0Assigned ID: 7548
----- Attempting Submission 1 (Thu Apr 16 19:02:14 GMT 2026) -----
HST Phase I Proposal 7548 successfully submitted.
Receipt: # 7548-1For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
COORDINATES SHOULD BE IN THE ICRS REFERENCE SYSTEM FOR A SMALL APERTURE
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.
For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser.0----- Attempting Submission 1 (Sat Aug 01 03:06:18 GMT 2026) -----One FP-POS is used per orbit so that the five 3-orbit visits use the four positions approximately equally.
The SNR is expected to be far below FPN-limited levels.
The ICRS coordinates warning has been addressed but will not disappear.Domain expansion: Detecting the first extrasolar UV aurora with deep COS observationsAurora is the main thermodynamic driver in the upper atmospheres of our magnetized solar system planets, but its study here is complicated by the influence of an unpredictable solar wind. Free-floating brown dwarfs are powerful auroral engines suitable for testing aurora physics without this interference. However, existing radio and infrared observations cannot directly probe the results of the auroral precipitation process: for this the FUV emission produced by electrons impacting the hydrogen atmosphere is required. The FUV is the main emission mechanism and diagnostic tool for solar system aurora, and without this component the study of brown dwarf aurorae has reached a natural barrier. We propose deep observations of an extremely well studied auroral brown dwarf with HST/COS, in order to detect and study an extrasolar aurora in FUV for the first time. Because of the extensive atmospheric modelling for this target, we will be able to test multiple auroral luminosity predictions, compare it to Jupiter-based expectations, and measure the energetics and depth of the electron impact process. This discovery would have wide-ranging impacts in auroral, planetary, and brown dwarf physics at large, as well as permanently expanding the domain of UV astronomy.We request 15 orbits of HST/COS at G140L/800 to observe the aurora of SIMP J0136+0933 in the far-UV. The emission bands of interest are the Werner band at 95-130 nm and the Lyman band at 155-165 nm. FUV aurora has never been observed outside the solar system and the target is not known to be a UV source. There is a suitable NUV source for blind offset acquisition located 30" south of the target.
SCHEDULING: Program is divided into five 3-orbit visits that need to be executed within the span of about one week. There is a near-perfect 3:2 ratio between the target's rotation period and the HST's orbital period, so any 3 consecutive orbits ensures full phase coverage over 2 consecutive rotations. The constraint is so that the visits can be accurately phase folded: the target accumulates one radian of rotation phase error per week.E. Sun (PI) is a doctoral candidate at the University of Toronto. He is an experienced observer with multiple ground-based programs studying the atmospheres and rotation of brown dwarfs. He will lead the proposed work as a core part of his doctoral thesis.
Dr. K. Retherford has experience from leading one successful HST program as PI (ProgID=13805, Io Lyman-alpha transits Retherford et al., AJ, 2019; large program 17470), several as U.S. administrative PI, and many more as CoI. As PI of the Europa Clipper UV Spectrograph (UVS), Dep. PI of JUICE-UVS, and PI of LRO-LAMP he has extensive far-UV spectroscopic expertise.
Dr. J. Kammer is a planetary scientist specializing in the retrieval of atmospheric composition from ultraviolet observations. His current research includes the analysis of Juno-UVS auroral data sets to study the power and morphology of Jupiter's aurora, providing the technical and physical background necessary to help model the electron deposition environment and interpret the UV spectra of brown dwarf analogues.
Dr. M. Bryan is an Assistant Professor of Astronomy & Astrophysics at the Pennsylvania State University. She is an expert on observational studies of the connections between planetary spin and magnetism.
Dr. L. Flagg is an expert on spectroscopy. She has done past work with COS specifically (Flagg et al. 2021), as well as other projects with FUV spectra. She has done work on brown dwarfs (Flagg et al. 2025).
Dr. Y. Zhou is an expert on HST observations of brown dwarfs.Exoplanets and Exoplanet FormationStellar Physics and Stellar Types6falsetruefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFTNOSIMP-J013656.5+093347.3GAIA-DR3-2572901021957789568J2000J2000For acquisition purposes only. G=19.41197 J=13.252CALIBRATIONTARGET ACQUISITION TESTNOETC used Vmag and Pickles spectrum F8V based on Gaia Teff=6175.3 logg=4.2254GALEX-J013658.3+093320GAIA-DR3-2572900948943068288J2000G=15.975 GALEX NUVmag 19.89(8) FUVmag N/ACOS/FUVSpectroscopicNoNoG140L800/Users/ethensun/Documents/uoft/research/proposals/hubble proposal/OP-cache/antitled-v01.xmlTiming link suitability includes constraints ([Group (01 02 03 04 05) Within 7.0 days])The scheduling data was generated by CASM 34.2.CASM was run in Phase II mode.5 visits of 3 orbits each. Only requirement needed is group timing.
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