SMA Science Highlight How can SMA help your

SMA Science Highlight: How can SMA help your research? Nagayoshi Ohashi (ASIAA-Hawaii) and SMA Science team - Early science results; Ap. JL Special issues (Nov, 2004) - Recent results; Submillimeter Astronomy in the era of the SMA (ppt files are available at cfa-www. harvard. edu/smast 05/).

Current Status of the SMA n n n n Eight 6 -m telescopes are working together. Three RX bands (230, 345, 690 GHz) are available. A new 400 GHz RX is under testing. Dual-band system is operational. 2 GHz band width, 101. 6 k. Hz frequency resolution ( V~0. 13 km/s @230 GHz) Maximum baseline (~500 m) is available. Remote observations from Taiwan are doable. No day-time operation yet.

Field of View and Angular Resolution Angular resolution Frequency FOV compact extended very extended 230 GHz 54” 3”-4” 1”-2” ~0. 4” 345 GHz 36” 1”-2” 0. 7”-1” ~0. 3” 690 GHz 18” 0. 7”-1” ~0. 4” ~0. 2”

Velocity coverage and resolution Frequency Full velocity coverage (2 GHz) 230 GHz Velocity resolution Standard (800 k. Hz) Highest (100 k. Hz) 2600 km/s 1. 0 km/s 0. 13 km/s 345 GHz 1700 km/s 0. 68 km/s 0. 085 km/s 690 GHz 870 km/s 0. 36 km/s 0. 045 km/s

Highlight of SMA Science n n n n Molecular jets Circumstellar (protoplanetary) disks High-Z galaxies (submm galaxies) Magnetic field (polarization observations) Astrochemistry Observations at 690 GHz Observations at sub-arcsecond

HH 211 outflow Cavity & jet observed in the CO J=2 -1 Low-velocity component VLSR = 2. 2 – 18. 2 km/s Cavity structure HH 211 in H 2 line Mc. Caughrean et al. 2005 • High-velocity component VLSR < 2. 2 & > 18. 2 km/s Jet-like structure • • • Gueth et al. 1999 with Pd. BI Highly-collimated outflow (aspect ratio ~ 15: 1) Driven by the low-luminosity (3. 6 Lo) Class 0 protostar (Tbol ~ 33 K) Dynamical time scale ~ 750 yr Outflow axis ~ 10° from the plane of the sky

HH 211 molecular jet Si. O 5 -4 with the SMA (Hirano et al. ) beam: 1. 60” x 0. 88” P. A. -40. 7 deg.

Si. O 5 -4, 3 -2, and 1 -0 Si. O 5 -4 (SMA; Hirano et al. ) Si. O 3 -2 (NMA; Hirano et al. ) Si. O 1 -0 Chandler & Richer (2001), with the VLA n Higher transition of the Si. O is better collimated and strong in the vicinity of the protostar n The innermost knot pair (related to the latest activity) is seen only in the maps of higher transitions of Si. O

Circumstellar disk: Orion Proplyds

0. 019 M 0. 016 M 0. 024 M 0. 013 M Williams et al.

High-Z Galaxies GN 20 (Pope et al. 2005) Bootes-59 (Borys et al. 2005) * Both 20 m. Jy sources detected using SCUBA * GN 20 is a sub-mm galaxy found in the GOODS-N field of the HDF * Bootes-59 is discovered in the Bootes field of the Spitzer MIPS survey. The MIR galaxy is already identified, but possibility of lensing SMA will identify the optical counterpart for GN 20 and the possibility of lensing in Bootes-59

SMA 890 micron observations GN 20: Found NIR galaxy but no optical galaxy. Extinction? Merger? Bootes-59: Flux consistent with SCUBA, and point source is the best model fit to the visibilities. Lensing is not significant down to ~0. 2” size scale. (Iono et al. )

Continuum Polarization Observations Control computer Waveplate

Polarized Dust Emission NGC 1333 IRAS 4 A E-vectors n n n Rao et al. Contours - I Pixel - polarized flux density sqrt(Q^2+U^2) RMS = 3 m. Jy/bm Peak pol = 9 % at PA 153 degrees At the peak of Stokes I - pol = 1% Averaged pol = 4. 7% @ 145 degrees

NGC 1333 IRAS 4 A B-field • Polarization hole • Polarization peak is offset • Hour glass shape of the magnetic field structure in the circumbinary envelope • The large scale field is well aligned with the minor axis • We will need some higher angular resolution observations to map the structure of the field between the two cores Rao et al.

Astrochemistory: Orion Line Forest 338 GHz 348 GHz 2 GHz - Approximately 150 spectral lines from 26 species - 90% of them could be identified - Additional low-level emission which needs further work - 15% of the lines were not detected by previous single-dish studies (plus low-level emission) Beuther et al. 2004, 2005

Orion submm molecular maps Beuther et al. 2004, 2005 - Toward source I mainly Si. O - Sulphur-bearing species toward Hot Core and Compact Ridge - Sulphur- and oxygen-bearing species toward IRc 6 - Imaging helps to identify lines - Oxygen-bearing molecules weaker toward Hot Core and strong toward Compact Ridge - Nitrogen-bearing molecules strong toward Hot Core

Orion 690 GHz Spectra and Maps Beuther et al.

Orion 690 GHz molecular maps Beuther et al.

SMA 690 GHz Observations: Dual-band Calibration Antenna based 230/650 phase-phase plots of Ganymede Ant 1 Ant 4 Ant 2 Ant 5 Ant 3 Ant 6 the slopes are very similar to theoretical predictions

SMA Science Program at IAA n Star formation n n Extragalactic n n n Molecular outflow (HH 211) Circumstellar disk (AB Aur, HD) Massive star formation (IRAS 20126) Astrochemistry (Orion KL, IRAS 20126, IRAS 16293) AGN/Syfert (M 51) Starburst/ULIRG Evolved star n n Detailed structures of circumstellar envelopes Shaping mechanism of envelopes

Circumstellar disks around Herbig Ae AB Aurige (Fukagawa et al. 2004) Lin et al. (2005)

Massive Star Formation IRAS 20126+4104 Liu et al.

Detached shell around R Scl Violent phenomenon to crate this kind of shall structure. à Helium flush?

Pi Gru: Disk and Jet Disk & high velocity outflow are present in an envelope of a normal AGB star. Chiu et al. (2005)

Future Plan n Link with JCMT and CSO, providing ~3 times better sensitivity. n n First fringe between SMA and JCMT was obtained! More test dual-band calibration technique for higher freq. observations. Install 400 GHz RXs on all the antennas, providing a capability of dual polarization observations at 350 GHz. Develop phase correction technique (fast switching, WVM) to achieve the highest resolution of 0. 1”.

What can the IAA-SMA team help to promote good projects? n n Regular interaction/discussions Technical advice Interferometer school for students Promote collaborative projects We do need supports/inputs from people outside, too!