The Angular Momentum Architecture of Long-Period Giant Planets and Brown Dwarf Companions

0 Assigned ID: 1745 ----- Attempting Submission 1 (Thu Apr 08 23:04:42 GMT 2021) ----- HST Phase I Proposal 1745 successfully submitted. Receipt: # 1745-1 ----- Attempting Submission 2 (Fri Apr 09 14:04:36 GMT 2021) ----- 0 ----- Attempting Submission 1 (Wed Jul 28 20:30:45 GMT 2021) ----- The Angular Momentum Architecture of Long-Period Giant Planets and Brown Dwarf Companions The origin of giant planets and brown dwarfs discovered with direct imaging at wide separations (>10 AU) is challenging to establish because multiple formation and migration mechanisms are possible. The goal of this program is to determine the angular momentum architecture of systems hosting imaged substellar companions to constrain their formation and evolutionary history. We propose WFC3/IR time-series observations of three substellar companions spanning 10-60 Mjup to search for rotationally modulated photometric variability. Rotation periods will be combined with projected rotational velocities (vsini values) and orbit monitoring efforts from the ground to assess the geometric alignment between the orbital angular momentum vector and both the stellar and companion spin axes. Mutual alignment would point to a disk-based origin while misalignment will indicate an alternative route or dynamical evolution. To date, only a single obliquity angle has been measured for a substellar companion; we aim to broaden this to a larger sample, paving the way for similar studies of lower-mass planets at longer wavelengths with JWST. The science goal of this program is to measure the rotation periods of three substellar companions with time-series WFC3 imaging (for one object) and grism spectroscopy (for the other two). The relative amplitude, wavelength-dependency, and possible phase shifts of the variability provide information about cloud structure and dynamics in these low-mass companions. Detailed observing description: The companions are separated by 3-8" from their hosts, have contrasts of dJ=5.7-10 mag, and apparent J-band magnitudes between 13.6-20.0 mag. The host stars range from J=5.1 to 10.0 mag. For CD-35 2722 B and Gl 229 B, we empoy the G141 grism to disperse their 1.1-1.7 um spectra and capture more flux than a broadband filter. This will also provide spectra covering the water absorption band and enables the opportunity to search for wavelength-dependent variability, a signature of mid-altitude clouds. The contrast between 2M2236+4751 A and b is much higher (dJ=10 mag) and the companion is fainter, so the F125W filter is preferred. The 256x256 subarray (~30"x30" field of view) will be read out to eliminate the need for in-orbit buffer dumps and improve duty cycle. The 2M2236+4751 observations will comprise consecutive exposures throughout each orbit in imaging mode followed by a reorientation of the telescope by ~30 deg in adjacent orbits to facilitate PSF roll subtraction. For CD-35 2722 B and Gl 229 B, we will obtain a single image in F132N immediately at the start of each orbit to determine the location of the companion in the grism data. This is also useful for wavelength calibration. For these two targets, the telescope roll angle should be oriented so that the grism dispersion direction is orthogonal to the binary PA. The six orbit allocations for each target should be carried out consecutively in one block to maximize uninterrupted coverage. To minimize flat-fielding errors, each target will be positioned at the same location on the detector for each orbit. As a result there will be no dithering for these observations. This program requires roll constraints for the G141 observations to maximize the separation between the dispersion of the host and companion spectra (25-45 deg or 225-245 deg for Gl 229 B, and 97-117 deg or 277-297 deg for CD-35 2722 B). All six orbits for each target must also be acquired back-to-back to obtain one continuous 8.5 hour light curve (except during parts of the orbit when the target is out of view). For 2M2236, to facilitate PSF roll subtraction, adjacent orbits should be oriented with roll angles of about +/-20-40 deg from the original configuration while also avoiding diffraction spikes. Our team members have expertise in high-contrast imaging, substellar variability, WFC3 data reduction, orbit fitting, and atmospheric modeling. PI Bowler's research focuses on detecting and characterizing giant planets with direct imaging and statistical properties of planets on wide orbits. He has led large surveys using adaptive optics imaging from the ground and with HST. Co-I's Apai and Zhou are experts in time series monitoring of brown dwarfs and planetary-mass companions with WFC3. D. Apai led the "Cloud Atlas" Treasury Survey which mapped the rotation and cloud structure of brown dwarfs with WFC3 and resulted in six publications over the past three years. Y. Zhou led several of these papers and also developed a model to predict and correct charge trap systematics in the WFC3 detector, removing the need to discard the first orbit for programs measuring precision time-series photometry. Co-I Bryan is leading a ground-based high-resolution spectroscopy program with Keck/NIRSPEC to measure vsini values for planetary-mass companions and brown dwarfs in this sample. She is also an expert on the angular momentum evolution of this population. Co-I's Nielsen and Blunt are experts in the orbital properties and demographics of companions on wide orbits. S. Blunt recently developed an efficient Bayesian orbit fitting package to infer the orbital elements of companions that have traced out small orbit arcs. Co-I Wu's research focuses on the origin, atmospheric properties, and circumplanetary disks of giant planets at large separations. Co-I Morley is an expert in modeling substellar atmospheres, including reproducing and interpreting the light curves of variable brown dwarfs. Exoplanets and Exoplanet Formation 6 false false false false false false false false SUPPORTED STAR BROWN DWARF NO The spectral type of the science target (Gl 229 B) is ~T7. The coordinates and magnitudes listed here are for the companion Gl 229 B, which is located 6.2 arcsec from its host at a PA of 171 deg. The J2000 coordinates for the host star (M1 spectral type) are RA=06:10:34.615, Dec=-21:51:52.66. The host star magnitudes are: V=8.1, J=5.1, H=4.4. J2000 J2000 J=14.2 STAR BROWN DWARF NO The quoted photometry is for the companion, which is red and has a spectral type of late-L. The K7 host star photometry is as follows: V=12.8, J=10.0, H=9.3. The companion is located 3.7" from the host at a PA of 135 deg. 2MASSJ22362452+4751425 J2000 J2000 J=20.0 STAR BROWN DWARF NO The quoted photometry is for the companion, which is red and has a spectral type of L4. The M1 host star photometry is as follows: V=11.1, J=7.9, H=7.3. The companion is located 3.1" from the host at a PA of 243 deg. J2000 J2000 J=13.6 WFC3/IR Spectroscopic No No G141 WFC3/IR Imaging No No F125W WFC3/IR Spectroscopic No No G141 1627490857108 /Users/bb35393/Dropbox/Research/Proposals/2021_HST_C29_BD_Rotation/Phase2/APT_saves/OP-cache/HST_C29_phase2_BD_rotation_final-v01.xml The scheduling data was generated by CASM 29.2. 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