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0
Assigned ID: 2565
----- Attempting Submission 1 (Thu Jan 08 17:26:42 GMT 2015) -----
joint
Changed visits 7,8,9 to have only 19 exposures (to cut 5 min).
-1065788342
----- Attempting Submission 1 (Tue Feb 17 20:23:45 GMT 2015) -----
----- Attempting Submission 2 (Thu Feb 26 03:46:44 GMT 2015) -----
----- Attempting Submission 3 (Fri Mar 13 15:29:17 GMT 2015) -----
A Spitzer/HST Case Study of Weather on a Y Dwarf
Condensate clouds play a critical role in shaping the emergent spectra of both brown dwarfs and gas giant planets. Our understanding of the vertical structure and horizontal distribution of these clouds remains limited, however, because we typically lack the multi-epoch observations required to study the disk-integrated emergent spectrum modulated by the brown dwarf's rotation. Variability studies can be used to advance our understanding of the three dimensional structure of brown dwarf atmospheres but simultaneous, multi-wavelength observations with broad spectral coverage are required. Noticeably absent from all variability studies of brown dwarfs to date are the Y dwarfs which are the coolest brown dwarfs currently known (Teff < 450 K). Our Cycle 9 Spitze date no near-infrared variability has been detected. We therefore propose an HST/Spitzer case study of the Y0.5 dwarf WISE 1405+5534. We will obtain simultaneous F105W, F125W, [3.6] and [4.5] photometry of this dwarf and compare the light curves to predictions of partly cloudy model atmospheres. These observations will not only provide critical information for dynamical models of brown dwarf atmospheres but also directly inform the interpretation and characterization of cool gas giant exoplanets detected with the next generation of high-contrast imagers like the Gemini Planet Imager (GPI) and the SPHERE instrument for the VLT. program has shown that Y dwarfs do indeed show variability in the mid-infrared, but to
Since we are searching for near-infrared variability in a Y dwarf for the first time, we do not know a priori what level of variability to expect. Based on our HST Cycle 20 observations of WISE 1405+5534 we can achieve a photometric precision of 6/3% in a single F105W/F125W 100 sec exposure (this is consistent with the WFC3 ETC). Binning the data by 5 minutes gives precisions of 3.5/1.7% which is much better than we achieved from the ground with Gemini North on the brighter Y dwarf WISE 1738+2732. To match the Spitzer observations, we require 20 hours or 14 consecutive orbits split equally between F105W and F125W. WISE 1405+5534 can only be observed for ~60 min of each orbit and so we will obtain roughly thirty frames per orbit. We will also read subarrays of the detector in order to minimize the data volume.
COOL STARS
12
Regular
false
false
20
false
false
false
SUPPORTED
STAR
T
J2000
J2000
J=21.2
WFC3/IR
Imaging
No
No
F105W
WFC3/IR
Imaging
No
No
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