0Assigned ID: 3500
----- Attempting Submission 1 (Fri Mar 25 20:17:32 GMT 2022) -----
HST Phase I Proposal 3500 successfully submitted.
Receipt: # 3500-1
----- Attempting Submission 2 (Fri Mar 25 23:00:04 GMT 2022) -----
HST Phase I Proposal 3500 successfully submitted.
Receipt: # 3500-2
----- Attempting Submission 3 (Fri Mar 25 23:05:58 GMT 2022) -----
HST Phase I Proposal 3500 successfully submitted.
Receipt: # 3500-3FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser0----- Attempting Submission 1 (Tue Jul 12 23:56:59 GMT 2022) -----The region of interest is 0.6 arcsec away from the stellar PSF center. This area contains a significant amount of flux from the stellar PSF halo. As a result, our exposure does not suffer severe charge transfer loss. We set the post-flash level to be 12 electron, lower than the 20 electron requirement. This is consistent with the Cycle 29 observations. The strategy has been proven to be successful.Confirming the Protoplanet Candidate AB Aur b with Accretion Light EchoesGiant planets generate accretion luminosity as they form. Much of this energy is radiated in the form of strong Halpha line emission, enabling direct constraints on accretion mechanisms in the plaentary regime and the transport of material from circumplanetary disks onto young planets. However, compact disk features can mimic accreting planets by scattering Halpha emission generated by the host star; this can greatly complicate the interpretaion of point sources detected within protoplanetary disks. Recently a protoplanet candidate was directly imaged in Halpha with HST inside the transition disk of the young Herbig Ae/Be star AB Aurigae. We propose a novel test of the protoplanet hypothesis in this system using accretion light echoes by assessing whether the emission line strength is correlated between the candidate planet and the host star---a measurement only possible with HST. Strong positive correlation would point to scattering whereas no correlation would support the planet interpretation. If confirmed, this protoplant would explain many substructures in the AB Aur disk and would join only two other uncontested accreting giant planets detected with direct imaging.Instrument setups:
We will take direct imaging observations of AB Aur using WFC3/UVIS in the F656N filter to observe its H-alpha emission line. A four-point box dithering pattern will be adopted for observations in each orbit. The dithering distance is one half pixel (20~mas) in either direction. A set of four images taken at the four dithering pointings will be combined
using the Fourier interlacing algorithms, which guarantees the combined images to be Nyquist sampled and has been demonstrated to be successful in assisting high-contrast imaging observations. At each dithering pointing, a series of 2.7~s exposures will be taken using the WFC3 UVIS2 C512C subarray, resulting in a raw SNR of 450 per image.
This program requires roll constraints to avoid the host star's diffraction spikes falling on the companion. Different relative orientation angles are also required to facilitate ADI for each epoch using two telescope roll angles with a difference of 25 to 35 degrees.
The region of interest is 0.6 arcsec away from the stellar PSF center. This area contains a significant amount of flux from the stellar PSF halo. As a result, our exposure does not suffer severe charge transfer loss. We set the post-flash level to be 12 electron, lower than the 20 electron requirement. This is consistent with the Cycle 29 observations. The strategy has been proven to be successful.
Timing consideration:
The light travel time from the host out to the (deprojected) separation of the candidate at ~100~AU is approximately 13 hours. Therefore, any accretion variability that AB Aur undergoes will only be seen at the location of the point source 13 hours later. The "effective time resolution'' of each 4-orbit set of observations is ~96 min/orbit x 4 orbits, or 6 hours if they are taken in a contiguous block. With this back-to-back scheduling, the main science observations of the companion will not perfectly sample the host star's behavior in the same dataset owing the large star-companion distance.
Each epoch will require four orbits of observations. To account for potential light-travel time effects, we require the first orbit separated by a gap of ~7 orbits (0.5--0.6~days) before the next three contiguous orbits are carried out. Each group (four orbits) observations requires a gap of at least two weeks to ensure each epoch is an independent measurement.Dr. Jaehan Bae is a leading expert in theoretical studies of planet formation and protoplanetary disks. He is an assistant professor at the University of Florida.
Dr. Brendan Bowler is an expert on high-contrst direct imaging observations of giant planets. Dr. Bowler has multiple discoveries of planetary mass companions. Dr. Bowler is an assistant professor at UT Austin.
Ms. Lauren Biddle is an expert in planet-disk interactions and light curve analysis. She is a graduate student at Northern Arizona University.
Dr. Laird Close is a pioneer for using H alpha emission to search for directly-imaged giant planets. As the PI of MagAO, Dr. Close has been involved in multiple ground-based discoveries of accreting young giant planets. Dr. Close is a professor at the University of Arizona.
Dr. Katherine Follette is an expert in high-contrast imaging observations. She has led multiple discovery and characterization studies of protoplanets. Dr. Follette is an assistant professor at Amherst College.
Dr. Ya-Lin Wu is an expert in direct-imaging observations and planet formation studies. Dr. Wu has developed ground-based observing programs to monitor wide-separated planetary-mass objects at visible through sub-mm wavelengths. He is an assistant professor at Nationa Taiwan Normal University.
Dr. Adam Kraus is an expert on high-contrast direct imaging observations, low mass star formation, and giant planet formation. Dr. Kraus is an assistant professor at UT Austin.
Dr. Feng Long is experienced in observations and the interpretation of millimeter emission from protoplanetary disks.
Mr. Aniket Sanghi is an undergraduate student at UT Austin working with Dr. Bowler and Dr. Zhou. Mr. Sanghi is developing a strong skillset for high-contrast imaging data reduction and planet formation studies.
Mr Quang Tran is an expert at precision radial velocities and interpreting light curve variability. Mr. Tran is a graduate student at UT Austin working with Dr. Bowler.
Dr. Kim Ward-Duong is an expert in planet formation and high-contrast imaging observations. She has led multiple programs characterizing young substellar objects and protoplanetary disks. Dr. Ward-Duong is an assistant professor at Smith College.
Dr. Yifan Zhou is an expert in space-based direct-imaging observations and planet formation studies. Dr. Zhou is the PI of an ongoing HST observing program on PDS70. Results from this proposal and the HST programs will be complementary to each other.
Dr. Zhaohuan Zhu is an expert in modeling protoplanetary disks. He led many studies that predict and interpret disk structures induced by forming planets. Dr. Zhu is an associate professor at University of Nevada, Las Vegas.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETARY SYSTEMHERBIG AE/BEThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NPOS-TARGDITHER0.02LINE0.02falsefalse9040BOX1falseTiming link suitability includes constraints ([A1 After A0 by 0.4 to 0.5 days])The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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