Feeding and Feedback in U/LIRGs: ALMA Case Studies in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220 • NGC 3256 • Dual molecular outﬂows from a merger: Starburst superwind + radio-mode

Feeding and Feedback in U/LIRGs: ALMA

Case Studies

Kazushi Sakamoto

2015-06-01, "Galaxies of many colours" @Marstrand, Sweden

Feedback in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220

• NGC 3256

• Dual molecular outflows from a merger: Starburst superwind + radio-mode jet (Sakamoto+2014)

• AGN revelaed in OIR-X analysis (Ohyama+2015)

• More to come: VLA, ALMA, HST, etc.

• Arp 220

• ALMA spectral scan ongoing

• Preview. dual outflows in P-Cyg, SiO, Extended CO

• More to come: Line modeling, ALMA Cyc. 3

• N4418 :

• outflow data: taken, not delivered

• talk by Costagliola today


M81VT = 6.94mag

M82VT = 8.41mag

M81 > M82 by a factor of Four

In the Visible Light ...

What is Essential is Invisible to the eye

Visible LightFar-,Mid-IR

M81 < M82in Lbolometric

8 10 12 14 16 18 20log (Frequency / Hz)

−18

−16

−14

−12

−10

log

(i f i

/ W

m−2

)

0 −2 −4 −6 −8 −10log (Wavelength / m)

M81M82

red = Hαbiconical outflow

Luminous&Active M82 has an Outflow

IR-bright Galaxies in the Local Universe

1 10 100Distance [Mpc]

9

10

11

12

13lo

g L(

8-10

00 µ

m)/L

O •

M33

M51

M81

LIRG

ULIRG

log

L 8-1

000μ

m /

L ⊙

M31

NGC 253

M82

NGC 1068NGC 3256

Arp 299Arp 220

Mrk 231

588 galaxies S(60μm) > 5.24 Jy | b | > 10 degfrom RBGS (Sanders et al. 2003)

M87 Lbol

Distance / Mpc

NGC 3256: ALMA

Dual Molecular Outflowsapparently

Radio-mode AGN feedback + Starburst feedback

Sakamoto, Aalto, Combes, Evans, & Peck, ApJ, 20142015-06-01, "Galaxies of many colours" @Marstrand, Sweden

18"

NGC 3256 LIR=4x1011L⊙, 35 Mpc

3 kpc

Two nuclei at 5" (0.8 kpc) separation

NA

SA/E

SA/H

ubbl

e H

erita

ge/A

. Eva

ns

−20 −10 0 10 20offset along P.A.=−90 deg [arcsec]

2600

2700

2800

2900

3000

3100

Velo

city

[km

/s]

1 kpc

NGC 3256SMA CO(2−1)

[K]

0 2 4 6

SMA Discovery of Molecular Outflow in NGC 3256Sakamoto, Ho, Peck (2006)

10h 27m 52.5s52.0s 51.5s 51.0s 50.5s 50.0s 49.5s

-43° 54v 35w

30w

25w

20w

15w

10w

05w

00w

Right Ascention (J2000)

Dec

linat

ion

(J20

00)

2.0" x 1.0" 1 kpc

(b) NGC 3256

mean velocity

2650 2700 2750 2800 2850 2900

slit

18"3 kpc

line wings → outflow

2600 2800 3000 3200Velocity (radio,LSR) [km/s]

0

1

2

3

4

5

Inte

nsity

[Jy/

beam

]

NGC 325612CO(2−1)

Central 5"


2600

2700

2800

2900

3000

3100

Velo

city

[km

/s]

1 kpc

NGC 3256SMA CO(2−1)

[K]

0 2 4 6


2000

2500

3000

3500

Velo

city

[km

/s]

1 kpc

NGC 3256ALMA CO(1−0)

[K]

0 1 2 3

VFW

~ 6

00 k

m/s

ALMA CSV revealed larger outflow(Sakamoto 2013, ASPC, IAUS)

0

+300

+600

+900

-300

-600

-900

V-Vsys [km/s]

VFW

≳ 1

000

km/s

!

