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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

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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

>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

Super & “Less-than-Super” Shells

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


331 hours 1 phd 1 great old friend

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


Less than super shells

“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

Barnard’s Ophiuchus


Comple te re discovery of a heated smoke ring in ophiuchus

2 pc

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

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


Complete

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)


Barnard s ophiuchus1

Dust

Temperature

Dust

Column Density

Barnard’s Ophiuchus


Ionized gas in the ophiuchus smoke shell

Ha

Ionized Gas in the Ophiuchus Smoke Shell

SII

SHASSA Data courtesy of John Gaustad


Smoke signals from ophiuchus

T

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Smoke Signals from Ophiuchus

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??0.5 x 1051 erg SNinto 105 cm-32 pc in 200,000 yr T=38Kvexp=1.7 km s-1??

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from Goodman, Gaensler, Lada, Wolk & Schnee 2003/4 Chandra/XMM Proposals

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Questions we can address

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


331 hours 1 phd 1 great old friend

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 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

Hot Source in a Warm Shell

Column Density

Temperature

+

=


331 hours 1 phd 1 great old friend

IRAS Ndust

H

2MASS/NICER Extinction

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


Why complete

Why “COMPLETE”?

Schnee et al. 2004

Ridge et al. 2004

IRAS

Column Density

IRAS

Temperature

+

=

NICER

Extinction Map

Alves, Lombardi & Foster+ 2004


Why complete1

Why “COMPLETE”?

Schnee et al. 2004

Ridge et al. 2004

IRAS

Column Density

IRAS

Temperature

+

=

NICER

Extinction Map

Alves, Lombardi & Foster+ 2004


Perseus iras fcrao 100 000 13 co spectra

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


Giving carl s ism students all they need to do his calculations

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

“But what about the Magnetic Field?”


Polarization

Polarization

Goodman et al. 1990


Polarization1

Polarization


For the real molecular cloud people please please ask me later

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


Embracing the confusion is the key to understanding

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)


Theory good old days

Observation(Now)

Theory(Good Old Days)

Shu, Adams & Lizano 1987


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