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