1Center for Astrophysics and Space Astronomy CASA

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The Bolocam 1.1 mm Galactic Plane Survey
(BGPS) 104 cores in 150 Square Degrees John
Bally1, Adam Ginsburg1, Guy Stringfellow1 Jason
Glenn1, James Aguirre1, Meredith Drosback1, Paul
Harvey1, 2 Neal Evans2, Miranda Nordhaus2 Claudia
Cyganowski3, Erik Rosolowski4 Todd Bradley5,
Josh Walawneder6, Jonathan Williams6

1Center for Astrophysics and Space Astronomy
(CASA) Department of Astrophysical and
Planetary Sciences (APS) University of
Colorado, Boulder 2University of Texas,
Austin 3University of Wisconsin 4University of
British Columbia 5University of Central
Florida 6University of Hawaii
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• Bolocam Galactic Plane Survey
• (BGPS)
• Survey the Northern Milky Way in the 1.1 mm
  dust continuum
• Trace material most directly associated
  with star formation
• Rayleigh-Jeans limit, low optical
  depth, 20 mJy/beam
• Stable atmosphere gt good flux
  calibration, sensitivity
• Find catalog dense cloud cores
• Masses, sizes, mass spectra,
  correlation function,
• galactic distribution and variation of
  properties
• Association with other surveys
• Radio continuum (HII, SNR), HI, CO,
  Spitzer, near-IR
• How do cores form, evolve, disrupt?
• Finder chart for interferometers follow-up
• (CARMA, ALMA, SOFIA, etc. )

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Bolocam
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• Bolocam Galactic Plane Survey (BGPS)
• 144 (115) Element bolometer camera on CSO 10 m
  (Mauna Kea)
• 1.1 mm (235 - 280 GHz) avoids bright lines
• 0.35 mm SHARC2 follow-up of selected cores
• Heterodyne CS J 5-4 gt radial velocity, line
  width, density
• Heterodyne NH3 (GBT) gt radial velocity, line
  width, Tgas
• Part of Herschel Hi-Gal 60 to 600 ?m
  continuum
• Detailed study of W3/4/5
• Narrow-band H?, SII, H2 NOAO 4
  meter/ ARC 3.5 m
• Sub-mm CO J-3-2 JCMT HARP
  15 feed heterodyne

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Bolocam Galactic Plane survey (to Sept 07)

• On MSX survey
• 150 Square deg.
• 104 cores
• Coverage
• - 1st quadrant
• (l -10 to 54)
• Cyg-X
• IC 1396
• Perseus Arm
• l 110 / NGC 7538
• l 145 / W3/4/5
• Gem OB1

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• BGPS
• How do stars, massive stars,
• clusters form?
• Isolated collapse?
• Competitive Accretion?
• Cooperatives?
• Is star formation triggered?
• HII, winds, SN, super-bubbles?
• Spiral arm shocks?
• How do clouds cluster?
• What is the core mass function?
• How long do they last?

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Bolocam 1.1 mm
MSX 8 ?m
Bolocam 1.1 mm is best tracer of pre-stellar
cores, cluster-forming cores, and hot dust
associated with hot cores, hypercompact
compact HII regions.
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• The Bolocam 1.1 mm survey (l 29)
• 1.1 mm (top)
• 0.35 mm (bottom)
• W43 cluster forming complex

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Finding Distances (and Masses)

• For optically thin dust, the mass is extremely
  sensitive to the assumed distance
• For 15 lt l lt 56, the BU-FCRAO 13CO(1?0) Survey
  provides a way of obtaining velocities, provided
  freeze out is not too extreme, and the CO
  morphology traces the dust

• HI self-absorption (HISA) can be used to resolve
  the distance ambiguity in the inner Galaxy data
  available from the VGPS

http//www.ras.ucalgary.ca/VGPS/VGPS.html
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1.1 mm vs. 13CO
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Heterodyne spectra
NH3 13CO 1-0
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NH3 Heterodyne spectra VR on 13CO FCRAO
survey Statistics of 200 cores
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Gem OB1 (anti-center) GBT NH3, H2O Survey
Gem OB1
NH3 only NH3 H2O No detection
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W3 main
W4
W5
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Bolocam 1.1 mm 1 square degree near W3
W3 main
W3(OH)
AFGL 333
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Microjet
Jet
Fish
W5 (Spitzer 24 ?m,L. Allen et al. 2008)
KPNO 4m Mosaic H?
Jet
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W5 East
JCMT HARP CO J3-2
Microjet
Jet
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Microjet
2
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Microjet
2
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Microjet
SII
NII
NII
H?
625 km/s
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Fish North Bow shocks
2
North
South
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Fish North Bow shocks
2
North
South
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H?
Fish North Bow shocks
SII
NII
NII
Fish
South
Vlsr 50 km/s
Vlsr 80 km/s
North
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Galactic Center at 1.1 mm Bolocam at CSO
Sgr B2
Sgr A
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Galactic Center 1.1 mm SCUBA vs. Bolocam
SCUBA 450 ?m
BGPS 1100 ?m
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The
Galactic Center 21 cm 1.1 mm
0.85 mm 0.45 mm 0.35 mm
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• Summary
• BGPS Survey the Northern Milky Way _at_ 1.1 mm
  (dust)
• Trace material most directly associated
  with star formation
• Rayleigh-Jeans limit, low optical depth,
  20 mJy/beam
• Stable atmosphere gt good flux
  calibration, sensitivity
• Find catalog 104 cloud cores in 150 square
  deg. _at_ 1.1 mm
• NH3 is the best tracer of
• Radial velocity, Gas temperature,
  Line-width, Density
• Distance, Size, Mass,
  Dust-to-gas ratio,
• Core mass Function (CMF),
  Autocorrelation Function
• Detailed studies of Gem OB1, W3/4/5, inner
  plane, Galactic
• center underway.
• Finder chart for interferometers follow-up
• (CARMA, ALMA, SOFIA, etc. )

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