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SMA Science Highlight: How can SMA help your research?

SMA Science Highlight: How can SMA help your research?. Nagayoshi Ohashi (ASIAA-Hawaii) and SMA Science team. - Early science results; ApJL Special issues (Nov, 2004) - Recent results; Submillimeter Astronomy in the era of the SMA (ppt files are available at cfa-www.harvard.edu/smast05/).

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SMA Science Highlight: How can SMA help your research?

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  1. SMA Science Highlight:How can SMA help your research? Nagayoshi Ohashi (ASIAA-Hawaii) and SMA Science team - Early science results; ApJL Special issues (Nov, 2004) - Recent results; Submillimeter Astronomy in the era of the SMA (ppt files are available at cfa-www.harvard.edu/smast05/).

  2. Current Status of the SMA • 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 kHz 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.

  3. Field of View and Angular Resolution

  4. Velocity coverage and resolution

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

  6. Cavity & jet observed in the CO J=2-1 Low-velocity component VLSR = 2.2 – 18.2 km/s Cavity structure HH 211 in H2 line High-velocity component VLSR < 2.2 & > 18.2 km/s Jet-like structure Gueth et al. 1999 with PdBI HH 211 outflow McCaughrean et al. 2005 • 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

  7. SiO 5-4 with the SMA (Hirano et al.) beam: 1.60” x 0.88” P.A. -40.7 deg. HH 211 molecular jet

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

  9. Circumstellar disk:Orion Proplyds

  10. 0.019 M 0.016 M 0.024 M 0.013 M Williams et al.

  11. High-Z Galaxies GN 20 (Pope et al. 2005) Bootes-59 (Borys et al. 2005) * Both 20mJy sources detected using SCUBA * GN20 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

  12. 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.)

  13. Continuum Polarization Observations Control computer Waveplate

  14. NGC 1333 IRAS 4A E-vectors Polarized Dust Emission • Contours - I • Pixel - polarized flux density sqrt(Q^2+U^2) • RMS = 3 mJy/bm • Peak pol = 9 % at PA 153 degrees • At the peak of Stokes I - pol = 1% • Averaged pol = 4.7% @ 145 degrees Rao et al.

  15. NGC 1333 IRAS 4A 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.

  16. 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

  17. Orion submm molecular maps Beuther et al. 2004, 2005 • Toward source I mainly SiO • Sulphur-bearing species toward • Hot Core and Compact Ridge • Sulphur- and oxygen-bearing • species toward IRc6 • Imaging helps to identify lines • Oxygen-bearing molecules • weaker toward Hot Core and • strong toward Compact Ridge • Nitrogen-bearing molecules • strong toward Hot Core

  18. Orion 690 GHz Spectra and Maps Beuther et al.

  19. Orion 690 GHz molecular maps Beuther et al.

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

  21. SMA Science Program at IAA • Star formation • Molecular outflow (HH211) • Circumstellar disk (AB Aur, HD) • Massive star formation (IRAS20126) • Astrochemistry (Orion KL, IRAS20126, IRAS16293) • Extragalactic • AGN/Syfert (M51) • Starburst/ULIRG • Evolved star • Detailed structures of circumstellar envelopes • Shaping mechanism of envelopes

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

  23. Massive Star Formation IRAS 20126+4104 Liu et al.

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

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

  26. Future Plan • Link with JCMT and CSO, providing ~3 times better sensitivity. • 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”.

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

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