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The dust-to-dust gas ratio in the Small Magellanic Cloud Tail

  • Gordon, K. D.
  • Bot, C.
  • Muller, E.
  • Misselt, K. A.
  • Bolatto, A.
  • Bernard, J.-P.
  • Reach, W.
  • Engelbracht, C. W.
  • Babler, B.
  • Bracker, S.
  • Block, M.
  • Clayton, G. C.
  • Hora, J.
  • Indebetouw, R.
  • Israel, F. P.
  • Li, A.
  • Madden, S.
  • Meade, M.
  • Meixner, M.
  • Sewilo, M.
  • And 4 more
Publication Date
Jan 01, 2009
Caltech Authors
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The Tail region of the Small Magellanic Cloud (SMC) was imaged using the MIPS instrument on the Spitzer Space Telescope as part of the SAGE-SMC Spitzer Legacy. Diffuse infrared emission from dust was detected in all the MIPS bands. The Tail gas-to-dust ratio was measured to be 1200 ± 350 using the MIPS observations combined with existing IRAS and H I observations. This gas-to-dust ratio is higher than the expected 500-800 from the known Tail metallicity indicating possible destruction of dust grains. Two cluster regions in the Tail were resolved into multiple sources in the MIPS observations and local gas-to-dust ratios were measured to be ~440 and ~250 suggest dust formation and/or significant amounts of ionized gas in these regions. These results support the interpretation that the SMC Tail is a tidal Tail recently stripped from the SMC that includes gas, dust, and young stars.

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