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Resolving Debris Disks with (Sub)Millimeter Interferometry

Resolving Debris Disks with (Sub)Millimeter Interferometry. David J. Wilner (Harvard-Smithsonian CfA). Why (Sub)Millimeter? Interferometry & Limitations A Few Examples Future Prospects. Why Millimeter and Submillimeter?. (Sub)millimeter: thermal emission from dust particles

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Resolving Debris Disks with (Sub)Millimeter Interferometry

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  1. Resolving Debris Disks with (Sub)Millimeter Interferometry David J. Wilner (Harvard-Smithsonian CfA) • Why (Sub)Millimeter? • Interferometry & Limitations • A Few Examples • Future Prospects STScI Workshop: Nearby Resolved Debris Disks

  2. Why Millimeter and Submillimeter? • (Sub)millimeter: thermal emission from dust particles • sample low temperature dust • favorable contrast with stellar photosphere • sample large dust G2V star HD107146 excess >25 mm T=51 K T=100 K Williams et al. 2004 STScI Workshop: Nearby Resolved Debris Disks

  3. Observational Probes of Structure scattered light emitted light optical/near-ir mid-ir far-ir/submm • spatial resolution • contrast with star  temperature dependence HST Ardila et al. 2005 JCMT Williams et al. 2004 Williams et al. 2004 STScI Workshop: Nearby Resolved Debris Disks

  4. OVRO BIMA IRAM PdBI SMA (Sub)Millimeter Interferometry • way to achieve high angular resolution • obtain q ~1 arcsec (l/1.3mm)(D/300 m) • excellent control of systematics for weak continuum STScI Workshop: Nearby Resolved Debris Disks

  5. Limitations: Sensitivity • nearby debris disks: 10’s of mJy (850 mm) • interferometer sensitivity: rms ~1 mJy in ~8 hours • modest collecting area (SMA ~ JCMT, PdBI ~ IRAM 30m) • modest bandwidths (~2 GHz) vs. bolometers (~50 GHz) • room for improvement in detectors (not quantum limited) • problematic atmosphere: transparency & seeing STScI Workshop: Nearby Resolved Debris Disks

  6. Limitations: Imaging Capability • (Sub)millimeter fields of view are small (<1 arcmin) • measure Fourier components of source brightness • this is not direct imaging... • sampling is limited (“uv coverage”) with small N (<9) arrays • largest structures not sampled STScI Workshop: Nearby Resolved Debris Disks

  7. Large dust  Small dust • structure depends on b=Frad/Fgrav • smallest particles blown out quickly • small particles drop of out resonances • large particles stay in resonances • Vega (Su et al. 2005) • mid-ir & far-ir  smooth; submm  clumpy Moro-Martin & Malhotra 2003 small large Holland et al. 1998 STScI Workshop: Nearby Resolved Debris Disks

  8. Vega: 1.3 mm Interferometry • angular resolution: 2 to 5 arcsec • stellar photosphere provides calibration check • dust blobs are robust, spatially extended • motivates dynamical modeling PdBI: Wilner et al. 2002 OVRO: Koerner et al. 2001 STScI Workshop: Nearby Resolved Debris Disks

  9. Dynamical Scenarios • structure created when resonances filled by • inward migration of dust due to P-R drag • outward migration of planet traps planetesimals (like Neptune) Wilner et al. 2002 Wyatt 2003 STScI Workshop: Nearby Resolved Debris Disks

  10. HD107146: 3 mm Interferometry • OVRO resolves dust (Carpenter et al. 2005) STScI Workshop: Nearby Resolved Debris Disks

  11. HD107146 (cont.) • predictions for SMA: STScI Workshop: Nearby Resolved Debris Disks

  12. Future Prospects: SMA, CARMA, ALMA • good sites • SMA • access to 850, 450 mm • CARMA: • 1.3 mm • larger bw • larger N (15 to 23) STScI Workshop: Nearby Resolved Debris Disks

  13. Atacama Large Millimeter Array 2012? • very large array (n= >50 x 12 m + 12 x 7 m), North America, Europe, and Japan: ~$1B • best possible site, Atacama at 5000 m, sensitivity 100x, high fidelity imaging STScI Workshop: Nearby Resolved Debris Disks

  14. Summary • (Sub)millimeter: key spectral regime for debris disk structure • interferometry: (only) way to obtain high angular resolution, but limited: sensitivity, imaging, small fields of view • examples: IRAM/OVRO results are few but intriguing • future prospects: SMA, CARMA will provide new data; ALMA will qualitatively change the debris disk field STScI Workshop: Nearby Resolved Debris Disks

  15. END STScI Workshop: Nearby Resolved Debris Disks

  16. JCMT 850 mm SCUBA Images • “Fantastic Four”: ring morphologies, cleared interiors, offset peaks (Holland et al. 1998, Greaves et al. 1998, etc., ...) • sculpting by planets? only viable explanation • submillimeter probes outer cold regions, long orbital periods STScI Workshop: Nearby Resolved Debris Disks

  17. e Eridani: 350 mm CSO Image Wilner, Dowell, et al. STScI Workshop: Nearby Resolved Debris Disks

  18. Debris Disk Evolution • Sptizer A star data: 24 mm excess declines, scatter (“outbursts”) present at all ages (Rieke et al. 2004) • compatible? with collisionally dominated planetismal disks (Dominik & Decin 2003, Kenyon & Bromley 2004) ~1/t STScI Workshop: Nearby Resolved Debris Disks

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