0
Assigned ID: 161
----- Attempting Submission 1 (Wed Mar 04 17:11:21 GMT 2020) -----
HST Phase I Proposal 161 successfully submitted.
Receipt: # 161-1
----- Attempting Submission 2 (Fri Mar 06 10:28:31 GMT 2020) -----
HST Phase I Proposal 161 successfully submitted.
Receipt: # 161-2
Updates for visits using the F105W filter to have exposures in this band taken in the middle of the orbits, using Non-Interruptible Sequences.
Re-organised the exposures between visits 01 and 02.
63557777
----- Attempting Submission 1 (Mon Jun 22 12:07:56 GMT 2020) -----
HST Phase II Proposal 16229 successfully submitted.
Receipt: # 16229-1
----- Attempting Submission 2 (Thu Aug 20 12:51:28 GMT 2020) -----
HST Phase II Proposal 16229 successfully submitted.
Receipt: # 16229-2
----- Attempting Submission 3 (Thu Aug 20 16:38:58 GMT 2020) -----
Precise distances and photometry for the Y dwarf population: unlocking the secrets of our coolest neighbours
We propose for WFC3/IR imaging of 19 Y brown dwarfs to measure the most precise parallaxes and proper motions to date, and define a uniform catalogue of near-infrared F105W/F125W/F160W photometry for the vast majority of ultracool Y dwarfs. Accurate distances are vital for confident interpretations of measured quantities and assessments of inherent properties, which are indispensable to characterise the atmospheres of these giant planet analogues. The challenges associated with astrometric and spectrophotometric observations for such intrinsically faint objects result in highly incomplete and heterogeneous datasets, that severely lack reliable absolute calibrations.
HST provides a unique platform to obtain both precise astrometric parameters and photometry for Y dwarfs, with an exquisite astrometric precision and unmatched capabilities at these wavelengths for observations of such cold objects. Robust and uniform parallax measurements for the major part of the Y population will be essential to enhance our heavily scattered understanding of their characteristics, and improve theoretical models that lack empirical validation at the coldest temperatures.
Homogeneous sets of reliable distances and multiband photometry will allow for unprecedented analyses of colour-magnitude diagrams for the Y spectral sequence, enabling key tests of secondary effects like gravity or metallicity on the complex appearances of Y dwarfs. Constraining the kinematics and fundamental properties of these objects will be crucial in preparation of upcoming missions like JWST, which, combined with robust calibrations, will offer invaluable new glimpses into these puzzling planetary atmospheres.
This program consists of 26 orbits of WFC3 IR channel imaging for precise photometry and astrometry of 19 nearby ultracool Y dwarfs. All orbits are planned as single-orbit visits. We apply large and fractional-pixel dithering patterns to allow both removal of hot pixels and increase the spatial resolution of the datasets. All observations are taken in full frame mode, in order to maximise the number of reference sources in the fields of view. We use ~300 s exposures in MULTIACCUM mode in all cases, varying the exact exposure times from NSAMP=12-13-14, with SAMP-SEQ=SPARS25, to fit within the orbital visibility of each orbit.
This allows for a total of 8 individual images per 1-orbit visit. Various combinations of the F105W, F125W and F160W filters are used for each target, to complement existing archival data. For each orbit, we will hence have at least 4 (and up to 8) dithered exposures in at least one band, which will be crucial for precision astrometry within each epoch given the under-sampled detector of the WFC3 IR channel. A minimum of 2 images in F105W/F125W observations, and at least 6 exposures for observations in the redder F160W band, we will also allow for robust photometric measurements.
We request specific time constraints for each visit, in order to optimise our science results in the derivation of parallaxes and proper motions of our targets. We have hence defined optimal observing windows for each new orbit, based on the yearly phases already covered by archival datasets. These typically correspond to ~2-week windows intended as a repeat of the time of year observed in a previous epoch and/or annual phases covering the maximum or minimum parallax elongations. When additional constraints are required, we provide short comments about the specific constraints requested within each visit.
Dr. Clemence Fontanive (PI, Universtiy of Bern) is an expert on studies of brown dwarf populations. She has extensive experience with astrometric and photometric HST observations of nearby late-type T and Y dwarfs (Fontanive et al. 2018, MNRAS, 479, 2702) and has two succesful HST programs targeting low-mass brown dwarfs (GO 14686 and GO 15201). Dr. Fontanive will manage the overall program, coordinate observations, contribute to the analysis and interpretation of the data, and lead publications of results.
Dr. Luigi Bedin (Co-I, INAF-OAPD) is an expert on imaging photometry and astrometry with HST under-sampled images, and has contributed to state of the art calibrations and corrections of HST data. Dr. Bedin, with Dr. Fontanive, has led the development and application of precision astrometric techniques with HST/WFC3 for low-temperature brown dwarfs (Bedin et al. 2017, MNRAS, 470, 1140), in particular to link HST astrometry to the Gaia reference system at sub-mas levels (Bedin & Fontanive 2018, MNRAS, 481, 5339; Bedin & Fontanive 2020, MNRAS, in press, arXiv:2002:09331). Dr. Bedin will lead the data reduction and technical analyses of the observations, and conduct with Dr. Fontanive the extraction of photometric and astrometric measurements and derivation of astrometric parameters.
Dr. Daniella Bardalez Gagliuffi (Co-I, AMNH) specialises in the characterisation of ultracool brown dwarfs with imaging photometry (Bardalez Gagliuffi et al. 2015, AJ, 150, 163) and near-infrared spectroscopy (Bardalez Gagliuffi et al. 2014, ApJ, 794, 173; Bardalez Gagliuffi et al. 2018, ApJ, 854, 101). Dr. Bardalez also has expertise in population studies of ultracool dwarfs (Bardalez Gagliuffi et al. 2019, ApJ, 883, 205) and recently characterised one of the coldest brown dwarfs with HST/WFC3 photometry (Bardalez Gagliuffi et al. submitted), as a Co-I on a successful HST program (GO 15468). Dr. Bardalez Gagliuffi will contribute to the photometric analyses and interpretation of the data.
Stellar Physics and Stellar Types
Exoplanets and Exoplanet Formation
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