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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


>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

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


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


“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?


Barnard’s Ophiuchus


2 pc

COMPLETE(Re)Discovery of a Heated Smoke Ring in Ophiuchus

D. Li, A. Goodman, J. Li & S. Schnee 2004


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)


Dust

Temperature

Dust

Column Density

Barnard’s Ophiuchus


Ha

Ionized Gas in the Ophiuchus Smoke Shell

SII

SHASSA Data courtesy of John Gaustad


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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


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??


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)


Hot Source in a Warm Shell

Column Density

Temperature

+

=


IRAS Ndust

H

2MASS/NICER Extinction

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


Why “COMPLETE”?

Schnee et al. 2004

Ridge et al. 2004

IRAS

Column Density

IRAS

Temperature

+

=

NICER

Extinction Map

Alves, Lombardi & Foster+ 2004


Why “COMPLETE”?

Schnee et al. 2004

Ridge et al. 2004

IRAS

Column Density

IRAS

Temperature

+

=

NICER

Extinction Map

Alves, Lombardi & Foster+ 2004


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


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)


“But what about the Magnetic Field?”


Polarization

Goodman et al. 1990


Polarization


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


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)


Observation(Now)

Theory(Good Old Days)

Shu, Adams & Lizano 1987


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