1. 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. 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 L bol T bol Mass HMPOs (kpc) (Jy in 20”) (10 4 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 84 280 Mueller et al. (2002)

3. 3 W33A SMA 875  m 2” = 8000 AU MM1 MM2 CH 3 CH 2 CN H 2 CS CH 3 OCH 3 H 2 CS CS 33 SO HCOOCH 3 SO 2 H 2 CS CH 2 CO CH 3 OCH 3 HCOOCH 3 34 SO 2 HCOOCH 3 CH 3 CH 2 CN CH 3 OH SCUBA 850  m Shirley et al. (2005) MM2 also detected at 106 and 230 GHz by Van der Tak (2000)

4. 4 W33A submm and Infrared 2MASS 2.17  m X H 2 O masers SMA 875  m MM1 MM2

5. 5 Integrated Intensity Complex Kinematics of W33A 1 st 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 1 st Moment Methanol dv=3.3 km/s SMA CS(7-6) Self-absorption? JCMT CS(5-4)

6. 6 G12.89+0.49 (IRAS 18089-1732) SMA 875  m 1” = 3590 AU SCUBA 850  m Shirley et al. (2005) CH 3 CH 2 CN HCOOCH 3 H 2 CS SO 2 HCOOCH 3 34 SO 2 HCOOCH 3 CH 3 OH 29 SiO CH 3 CH 2 CN H 2 CS 33 SO CH 2 CO HCOOCH 3 CH 3 OCH 3 H 2 CS HCOOCH 3 CH 3 OCH 3

7. 7 G12.89-0.49 Kinematics CH 3 OCH 3 CHOOCH 3 H 2 CS CH 3 OH 875  m CH 3 OH integrated intensity CH 3 OH 1 st moment maps  v=4 km/s

8. 8 G12.89-0.49 Rotation? CH 3 OH 0-2+2+4-4-6 dv (km/s) +6 P-V diagram after 50 o rotation Disk Rotation? v ~ ±4.5 km/s r =1” = 0.017pc = 3,400 AU M ~ 75 M  /sin 2 ( i )  v=9 km/s (also see Beuther et al. 2004, 2005) SO 2

9. 9 Archival VLA Ammonia Data  v=6.0 km/s NH 3 (1,1) moment 0 NH 3 (1,1) moment 1 NH 3 (1,1) sat/main ~ 30% NH 3 (2,2) sat/main ~ 7%

10. 10 Previous SMA Observations of G12.89-0.49 SiO (5-4) SO 2  v=6.0 km/s NH 3 (1,1) moment 1 Beuther et al. (2004) Also Beuther et al. (2005)

11. 11 CepA-East & H 2 CS HCOOCH 3 CH 3 CH 2 CN H 2 CS CH 3 OCH 3 CS 33 SO HCOOCH 3 CH 3 OH H 2 CS CH 2 CO CH 3 OCH 3 HCOOCH 3 34 SO 2 29 SiO HCOOCH 3 SO 2 HCOOCH 3 CH 3 CH 2 CN 875  m 1” = 725 AU

12. 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. 13 Disk Rotation? - 2 - 4 - 6 - 8 -10 -12 km/s 1 st Moment CS(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  /sin 2 ( i ) P-V with P.A.-45 o systemic dv=5.0 km/s SO 2

14. 14 Extreme Velocity Complexity CS (7—6) Blue Red

15. 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 H 2 S, instead OCS Shock chemistry independent of age (Rodgers & Charnley 2003; van der Tak et al. 2003; Wakelem astro-ph0404246)

16. 16 Hot Core Forest - USB CH 3 CH 2 CN H 2 CS CH 3 OCH 3 H 2 CS CS 33 SO HCOOCH 3 CH 3 OH SO 2 H 2 CS CH 2 CO CH 3 OCH 3 HCOOCH 3 34 SO 2 W33A G12.89+0.5 HCOOCH 3 CH 3 CH 2 CN & H 2 CS HCOOCH 3 CH 3 CH 2 CN H 2 CS CH 3 OCH 3 CS 33 SO HCOOCH 3 CH 3 OH H 2 CS CH 2 CO CH 3 OCH 3 34 SO 2 29 SiO HCOOCH 3 SO 2 CepA- East HCOOCH 3 CH 3 CH 2 CN

17. 17 Summary For 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