21 november 2002millimetre workshop 2002, atnf first atca results at millimetre wavelengths vincent...
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21 November 2002 Millimetre Workshop 2002, ATNF
First ATCA results at millimetre
wavelengthsVincent MinierSchool of Physics
University of New South Wales
• 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)
Australia Telescope Compact Array
ATCA site
E-W tra
ck
S-N spur
Control roomMm receivers
First light on 30th Nov. 2000
Orion SiOOrion SiO
86.243 86.243 GHzGHz
ATCA at 3 & 12 mm – Current Status
3 mm system3 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 system12 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
86.243 GHz SiO 2-1 v=1 (maser)
85-87 CH3OH (maser+thermal)
86.846 SiO 2-1 v=0 (thermal)
88.631 HCN 1-0
89.188 HCO+ 1-0
22.235 GHz H2O maser
23 to 25 NH3
What can we observe with ATCA-mm?
• Molecular lines:
• Continuum emission: dust (3 mm) and ionised gas (22 GHz)
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)
1. Pre-planetary disks around young stars
Dust in Pre-planetary Disks (Wilner et al. 2003 in press)
TW HyaT Tauri star41±4 mJy
HD 100546Herbig Be star
36±3 mJy
• 3.4 mm continuum emission dust emission from disks • 2 ATCA runs 6 baselines (2’’= 100/200 AU)
See poster by Bourke et al.
2. Massive star formation in the Galactic Plane
Methanol masers = massive YSOs ?
CO Dame et al. 2001
IRAS 100 m
IRAS
Masers
SIMBA 1.2 mm
240 M
(Hill et al. in prep; Walsh et al. 1998)
MaserUCHII
ATCA 3 mm
15 M
(Minier et al. in prep)
• Unresolved CH3OH core < 0.04 pc
• Resolved HCO+ core: R=0.06 pc =33 NH2=5.51022 cm-2
Mgas=15 M
Mvir=120 M
• Resolved HCO+ wings outflows.
• Massive protostellar core
A hot molecular core in G318.95
Posters by Tracey Hill et al., Cormac Purcell et al., Peter Barnes et al. and Vincent Minier et al.
Res.: 4 – 22’’ = 0.04 – 0.26 pc
HCO+
Hot coreCH3OH
Methanol masers in G345.01+1.79
85.5 GHz maser
86.9 GHz maser
All masers coincide in velocity and position coincide in space
(Minier et al. in 2002)
UC HII region
Masers
Probing gas/dust conditions with methanol masers
Ellingsen et al. 2003, in press
Using model by Cragg et al. (2001).
Hot dust: 200-300 K
Cold gas <50 K
Density: 106 cm-3
25 GHz methanol maser in Orion BN/KL
(Voronkov et al. in 2003)
52 - 51 E
Deuterated ammonia in NGC 6334 I(N)(Wong, Minier & Forster in 2003)
Burton et al. 2000
85.9 GHz NH2D
• EW 352 • 19 and 86 GHz• Continuum + NH2D
3. Massive star formation in the LMC
HCO+ core in N113
For a virialized cloud, ignoring optical depth effects,
M 200(Rpc)(vkm/s)2 5000 M.
For constant density, nH ~ 5 x 104 cm-3.
FWHM 1.5 pc
R ~ 1 pc.
v ~ 5 km s-1.
( Wong et al. in 2001-2003)
Previous Parkes
detections (Scalise & Braz 1982; Whiteoak
et al. 1983; Whiteoak &
Gardner 1986)
New ATCA
detections
New water maser sites in the LMC
(Beasley, Claussen, Marvel & Staveley-Smith 2002)
Conclusions 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)
NEXT PROPOSAL DEADLINES :
Oct. 15th, Feb. 15th, June 15th
(might change to 6 month-observing terms)
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.ht
ml
Phase stability Clear Night, 8pm local time
45m75m 120m
rms: 22º 34º 19º
b:
4 hours later (midnight)
45m75m 120m
rms: 22º 34º 19º
b:
rms: 16º 24º 13º