SMA Observations of High Mass Protostellar Objects HMPOs

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

Single Dish Dust Properties d 850 mm (kpc) (Jy in 20”) 4. 0 Tbol Mass (104 L ) (K) (M ) 45 10 65 320 G 12. 89+0. 49 3. 5 17 3. 9 56 120 Cep. A-East 86 2. 2 84 280 HMPOs W 33 A 0. 7 Lbol Mueller et al. (2002) The SMA Data v Observed April - Sept. 2004 (one track each) v USB centered on CS(7 -6) at 342. 9 GHz (875 mm) v Resolution ~2” v Continuum rms noise ~ 15 m. Jy/beam Only line free channels used v Line rms noise ~ 300 m. Jy/beam 2

W 33 A SMA 875 mm SCUBA 850 mm MM 2 MM 1 2” = 8000 AU Shirley et al. (2005) H 2 CS CH 3 OCH 3 H 2 CS HCOOCH 3 CH 2 CO H 2 CS HCOOCH 3 CH 2 CN 33 SO H 2 CS SO 2 CS CH 3 OH CH 3 OCH 3 HCOOCH 3 CH 2 CN 34 SO 2 HCOOCH 3 MM 2 also detected at 106 and 230 GHz by Van der Tak (2000) 3

W 33 A submm and Infrared SMA 875 mm MM 1 MM 2 2 MASS 2. 17 mm X H 2 O masers 4

Complex Kinematics of W 33 A 1 st Moment P. A. of 0. 5” linear OH maser feature (Argon, Reid, & Menten 2000) CS(7 -6) • Also show small N/S velocity gradient Integrated Intensity Self-absorption? 1 st Moment dv=3. 3 km/s Other molecules SMA CS(7 -6) JCMT CS(5 -4) • All peak on submm continuum • None show extended emission Methanol 5

2 HCOOCH 3 H 2 CS CH 3 OCH 3 HCOOCH 3 H 2 CS HCOOCH 3 CH 2 CO SMA 875 mm H 2 CS 1” = 3590 AU HCOOCH 3 CH 2 CN 33 SO 29 Si. O SO 2 CH 3 OH CH 3 OCH 3 HCOOCH 3 SO 2 HCOOCH 3 CH 2 CN 34 SO G 12. 89+0. 49 (IRAS 18089 -1732) SCUBA 850 mm Shirley et al. (2005) 6

G 12. 89 -0. 49 Kinematics 875 mm CH 3 OH CH 3 OCH 3 Dv=4 km/s H 2 CS CHOOCH 3 OH 1 st moment maps CH 3 OH integrated intensity 7

G 12. 89 -0. 49 Rotation? CH 3 OH P-V diagram after 50 o rotation Dv=9 km/s Disk Rotation? SO 2 +6 +4 +2 0 -2 -4 -6 dv (km/s) v ~ ± 4. 5 km/s r =1” = 0. 017 pc = 3, 400 AU M ~ 75 M /sin 2(i) (also see Beuther et al. 2004, 2005) 8

Archival VLA Ammonia Data NH 3 (1, 1) moment 1 Dv=6. 0 km/s NH 3 (1, 1) moment 0 NH 3 (1, 1) sat/main ~ 30% NH 3 (2, 2) sat/main ~ 7% 9

Previous SMA Observations of G 12. 89 -0. 49 Si. O (5 -4) Dv=6. 0 km/s NH 3 (1, 1) moment 1 SO 2 Beuther et al. (2004) Also Beuther et al. (2005) 10

2 HCOOCH 3 OCH 3 HCOOCH 3 & H 2 CS CH 2 CO H 2 CS HCOOCH 3 CH 2 CN 33 SO 29 Si. O H 2 CS CS CH 3 OH SO 2 CH 3 OCH 3 HCOOCH 3 SO 2 HCOOCH 3 CH 2 CN 34 SO Cep. A-East 875 mm 1” = 725 AU 11

Cep. A-East: Submm vs. cm Sources HW 4 Thermal Jet HW 2 HW 9 Garay et al. (1996) HW 8 HW 3 a HW 3 d HW 3 c Also see posters by: A. Sarma & S. Curiel HW 3 b Archival VLA 3. 6 cm image with 875 mm contours 12

Disk Rotation? SO 2 dv=5. 0 km/s -2 1 st Moment CS(7 -6) -4 km/s -6 -8 -10 P-V with P. A. -45 o -12 1” sizescale features P. A. of linear H 2 O maser feature (Torrelles et al. 1998) systemic P. A. of Si. O disk (Gomez et al. 1999) P. A. of thermal jet (Rodriguiz et al. 1994) v ~ ± 4 km/s r =2” = 0. 007 pc, 1450 AU ~ 15 M /sin 2(i) M 13

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

Chemical Clocks Ø Chemical differentiation driven by evaporation of dust ice mantles Ø Temporal changes due to temperature and reaction rates Ø CHO, CN, and Sulfur bearing molecules among most promising ØRecent 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 Charnley et al. 1995 (Rodgers & Charnley 2003; van der Tak et al. 2003; Wakelem astro-ph 0404246) 15

2 HCOOCH 3 OCH 3 HCOOCH 3 H 2 CS HCOOCH 3 CH 2 CO H 2 CS CH 3 OCH 3 HCOOCH 3 & H 2 CS CH 2 CO H 2 CS HCOOCH 3 CH 3 CH 2 CN 29 Si. O H 2 CS CS CH 3 OH SO 2 CH 3 OCH 3 HCOOCH 3 SO 2 HCOOCH 3 CH 2 CN 34 SO 33 SO CS G 12. 89+0. 5 33 SO H 2 CS SO 2 CH 3 OH CH 3 OCH 3 HCOOCH 3 CH 2 CN HCOOCH 3 W 33 A 2 Cep. AEast 34 SO Hot Core Forest - USB 16

Summary For the first time the SMA allows submm study of HMPOs in exquisite detail Ø Multiplicity within HMPOs * Both W 33 A (4 kpc) and Cep. A-E (0. 7 kpc) composed multiple components * G 12. 89 -0. 49 (3. 6 kpc) strongest component compact Ø Role and characteristics of HMPO jets and disks * Complex velocity gradients -> disks * Self-absorption complicates interpretation Ø Evolutionary sequence * Some evidence for evolution Ø Density and temperature profiles * Rotation diagrams support temperature profile models for W 33 A -> see Wootten et al. poster 17