Diameters and Teff for Late-M, L and T Dwarfs: Spitzer 24um Photometry

Details Diameters and Teff for Late-M, L and T Dwarfs: Spitzer 24um Photometry Diameters and Teff for Late-M, L and T Dwarfs: Spitzer 24um Photometry

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...208.0902s&link_type=abstract

American Astronomical Society Meeting 208, #9.02; Bulletin of the American Astronomical Society, Vol. 38, p.88

Astronomy and Astrophysics

Astronomy

Scientific paper

We measured the 24um fluxes of a sample of low-mass field dwarfs (22 late-M, 17 L, and 11 T) using the Multiband Imaging Photometer for Spitzer (MIPS). One goal of the observations was to search for excess thermal emission due to dusty debris disks: no such disks were found. However, the data are useful for determining the diameters and effective temperatures of the objects via the infrared flux method IRFM (e.g. Ramirez & Melendez, 2005, AJ 626, 446; Leggett et al. 1986, A&A 159, 217). Our implementation of the IRFM is based on an empirical determination of the emissivity of the atmospheres of the objects in our sample, by comparison of their near-IR to 24um colors with those of main sequence A and G stars. Three of our targets have independently determined diameters and Teff from interferometry (Segransan et al. 2003, A&A 397, 5), and in each case our results are in excellent agreement. This method should be useful for constraining the fundamental properties of L and T dwarfs in the transition region between those types, where clouds are thought to play an important role in determining their radiative balance. The K-[24um] vs. Teff diagram for our sample is rather ratty when constructed using Teff based on spectral types; use of our values of Teff corrects all the outliers. We also find significant differences between our results and atmospheric models, suggesting that some refinements to the models may be possible.

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