SMA CO(2-1)

ALMA CO(1-0)

S molecular bipolar jet

4 3 2 1 0 −1−2−3−4

−6

−4

−2

0

2

4

6

4 3 2 1 0 −1−2−3−4R.A. offset [arcsec]

−6

−4

−2

0

2

4

6

Dec

. offs

et [a

rcse

c]

−199 km/s

+200 km/s

0.6" x 0.4" 300 pc

(b)

3 2 1 0 −1−2−3

3 2 1 0 −1−2−3R.A. offset [arcsec]

−260 km/s

+260 km/s

3 2 1 0 −1−2−3


−321 km/s

+321 km/s

3 2 1 0 −1−2−3


−381 km/s

+382 km/s

3 2 1 0 −1−2−3


−442 km/s

+442 km/s

CO(3-2)

offset from VSYS

20 10 0 −10 −20

−20

−10

0

10

20

20 10 0 −10 −20R.A. offset [arcsec]

−20

−10

0

10

20

Dec.

offs

et [a

rcse

c]

1.6" x 1.2" 1 kpc

CO(1−0)

−150 −100 −50 0 50 100 • High V gas, |V-Vsys|>200 km/s, - bisymmetric about the S nucleus - velocity gradient ⊥ disk rotation⇒ bipolar molecular jet ! highly collimated (θop ~20°), l ~ 0.7 kpc

• S nucleus nearly edge-on (i ~ 80°) incl.-corrected Vmax ~2000 km/s

• Highest-V gas off the nucleus⇒ appears to accelerate out to ~300 pc

(Sakamoto et al. 2014)

10 5 0 −5 −10

−10

−5

0

5

10


−10

−5

0

5

10

Dec.

offs

et [a

rcse

c]

[+224,+752] km/s

[−223,−751] km/s

2.9" x 2.6" 500 pc

CO(1−0)

4 3 2 1 0 −1−2−3−4

−6

−4

−2

0

2

4

6

4 3 2 1 0 −1−2−3−4R.A. offset [arcsec]

−6

−4

−2

0

2

4

6

Dec

. offs

et [a

rcse

c]

−199 km/s

+200 km/s

0.6" x 0.4" 300 pc

(b)

3 2 1 0 −1−2−3


−260 km/s

+260 km/s

3 2 1 0 −1−2−3


−321 km/s

+321 km/s

CO(3-2)

-

• from N nucleus• bipolar, near pole-on (iN ~ 30°)• Vmax ~1000 km/s• extended, wide-open• probably starburst-driven wind

N molecular bipolar wind

S molecular jet: Association with a Radio Jet (?)

!"#$%"%&'()* + !"#(%+ !"#%%+

,$- '!$.'((/

(%/

"0/

"1/

"$/

"(/

234&5'6+78953:9';<(%%%=

>8

7?39

@53:

9';

<(%

%%

=

,-0"'A*B+C-0('A*B+

-%%'D7

black contour:VLA 3.6 cm

Neff et al. (2003)

radio spursor a bipolar jet

highest Vmolecular gas

4 3 2 1 0 −1−2−3−4

−6

−4

−2

0

2

4

6

4 3 2 1 0 −1−2−3−4R.A. offset [arcsec]

−6

−4

−2

0

2

4

6

Dec

. offs

et [a

rcse

c]

−199 km/s

+200 km/s

0.6" x 0.4" 300 pc

(b)

3 2 1 0 −1−2−3


−260 km/s

+260 km/s

CO(3-2)

8 6 4 2 0 −2 −4 −6 −8

−8

−6

−4

−2

0

2

4

6

8

8 6 4 2 0 −2 −4 −6 −8R.A. offset [arcsec]

−8

−6

−4

−2

0

2

4

6

8

Dec

. offs

et [a

rcse

c]

1.0" x 0.5" 500 pc

(a) 3.6 cm 0 1 2 3 4 5 6

VLA Neff et al. (2003)

• Curved spur in both 3.6cm cont. and CO(3-2)

• curvature may be due to ram pressure

S molecular jet: Association with a Radio Jet (?)

