The SMA CO(6-5) &The SMA CO(6-5) &690 GHz Continuum690 GHz Continuum

Observations of Arp 220Observations of Arp 220

Satoki Matsushita (ASIAA)Satoki Matsushita (ASIAA)D. Iono (CfA), C.-Y. Chou (ASIAA), M. Gurwell (CfA),D. Iono (CfA), C.-Y. Chou (ASIAA), M. Gurwell (CfA),

P.-Y. Hsieh (NTU, ASIAA), T. Hunter(CfA), J. Lim (ASIAA),P.-Y. Hsieh (NTU, ASIAA), T. Hunter(CfA), J. Lim (ASIAA),S. Muller (ASIAA), A.B. Peck (CfA), G. Petitpas (CfA), S. Muller (ASIAA), A.B. Peck (CfA), G. Petitpas (CfA), K. Sakamoto (NAOJ, CfA), S. Sawada-Satoh (ASIAA),K. Sakamoto (NAOJ, CfA), S. Sawada-Satoh (ASIAA),Dinh-V-Trung (ASIAA), M.C. Wiedner (Univ. Koln, CfA),Dinh-V-Trung (ASIAA), M.C. Wiedner (Univ. Koln, CfA),

D. Wilner (CfA)D. Wilner (CfA)

IntroductionIntroduction Arp 220Arp 220

Prototypical Ultra Luminous Infrared Galaxy (ULIRG).Prototypical Ultra Luminous Infrared Galaxy (ULIRG). One of the nearest ULIRGs (77 Mpc)One of the nearest ULIRGs (77 Mpc) LL8-10008-1000mm = 1.4 x 10 = 1.4 x 101212 L Lsunsun (Soifer et al. 1987) (Soifer et al. 1987)

Final stage of galaxy merger.Final stage of galaxy merger. Two nuclei at the center (~1” / 370 pc separation).Two nuclei at the center (~1” / 370 pc separation).

High resolution high-J CO lines & dust imagings are importanHigh resolution high-J CO lines & dust imagings are important to know about the conditions of extreme starburst in mergint to know about the conditions of extreme starburst in merging sequence.g sequence.

ULIRGs are believe to be nearby counterparts for higULIRGs are believe to be nearby counterparts for high-z starburst galaxies.h-z starburst galaxies.

Due to the redshift, many of the high-z galaxies observed witDue to the redshift, many of the high-z galaxies observed with high-J CO lines.h high-J CO lines.

Observing high-J CO lines of nearby ULIRGs are important fObserving high-J CO lines of nearby ULIRGs are important for the study of high-z starburst galaxies.or the study of high-z starburst galaxies.

2.8’

2.2’

Arp 1966Palomar 5m

Scoville et al. 1998HST/NICMOS

19”

Observation & CalibrationObservation & Calibration Telescope: SMATelescope: SMA

Antennas: 1,2,3,4,5,6Antennas: 1,2,3,4,5,6 Date: March 2Date: March 2ndnd, 2005, 2005

225 GHz opacity = 0.03-0.04225 GHz opacity = 0.03-0.04 Frequency SettingFrequency Setting

LSB: 679.2 GHz CO(6-5)LSB: 679.2 GHz CO(6-5) USB: 689.2 GHz ContinuumUSB: 689.2 GHz Continuum

CalibratorsCalibrators Amplitude & Phase: Callisto (~50Amplitude & Phase: Callisto (~50oo away) away)

Flux of Ceres shows 78% of the actual. Flux of Ceres shows 78% of the actual. => => Flux accuracy ~ 20%-25%Flux accuracy ~ 20%-25%

Position of Arp 220 shifted for ~0.7”, consistent with the basePosition of Arp 220 shifted for ~0.7”, consistent with the baseline errors.line errors.

Bandpass: Mars, Callisto, & GanymedeBandpass: Mars, Callisto, & Ganymede ImagingImaging

Beam size: 1.2” x 0.8” (450 pc x 300 pc)Beam size: 1.2” x 0.8” (450 pc x 300 pc)

ResultsResultsArp 220 689 GHz (435 Arp 220 689 GHz (435 m) continuumm) continuum

Total flux: 2.3 JyTotal flux: 2.3 JySingle-dish 450Single-dish 450mm

UKIRT UKT14UKIRT UKT14 Eales et al. 1989Eales et al. 1989 3.0+-1.1 Jy3.0+-1.1 Jy Missing flux = 23%Missing flux = 23%

JCMT SCUBAJCMT SCUBA Dunne & Eales 2001Dunne & Eales 2001 6.3+-0.8 Jy6.3+-0.8 Jy Missing flux = 63%Missing flux = 63%

Contours: -2, 2, 4, 6Contours: -2, 2, 4, 61.2” x 0.8”1.2” x 0.8”

ResultsResultsComparison between other continuum Comparison between other continuum

images in different wavelengths.images in different wavelengths.

W NucleusW Nucleus0.96 Jy/beam0.96 Jy/beam

E NucleusE Nucleus0.90 Jy/beam0.90 Jy/beam

Sakamoto et al.Sakamoto et al.

