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CO Emission from Disks around Young Stars: CRIRES Observations

This study presents CRIRES observations of CO emission from 10 young star disks, investigating the presence and properties of CO emission, as well as the differences in inner disk structure and emission variability. The observations reveal the complex nature of CO emission and its potential as a probe for understanding disk properties.

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CO Emission from Disks around Young Stars: CRIRES Observations

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  1. CRIRES observations of CO emission from disks around embedded young starsGregory Herczeg (MPE)Collaborators: Ewine van DishoeckKlaus PontoppidanJoanna BrownJeanette Bast

  2. CRIRES Observations • 10 sources: • IRS 43, IRS 44, IRS 63, Elias 23, Elias 29, Elias 32, HH 100, WL 6, WL 12, CrA IRS 2 • Several observed in multiple epochs • Usually a few wavelength settings • Need to add a few more (mostly non-detections) • NGS AO not possible • Limited spatial information

  3. Goals: • Do young disks emit in CO? • What else is CO probing? • Why do some disks show no CO? • Does inner disk structure differ from CTTS disks? • Luminosity • Temperature/Excitation

  4. Red: CRIRES black: ISAAC

  5. IRS 44: resolved emission • 0.3 arcsec binary • 0.69 mag difference in M • Equal brightness in L • (Duchêne et al. 2007) • Primary is barely (or not) detected in K, never in J • Ratzka et al. 2005, Terebey et al. 2001, Allen et al. 2002 • CO and H2 emission: only detected from secondary • 13CO emission: blueshifted, offset from 12CO emission

  6. H2 S(9) Emission

  7. Variability?

  8. Seeing in Aug.: 0.33 arcsec • Seeing in Apr.: 0.56 arcsec • Blueshifted CO emission from IRS 44 also variable in EW

  9. Conclusions: CO emission from embedded objects • CO absorption can make analysis difficult • Sometimes impossible, sometimes not so bad • Better than H2, which often probes extended material • Most emission consistent with a disk origin • Double-peaked profile from Elias 23 • Winds can also play a role (IRS 44) • Two components • Narrow, colder, optically-thick • Hot, vibrationally excited broad component • TO DO: Add a few sources, temps, luminosities, optical depths

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