Cloud Atlas: Rotational Modulations in the L/T Transition Brown Dwarf Companion HN Peg B

Zhou, Yifan ; Apai, Daniel ; Metchev, Stanimir ; Lew, Ben W P ; Schneider, Glenn ; Marley, Mark S ; Karalidi, Theodora ; Manjavacas, Elena ; Bedin, Luigi R ; Cowan, Nicolas B(McGill Univ, Dept of Earth & Planetary Sciences and Dept of Physics, Montreal, Quebec, Canada)

关键词: CLOUDS (METEOROLOGY);    PLANETARY ATMOSPHERES;    ROTATIONAL SPECTRA;    AMPLITUDE MODULATION;    BROWN DWARF STARS;    PLANET DETECTION;    LIGHT CURVE;    ABSORPTION SPECTRA;    STELLAR MODELS;    PLANETARY GRAVITATION;    CONDENSATES;    INTERPOLATION;    GOODNESS OF FIT;    WAVELENGTHS;    WATER;    VARIATIONS;    ASTRONOMICAL PHOTOMETRY;    IMAGE PROCESSING;    COMPANION STARS;    HUBBLE SPACE TELESCOPE;   

RP-ID  :  ARC-E-DAA-TN52248

学科分类：天体物理学

美国|英语

来源: NASA Technical Reports Server

【 摘 要 】

Time-resolved observations of brown dwarfs' rotational modulations provide powerful insights into the properties of condensate clouds in ultra-cool atmospheres. Multi-wavelength light curves reveal cloud vertical structures, condensate particle sizes, and cloud morphology, which directly constrain condensate cloud and atmospheric circulation models. We report results from Hubble Space Telescope/Wide Field Camera 3 (WFC3) near-infrared G141 taken in six consecutive orbits observations of HNPeg B, an L/T transition brown dwarf companion to a G0V type star. The best-fit sine wave to the 1.1 to 1.7 micron broadband light curve has the amplitude of and period of hour. The modulation amplitude has no detectable wavelength dependence except in the 1.4 micron water absorption band, indicating that the characteristic condensate particle sizes are large (greater than 1 micron). We detect significantly (4.4 sigma) lower modulation amplitude in the 1.4 micron water absorption band, and find that HN Peg B's spectral modulation resembles those of early T type brown dwarfs. We also describe a new empirical interpolation method to remove spectral contamination from the bright host star. This method may be applied in other high-contrast time-resolved observations with WFC3.