Feeding and Feedback in U/LIRGs: ALMA Case Studies

Transcription

1 Feeding and Feedback in U/LIRGs: ALMA Case Studies Kazushi Sakamoto , "Galaxies of many Sweden

2 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 , "Galaxies of many Sweden

3 In the Visible Light... M81 V T = 6.94mag M82 V T = 8.41mag M81 > M82 by a factor of Four

4 What is Essential is Invisible to the eye log (Wavelength / m) log ( f / W m 2 ) M81 < M82 in L bolometric 18 Far-,Mid-IR Visible Light log (Frequency / Hz)

5 M81 M82

6 Luminous&Active M82 has an Outflow red = Hα biconical outflow

7 IR-bright Galaxies in the Local Universe ULIRG Arp 220 Arp 299 Mrk 231 log L μm / L LIRG M82 NGC 253 NGC 1068 M51 NGC 3256 M87 Lbol M31 M81 9 M galaxies S(60μm) > 5.24 Jy b > 10 deg from RBGS (Sanders et al. 2003) Distance [Mpc] Distance / Mpc

8 NGC 3256: ALMA Dual Molecular Outflows apparently Radio-mode AGN feedback + Starburst feedback Sakamoto, Aalto, Combes, Evans, & Peck, ApJ, , "Galaxies of many Sweden

9 NGC 3256 L IR =4x10 11 L, 35 Mpc 3 kpc 18" Two nuclei at 5" (0.8 kpc) separation NASA/ESA/Hubble Heritage/A. Evans

10 SMA Discovery of Molecular Outflow in NGC 3256 Sakamoto, Ho, Peck (2006) 5 NGC CO(2 1) line wings outflow [K] Intensity [Jy/beam] Central 5" Velocity [km/s] NGC 3256 SMA CO(2 1) kpc Velocity (radio,lsr) [km/s] offset along P.A.= 90 deg [arcsec] (b) NGC 3256 mean velocity slit 3 kpc 18" 2.0" x 1.0" 1 kpc

11 ALMA CSV revealed larger outflow V-Vsys [km/s] (Sakamoto 2013, ASPC, IAUS) [K] +900 ALMA CO(1-0) NGC 3256 ALMA CO(1 0) [K] Velocity [km/s] NGC 3256 SMA CO(2 1) SMA CO(2-1) 1 kpc offset along P.A.= 90 deg [arcsec] VFW ~ 600 km/s Velocity [km/s] VFW 1000 km/s! kpc offset along P.A.= 90 deg [arcsec]

12 S molecular bipolar jet offset from VSYS (Sakamoto et al. 2014) 6 (b) CO(3-2) 199 km/s +200 km/s 260 km/s +260 km/s 321 km/s +321 km/s 381 km/s +382 km/s 442 km/s +442 km/s Dec. offset [arcsec] " x 0.4" 300 pc Dec. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] High V gas, V-Vsys >200 km/s, CO(1 0) 1.6" x 1.2" 1 kpc R.A. offset [arcsec] - 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 V max ~2000 km/s Highest-V gas off the nucleus appears to accelerate out to ~300 pc

13 N molecular bipolar wind 10 CO(1 0) [ 223, 751] km/s [+224,+752] km/s Dec. offset [arcsec] Dec. offset [arcsec] CO(3-2) (b) 199 km/s +200 km/s 0.6" x 0.4" 300 pc 260 km/s +260 km/s 321 km/s +321 km/s " x 2.6" 500 pc R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] from N nucleus bipolar, near pole-on (i N ~ 30 ) V max ~1000 km/s extended, wide-open probably starburst-driven wind

14 S molecular jet: Association with a Radio Jet (?) black contour: VLA 3.6 cm Neff et al. (2003) highest V molecular gas radio spurs or a bipolar jet

15 S molecular jet: Association with a Radio Jet (?) (a) VLA Neff et al. (2003) 3.6 cm 6 (b) CO(3-2) 199 km/s +200 km/s 260 km/s +260 km/s 4 4 Dec. offset [arcsec] Dec. offset [arcsec] " x 0.4" 300 pc 8 1.0" x 0.5" 500 pc R.A. offset [arcsec] R.A. offset [arcsec] R.A. offset [arcsec] Curved spur in both 3.6cm cont. and CO(3-2) curvature may be due to ram pressure

16 Dust-scattered Light-Echo of AGN dimmed 104 yr ago? Broad off-nuclear Hα, FWZI ~ 5000 km/s (a) 30 Dec. offset [arcsec] kpc R.A. offset [arcsec] (Moran et al. 1999)

17 NGC 3256: OIR-X Low-L AGN is in the S nucleus Ohyama, Terashima, & Sakamoto, ApJ, , "Galaxies of many Sweden

18 NGC 3256: AGN in the S nucleus Ohyama, Terashima, & Sakamoto 2015, ApJ 20 (b) 4.5/5.8/8 µm Literature has been mostly negative: Lira+02 (Chandra), Santaella+11 (XMM- Newton), Alonso-Herrero+12 (Spitzer) Dec. offset [arcsec] kpc R.A. offset [arcsec] 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.

