THE 0.8-14.5 {mu}m SPECTRA OF MID-L TO MID-T DWARFS: DIAGNOSTICS OF EFFECTIVE TEMPERATURE, GRAIN SEDIMENTATION, GAS TRANSPORT, AND SURFACE GRAVITY
- BYU Department of Physics and Astronomy, N486 ESC, Provo, UT 84602 (United States)
- Gemini Observatory, Northern Operations Center, 670 North A'ohoku Place, Hilo, HI 96720 (United States)
- Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822 (United States)
- NASA Ames Research Center, MS 245-3, Moffett Field, CA 94035 (United States)
- Los Alamos National Laboratory, P.O. Box 1663, MS F663, Los Alamos, NM 87545 (United States)
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218 (United States)
We present new 5.2-14.5 {mu}m low-resolution spectra of 14 mid-L to mid-T dwarfs. We also present new 3.0-4.1 {mu}m spectra for five of these dwarfs. These data are supplemented by existing red and near-infrared spectra ({approx}0.6-2.5 {mu}m), as well as red through mid-infrared spectroscopy of seven other L and T dwarfs presented by Cushing et al. We compare these spectra to those generated from the model atmospheres of Saumon and Marley. The models reproduce the observed spectra well, except in the case of one very red L3.5 dwarf, 2MASS J22244381-0158521. The broad wavelength coverage allows us to constrain almost independently the four parameters used to describe these photospheres in our models: effective temperature (T {sub eff}), surface gravity, grain sedimentation efficiency (f{sub sed}), and vertical gas transport efficiency (K{sub zz} ). The CH{sub 4} bands centered at 2.2, 3.3, and 7.65 {mu}m and the CO band at 2.3 {mu}m are sensitive to K{sub zz} , and indicates that chemical mixing is important in all L and T dwarf atmospheres. The sample of L3.5 to T5.5 dwarfs spans the range 1800 K{approx}> T{sub eff} {approx}>1000 K, with an L-T transition (spectral types L7 to T4) that lies between 1400 and 1100 K for dwarfs with typical near-infrared colors; bluer and redder dwarfs can be 100 K warmer or cooler, respectively, when using infrared spectral types. When using optical spectral types, the bluer dwarfs have more typical T {sub eff} values as they tend to have earlier optical spectral types. In this model analysis, f {sub sed} increases rapidly between types T0 and T4, indicating that increased sedimentation can explain the rapid disappearance of clouds at this stage of brown dwarf evolution. There is a suggestion that the transition to dust-free atmospheres happens at lower temperatures for lower gravity dwarfs.
- OSTI ID:
- 21333843
- Journal Information:
- Astrophysical Journal, Vol. 702, Issue 1; Other Information: DOI: 10.1088/0004-637X/702/1/154; Country of input: International Atomic Energy Agency (IAEA); ISSN 0004-637X
- Country of Publication:
- United States
- Language:
- English
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