1 / 23

First ATCA results at millimetre wavelengths

First ATCA results at millimetre wavelengths. Vincent Minier School of Physics University of New South Wales. Australia Telescope Compact Array. Narrabri, NSW, 500 km NW from Sydney; 6 antennas, 22-m diameter, baselines 31 m to 6 km; Traditional frequency range: 1 – 10 GHz (20, 13, 6

karma
Download Presentation

First ATCA results at millimetre wavelengths

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. First ATCA results at millimetre wavelengths Vincent Minier School of Physics University of New South Wales Millimetre Workshop 2002, ATNF

  2. Australia Telescope Compact Array • Narrabri, NSW, 500 km NW from Sydney; • 6 antennas, 22-m diameter, baselines 31 m to 6 km; • Traditional frequency range: 1 – 10 GHz (20, 13, 6 • and 3 cm or L, S, C, X) • Upgrade of ATCA at 3 and 12 mm : • 85 – 110 GHz (5 antennas) • 16 – 26 GHz (full array)

  3. ATCA site Mm receivers Control room E-W track S-N spur

  4. First light on 30th Nov. 2000 Orion SiO 86.243 GHz

  5. ATCA at 3 & 12 mm – Current Status 3 mm system • Frequency range: (1) 84.906-87.305 GHz (2) 88.506-91.305 GHz • 3 baselines, 2 pol.: CA02, CA03, CA04 • System temperature: 250 – 400 K • Bandwidth: 64, 128 MHz, spectral res. = 0.86 km/s • Sensitivity in 1 hr: 3.6 mJy (cont.) and 96 mJy (line) 12 mm system • Frequency range: 16-26 GHz • 15 baselines, 2 pol.: CA01, CA02, CA03, CA04, CA05, CA06 • System temperature: 60 – 70 K • Sensitivity in 1 hr: 20 mJy (line) with 16 MHz and 512 channels

  6. What can we observe with ATCA-mm? • Molecular lines: • Continuum emission: dust (3 mm) and • ionised gas (22 GHz)

  7. Recent Results at 3 and 12 mm • Pre-planetary disks around young stars (Wilner, Bourke, Wright, Jorgensen, van Dishoeck, Wong in 2002) • Massive star formation in the Galactic Plane (Minier, Burton, Wong, Purcell, Hill, Hunt, Barnes, Jones, Ellingsen, Cragg, Sobolev, Voronkov in 2002 – 2003) • Massive star formation in the LMC (N113: Wong, Ott, Mizuno et al. in 2001 – 2003; Water masers: Beasley, Claussen, Marvel & Staveley-Smith in 2002)

  8. Pre-planetary disks around young stars

  9. TW Hya T Tauri star 41±4 mJy HD 100546 Herbig Be star 36±3 mJy Dust in Pre-planetary Disks(Wilner et al. 2003 in press) • 3.4 mm continuum emission  dust emission from disks • 2 ATCA runs  6 baselines (2’’= 100/200 AU) See poster by Bourke et al.

  10. 2. Massive star formation in the Galactic Plane

  11. ATCA 3 mm IRAS 100 mm SIMBA 1.2 mm 15 M UCHII Maser 240 M (Hill et al. in prep; Walsh et al. 1998) (Minier et al. in prep) Methanol masers = massive YSOs ? CO Dame et al. 2001 IRAS Masers

  12. A hot molecular core in G318.95 • Unresolved CH3OH core • < 0.04 pc • Resolved HCO+ core: • R=0.06 pc • t=33 • NH2=5.51022 cm-2 • Mgas=15 M • Mvir=120 M • Resolved HCO+ wings •  outflows. • Massive protostellar core Res.: 4 – 22’’ = 0.04 – 0.26 pc HCO+ Hot core CH3OH Posters by Tracey Hill et al., Cormac Purcell et al., Peter Barnes et al. and Vincent Minier et al.

  13. Methanol masers in G345.01+1.79 (Minier et al. in 2002) 85.5 GHz maser UC HII region 86.9 GHz maser Masers All masers coincide in velocity and position  coincide in space

  14. Probing gas/dust conditions with methanol masers • Using model by Cragg et al. (2001). • Hot dust: 200-300 K • Cold gas <50 K • Density: 106 cm-3 Ellingsen et al. 2003, in press

  15. 25 GHz methanol maser in Orion BN/KL (Voronkov et al. in 2003) 52 - 51 E

  16. Deuterated ammonia in NGC 6334 I(N) (Wong, Minier & Forster in 2003) 85.9 GHz NH2D Burton et al. 2000 • EW 352 • 19 and 86 GHz • Continuum + NH2D

  17. 3. Massive star formation in the LMC

  18. FWHM  1.5 pc  R ~ 1 pc. Dv ~ 5 km s-1. HCO+ core in N113 ( Wong et al. in 2001-2003) • For a virialized cloud, ignoring optical depth effects, M  200(Rpc)(Dvkm/s)2  5000 M. • For constant density, nH ~ 5 x 104 cm-3.

  19. New water maser sites in the LMC Previous Parkes detections ( Scalise & Braz Whiteoak 1982; et al. 1983; Whiteoak & Gardner 1986) New ATCA detections (Beasley, Claussen, Marvel & Staveley-Smith 2002)

  20. 12 mm system is fully operational and works well; • 3 mm upgrade on its way and expected to be • complete for next winter (May 2004?); • 3/12 mm results since 2002: 43 projects • of which 27 in star formation; • Next observing session: mid-April to mid-Oct. • (or mid-Nov. depending on the configuration) Conclusions NEXT PROPOSAL DEADLINES : Oct. 15th, Feb. 15th, June 15th (might change to 6 month-observing terms)

  21. 3 mm user guide web page:http://www.atnf.csiro.au/observers/docs/3mm/12 mm system web page:http://www.atnf.csiro.au/projects/mnrf/12mm_details.html

  22. Phase stability Clear Night, 8pm local time b: 75m 120m 45m 34º 19º rms: 22º

  23. 4 hours later (midnight) b: 75m 120m 45m 34º 19º rms: 22º 24º 13º rms: 16º

More Related