30 15 0 −15 −30

−30

−15

0

15

30


−30

−15

0

15

30

Dec

. offs

et [a

rcse

c]

1 kpc

(a)

Dust-scattered Light-Echo of AGN dimmed 104 yr ago?

Broad off-nuclear Hα, FWZI ~ 5000 km/s (Moran et al. 1999)

NGC 3256: OIR-X

Low-L AGN is in the S nucleus

Ohyama, Terashima, & Sakamoto, ApJ, 2015


NGC 3256: AGN in the S nucleus

20 10 0 −10 −20

−20

−10

0

10

20


−20

−10

0

10

20

Dec

. offs

et [a

rcse

c]

1 kpc

(b) 4.5/5.8/8 µm

Ohyama, Terashima, & Sakamoto 2015, ApJ

• Literature has been mostly negative: Lira+02 (Chandra), Santaella+11 (XMM-Newton), Alonso-Herrero+12 (Spitzer)

• But, new evidence for a low-L AGN

✴ molecular (& radio?) bipolar jet

✴ NIR-color

✴ near/mid-IR SED fit, including deep silicate absorption

✴ red point source in HST/NICMOS, in agreement with AGN-SED modeling

✴ Chandra X-ray spectrum (x 2.7 more data than in Lira+02) consistent with a typical Compton-thin Seyfert 2.



IR-color diagnostics

An AGN in the NGC 3256 Southern Nucleus 21

Figure 6. The IRAC color-color diagrams of the N (open square) and S (open circle) nuclei with boundaries for AGN selection. Errorbars are ±1σ. Also shown in filled symbols are rest frame colors/flux ratios of ULIRG IRAS 22491-1808 from Polletta et al. (2007) (square),starburst M 82 from Polletta et al. (2007) (star), a template of normal star-forming spiral galaxy from Dale & Helou (2002) (triangle), anda representative elliptical galaxy from Polletta et al. (2007) (circle). Connected diamonds are for pure power-law SEDs, and each trianglecorresponds to a power-law index of α from −0.5 (lower left) to −3.0 (upper right) in steps of 0.5. Connected pluses represent colors/fluxratios for pure blackbody SEDs, and each plus corresponds to a blackbody temperature of 600 K (upper right), 1000 K, 3000 K, 6000 K,and 10000 K (lower left). The boundaries for AGN selection are from Donley et al. (2012).

Figure 7. Comparison of extinction curves used in our SED modeling. We show the extinction curve of Chiar & Tielens (2006) for theGalactic center (black solid line), the original PAHFIT (Smith et al. 2007b) extinction curve (blue solid line), the original extinction curveof Fritz et al. (2011) (broken magenta line), and the modified PAHFIT extinction curve (red solid line) to reproduce the curve of Fritz etal. (2011). See the main text for the details of the modified PAHFIT extinction curve.

An AGN in the NGC 3256 Southern Nucleus 21

Figure 6. The IRAC color-color diagrams of the N (open square) and S (open circle) nuclei with boundaries for AGN selection. Errorbars are ±1σ. Also shown in filled symbols are rest frame colors/flux ratios of ULIRG IRAS 22491-1808 from Polletta et al. (2007) (square),starburst M 82 from Polletta et al. (2007) (star), a template of normal star-forming spiral galaxy from Dale & Helou (2002) (triangle), anda representative elliptical galaxy from Polletta et al. (2007) (circle). Connected diamonds are for pure power-law SEDs, and each trianglecorresponds to a power-law index of α from −0.5 (lower left) to −3.0 (upper right) in steps of 0.5. Connected pluses represent colors/fluxratios for pure blackbody SEDs, and each plus corresponds to a blackbody temperature of 600 K (upper right), 1000 K, 3000 K, 6000 K,and 10000 K (lower left). The boundaries for AGN selection are from Donley et al. (2012).