1.2” x 0.8”1.2” x 0.8”

Sakamoto et al. (1999)Sakamoto et al. (1999)

Discussion (Continuum)Discussion (Continuum) Arp 220 689 GHz continuumArp 220 689 GHz continuum

East Nucleus: 900 +- 0.16 mJy/BEast Nucleus: 900 +- 0.16 mJy/B West Nucleus: 960 +- 0.16 mJy/BWest Nucleus: 960 +- 0.16 mJy/B E/W flux ratio: 0.94 +- 0.23E/W flux ratio: 0.94 +- 0.23

Arp 220 230 GHz continuum Arp 220 230 GHz continuum (S(Sakamoto et al. 1999)akamoto et al. 1999) East Nucleus: 66 +- 9.3 mJy/BEast Nucleus: 66 +- 9.3 mJy/B West Nucleus: 142 +- 9.3 mJy/BWest Nucleus: 142 +- 9.3 mJy/B E/W flux ratio: 0.46 +- 0.07E/W flux ratio: 0.46 +- 0.07

Arp 220Arp 220

Comparison of SED with that of the high-z QSO Comparison of SED with that of the high-z QSO BR1202-0725BR1202-0725

Discussion (Continuum)Discussion (Continuum)

Arp 220Arp 220

Blue: Total fluxBlue: Total fluxRed: W NucleusRed: W NucleusGreen: E NucleusGreen: E Nucleus

3.23.2

1.81.8

.9.9

D. Iono et al., poster in this meeting.D. Iono et al., poster in this meeting.

.5.5

.4.4

SMA 333 GHzSMA 333 GHz(900 (900 m) imagem) image

BR1202-0725BR1202-0725

The two nuclei/sources in both galaxies seem to have different speThe two nuclei/sources in both galaxies seem to have different spectral indices.ctral indices.

Different dust properties?Different dust properties? Effect of synchrotron / free-free emission?Effect of synchrotron / free-free emission?

Note that separations of the nuclei are very different:Note that separations of the nuclei are very different: Arp 220: ~ 300-400 pc vs BR 1202-0725: ~ 30-40 kpcArp 220: ~ 300-400 pc vs BR 1202-0725: ~ 30-40 kpc

Note that BR1202-0725 is z ~ 4.7 => 350 GHz -> 2 THzNote that BR1202-0725 is z ~ 4.7 => 350 GHz -> 2 THz

ResultsResultsArp 220 CO(6-5) Integrated IntensityArp 220 CO(6-5) Integrated Intensity

1.2” x 0.8”1.2” x 0.8”

Sakamoto et al.Sakamoto et al.

Sakamoto et al. (1999)Sakamoto et al. (1999)

ResultsResultsArp 220 CO(6-5) Velocity MapArp 220 CO(6-5) Velocity Map

SMA CO(6-5)SMA CO(6-5)

Sakamoto et al. 1999Sakamoto et al. 1999

ResultsResults ARP 220 CO(6-5) SpectraARP 220 CO(6-5) Spectra

Peak Temperature Peak Temperature @ @ 1.2” x 0.8” beam1.2” x 0.8” beam

E Nucleus: Peak = 9.4 KE Nucleus: Peak = 9.4 K W Nucleus: Peak = 10.6 KW Nucleus: Peak = 10.6 K

Peak TemperaturePeak Temperatureassuming 0.57” x 0.52” sizeassuming 0.57” x 0.52” size

E Nucleus: Peak = 30 KE Nucleus: Peak = 30 K W Nucleus: Peak = 34 KW Nucleus: Peak = 34 K

ARP 220 CO(2-1)ARP 220 CO(2-1) Peak Temperature Peak Temperature

@ 0.57” x 0.52” size@ 0.57” x 0.52” size E Nucleus: Peak = 38 KE Nucleus: Peak = 38 K W Nucleus: Peak = 37 KW Nucleus: Peak = 37 K

8.3 K8.3 K

5.6 K5.6 K

8.3 K8.3 K

5.6 K5.6 K

E NucleusE Nucleus

W NucleusW Nucleus

0.0 K0.0 K

0.0 K0.0 K

5350 km/s5350 km/s

Discussion (CO lines)Discussion (CO lines) Comparison of CO intensities between nearby to Comparison of CO intensities between nearby to

high-z galaxieshigh-z galaxies

Arp 220Arp 220

Kawabe et al. 1999Kawabe et al. 1999

Arp 220 CO intensities are similar to nearby starArp 220 CO intensities are similar to nearby starburst & high-z starburst galaxy.burst & high-z starburst galaxy.

ConclusionConclusion We succeeded to image CO(6-5) & 690 GHz (43We succeeded to image CO(6-5) & 690 GHz (43

5 5 m) continuum maps of Arp 220 with the SMA.m) continuum maps of Arp 220 with the SMA. 690 GHz continuum image 690 GHz continuum image

Two nuclei seems to have different spectral indices at Two nuclei seems to have different spectral indices at sub-mm.sub-mm.

CO(6-5) imageCO(6-5) image CO(6-5) emission seems to have similar distribution & CO(6-5) emission seems to have similar distribution &

kinematics to that of CO(2-1).kinematics to that of CO(2-1). Physical conditions of CO gas seems to have similar tPhysical conditions of CO gas seems to have similar t

o that of nearby & high-z starbursts.o that of nearby & high-z starbursts.=> Support the idea that ULIRGs are the nearb=> Support the idea that ULIRGs are the nearb

y y counter part of high-z starburst galaxies.counter part of high-z starburst galaxies.