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331 Hours, 1 PhD, 1 Great (Old!) Friend

331 Hours, 1 PhD, 1 Great (Old!) Friend. >The Impact of ( “ Less-than-Super ” ) Shells on Star-Forming Molecular Clouds. >Alyssa A. Goodman >Harvard-Smithsonian Center for Astrophysics >Carl ’ s Birthday Party >Arecibo, September 2004. >. Super & “Less-than-Super” Shells.

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331 Hours, 1 PhD, 1 Great (Old!) Friend

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  1. 331 Hours, 1 PhD, 1 Great (Old!) Friend

  2. >The Impact of (“Less-than-Super”) Shells on Star-Forming Molecular Clouds >Alyssa A. Goodman >Harvard-Smithsonian Center for Astrophysics >Carl’s Birthday Party >Arecibo, September 2004 >

  3. Super & “Less-than-Super” Shells H- emission,WHAM/SHASSA Surveys (see Finkbeiner 2003)

  4. H- emission,WHAM/SHASSA Surveys (see Finkbeiner 2003)

  5. “Less-than-Super” Shells Super Shells (>>10 pc diameter) produced by SN(e), GRBs Drive ISM turbulence on large scales Trigger molecular cloud formation(and subsequent star formation)? “Less-than-Super” Shells (<10 pc diameter) from stellar winds/HII Regions Trigger star formation in extant molecular clouds? Help Marijke et al. create the added structures?

  6. Barnard’s Ophiuchus

  7. 2 pc COMPLETE(Re)Discovery of a Heated Smoke Ring in Ophiuchus D. Li, A. Goodman, J. Li & S. Schnee 2004

  8. The COordinated Molecular Probe Line Extinction Thermal Emission Survey COMPLETE Alyssa A. Goodman, Principal Investigator (CfA) João Alves (ESO, Germany) Héctor Arce (Caltech) Paola Caselli (Arcetri, Italy) James DiFrancesco (HIA, Canada) Jonathan Foster (CfA, PhD Student) Mark Heyer (UMASS/FCRAO) Helen Kirk (HIA, Canada) Di Li (CfA) Doug Johnstone (HIA, Canada) Naomi Ridge (CfA) Scott Schnee (CfA, PhD student) Mario Tafalla (OAN, Spain) Tom Wilson (ESO, Germany)

  9. Dust Temperature Dust Column Density Barnard’s Ophiuchus

  10. Ha Ionized Gas in the Ophiuchus Smoke Shell SII SHASSA Data courtesy of John Gaustad

  11. T he s t a r -O p h  a n d RXJ 1 62 5 . 5- 2 3 26 R eg i o n k no w n a s “ - Oph  Cl u s te r ” h e a t e d ri n g R e- cal i b r a t e d I R AS D us t C ol um n De n si t y R e- Ca l i b r ate d I R A S D u s t T em p erat u re Smoke Signals from Ophiuchus H e a t ed D u st R i ng ??0.5 x 1051 erg SNinto 105 cm-32 pc in 200,000 yr T=38Kvexp=1.7 km s-1?? R O SA T PSP C R O SA T P o in t e d O b se r va t i o n R e a l - O p h  C l u st e r i n s i d e from Goodman, Gaensler, Lada, Wolk & Schnee 2003/4 Chandra/XMM Proposals 1 R XS J 1 6 2 55 4 . 5- 23 3 03 7 I n eac h p a n el w h e r e i t is sho n , th e w h it e r in g s ho w s a 2 p c c i r c l e , co rre spo n d i ng t o t h e size a n d sh a pe o f t h e h e a t ed r i n g ap p a re n t i n t h e I R AS T e m p er a t u r e M a p.

  12. Questions we can address: Which matters “most” inside what kind ofmolecular clouds: babys (YSOs), adults (O & B star winds), or ghosts (SNe)? What is the “expected” combination of these in a given region? (Spitzer key for this) How can we tell a wimpy SNR from a stellar wind? (X-rays (& You-Hua) key) So far: Ophiuchus Shell Paper:Li, D., Goodman, A., Li, J., Ridge, N. & Schnee, S. 2004, ApJ, in prep Perseus Shell Paper:Ridge, N., Goodman, A., Li, J. & Schnee, S. 2004, ApJ, in prep IRAS Re-analysis Method:Schnee, S., Goodman, A., Li, J. & Ridge, N. 2004, ApJ, in prep

  13. COMPLETEWarm Dust Emission showsGreat Bubble in Perseus??2 x 1051 erg SNinto 104 cm-35 pc in 1 MyrT=30Kvexp=1.5 km s-1??

  14. Dust Density & Temperature in Perseus Dust Temperature (25 to 45 K) (Based on 60/100 microns) Total Dust Column (0 to 15 mag AV) (Based on 60/100 microns)

  15. Hot Source in a Warm Shell Column Density Temperature + =

  16. IRAS Ndust H 2MASS/NICER Extinction H- emission,WHAM/SHASSA Surveys (see Finkbeiner 2003)

  17. Why “COMPLETE”? Schnee et al. 2004 Ridge et al. 2004 IRAS Column Density IRAS Temperature + = NICER Extinction Map Alves, Lombardi & Foster+ 2004

  18. Why “COMPLETE”? Schnee et al. 2004 Ridge et al. 2004 IRAS Column Density IRAS Temperature + = NICER Extinction Map Alves, Lombardi & Foster+ 2004

  19. PerseusIRAS + FCRAO(~100,000 13CO Spectra)

  20. Giving Carl’s ISM Students all they Need to do His Calculations Direct Imaging (X-ray, uv, optical, near-infrared) Continuum & Line Imaging (shows hot, excited shells) Extinction mapping (true column density) Thermal Emission from Dust (mid & far-infrared, sub-mm) Reveals (and is biased by) dust temperature Spectral-Line Mapping (radio) Reveals gasmotion(+temperature & composition)

  21. “But what about the Magnetic Field?”

  22. Polarization Goodman et al. 1990

  23. Polarization

  24. For the “Real” Molecular Cloud People… please Please Ask Me Later

  25. Embracing the Confusion is The Key to Understanding conspiracies of chemical depletion, optical depth, excitation, Tdust, Tgas, “,” can be critically misleading (especially for gullible theorists)

  26. Observation(Now) Theory(Good Old Days) Shu, Adams & Lizano 1987

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