SMA Observations of High Mass Protostellar Objects
(HMPOs)
Submm Astronomy in Era of SMA June 15, 2005
Crystal Brogan (U. of Hawaii)
Y. Shirley (NRAO), A. Sarma (DePaul), C. Chandler (NRAO)
Goals• Multiplicity of individual protostars
• Nature of HMPO jets and disks
• Evolutionary sequence
• Density and temperature profiles
2
The SMA Data
Observed April - Sept. 2004 (one track each)
USB centered on CS(7-6) at 342.9 GHz (875 m)
Resolution ~2”
Continuum rms noise ~ 15 mJy/beam
Only line free channels used
Line rms noise ~ 300 mJy/beam
Single Dish Dust Properties
d 850 m Lbol Tbol Mass
HMPOs (kpc) (Jy in 20”) (104 L ) (K) (M )
W33A 4.0 45 10 65 320
G12.89+0.49 3.5 17 3.9 56 120
CepA-East 0.7 86 2.2 84 280Mueller et al. (2002)
3
W33A
SMA 875 m
2” = 8000 AU
MM1MM2
CH
3C
H2C
N
H2C
S
H2C
S
CH
3OC
H3
H2C
S
CS
33S
O
HC
OO
CH
3
SO
2 H2C
S
CH
2C
O
CH
3O
CH
3
HC
OO
CH
3
HC
OO
CH
3
34S
O2
HC
OO
CH
3
HC
OO
CH
3
CH
3C
H2C
N
CH
3O
H
SCUBA 850 m
Shirley et al. (2005)
MM2 also detected at 106 and 230 GHz by Van der Tak (2000)
5
Integrated Intensity
Complex Kinematics of W33A1st Moment
CS(7-6)
P.A. of 0.5” linear OH maser feature (Argon, Reid, & Menten 2000)
Other molecules
• Also show small N/S velocity gradient
• All peak on submm continuum
• None show extended emission
1st Moment
Methanol
dv=3.3 km
/s
SMA CS(7-6) Self-absorption?
JCMT CS(5-4)
6
G12.89+0.49 (IRAS 18089-1732)SMA 875 m
1” = 3590 AU
SCUBA 850 m
Shirley et al. (2005)
CH
3C
H2C
N
HC
OO
CH
3
H2C
S
SO
2
SO
2HC
OO
CH
3
HC
OO
CH
3
34S
O2
HC
OO
CH
3
CH
3OH
29S
iO
CH
3CH
2CN H2C
S
H2C
S
33S
O
CH
2C
O
HC
OO
CH
3
CH
3O
CH
3
H2C
S
HC
OO
CH
3
CH
3O
CH
3
7
G12.89-0.49 Kinematics
CH3OCH3
CHOOCH3H2CS
CH3OH875 m
CH3OH integrated intensity
CH3OH
1st moment maps
v=4 km/s
8
G12.89-0.49 Rotation?CH3OH
0 -2+2+4 -4 -6dv (km/s)
+6
P-V diagram after 50o rotation
Disk Rotation?
v ~ ±4.5 km/s
r =1” = 0.017pc = 3,400 AU
M ~ 75 M /sin2(i)
v=9 km/s
(also see Beuther et al. 2004, 2005)
SO2
9
Archival VLA Ammonia Data
v=
6.0 km/s
NH3 (1,1) moment 0
NH3 (1,1) moment 1
NH3 (1,1) sat/main ~ 30%
NH3 (2,2) sat/main ~ 7%
10
Previous SMA Observations of G12.89-0.49
SiO (5-4)
SO2
v=
6.0 km/s
NH3 (1,1) moment 1
Beuther et al. (2004)
Also Beuther et al. (2005)
11
CepA-East
& H
2C
S
HC
OO
CH
3
CH
3CH
2CN
H2C
S
H2C
S
CH
3O
CH
3CS
33S
O
HC
OO
CH
3
CH
3OH
H2C
S
CH
2C
O
CH
3O
CH
3
HC
OO
CH
3
34S
O2 29S
iO
HC
OO
CH
3
HC
OO
CH
3
SO
2
SO
2
HC
OO
CH
3
CH
3C
H2C
N
875 m
1” = 725 AU
12
CepA-East: Submm vs. cm Sources
Garay et al. (1996)HW9
HW4
HW2
HW3d
HW3b
HW8
HW3c
HW3a
Thermal Jet
Archival VLA 3.6cm image with 875 m contours
Also see posters by:
A. Sarma & S. Curiel
13
Disk Rotation?- 2
- 4
- 6
- 8
-10
-12
km/s
1st MomentCS(7-6)
P.A. of linear H2O maser feature (Torrelles et al. 1998)
P.A. of SiO disk (Gomez et al. 1999)
1” sizescale features
P.A. of thermal jet (Rodriguiz et al. 1994)
v ~ ±4 km/s r =2” = 0.007 pc, 1450 AU M ~ 15 M /sin2(i)
P-V with P.A.-45o
systemic
dv=
5.0 km/s
SO2
15
Chemical Clocks
Charnley et al. 1995
Chemical differentiation driven by evaporation of dust ice mantles
Temporal changes due to temperature and reaction rates
CHO, CN, and Sulfur bearing molecules among most promising
Recent observational tests suggest Sulfur not as promising as first thought
Ice phase carrier probably not H2S, instead OCS
Shock chemistry independent of age
(Rodgers & Charnley 2003; van der Tak et al. 2003; Wakelem astro-ph0404246)
16
Hot Core Forest - USB
CH
3C
H2C
N
H2C
S
H2C
S
CH
3OC
H3
H2C
S
CS
33S
O
HC
OO
CH
3CH
3OH
SO
2 H2C
S
CH
2C
O
CH
3OC
H3
HC
OO
CH
3
HC
OO
CH
3
34S
O2
W33A
G12.89+0.5H
CO
OC
H3
HC
OO
CH
3 HC
OO
CH
3
CH
3C
H2C
N
& H
2CS
H
CO
OC
H3
CH
3CH
2CN
H2C
S
H2C
S
CH
3OC
H3C
S
33S
O
HC
OO
CH
3
CH
3O
H
H2C
S
CH
2CO
CH
3O
CH
3
34S
O2 29S
iO
HC
OO
CH
3
SO
2
SO
2
CepA-East
HC
OO
CH
3
HC
OO
CH
3
HC
OO
CH
3
CH
3CH
2CN
17
SummaryFor the first time the SMA allows submm study of HMPOs in exquisite detail
Multiplicity within HMPOs
* Both W33A (4 kpc) and CepA-E (0.7 kpc) composed multiple components
* G12.89-0.49 (3.6 kpc) strongest component compact
Role and characteristics of HMPO jets and disks
* Complex velocity gradients -> disks
* Self-absorption complicates interpretation
Evolutionary sequence
* Some evidence for evolution
Density and temperature profiles
* Rotation diagrams support temperature profile models for W33A -> see Wootten et al. poster