first WDBD submission-617740595Assigned ID: 300
----- Attempting Submission 1 (Fri Apr 05 00:02:08 GMT 2019) -----
HST Phase I Proposal 300 (WDBD27.apt) successfully submitted.
Receipt: # 300-1First submission-540248356----- Attempting Submission 1 (Tue Jul 23 00:13:51 GMT 2019) -----Dancing with the Dwarfs: Very High Quality Spatial and Spectral Maps of Hot Jupiters ProxiesHot Jupiters are fascinating, but have complex atmospheres, in which the interplay of radiation transport, atmospheric dynamics, condensation, and chemistry shape the atmospheres's structure and spectra. Current data on hot Jupiters offers tantalizing insight into these worlds, but do not have high enough quality to settle several fundamental questions. A rare group of tight white dwarf-brown dwarf binaries provide a unique opportunity to sample highly irradiated ultracool atmospheres with very high significance level observations. In these systems the signal level between dayside and nightside spectra are typically a hundred times higher than that for any hot jupiter.
We propose HST time-resolved spectroscopy of six BD+WD pairs that encompass the entire temperature range of hot Jupiters and ultra hot jupiters: from 800K to 4300K. The very high data quality and the complete temperature sequence will allow us to address three key processes that challenge hot Jupiter models: a) Localized formation and destruction of condensate clouds; b) Day/nightside heat transport and irradiation- driven circulation; and 3) Dayside thermal dissociation of molecules. Our observations will provide a high- fidelity, spatially resolved spectral library for objects spanning the entire temperature range of hot jupiters with less telescope time than that is typically spent on detailed study of a single hot Jupiter. The high quality benchmark spectra will verify temperature- and irradiation-dependent trends and will provide a reference library for future hot Jupiter studies. HST can uniquely obtain the high-precision, time-resolved, near-infrared spectroscopy required by our science goals.Sample Size: In this proposal we explore three atmospheric processes: cloud formation through silicate condensation, day-night heat transport, and molecular dissociation and recombination. We will obtain longitudinal spectral maps of our targets, allowing us to explore how a given atmosphere changes with longitude. The most important parameter influencing these processes is temperature; therefore, we will observe a sample of WD+BD pairs that define a temperature sequence, encompassing the temperature range from hottest to coldest hot jupiters. The targeted six WD+BD pairs have brown dwarf equilibrium temperatures that are almost uniformly distributed from 700 K to 4,000 K. Our targets encompass the near-complete temperature range present in hot jupiters and ultra-hot jupiters (e.g., Parmentier et al. 2018). The six targets are the smallest sample that is robust to outliers when exploring trends in three different processes.
Target Selection: There are nine known detached WD+BD systems (Parsons et al. 2017). In evaluating the possible targets we considered the J-band brightness of the system, the predicted range of near-infrared variability, the predicted difference between the day and night spectra, and the orbital period of the system. On the basis of our comprehensive assessment we identified six targets as ideal systems for this study. Our sample of six objects encompasses the near-complete range of effective temperatures represented in hot jupiters.
Predicted Results: In our calculations we included a realistic observing efficiency and sampling strategy and used the WFC3 ETC 26.1 to estimate the signal-to-noise ratio. In summary, we will be able to observe 5--10%-level near-infrared modulations at SNRs of 169--1325 for the WFC3/G141 white light curves at cadences of 100--400 seconds or SNRs of 94--1071 for the phase-folded spectral light curves with seven-pixels-wide bands at a sample rate of 15 samples per full phase. Such high-quality spectral series will enable us to retrieve longitudinally resolved maps for every target.
Observing Mode: All observations will use the WFC3/IR G141 instrument in time-series mode. The instrument's high throughput from 1.1 to 1.7 $\mu$m, the remarkable sensitivity in the 1.4\,$\mu$m water absorption band, and the extraordinary photometric stability make WFC3/IR G141 the best and only choice to achieve our goals. Due to the relative faintness of our targets, we opt to conduct the observations in staring mode. Depending on the brightness of the targets, the exposure setup will be SPARS25, NSAMP=5-15, which result in cadences from 130 to 410 seconds. Light curves at these cadences will resolve the spectral modulations at sample rates greater than ten per brown dwarf orbit.
