1. Massive Star Formation: The Role of Disks Cassandra Fallscheer In collaboration with: Henrik Beuther, Eric Keto, Jürgen Sauter, TK Sridharan, Sebastian Wolf, Qizhou Zhang Great Barriers in Massive Star Formation September 16, 2010

2. Three sources in an evolutionary sequence Infrared Observations Infrared Observations C 18 O line width C 18 O line width Decrease in size of possible disk observations Decrease in size of possible disk observations Amplitude (Jy/beam) IRDC 18223-3 IRAS 18151-1208IRAS 18507+0121

3. Three Case Studies IRDC 18223-3 IRDC 18223-3 IRAS 18151-1208 IRAS 18151-1208 IRAS 18507+0121 IRAS 18507+0121 AGEAGE

4. IRDC 18223-3: Infrared Dark Cloud Distance~3.7 kpc Distance~3.7 kpc Beuther, Sridharan & Saito 2005 3-color Spitzer image with 3mm cont. contours 1.2 mm single dish contours, 8 micron MSX image 1 pc

5. IRDC 18223-3: Infrared Dark Cloud Distance~3.7 kpc Distance~3.7 kpc Beuther, Sridharan & Saito 2005 3-color Spitzer image with 3mm cont. contours 1.2 mm single dish contours, 8 micron MSX image 1 pc Rolf Kuiper’s talk tomorrow Fallscheer et al. 2009, A&A, 504, 127 outflow CH 3 OH Velocity Moment Map

6. Infall model Infall model Density distribution Velocity distribution Input quantities: 50 M sun 1.5 km/s observed at 14000 AU Model collapse of an initially rotating structure Model includes gravity and conserves angular momentum 10 4 AU

7. Three Case Studies IRDC 18223-3 IRDC 18223-3 IRAS 18151-1208 IRAS 18151-1208 IRAS 18507+0121 IRAS 18507+0121 AGEAGE

8. The high mass protostellar object IRAS 18151-1208 3.0 kpc away 3.0 kpc away Davis et al. 2004, A&A, 425, 981 3000 AU

9. Modeling with MC3D Low Mass: Butterfly Star High mass: IRAS 18151-1208 α, radial density parameter 2.42.4 β, disk flaring parameter 1.31.3 M dust 0.0007 M  2.2 M  R out, radius where density=0 300 AU 5000 AU R *, T *, L * 2 R , 4000 K, 0.92 L  6.4 R , 25400 K, 16000 L  Observations +/- 1σ Model ____ ……… - - Fallscheer et al. 2010, submitted

10. Predictions for the Future Predictions for ALMA, JWST, E-ELT Predictions for ALMA, JWST, E-ELT Mid-infrared to millimeter wavelengths Mid-infrared to millimeter wavelengths

11. Three Case Studies IRDC 18223-3 IRDC 18223-3 IRAS 18151-1208 IRAS 18151-1208 IRAS 18507+0121 IRAS 18507+0121 AGEAGE

12. Hot Molecular Core: IRAS 18507+0121 L bol ~32,000 L sun (O9.5) L bol ~32,000 L sun (O9.5) D~3.9 kpc D~3.9 kpc Moment maps do not reveal evidence for rotation Moment maps do not reveal evidence for rotation

13. Points to remember Three sources in an evolutionary sequence may be used to deduce a scenario for disk evolution Three sources in an evolutionary sequence may be used to deduce a scenario for disk evolution Elongated disk-like features decrease with evolutionary stage Elongated disk-like features decrease with evolutionary stage 20,000 AU velocity structure can be reproduced with a collapsing rotating model…disk possibly in the center 20,000 AU velocity structure can be reproduced with a collapsing rotating model…disk possibly in the center Elongation in the dust continuum modelled with a scaled up version of a low mass disk Elongation in the dust continuum modelled with a scaled up version of a low mass disk

14. How the parameters affect the SED H 0 =5 H 0 =10 H 0 =15 θ =60° θ =90° M=2.2 M=1.2 Scale height at 100AUInclination Angle Central starDust mass of disk

15. The importance of short spacings Comparison with and without short spacings Comparison with and without short spacings +=

16. Where new files come from SED & Radial Brightness profile: run 68 SED & Radial Brightness profile: run 68 SED H_0: seds 61, 59B, 53 SED H_0: seds 61, 59B, 53 SED theta: 67A,67B SED theta: 67A,67B SED mass: 68,67A SED mass: 68,67A Img68.jpg Img68.jpg JWST/E-ELT Figure from Henrik, overlay_cassie.eps JWST/E-ELT Figure from Henrik, overlay_cassie.eps