Figure 7. Comparison of extinction curves used in our SED modeling. We show the extinction curve of Chiar & Tielens (2006) for theGalactic center (black solid line), the original PAHFIT (Smith et al. 2007b) extinction curve (blue solid line), the original extinction curveof Fritz et al. (2011) (broken magenta line), and the modified PAHFIT extinction curve (red solid line) to reproduce the curve of Fritz etal. (2011). See the main text for the details of the modified PAHFIT extinction curve.

log (S5.8/S3.6)

log

(S8.

0/S4

.5)

[5.8] - [8.0] Vega

[3.6

] -

[4.5

] Veg

a

N S

NAGN regionElliptical

M82

BB

power-

law

600 K

1000 K

α = -3

α = -0.5

AGN region

S



AGN+SB

single SB

SB+SB

Observed Wavelength (μm)

log

Flux

(Jy)

4.5 μm (excess at S)

IR SED SED fitting

0.36"

3.6"



A red source in HST data: unresolved (<0.26") core + 0.75" FWHM sourceAn AGN in the NGC 3256 Southern Nucleus 19

Figure 4. Zoom-up NICMOS images of the S nucleus and results of our analysis. (a)–(c) NICMOS F110W, F160W, and F222M images.(d) Synthetic F222M image of the stellar component. See the main text for the details of the synthesis. (e) A flux ratio image ofF222M/F160W. (f) The F222M nuclear component, made by subtracting the synthetic F222M stellar component image from the observedF222M image. The NICMOS resolution (0.′′26 FWHM) is indicated by a white circle. (g)–(h) The residual images of the F222M nuclearcomponent after subtracting the fitted Gaussian models. The panel (g) shows a case of single-Gaussian model, and (h) shows a case ofdouble-Gaussian model. The fitted positions of Gaussian components are marked with white pluses in panels (g) and (h). All panels areshown in linear scale, and flux (in units of MJy/steradian) and flux ratio (for only panel f) scale are indicated in scale bars for each panel.The zero flux levels in the residual images are also indicated by black contours.



HST unresolved source: on the model AGN SED

HST

AGN+SB SED model

AGN with NH ~ 1023 cm-2

(τ9.7 ~ 10, AV ~ 80 mag)

Arp 220

Spectral Scan is ongoingOutflow to be studied, among others


Arp 220 : the Nearest ULIRG

1 10 100Distance [Mpc]

9

10

11

12

13lo

g L(

8-10

00 µ

m)/L

O •

M33

M51

M81

LIRG

ULIRG

log

L 8-1

000μ

m /

L ⊙

M31

NGC 253

M82

NGC 1068NGC 3256

Arp 299Arp 220

Mrk 231

M87 Lbol

Distance / Mpc

知らない人のためにHST image,

counter-rot modelP-Cyg. profile => outflow

Arp 220: double nucleus

Arp 220NIR/HST

1"= 360 pc(Scoville et al. 1998)

1012.2L⦿

(Sakamoto, Scoville et al. 1999)

Arp 220 system

Arp 220WArp 220E

outer disk

nuclear disks

Arp 220E

Arp 220W

Arp 220NIR/HST

1"= 360 pc(Scoville et al. 1998)

4500 5000 5500 6000 6500Velocity (radio, LSR) [km s-1]

Inte

nsity

[mJy

bea

m-1]

-200

-100

0

100

200

1 m

Arp 220 EHCO+(4-3)

4500 4700 4900HCN(4-3) Velocity -1.0

-0.50.0

0

100

1 m

HCO+(3-2)

-1.0-0.50.0

0

200

400

1 m

CO(3-2)CO(3-2), 0.5" data

-1.0-0.50.0

4500 5000 5500 6000 6500Velocity (radio, LSR) [km s-1]

Inte

nsity

[mJy

bea

m-1]

-200

-100

0

100

200

1 m

Arp 220 WHCO+(4-3)

4500 4700 4900HCN(4-3) Velocity

-0.5

0.0

0

100

1 m

HCO+(3-2)

