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Published January 1, 2004 | Published + Submitted
Journal Article Open

Ten Micron Observations of Nearby Young Stars


We present new 10 μm photometry of 21 nearby young stars obtained at the Palomar 5 m and at the Keck I 10 m telescopes as part of a program to search for dust in the habitable zone of young stars. Thirteen of the stars are in the F-K spectral type range ("solar analogs"), four have B or A spectral types, and four have spectral type M. We confirm existing IRAS 12 μm and ground-based 10 μm photometry for 10 of the stars and present new insight into this spectral regime for the rest. Excess emission at 10 μm is not found in any of the young solar analogs, except for a possible 2.4 σ detection in the G5 V star HD 88638. The G2 V star HD 107146, which does not display a 10 μm excess, is identified as a new Vega-like candidate, based on our 10 μm photospheric detection, combined with previously unidentified 60 and 100 μm IRAS excesses. Among the early-type stars, a 10 μm excess is detected only in HD 109573A (HR 4796A), confirming prior observations; among the M dwarfs, excesses are confirmed in AA Tau, CD -40°8434, and Hen 3-600A. A previously suggested N-band excess in the M3 dwarf CD -33°7795 is shown to be consistent with photospheric emission. We calculate infrared to stellar bolometric luminosity ratios for all stars exhibiting mid-infrared excesses and infer the total mass of orbiting dust in the cases of optically thin disks. For a derived median photometric precision of ±0.11 mag, we place an upper limit of M_(dust) ≈ 2 × 10^(-5) M_⊕ on the dust mass (assuming a dust temperature of 300 K) around solar analogs not seen in excess at 10 μm. Our calculations for the nearby K1 V star HD 17925 show that it may have the least massive debris disk known outside our solar system (M_(dust) ≳ 7 × 10^(-6) M_⊕). Our limited data confirm the expected tendency of decreasing fractional dust excess f_d = L_(IR)/L^* with increasing stellar age. However, we argue that estimates of f_d suffer from a degeneracy between the temperature and the amount of circumstellar dust M_(dust), and we propose a relation of M_(dust) as a function of age instead.

Additional Information

© 2004 American Astronomical Society. Received 2003 July 30. Accepted 2003 September 16. We would like to thank Randy Campbell and Gregory Wirth for their assistance with LWS, Tom Hayward and Rick Burress for help with SC-10, and Jonathan Foster for help with the LWS data reduction. This research has made use of the IPAC Infrared Science Archive, which is operated by the California Institute of Technology, under contract with NASA, and of the SIMBAD database, operated at CDS, Strasbourg, France. Data presented in this paper were analyzed at ESA's ISO Data Centre at Vilspa, Spain. The publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the IPAC/California Institute of Technology, funded by NASA and the NSF.

Attached Files

Published - Metchev_2004_ApJ_600_435.pdf

Submitted - 0309453.pdf


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