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Identifying Triggered Star Formation with Herschel and SCUBA-2 - PowerPoint PPT Presentation


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Larry Morgan (LJMU) Toby Moore (LJMU) David Eden(LJMU) James Urquhart (ATNF) Mark Thompson (University of Hertfordshire) Charles Figura (Wartburg College) Rene Plume(Calgary) Annie Zavagno(Marseille) +HiGal and JPS Teams. Identifying Triggered Star Formation with Herschel and SCUBA-2.

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Presentation Transcript
slide1

Larry Morgan (LJMU)

Toby Moore (LJMU)

David Eden(LJMU)

James Urquhart (ATNF)

Mark Thompson (University of Hertfordshire)

Charles Figura (Wartburg College)

Rene Plume(Calgary)

Annie Zavagno(Marseille)

+HiGal

and JPS Teams

Identifying Triggered Star Formation with Herschel and SCUBA-2

triggered star formation
Triggered Star-Formation
  • “A shock front can compress pre-existing dense clumps forcing them to contract and form new stars. The swept-up shell itself may become gravitationally unstable and fragment into new protostars.”
  • Kirsanova et al. (2008)
slide3

3°x 3° field at l=30

  • ∼300 Class 0 YSOs identified
  • 76 HII regions coincident with high source densities

HiGal Science Demonstration Image (Molinari et al. 2010)

N49

slide4

Zavagno et al. (2010)

  • 3 colour image of HII region in SDP field
  • 2nd generation massive stars observed on periphery of ionized region
  • Seen in 20% of ionized bubbles (Deharveng et al.,2010)

Blue - 8 µm, Green - 24 µm, Red - 20 cm, Contours - 870 µm

more direct evidence
More Direct Evidence
  • Herschel/HiGal + SCUBA2/JPS allow SED fitting of large samples for first time
  • Fits degenerate at shorter wavelengths are well constrained at Herschel/SCUBA2 wavelengths

Zavagno et al. (2010) using Robitaille’s SED tool

  • Parameterisation (Tdust/Lbol/Menv) of 1,000’s of YSOs
slide7

Case Study

  • SFO 13 - Bright-Rimmed Cloud at edge of W5 HII region
  • Host to B-star dominated cluster

Green - 4.5 µm, Blue - 8.0 µm, Red - 24 µm. White contours - 21 cm, yellow contours - 850 µm

slide8

Radio contours inform us on ionized boundary

  • Spitzer shows us the PDR/transition region
  • HiGal/JPS quantify the properties of the embedded core
  • Environmental factors (ionized layer/PDR) can now be compared to protostellar properties themselves
identifying triggering
Identifying Triggering
  • Previous small samples show potential characteristics of triggered regions
  • Mass functions in probable triggered regions show bias toward massive YSOs
  • Star forming efficiencies higher in shocked regions (Moore et al., 2007)
slide10

Molecular Observations

  • Measurements of turbulence show distinct population of triggered sources
  • Potential observational signatures of triggering though currently based on small source no’s
molecular maps
Molecular Maps
  • Maps allow for detailed comparison with models
  • Prohibitively time-consuming
conclusions
Conclusions
  • JPS and Hi-Gal projects likely to observe 1,000s of intermediate to high-mass protostars in all stages of development
  • JPS, Hi-Gal, GLIMPSE, MIPSGAL + molecular followups provide complete census of star forming cores/clumps and relationship to environment
  • Using newly established techniques a great number of star forming clumps and cores can be identified and classified
  • Estimated 10-15% of YSOs are related to triggered formation, this will result in 100s of triggered YSOs in upcoming surveys
  • Good for modelling and observation