Exposure Time Calculation and Signal-to-Noise Ratio Estimate: We estimate the required exposure times and SNR achieved using the WFC3 Exposure Time Calculator. For the three brightest targets in our sample (GD1400, WD 0137-349, and NLTT5306) we will achieve an SNR> 1,000 in a single G141 exposure in white light. With a 10 pixel-wide spectral bins---typical in exoplanet transmission spectroscopy---the average SNR in the each bin will exceed 300. For the faintest target in our sample, WD~1557+0916, we will obtain an SNR of 169 in white light for a single SPARS25, NSAMP=15 exposure (exposure time: 313~s.), and an average SNR of 53 for the 10-pixel wide spectral bands. All targets have precise period measurements from radial velocity measurements, allowing us to phase-fold the light curves, further increasing the precision.
Telescope Time Justification: We request the minimum number of HST orbits to meet the goals we identified previously. Our goals require full phase coverage for the brown dwarf orbits and high-SNR spectral time series. WD+BD binaries GD1400 and NLTT5306 require a special approach for obtaining full phase coverage. For GD1400, which has the longest orbital period (10.0 hours) in our sample, we request eight consecutive orbits to ensure complete phase coverage. NLTT5306's orbital period is only 0.06% longer than the HST period. For this object we will use two 3-orbit-long visits separated by eight orbits to sample its complete phase curve.
We calculate the SNR requirements on the basis of distinguishing spectral modulations from three representative cases that are outlined in the Predicted Results section. We set the SNR criterion so that the day/night differential spectra are separated by more than $5\sigma$ at 1.4~$\mu$m. In the simulation we also assume a J-band modulation amplitude of 6% (same as WD~0137-329 in J Casewell et al. (2015)). With this criterion, we request six and ten HST orbits for the two faintest targets, WD~1411+2009 and WD~1557+0916.
Special Requirements
For NLTT5306 we require two coordinated visits, separated by 8 orbits. For our faintest object WD~1557+0916 we require 10 orbits, preferably obtained consecutively. However, two 5-orbit visits are also suitable. In the apt file, we set two 5-orbit visits and place a timing constraint so that the two visits do not separate for more than 4 orbits.Dr. Daniel Apai is an expert on the observational characterization of extrasolar planet and brown dwarf atmospheres. Dr. Apai has led six HST programs on these topics that resulted in over 20 refereed papers, most of which utilized the same instrument and observing strategy as proposed for in the current proposal. Apai's group has also published numerous observational studies on hot Jupiters, both in transmission and in emission. Apai will lead the program and will be responsible for the management, planning, data interpretation and will play major roles in the publication process. Dr. Apai is an Associate Professor of Astronomy and Planetary Sciences at The University of Arizona.
Dr. Siyi Xu is an expert on white dwarfs and has led numerous studies on observational characterization of polluted white dwarfs, including HST and Keck studies. Dr. Xu will lend her expertise on white dwarfs and white dwarf characterization/properties to this program. Dr. Xu is an Assistant Astronomer at the Gemini Observatory.
Mr. Yifan Zhou is an expert in HST/WFC3 time-resolved observations of brown dwarfs and planetary-mass objects. Mr. Zhou has published five papers based on such data, and hasadditional papers in preparation. Among other results Mr. Zhou has provided a new, physically-motivated model for the HST/WFC3 charge trap and delayed release systematics, which has been widely adopted in the community. This correction significantly enhanced the accuracy and efficiency of HST time-resolved observations. He will lend his expertise on HST/WFC3 time-resolved observations to this project. Mr. Zhou is an astronomy graduate student at The University of Arizona, working in the group of Dr. Apai; and, during the execution of this program, will be a McDonald Fellow at UT Austin.
Dr. Mark Marley is an expert on the atmospheric modeling of extrasolar planets and brown dwarfs. Dr. Marley has lead and c-authored over 200 refereed papers on atmospheric characterization. He will support this program through atmospheric modeling utilizing his state-of-the-art models. Dr. Marley is a Senior Research Scientist at the NASA Ames Research Center.
Dr. Adam Showman is an expert on atmospheric dynamics. He has published seminal papers on atmospheric circulation in exoplanets and brown dwarfs. Dr. Showman will lend his atmospheric dynamics expertise to the project. He is Professor of Planetary Sciences at The University of Arizona.Stellar PhysicsPlanets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=14.92STARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=16.23STARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000r=17.981STARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=18.82STARBROWN DWARFNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=17.512WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.1592678252000236.4036444546113(Tic-Visit
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