19 NGC 3256: AGN in the S nucleus IR-color diagnostics N S AGN region log (S8.0/S4.5) Elliptical α = K M82 power-law BB α = K S AGN region [3.6] - [4.5] Vega N log (S5.8/S3.6) [5.8] - [8.0] Vega Figure 6. The IRAC color-color diagrams of the N (open square) and S (open circle) nuclei with boundaries for AGN selection. Error bars are ±1σ. Alsoshowninfilledsymbolsarerestframecolors/fluxratiosofULIRGIRAS fromPolletta etal.(2007)(square), starburst M 82 from Polletta et al. (2007) (star), a template of normal star-forming spiral galaxy from Dale & Helou (2002) (triangle), and arepresentativeellipticalgalaxyfrompolletta etal.(2007) (circle). Connected diamonds are for pure power-law SEDs, and each triangle corresponds to a power-law index of α from 0.5 (lowerleft)to 3.0 (upperright)instepsof0.5. Connectedplusesrepresentcolors/flux ratios for pure blackbody SEDs, and each plus corresponds to ablackbodytemperatureof600k(upperright),1000k,3000k,6000k, and K (lower left). The boundaries for AGN selection are fromdonleyetal.(2012). Ohyama, Terashima, & Sakamoto 2015, ApJ

20 NGC 3256: AGN in the S nucleus IR SED SED fitting single SB 3.6" 0.36" AGN+SB log Flux (Jy) SB+SB 4.5 μm (excess at S) Observed Wavelength (μm) Ohyama, Terashima, & Sakamoto 2015, ApJ

21 NGC 3256: AGN in the S nucleus A red source in HST data: unresolved (<0.26") core " FWHM source 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 of F222M/F160W. (f) The F222M nuclear component, made by subtracting the synthetic F222M stellar component image from the observed F222M image. The NICMOS resolution (0. 26 FWHM) is indicated by a white circle. (g) (h) The residual images of the F222M nuclear component after subtracting the fitted Gaussian models. The panel (g) shows a case of single-gaussian model, and (h) shows acaseof double-gaussian model. The fitted positions of Gaussian components are marked with white pluses in panels (g) and (h). All panelsare shown in linear scale, and flux (in units of MJy/steradian) and fluxratio(foronlypanelf)scaleareindicatedinscalebarsforeachpanel. The zero flux levels in the residual images are also indicated by black contours. Ohyama, Terashima, & Sakamoto 2015, ApJ

22 NGC 3256: AGN in the S nucleus HST unresolved source: on the model AGN SED AGN+SB SED model HST AGN with N H ~ cm -2 (τ 9.7 ~ 10, A V ~ 80 mag) Ohyama, Terashima, & Sakamoto 2015, ApJ

23 Arp 220 Spectral Scan is ongoing Outflow to be studied, among others , "Galaxies of many Sweden

24 13 Arp 220 : the Nearest ULIRG 12 ULIRG Arp 220 Arp 299 Mrk 231 log L μm / L LIRG M82 NGC 253 NGC 1068 M51 NGC 3256 M87 Lbol M31 M81 9 M Distance [Mpc] Distance / Mpc

25 Arp 220: double nucleus L Arp 220 NIR/HST HST image, counter-rot model P-Cyg. profile => outflow 1"= 360 pc (Scoville et al. 1998) (Sakamoto, Scoville et al. 1999)

26 Arp 220: dual outflows Arp 220 NIR/HST Dec. offset [arcsec] (a) Arp 220 HCO HCO + (4-3) " x 0.28" 300 pc (b) Arp 220 HCO HCO + (3-2) + (3-2) 0.45" x 0.34" 300 pc 1"= 360 pc (Scoville et al. 1998) Dec. offset [arcsec] (c) Arp 220 CO(3-2) 0.34" x 0.28" CO(3-2) (d) Arp mm 0.34" x 0.28" 300 pc Arp 220 E HCO + (4-3) + (4-3) Arp 220 E R.A. offset [arcsec] R.A. offset [arcsec] Arp 220 W HCO + (4-3) + (4-3) Arp 220 W Arp 220E Arp 220W Arp 220W V-V SYS ~ 100 km s -1 N H2 ~ cm -2 (T ex, [HCO + /H 2 ] assumed) dm/dt ~ 100 M yr -1 (r absorber 50 pc assumed) Intensity [mjy beam -1 ] HCO + (3-2) + (3-2) 1 CO(3-2) CO(3-2) CO(3-2), 0.5" data Vsys (E) Velocity (radio, LSR) [km s -1 ] HCN(4-3) Velocity HCO + (3-2) + (3-2) 1 CO(3-2) CO(3-2) CO(3-2), 0.5" data 1 Vsys (W) HCN(4-3) Velocity Velocity (radio, LSR) [km s -1 ] (Sakamoto et al. 2009, ApJ, 700, L104) -0.4

27 ALMA Spectral Bands 1.0 PWV= 0.25 mm; 5% of ALMA time PWV= 1 mm; 50% of ALMA time 0.8 Transmission Band 3 Band 4 Band 5 Band 6 Band 7 Band O2@119 H2O@183 H2O@325 H2O@380 O2@368 O2@425 H2O@448 H2O@475 O2@ Frequency / GHz

28 Arp 220 Spectral Scan : Project Overview 1.0 PWV= 0.25 mm; 5% of ALMA time PWV= 1 mm; 50% of ALMA time 0.8 Transmission B3 C.3? B4 C.3? P.I. Sergio Martin B6 Cyc. 1/2 B7 Cyc. 1/2 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 Frequency / GHz

29 Arp 220 Spectral Scan : Project Overview 1.0 PWV= 0.25 mm; 5% of ALMA time PWV= 1 mm; 50% of ALMA time 0.8 Transmission B3 C.3? B4 C.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.? Frequency / GHz

30 Arp 220 Spectral Scan : Project Overview 1.0 PWV= 0.25 mm; 5% of ALMA time PWV= 1 mm; 50% of ALMA time 0.8 Transmission B3 C.3+ B4 C.3+ B6 Cyc. 1/2 Bands 6,7 (Cyc. 1 2) B7 Cyc. 1/2 90% done 0.2 other bands (Cyc. 3+) Frequency / GHz

31 Arp 220 Spectral Scan A preview was given in the talk. Results will be published soon. Stay tuned

32 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 , "Galaxies of many Sweden