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The SMA CO(6-5) & 690 GHz Continuum Observations of Arp 220

The SMA CO(6-5) & 690 GHz Continuum Observations of Arp 220. Satoki Matsushita (ASIAA) D. Iono (CfA), C.-Y. Chou (ASIAA), M. Gurwell (CfA), P.-Y. Hsieh (NTU, ASIAA), T. Hunter(CfA), J. Lim (ASIAA), S. Muller (ASIAA), A.B. Peck (CfA), G. Petitpas (CfA),

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The SMA CO(6-5) & 690 GHz Continuum Observations of Arp 220

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  1. The SMA CO(6-5) &690 GHz ContinuumObservations of Arp 220 Satoki Matsushita (ASIAA) D. Iono (CfA), C.-Y. Chou (ASIAA), M. Gurwell (CfA), P.-Y. Hsieh (NTU, ASIAA), T. Hunter(CfA), J. Lim (ASIAA), S. Muller (ASIAA), A.B. Peck (CfA), G. Petitpas (CfA), K. Sakamoto (NAOJ, CfA), S. Sawada-Satoh (ASIAA), Dinh-V-Trung (ASIAA), M.C. Wiedner (Univ. Koln, CfA), D. Wilner (CfA)

  2. 2.2’ 19” 2.8’ Introduction • Arp 220 • Prototypical Ultra Luminous Infrared Galaxy (ULIRG). • One of the nearest ULIRGs (77 Mpc) • L8-1000mm = 1.4 x 1012 Lsun (Soifer et al. 1987) • Final stage of galaxy merger. • Two nuclei at the center (~1” / 370 pc separation). • High resolution high-J CO lines & dust imagings are important to know about the conditions of extreme starburst in merging sequence. • ULIRGs are believe to be nearby counterparts for high-z starburst galaxies. • Due to the redshift, many of the high-z galaxies observed with high-J CO lines. • Observing high-J CO lines of nearby ULIRGs are important for the study of high-z starburst galaxies. Scoville et al. 1998 HST/NICMOS Arp 1966 Palomar 5m

  3. Observation & Calibration • Telescope: SMA • Antennas: 1,2,3,4,5,6 • Date: March 2nd, 2005 • 225 GHz opacity = 0.03-0.04 • Frequency Setting • LSB: 679.2 GHz CO(6-5) • USB: 689.2 GHz Continuum • Calibrators • Amplitude & Phase: Callisto (~50o away) • Flux of Ceres shows 78% of the actual. => Flux accuracy ~ 20%-25% • Position of Arp 220 shifted for ~0.7”, consistent with the baseline errors. • Bandpass: Mars, Callisto, & Ganymede • Imaging • Beam size: 1.2” x 0.8” (450 pc x 300 pc)

  4. Results • Arp 220 689 GHz (435 mm) continuum • Total flux: 2.3 Jy • Single-dish 450mm • UKIRT UKT14 • Eales et al. 1989 • 3.0+-1.1 Jy • Missing flux = 23% • JCMT SCUBA • Dunne & Eales 2001 • 6.3+-0.8 Jy • Missing flux = 63% 1.2” x 0.8” Contours: -2, 2, 4, 6s

  5. Results • Comparison between other continuum images in different wavelengths. E Nucleus 0.90 Jy/beam W Nucleus 0.96 Jy/beam 1.2” x 0.8” Sakamoto et al. Sakamoto et al. (1999)

  6. Discussion (Continuum) • Arp 220 689 GHz continuum • East Nucleus: 900 +- 0.16 mJy/B • West Nucleus: 960 +- 0.16 mJy/B • E/W flux ratio: 0.94 +- 0.23 • Arp 220 230 GHz continuum (Sakamoto et al. 1999) • East Nucleus: 66 +- 9.3 mJy/B • West Nucleus: 142 +- 9.3 mJy/B • E/W flux ratio: 0.46 +- 0.07 Arp 220

  7. D. Iono et al., poster in this meeting. BR1202-0725 n2.5 n3.4 SMA 333 GHz (900 mm) image Discussion (Continuum) • Comparison of SED with that of the high-z QSO BR1202-0725 Arp 220 n3.2 n1.8 n2.9 Blue: Total flux Red: W Nucleus Green: E Nucleus • The two nuclei/sources in both galaxies seem to have different spectral indices. • Different dust properties? • Effect of synchrotron / free-free emission? • Note that separations of the nuclei are very different: • Arp 220: ~ 300-400 pc vs BR 1202-0725: ~ 30-40 kpc • Note that BR1202-0725 is z ~ 4.7 => 350 GHz -> 2 THz

  8. Sakamoto et al. (1999) Sakamoto et al. Results • Arp 220 CO(6-5) Integrated Intensity 1.2” x 0.8”

  9. Results • Arp 220 CO(6-5) Velocity Map SMA CO(6-5) Sakamoto et al. 1999

  10. Results E Nucleus 8.3 K • ARP 220 CO(6-5) Spectra • Peak Temperature @ 1.2” x 0.8” beam • E Nucleus: Peak = 9.4 K • W Nucleus: Peak = 10.6 K • Peak Temperature assuming 0.57” x 0.52” size • E Nucleus: Peak = 30 K • W Nucleus: Peak = 34 K • ARP 220 CO(2-1) • Peak Temperature @ 0.57” x 0.52” size • E Nucleus: Peak = 38 K • W Nucleus: Peak = 37 K 5.6 K 0.0 K W Nucleus 8.3 K 5.6 K 0.0 K 5350 km/s

  11. Arp 220 Discussion (CO lines) • Comparison of CO intensities between nearby to high-z galaxies Kawabe et al. 1999 • Arp 220 CO intensities are similar to nearby starburst & high-z starburst galaxy.

  12. Conclusion • We succeeded to image CO(6-5) & 690 GHz (435 mm) continuum maps of Arp 220 with the SMA. • 690 GHz continuum image • Two nuclei seems to have different spectral indices at sub-mm. • CO(6-5) image • CO(6-5) emission seems to have similar distribution & kinematics to that of CO(2-1). • Physical conditions of CO gas seems to have similar to that of nearby & high-z starbursts. => Support the idea that ULIRGs are the nearby counter part of high-z starburst galaxies.

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