-0.20.0

0

200

400

1 m

CO(3-2)CO(3-2), 0.5" data

-0.4-0.20.0

HCO+(4-3)

HCO+(3-2)

CO(3-2)

Vsys (E)Vsys (W)

Arp 220 E Arp 220 W

1 0 -1

1 0 -1R.A. offset [arcsec]

0.34" x 0.28" 300 pc

(d) Arp 2200.87 mm

1 0 -1

-1

0

1

1 0 -1R.A. offset [arcsec]

-1

0

1

Dec

. offs

et [a

rcse

c]

0.34" x 0.28"

(c) Arp 220CO(3-2)

0.45" x 0.34" 300 pc

(b) Arp 220HCO+(3-2)

-1

0

1

-1

0

1

Dec

. offs

et [a

rcse

c]

0.33" x 0.28" 300 pc

(a) Arp 220HCO+(4-3)HCO+(4-3)

HCO+(4-3)

HCO+(3-2)

CO(3-2)

HCO+(3-2)

CO(3-2)

(Sakamoto et al. 2009, ApJ, 700, L104)

• |V-VSYS| ~ 100 km s-1

• NH2 ~ 1023 cm-2

(Tex, [HCO+/H2] assumed)• dM/dt ~ 100 M⊙ yr-1

(rabsorber ≲ 50 pc assumed)

Arp 220: dual outflows

100 200 300 400 500Frequency / GHz

0.0

0.2

0.4

0.6

0.8

1.0

Tran

smis

sion

ALMA Spectral Bands

O2@

119

H2O

@18

3

H2O

@32

5

H2O

@38

0O

2@36

8

O2@

425 H

2O@

448

H2O

@47

5O

2@48

7

PWV= 0.25 mm; 5% of ALMA timePWV= 1 mm; 50% of ALMA time

Band 3

Band 4

Band 6

Band 7

Band 5

Band 8

Arp 220 Spectral Scan : Project Overview

100 200 300 400 500Frequency / GHz

0.0

0.2

0.4

0.6

0.8

1.0

Tran

smis

sion


B3C.3?

B4C.3?

B6 Cyc. 1/2

B7 Cyc. 1/2

P.I. Sergio Martin

•Target = Arp 220, the nearest ULIRG

•the first Sptaially-Resolved scan ✦ 0.5" to separate the two nuclei, recovering most flux ✦ high sensitivity ≈ line confusion limit

100 200 300 400 500Frequency / GHz

0.0

0.2

0.4

0.6

0.8

1.0

Tran

smis

sion


B3C.3?

B4C.3?

B6 Cyc. 1/2

B7 Cyc. 1/2


• Chemical composition

• Excitation from multi-transition data

• Unusual excitation, such as VIB or maser?

• Are the two nuclei similar or not?✦ Their energy sources?

• Outflow/inflow, in P-Cyg. etc. ?

100 200 300 400 500Frequency / GHz

0.0

0.2

0.4

0.6

0.8

1.0

Tran

smis

sion


B3C.3+

B4C.3+

B6 Cyc. 1/2

B7 Cyc. 1/2


• Bands 6,7 (Cyc. 1→2) 90% done

• other bands (Cyc. 3+)

A preview was given in the talk.

Results will be published soon.

Stay tuned

Arp 220 Spectral Scan

Feedback in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220

• NGC 3256

• Dual molecular outflows from a merger: Starburst superwind + radio-mode jet (Sakamoto+2014)

• AGN revelaed in OIR-X analysis (Ohyama+2015)

• More to come: VLA, HST, etc.

• Arp 220

• ALMA spectral scan ongoing

• Preview.

• More to come: Line/kinematics modeling, etc.

• N4418

• talk by Costagliola today

Feedback is diverse. Case studies are needed for important details


Documents

Feeding and Feedback in U/LIRGs: ALMA Case Studies in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220 • NGC 3256 • Dual molecular outﬂows from a merger: Starburst superwind + radio-mode