
Figures 9 and 10 show the intensity weighted mean
radial velocity field on both large and small scale. Points
with negative flux due to absorption have been excluded
from this calculation, and only emission brighter than
1.3 mJy has been taken into account. It is clear from thevelocity field that the main galaxy has a diﬀerentially rotating disk with characteristic rotational speed of about

Kreckel et al. 15
06 20
10RIGHT ASCENSION (B1950)

22

20

18

1

2

3

Jy * km/s

Figure 2. PACS spectroscopy line maps of (left to right) [O i] 63 µm, [O iii] 88 µm, [N ii] 122 µm, and [C ii] 158 µm of the intensity (top), velocity (middle), anddeconvolved velocity dispersion (bottom). The ellipse and center match those shown in Figure 1. All lines are masked in regions where the signal to noise is lessthan five. Uncertainties in the velocity dispersion are ∼5% in the regions above and below the disk, and are much lower (<1%) within the disk. [N ii] has velocity
dispersion peaking at ∼450 km s−1 . The point-spread function for each map is indicated in the lower left corner, and the 6 kpc ellipse shown for reference.
(A color version of this figure is available in the online journal.)

Figure 8. Line ratios of the far-IR fine-structure lines. The [O iii]/[C ii] and [O iii]/[O i] ratios are consistent with star formation within the disk. The [O i]/[C ii]
ratio shows a different morphology, with a bright nucleus and a structure of high [O i]/[C ii] that lies perpendicular to the disk, tracing the outflow. Uncertainties are
typically 5%. The stellar disk and kinematic center (black) are marked for reference.
(A color version of this figure is available in the online journal.)

SOFIA/FORCAST	  (FWHM_PSF~3.5”)	

Figure 9. Dust emission in NGC 2146. Warm dust is traced by the Spitzer MIPS 24 µm emission (top left) and SOFIA FORCAST 37 µm emission (top right). Cold
dust is traced by the Herschel PACS 100 µm (bottom left), 160 µm (bottom center), and SPIRE 250 µm (bottom right) emission. The emission generally follows thedisk of the galaxy, with extended features that trace the optical spiral arms seen extending beyond the field of view of our line maps. Hexagonal features in the PACS
images at low flux levels are due to the instrumental point-spread function. The stellar disk (blue oval) and kinematic center (cross) is marked for reference and is thesame in all figures.

The Astrophysical Journal, 790:26 (15pp), 2014 July 20

Kreckel et al.

Figure 9. Dust emission in NGC 2146. Warm dust is traced by the Spitzer MIPS 24 µm emission (top left) and SOFIA FORCAST 37 µm emission (top right). Col
dust is traced by the Herschel PACS 100 µm (bottom left), 160 µm (bottom center), and SPIRE 250 µm (bottom right) emission. The emission generally follows th
FigureTo identify
the amountof [C thatii] emission
the outflow
to the outflow
itself,model
the [C
intensity
distribution(left)featuresusing only
those
disk
of the10.
galaxy,with extendedfeaturestrace theinopticalspiralattributablearms seen extending
beyondthewefieldof viewofii]ourline maps.
Hexagonal
in thePAC
regions
withflux
lowlevels
velocityin black)with a two-dimensional
exponential
disk(center).
The residualfrom
this fitis (right)
an excessandin theimagesat loware dispersion
due to the (outlined
instrumental
point-spreadfunction. The stellar
disk (blueoval)
and kinematic
center(cross)markedshow
for referenceis thregionsand below the disk (in blue) that correspond to the regions with increased velocity dispersion (in black). From this we calculate an atomic gas outflow
samein allabove
figures.
8 M . If we assume that all [C ii] emission in regions of high velocity dispersion is due to the outflow (with no disk component), we calculate an
7.4 × of10this⊙(A masscolorofversionfigure is available in the online journal.)
The
Kreckel et al.
atomic gas mass of 3.9 × 109 M⊙ .Astrophysical Journal, 790:26 (15pp), 2014 July 20(A color version of this figure is available
in the online
journal.)The gas excitationin M82is dominated by stellar ionization

Matomic,ourlow~1e9	
  Msun	close to the disk with an increasing contribution from shocks
further away (Heckman et al. 1990; Shopbell & Bland-Hawthorn(see also Maiolino et al. 2012).
We estimate the mass asa lower limit in the case that we have a lower gas density o1998). We see this also very clearly in NGC 2146 (Figures 6
and 7), as beyond 1 kpc above the disk the excitation is notemperature.
"and suggests a significant If we assume that all the [C ii] emission from where w!longer consistent"!
with photoionization
1.4 × 10−4
Matomic
0.7L[C ii]from shocks.
contribution= 0.77 The far-IR fine-structure lines in M82 were observed byidentify the superwind through the increased [C ii] velocit
M⊙
L⊙et al. (2013). In X
C + 2146 we see that the [C ii] anddispersion is due to a massive outflow (with no disk component)
ContursiNGC[O i] showquite clearly a ∼100 km s−1 increase in the velocity
9
1 dispersion+ 2e−91K/T+ ncrit /nin the superwind
and along the minor axis to the diskwe find L[C ii] = 3.0×10 L⊙ in the northeast and L[C ii] = 1.5×× center, very−91K/T
similar to what is, seen in M82 and (1)suggestive of109 L⊙ in the southwest to give a total Matomic > 3.9 × 109 M⊙
2emoderate superwind velocities in the atomic gas. Both galaxies◦
also show a relatively wide opening angle in the [C ii] and [O i]However, given the 63 inclination, we may not be cleanl
diagnostics. In M82 this is different from what is seen in theseparating the disk contribution from the [C ii] emission in thwhere XC + is the C+ abundance
per hydrogen atom, T is the gas
Hα outflow, which is much more collimated. This is difficult
temperature, n is the gas density,
is thewhere
critical
to compareandwith nNGC
we do density
not see the outflowoutflow.
crit 2146,
FigureModeling ofkinematicallyspatially integrated [O i] and[C ii] line theprofilescontribution
assuming
3
clearly in(3Hα×in ourobservations
the central
region.
we13.cannot
isolateof [C iiof the [C ii] 158 µm transition
10
cmto−3). ofWeassumea both in Asa double
Gaussian fit (top). For [C ii] and [O i] the fits recover the instrumental
In
M82
dust
is
seen
up
6
kpc
along
the
minor
axis
resolution
fortheapproachingandreceding
sides
of
the
disk,
with
no
broad
+
emission
due to the outflow from [C ii] in a disk componen
C abundance typical of Milky
Way photodissociation
mid-IR continuumand polycyclic aromaticregionshydrocarbon emisresidual (bottom) that could indicate the contribution of the outflow.
−4
sion (Engelbracht et al. 2006), although the physical propertieswe fit the disk intensity in regions with low velocity dispersio

積分したスペクトルではアウトフロー成分を取り出すことはできなかった！	

3.	
  Kreckel	
  et	
  al.	  2014,	
  ApJ,	
  790,	
  26	
  
	
  
A	
  Far-­‐IR	
  View	
  of	
  the	
  Starburst-­‐driven	  Superwind	
  in	
  NGC	  2146	  	
  空間分解した[CII]速度分散マップ
からアウトフローが同定出来る	

まとめ	
• ひろがった[CII]輝線で銀河相互作用によるショック領域をトレースできる	  • 空間分解できなくても、	
  [CII]輝線領域のサイズが求められる（大きなサイズはインフローを示唆？）	
  • 空間分解できれば[CII]速度分散マップからアウトフローが同定（diskと分離）出来る（~1kpc、0.1-­‐0.2”@z=1-­‐3が必要）