Feeding and Feedback in U/LIRGs: ALMA Case Studies in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220...
Transcript of Feeding and Feedback in U/LIRGs: ALMA Case Studies in U/LIRGs: ALMA Studies on NGC 3256 and Arp 220...
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
2015-06-01, "Galaxies of many colours" @Marstrand, Sweden
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"
−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
−20 −10 0 10 20offset along P.A.=−90 deg [arcsec]
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
3 2 1 0 −1−2−3R.A. offset [arcsec]
−321 km/s
+321 km/s
3 2 1 0 −1−2−3
3 2 1 0 −1−2−3R.A. offset [arcsec]
−381 km/s
+382 km/s
3 2 1 0 −1−2−3
3 2 1 0 −1−2−3R.A. offset [arcsec]
−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 −10R.A. offset [arcsec]
−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
3 2 1 0 −1−2−3R.A. offset [arcsec]
−260 km/s
+260 km/s
3 2 1 0 −1−2−3
3 2 1 0 −1−2−3R.A. offset [arcsec]
−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
3 2 1 0 −1−2−3R.A. offset [arcsec]
−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 −30R.A. offset [arcsec]
−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
2015-06-01, "Galaxies of many colours" @Marstrand, Sweden
NGC 3256: AGN in the S nucleus
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 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.
NGC 3256: AGN in the S nucleus
Ohyama, Terashima, & Sakamoto 2015, ApJ
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
NGC 3256: AGN in the S nucleus
Ohyama, Terashima, & Sakamoto 2015, ApJ
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"
NGC 3256: AGN in the S nucleus
Ohyama, Terashima, & Sakamoto 2015, ApJ
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.
NGC 3256: AGN in the S nucleus
Ohyama, Terashima, & Sakamoto 2015, ApJ
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
2015-06-01, "Galaxies of many colours" @Marstrand, Sweden
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
PWV= 0.25 mm; 5% of ALMA timePWV= 1 mm; 50% of ALMA time
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
PWV= 0.25 mm; 5% of ALMA timePWV= 1 mm; 50% of ALMA time
B3C.3?
B4C.3?
B6 Cyc. 1/2
B7 Cyc. 1/2
Arp 220 Spectral Scan : Project Overview
• 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
PWV= 0.25 mm; 5% of ALMA timePWV= 1 mm; 50% of ALMA time
B3C.3+
B4C.3+
B6 Cyc. 1/2
B7 Cyc. 1/2
Arp 220 Spectral Scan : Project Overview
• 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
2015-06-01, "Galaxies of many colours" @Marstrand, Sweden