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The Star formation region near kes78

The Star formation region near kes78. Ping Zhou 09/08/09. Green’s SNR catalogue Who is KES78 3 HII regions SFRs are associated with SNRs?. outline. G32.8−0.1     Kes 78 Right Ascension: 18 51 25 Declination: −00 08 Size (/arcmin): 17 Type: S? Flux density at 1 GHz (/Jy): 11?

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The Star formation region near kes78

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  1. The Star formation region near kes78 Ping Zhou 09/08/09

  2. Green’s SNR catalogue Who is KES78 3 HII regions SFRs are associated with SNRs? outline

  3. G32.8−0.1     Kes 78 Right Ascension: 18 51 25 Declination: −00 08 Size (/arcmin): 17 Type: S? Flux density at 1 GHz (/Jy): 11? Spectral Index: 0.2? Notes:Part has been called G33.1−0.1. Radio: Elongated shell? Dave Green's Galactic sNRcatalogue

  4. Who is kes 78?

  5. G33.1-0.1----Original kes78

  6. R1: • maser,IR,radio • R2: • radio,IR • R3： • Maser, IR R2 3HIIregions R1 R3

  7. Optical depth and temperature(13CO,18CO) • τ1−0 = 2.9 ,τ2−1 = 3.3 for the outflow region • τ1−0 = 0.9,τ2−1 = 1.8 for the non-outflow region • τ1−0 = 1.4,τ2−1 = 2.7 for the maser region • τ1−0 = 1.4, τ2−1 = 2.2 for the non-maser region • Uncertainties of τ1−0 , τ2−1 are 16%,34% The association between masers and outflows in massive SFRs(Codella et al. 2004)

  8. Do these four classes outline an evolutionary sequence? (Codella et al. 2004)

  9. H 109α at g33.1-0.08 (Caswell and Clark. 1975) Vlsr=100km/s ,Kinematic distance: 7.1kpc(HI absorption)(Thomas A. Kuchar et al. 1994) H2O masersVlsr=75km/s (Codella et al. 2000) CH3OH and CO Outflow (Codella et al. 2004) Information about g33.1-0.1

  10. G33.1-0.1(R1) Outflows And their Directions

  11. Vlsr=100km/s ?Kinematic distance: 7.1kpc(HI absorption)(Thomas A. Kuchar et al. 1994)

  12. G33.2+0.0(R2) quadrpolar outflows?

  13. R1: • maser,IR,radio • R2: • radio,IR • R3： • Maser, IR R2 3HIIregions R1 R3

  14. Associated with g32.8-0.1(SNR)? IRS18488+0000(R3)

  15. Radio bright region • Direction of outflows R3

  16. Is g33.1-0.1(R1) near the shock front of a SNR?(shape, direction of outflow) • If it is, whether the SNR accelerated the formation of g33.1-0.1 • Are there quadrupolar outflows of R2? • g32.8-0.1(SNR) are interacting with the outflow lobe of IRS18488+0000(R3)?

  17. Thanks

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