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)

4

W33A submm and Infrared

2MASS 2.17 m

X H2O masers

SMA 875 m

MM1MM2

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

14

Extreme Velocity Complexity

CS (7—6)

Blue

Red

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