SMA Science Highlight: How can SMA help your research?

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

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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Current Status of the SMACurrent Status of the SMA

Eight 6-m telescopes are working together.Eight 6-m telescopes are working together. Three RX bands (230, 345, 690 GHz) are Three RX bands (230, 345, 690 GHz) are

available. A new 400 GHz RX is under testing.available. A new 400 GHz RX is under testing. Dual-band system is operational.Dual-band system is operational. 2 GHz band width, 101.6 kHz frequency 2 GHz band width, 101.6 kHz frequency

resolution (resolution (V~0.13 km/s @230 GHz)V~0.13 km/s @230 GHz) Maximum baseline (~500 m) is available.Maximum baseline (~500 m) is available. Remote observations from Taiwan are doable.Remote observations from Taiwan are doable. No day-time operation yet.No day-time operation yet.

Eight 6-m telescopes are working together.Eight 6-m telescopes are working together. Three RX bands (230, 345, 690 GHz) are Three RX bands (230, 345, 690 GHz) are

available. A new 400 GHz RX is under testing.available. A new 400 GHz RX is under testing. Dual-band system is operational.Dual-band system is operational. 2 GHz band width, 101.6 kHz frequency 2 GHz band width, 101.6 kHz frequency

resolution (resolution (V~0.13 km/s @230 GHz)V~0.13 km/s @230 GHz) Maximum baseline (~500 m) is available.Maximum baseline (~500 m) is available. Remote observations from Taiwan are doable.Remote observations from Taiwan are doable. No day-time operation yet.No day-time operation yet.

Field of View and Angular ResolutionField of View and Angular Resolution

Frequency FOVAngular resolution

compact extendedvery 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 resolutionVelocity coverage and resolution

FrequencyFull velocity coverage(2 GHz)

Velocity resolution

Standard(800 kHz)

Highest(100 kHz)

230 GHz 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 ScienceHighlight 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

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 outflowHH 211 outflowCavity & jet observed in the CO J=2-1

Gueth et al. 1999 with PdBI

Low-velocity component Low-velocity component VVLSRLSR = 2.2 – 18.2 km/s = 2.2 – 18.2 km/sCavity structureCavity structure

High-velocity component High-velocity component VVLSRLSR < 2.2 & > 18.2 km/s < 2.2 & > 18.2 km/sJet-like structureJet-like structure

•• Highly-collimated outflowHighly-collimated outflow(aspect ratio ~ 15:1) (aspect ratio ~ 15:1)

•• Driven by the low-luminosity Driven by the low-luminosity (3.6 Lo) Class 0 protostar (3.6 Lo) Class 0 protostar (T(Tbolbol ~ 33 K) ~ 33 K)

•• Dynamical time scale ~ 750 yrDynamical time scale ~ 750 yr•• Outflow axis ~ 10° from the plane Outflow axis ~ 10° from the plane

of the skyof the sky

HH 211 in HHH 211 in H22 line line

McCaughrean et al. 2005McCaughrean et al. 2005

HH 211 molecular jetHH 211 molecular jet

beam: 1.60” x 0.88” P.A. -40.7 deg.

SiO 5-4 with the SMA (Hirano et al.)SiO 5-4 with the SMA (Hirano et al.)

SiO 5-4, 3-2, and 1-0SiO 5-4, 3-2, and 1-0

SiO 5-4

SiO 3-2

SiO 1-0

Chandler & Richer (2001), with the VLA

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

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.)

Circumstellar disk:Orion Proplyds

Circumstellar disk:Orion Proplyds

0.019 M

0.016 M

0.024 M

0.013 M

Williams et al.Williams et al.

* 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 lensingSMA will identify the optical counterpart for GN 20 and the possibility of lensing in Bootes-59

GN 20 (Pope et al. 2005)

Bootes-59 (Borys et al. 2005)

High-Z GalaxiesHigh-Z Galaxies

SMA 890 micron observationsSMA 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

Continuum Polarization Observations

Waveplate

Control computer

Polarized Dust EmissionPolarized Dust Emission Contours - I Pixel - polarized flu

x density sqrt(Q^2+U^2)

RMS = 3 mJy/bm Peak pol = 9 % at

PA 153 degrees At the peak of Stok

es I - pol = 1% Averaged pol = 4.

7% @ 145 degrees

NGC 1333 IRAS 4A E-vectors

Rao et al.Rao et al.

NGC 1333 IRAS 4A B-fieldNGC 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.Rao et al.

Astrochemistory: Orion Line ForestAstrochemistory: Orion Line Forest

- Approximately 150 spectral linesApproximately 150 spectral lines from 26 speciesfrom 26 species- 90% of them could be identified90% of them could be identified- Additional low-level emissionAdditional low-level emission which needs further work which needs further work - 15% of the lines were not detected15% of the lines were not detected by previous single-dish studies (plusby previous single-dish studies (plus low-level emission)low-level emission)

338 GHz 348 GHz

2 GHz

Beuther et al. 2004, 2005Beuther et al. 2004, 2005

Orion submm molecular mapsOrion submm molecular maps- Toward source I mainly SiOToward source I mainly SiO- Sulphur-bearing species towardSulphur-bearing species toward Hot Core and Compact RidgeHot Core and Compact Ridge- Sulphur- and oxygen-bearingSulphur- and oxygen-bearing species toward IRc6species toward IRc6

- Oxygen-bearing moleculesOxygen-bearing molecules weaker toward Hot Core and weaker toward Hot Core and strong toward Compact Ridgestrong toward Compact Ridge- Nitrogen-bearing moleculesNitrogen-bearing molecules strong toward Hot Corestrong toward Hot Core

- Imaging helps to identify linesImaging helps to identify lines

Beuther et al. 2004, 2005Beuther et al. 2004, 2005

Orion 690 GHz Spectra and MapsOrion 690 GHz Spectra and Maps

Beuther et al.Beuther et al.

Orion 690 GHz molecular mapsOrion 690 GHz molecular maps

Beuther et al.Beuther et al.

SMA 690 GHz Observations:Dual-band Calibration

SMA 690 GHz Observations:Dual-band Calibration

Ant 1 Ant 2 Ant 3

Ant 4 Ant 5 Ant 6

Antenna based 230/650 phase-phase plots of Ganymede

the slopes are very similar to the theoretical predictions

SMA Science Program at IAASMA 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

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



(Fukagawa et al. 2004)(Fukagawa et al. 2004)

AB Aurige

Circumstellar disks around Herbig AeCircumstellar disks around Herbig Ae







Lin et al. (2005)

Massive Star FormationMassive Star FormationIRAS 20126+4104

Liu et al.

Detached shell around R SclDetached shell around R Scl

Violent phenomenonViolent phenomenonto crate this kind of to crate this kind of shall structure.shall structure. Helium flush?Helium flush?

Pi Gru: Disk and JetPi Gru: Disk and Jet

Disk & high velocity Disk & high velocity outflow are present in an outflow are present in an envelope of a normal AGB envelope of a normal AGB star.star.

Chiu et al. (2005)

Future PlanFuture 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”.

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”.

What can the IAA-SMA team help to promote good projects?

What can the IAA-SMA team help to promote good projects?

Regular interaction/discussions Technical advice Interferometer school for students Promote collaborative projects

Regular interaction/discussions Technical advice Interferometer school for students Promote collaborative projects

We do need supports/inputs from people outside, too!We do need supports/inputs from people outside, too!

SMA Science Highlight: How can SMA help your research?

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