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Near-Infrared Spectroscopy of the Cool Brown Dwarf, SDSS 1624+00
Using the Subaru Telescope, we have obtained multiple near-infraredspectra of the cool brown dwarf, SDSS 1624+00 (J162414.37+002915.8), insearch of spectral variability in an 80 minute time span. We have foundthe suspected variability of water vapor absorption throughout theobservations, which requires a confirmation with a longer time baseline.After coadding the spectra, we have obtained a high-quality spectrumcovering from 1.05 to 1.8 mu m. There are three kinds of spectralindicators, the water vapor bands, methane band and K I lines at 1.243and 1.252 mu m, which can be used to study the temperature and thepresence of dust. We compare the spectra of SDSS 1624+00 and Gliese229B, while paying special attention to these indicators. The shallowerwater vapor absorption of SDSS 1624+00 indicates that it is warmerand/or dustier. The shallower methane absorption suggests that SDSS1624+00 is warmer. We interpret the deeper K I lines in SDSS 1624+00 asbeing the result of its higher temperature. With the help of modelspectra, we conclude that SDSS 1624+00 is warmer and dustier than Gliese229B. For the first time in a cool brown dwarf, a finite flux is seen atthe bottom of the water vapor band between 1.34 and 1.42 mu m, whichmeans that the 1.4 mu m band of water can be completely observed fromthe ground.
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| Takýmyýldýz: | Yilanci |
| Sað Açýklýk: | 16h27m31.27s |
| Yükselim: | +00°28'42.9" |
| Görünürdeki Parlaklýk: | 8.975 |
| özdevim Sað Açýklýk: | -13.9 |
| özdevim Yükselim: | -30.6 |
| B-T magnitude: | 9.405 |
| V-T magnitude: | 9.011 |
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