Second C31 submission2028906487Assigned ID: 4073
----- Attempting Submission 1 (Tue May 23 04:28:57 GMT 2023) -----
HST Phase I Proposal 4073 successfully submitted.
Receipt: # 4073-1
----- Attempting Submission 2 (Wed May 24 20:16:41 GMT 2023) -----ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
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
ORBITAL VISIBILITY OVERRUN
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
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
ORBITAL VISIBILITY OVERRUN
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 browserVisits Z1 to Z6 are repeat observations for visits A1 to A6. This repeat is approved by HOPR 92831.94807842----- Attempting Submission 3 (Thu Mar 14 23:55:27 GMT 2024) -----
----- Attempting Submission 4 (Tue Jun 04 23:48:23 GMT 2024) -----These warnings are inherited from previous submissions. They do not affect the quality of the data.Monitoring the H-alpha Emission from the PDS 70 PlanetsProtoplanets that are actively accreting within their circumstellar disks offer an exciting opportunity to investigate planet formation. Strong H-alpha emission lines produced by accretion shocks have been detected in direct-imaging observations of the ~5 Myr old giant protoplanets PDS 70 b and c. These observations measured snapshots of these planets' mass accretion rate. However, the time-varying aspects of planetary accretion have not been explored.
Recent HST/WFC3/UVIS observations of PDS 70 b demonstrated this instrument's high-contrast imaging capability. We propose to apply similar observing strategies and leverage HST's excellent long-term photometric stability to monitor the PDS 70 planets' H-alpha emission. The observations are designed to cover three representative timescales, corresponding to the planetary rotational periods, circumplanetary disk Keplerian motion, and long-term irregular variability. These observations will allow us to determine whether the PDS 70 planets maintain a steady accretion rate. Comparing variability amplitudes between different timescales will help distinguish the physical origins of multiple potential shock fronts in this system. If rotational modulations are detected, we will measure the rotation rates, which will offer rare constraints on the angular momentum evolution of gas giants like Jupiter at young ages..The program's main objective is to monitor the H-alpha emissions from the accreting young planets PDS 70 b and c across three distinct timescales. The fourteen orbits are categorized into five visit-sets: A1-A6, B1-B2, C1-C2, D1-D2, and E1-E2. The initial set comprises six consecutive orbits, aimed at capturing variability linked to planetary rotation timescales. The remaining four sets consist of two orbits each, facilitating the observation of long-term and stochastic variabilities.
Timing of the observations is essential to establish the monitoring time baseline. The sequence starts with the A1 to A6 visit-set. Subsequently, the B1-B2 and C1-C2 sets should be scheduled approximately two days (1.5 to 2.5 days) after their respective preceding sets, while the D1-D2 and E1-E2 sets should be conducted at least 10 days after the preceding visits.
The two planets have small angular separations (5-8 WFC3/UVIS pixels) to the host star. To extract the planetary flux accurately, we intend to employ angular differential imaging. This technique has demonstrated its efficacy in furnishing precise point spread function references, thereby enabling planet recoveries. During the initial visit-set, the telescope's roll angle should alternate between two angles, ensuring a separation of no less than 25 degrees. For the subsequent B1 to E2 visit-sets, the roll angles are governed by a relative roll angle chain. This constraint mandates a minimum difference of 25 degrees in roll angle between consecutive visits.
The detector configurations mirror those employed in programs GO-15830, 16651, and 17280, which yielded successful recoveries of close companions. We implement a four-point dither pattern (20 arcsec) to facilitate the reconstruction of Nyquist-sampled images. At each dithering position, a sequence of six 65-second exposures will be acquired.
The background flux at the planets location is high. Based on previous WFC3 data collected in GO-15830 observations, we estimate the background levels to be 300 to 400 electrons near planets b and c. Therefore, we decide to ignore the warnings about the FLASH levels and not apply additional FLASH.
Our observation plan closely follows the description in the Phase I proposal. Nevertheless, there are several necessary changes:
1. The exposure time is shortened from the proposed 185 seconds to 65 seconds to ensure no saturation.
2. The time intervals between visits C2 and D1, and D2 and E1 are shortened from the proposed 30 days to 10 days. This change makes the observation schedulable in APT. However, we request the time intervals between the last three visit-sets to be as large as possible to establish a sufficiently long time baseline.Dr. Yuhiko Aoyama is an expert in modeling planetary accretion shocks. Dr. Aoyama's models will be essential in interpreting the planets' hydrogen emission lines.
Dr. Lauren Biddle is an expert in characterizing time-variable photometric accretion signatures of Classical T Tauri stars with data from space observatories. She has additional experience modeling accretion variability over short and long (minutes-weeks) timescales.
Dr. Brendan Bowler is an expert in high-contrast imaging and planet formation studies. Dr. Marta Bryan is an expert in planet spin and angular momentum evolution.
Dr. Nuria Calvet is an expert in observing and modeling of accretion shocks of T Tauri stars. She has published multiple works on variable accretion onto T Tauri stars.
Dr. Sebastiaan Haffert is an expert in visible and near-infrared direct imaging data processing and analysis, and in particular the analysis of accreting proto-planets. His expertise will be used for the data processing to achieve the required photometric precision.
Dr. Yasuhiro Hasegawa is an expert of giant planet formation and has experience in developing a theoretical model that will be used to interpret the proposed observational data.
Dr. Jun Hashimoto has an experience of Halpha observations of PDS70 planets with VLT/MUSE.
Dr. Gabriel-Dominique Marleau is an expert of gas-giant formation and structure and radiation-hydrodynamical simulations. He also collaborates with Dr. Aoyama on planetary shock-emission models, and has worked with several observers on the interpretation of direct-imaging results.
Mr. Aniket Sanghi is developing a strong skillset for high-contrast imaging data reduction and planet formation studies.
Dr. Takasao is an expert in planet accretion theories.
Mr. Thanathibodee is an expert in accretion onto stars and planets. He developed manetospheric accretion models for the PDS 70 planets and studied the variable accretion on PDS 70 the star.
Dr. Taichi Uyama is an expert of high-contrast imaging observations around young stellar objects at both NIR wavelength and H-alpha.
Dr. Kevin Wagner is an expert in planet formation and high-contrast imaging observations. Dr. Wagner led the Monitoring the H-alpha Emission from the PDS 70 Planets first discovery of H-alpha emission from the planet PDS 70 b
Dr. Ya-Lin Wu is an expert in direct-imaging observations and planet formation studies. Dr. Wu has developed ground-based observing programs for monitoring wide-separated planetary-mass objects.
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. Mickael Bonnefoy, Dr. Catherine Dougados, and Mr. Dorian Demars are experts in the study of young giant planets and actively involved in ground-based campaigns to investigate the variability of young PMCs. Their ongoing efforts complement the proposed observations and provide valuable insights.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETARY SYSTEMK V-IVT TAURI STARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF656NPOS-TARGDITHER0.02LINE0.02falsefalse9040BOX1falseTiming link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days])Hst Same orient constraint links visits (01 03 05)The scheduling data was generated by CASM 32.0.CASM was run in Phase II mode.1712602964000315.3(Tic-Visit
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