0 Assigned ID: 3191 ----- Attempting Submission 1 (Fri Mar 25 11:22:23 GMT 2022) ----- HST Phase I Proposal 3191 successfully submitted. Receipt: # 3191-1 ----- Attempting Submission 2 (Fri Mar 25 11:51:22 GMT 2022) ----- HST Phase I Proposal 3191 successfully submitted. Receipt: # 3191-2 ----- Attempting Submission 3 (Fri Mar 25 23:22:43 GMT 2022) ----- The number of orbits used exceeds the number allocated Resubmitted with copies of Visits 1 and 3. First observations failed due to guide star problem. -1838842809 Your proposal could not be saved. Submission aborted. ----- Attempting Submission 1 (Sun Jul 03 08:22:02 GMT 2022) ----- HST Phase II Proposal 17127 successfully submitted. Receipt: # 17127-1 ----- Attempting Submission 2 (Fri Aug 12 05:32:25 GMT 2022) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 3 (Tue May 02 02:01:44 GMT 2023) ----- No idea why the proposal says we are using 9 orbits and not the allocated 8 orbits. Testing models of accretion onto the Young Planetary System PDS 70 Observations of the planet-forming regions have revolutionized our understanding of how planets formed in the past decade. Of the many advances, the PDS 70 system is unique -- a system hosting two giant plants that are still growing from proto-lunary disks. When trying to understand the mass assembly of giant planets, such as PDS 70 b and c, this growth rate is a fundamental property. Typically the accretion rate is estimated by measuring H-alpha and then converting the line luminosity into accretion luminosity. However, this conversion was developed for the case where H-alpha emission is produced in the magnetospheric accretion flow. For forming planets, the magnetospheric accretion flow may not be hot enough to emit hydrogen lines. If the H line emission is instead produced by the accretion shock, more than half of the energy would escape as Ly-alpha photons. This uncertain interpretation leads to large errors in estimates of accretion rates from the observed H-alpha line. In this proposal, we request deep HST/ACS SBC PR130L prism spectra of PDS 70b and c to confirm whether the magnetospheric accretion flow emits hydrogen lines. We will use H2 emission, photoexcited by Ly-alpha photons, to compare Ly-alpha emission to H line emission. In addition, we will measure the C IV line luminosity and place it in the context of accretion flows onto low-mass stars and brown dwarfs. These observations will allow us to understand accretion onto PDS70 b and c and prepare to apply these models to the characterization of future discoveries with JWST and the ELTs. Two 4-orbit observations of PDS 70 to attempt to measure FUV emission from the planets. The position angles are set through ORIENT so that in each case, the planet is far enough from the star to be visible. In each orbit, I offset the star by a little for better spatial resolution. The target is acquired with the F150LP filter, with a count rate of ~1 cts/s, safe enough for a variable target. The star itself has a STIS G140L+G230L spectrum (PI Skinner) for use in the ETC. Dr. Yuhiko Aoyama has developed models for the accretion shock of the PDS 70 planets and applied them to MUSE observations. He provides the theoretical framework for interpreting the data and will lead any analysis. Dr. Jun Hashimoto led an analysis of MUSE observations of PDS 70, focused on the H-beta line and is generally an expert in observations of protoplanets and disks across the spectrum. Dr. Gregory Herczeg has extensive experience for FUV diagnostics of accretion onto solar-mass stars and brown dwarfs, including PI of GO-11151, GO-11616, and AR 16129. The GO-11151 program (Yang, Herczeg, et al. 2012) obtained ACS PR130L spectra when few HST instruments were working (before SM4), and as part of that program wrote a routine to calibrate PR130L spectra. He will lead the observational analysis. Dr. Yifan Zhou is also an expert on PDS 70 and accretion, including analysis and publication of WFC3 imaging of the source (Zhou et al. 2021; GO 15830) Dr. Tracy Beck is a scientist at STScI with an extensive career in analyzing high-resolution images of young stars and with experience with ACS SBC. Exoplanets and Exoplanet Formation Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED EXT-STAR T TAURI STAR NO This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 ACS/SBC Imaging No No F125LP ACS/SBC Spectroscopic No No PR130L ACS/SBC Imaging No No F150LP ACS/SBC Spectroscopic No No PR130L The scheduling data was generated by CASM 30.3. 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