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SMA Observations of High Mass Protostellar Objects (HMPOs)

Goals. Multiplicity of individual protostars Nature of HMPO jets and disks Evolutionary sequence Density and temperature profiles. SMA Observations of High Mass Protostellar Objects (HMPOs). Crystal Brogan (U. of Hawaii) Y. Shirley (NRAO), A. Sarma (DePaul), C. Chandler (NRAO).

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SMA Observations of High Mass Protostellar Objects (HMPOs)

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  1. Goals • Multiplicity of individual protostars • Nature of HMPO jets and disks • Evolutionary sequence • Density and temperature profiles SMA Observations of High Mass Protostellar Objects (HMPOs) Crystal Brogan (U. of Hawaii) Y. Shirley (NRAO), A. Sarma (DePaul), C. Chandler (NRAO) Submm Astronomy in Era of SMA June 15, 2005

  2. d 850 mm 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 84 280 Mueller et al. (2002) The SMA Data • Observed April - Sept. 2004 (one track each) • USB centered on CS(7-6) at 342.9 GHz (875 mm) • Resolution ~2” • Continuum rms noise ~ 15 mJy/beam Only line free channels used • Line rms noise ~ 300 mJy/beam Single Dish Dust Properties

  3. CS CH3OH CH3OCH3 H2CS HCOOCH3 H2CS CH3CH2CN CH3OCH3 CH3CH2CN HCOOCH3 H2CS HCOOCH3 H2CS HCOOCH3 HCOOCH3 33SO CH2CO SO2 34SO2 W33A SMA 875 mm SCUBA 850 mm MM2 MM1 2” = 8000 AU Shirley et al. (2005) MM2 also detected at 106 and 230 GHz by Van der Tak (2000)

  4. W33A submm and Infrared SMA 875 mm MM2 MM1 2MASS 2.17 mm X H2O masers

  5. P.A. of 0.5” linear OH maser feature (Argon, Reid, & Menten 2000) SMA CS(7-6) 1st Moment Self-absorption? • Other molecules • Also show small N/S velocity gradient • All peak on submm continuum • None show extended emission JCMT CS(5-4) dv=3.3 km/s Methanol Complex Kinematics of W33A 1st Moment CS(7-6) Integrated Intensity

  6. H2CS CH3OH H2CS HCOOCH3 HCOOCH3 CH3OCH3 CH3CH2CN CH3OCH3 H2CS HCOOCH3 HCOOCH3 H2CS HCOOCH3 CH3CH2CN HCOOCH3 33SO CH2CO SO2 29SiO 34SO2 SO2 G12.89+0.49 (IRAS 18089-1732) SMA 875 mm SCUBA 850 mm 1” = 3590 AU Shirley et al. (2005)

  7. G12.89-0.49 Kinematics 875 mm CH3OH CH3OCH3 Dv=4 km/s H2CS CHOOCH3 CH3OH 1st moment maps CH3OH integrated intensity

  8. SO2 G12.89-0.49 Rotation? CH3OH P-V diagram after 50o rotation Dv=9 km/s +6 +4 +2 0 -2 -4 -6 Disk Rotation? v ~ ±4.5 km/s r =1” = 0.017pc = 3,400 AU M ~ 75 M /sin2(i) dv (km/s) (also see Beuther et al. 2004, 2005)

  9. NH3 (1,1) moment 0 NH3 (1,1) moment 1 Dv=6.0 km/s Archival VLA Ammonia Data NH3 (1,1)sat/main ~ 30% NH3 (2,2)sat/main ~ 7%

  10. Dv=6.0 km/s SO2 Previous SMA Observations of G12.89-0.49 SiO (5-4) NH3 (1,1) moment 1 Beuther et al. (2004) Also Beuther et al. (2005)

  11. SO2 CS CH3OH HCOOCH3 CH3CH2CN CH3OCH3 CH3CH2CN HCOOCH3 & H2CS HCOOCH3 HCOOCH3 HCOOCH3 CH3OCH3 29SiO H2CS H2CS HCOOCH3 33SO CH2CO H2CS SO2 34SO2 CepA-East 875 mm 1” = 725 AU

  12. CepA-East: Submm vs. cm Sources HW4 Thermal Jet HW2 HW9 Garay et al. (1996) HW8 HW3a Also see posters by: A. Sarma & S. Curiel HW3d HW3c HW3b Archival VLA 3.6cm image with 875 mm contours

  13. SO2 dv=5.0 km/s P-V with P.A.-45o systemic 1” sizescale features P.A. of linear H2O maser feature (Torrelles et al. 1998) P.A. of SiO disk (Gomez et al. 1999) v ~ ±4 km/s r =2” = 0.007 pc, 1450 AU M ~ 15 M /sin2(i) P.A. of thermal jet (Rodriguiz et al. 1994) Disk Rotation? - 2 1st Moment CS(7-6) - 4 - 6 km/s - 8 -10 -12

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

  15. Charnley et al. 1995 Chemical Clocks • 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. SO2 Hot Core Forest - USB CS CepA-East CH3OH HCOOCH3 HCOOCH3 CH3OCH3 CH3CH2CN HCOOCH3 & H2CS HCOOCH3 HCOOCH3 CH3OCH3 CH3CH2CN H2CS 29SiO H2CS HCOOCH3 33SO CH2CO H2CS SO2 34SO2 G12.89+0.5 CS CH3OH W33A HCOOCH3 CH3OCH3 CH3OCH3 H2CS HCOOCH3 H2CS CH3CH2CN CH3CH2CN HCOOCH3 H2CS HCOOCH3 H2CS HCOOCH3 HCOOCH3 33SO CH2CO SO2 34SO2

  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

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