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 browser2nd submission-1144039164----- Attempting Submission 1 (Tue Jul 23 19:03:00 GMT 2019) -----
HST Phase II Proposal 15830 (PDS_PhaseII_revised_moreAngle.apt) successfully submitted.
Receipt: # 15830-1
----- Attempting Submission 2 (Tue Jul 23 19:05:42 GMT 2019) -----We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Systematics CTE-loss should be nigligible for our casethird, likely final submission-1101508105Assigned ID: 382
----- Attempting Submission 1 (Fri Apr 05 09:27:41 GMT 2019) -----
HST Phase I Proposal 382 (PDS.apt) successfully submitted.
Receipt: # 382-2
----- Attempting Submission 3 (Fri Apr 05 17:36:45 GMT 2019) -----
HST Phase I Proposal 382 (PDS.apt) successfully submitted.
Receipt: # 382-3
----- Attempting Submission 4 (Fri Apr 05 21:37:54 GMT 2019) -----
HST Phase I Proposal 382 (PDS.apt) successfully submitted.
Receipt: # 382-4A Planet is Born: Investigating the Accretion Process of PDS70b with WFC3/UVIS Direct Imaging ObservationsRecent direct imaging detection of H alpha emission from PDS70b, a giant young planet, revealed its rapid ongoing accretion. This discovery offers an exciting opportunity for constraining PDS70b's mass accretion rate, a critical parameter for studying its formation process. However, the correlation between the hydrogen line luminosity and the total accretion luminosity has not been established for Jovian mass objects. Therefore, both hydrogen line and continuum accretion luminosity for PDS70b are required to derive its mass accretion rate accurately.
We propose WFC3/UVIS direct imaging observations of PDS70b. Using HST's unique capability of high-contrast observations in the ultraviolet (UV) and optical wavelengths, we will measure the accretion-induced excess emissions of PDS70b in the F336W (Balmer break, UV continuum) and the F656N (H alpha) bands, and derive its mass accretion rate. We optimize the observations to enable KLIP-based angular differential imaging data reduction and maximize HST's high-contrast imaging capacity. This proposal will have three key results. 1) We will directly measure the total accretion luminosity of PDS70b and accurately derive its mass accretion rate. 2) By enabling the comparison of accretion luminosity in the UV and the H alpha bands, results from this proposal will advance our understanding of the accretion process of PDS70b. 3) By comparing the measured mass accretion rate to the empirical mass vs. accretion rate relationship, we will assess the formation pathway of PDS70b. The wavelengths used in this proposal also maximize the probability of detecting yet unknown accreting planets in this system.Observation Plan: We request 18 orbits WFC3/UVIS direct-imaging observation for PDS70b. We will observe PDS70b in the F336W (Balmer jump) and F656N (H-alpha) bands to directly measure its accretion luminosity. The photospheric emission is negligible at these wavelengths, we therefore do not request filters in the photospheric continuum. Each orbit will include ten 120 seconds F336W exposures and nine 20 seconds F656N exposures. For each filter, nine exposures will have unique dithering positions and one more F336W 120s exposure per orbit is added to increase signal-to-noise ratio (SNR). The WFC3/UVIS channel is chosen because it is the only instrument that is capable of multi-band UV-optical direct-imaging observations, and thus is the only one that can observe both of the accretion-induced Balmer jump and H-alpha emissions. The UVIS2-C512C-SUB subarray (20arcsec by 20arcsec) will be used to reduce detector readout time and to avoid buffer download overhead. We do not apply CRSPLIT to reduce the overheads of the observations. The multi-band and multiple dithering samples will provide sufficient information to remove cosmic rays.
We follow the recommendations in the instrument handbook and require FLASH=12 pre-flash to mitigate potential CTE-loss in the observations. We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures. CTE-loss will be negligible. Not scheduling pre-flash improves the total integration time and signal-to-noise.
Nyquist sampling: Nyquist sampling a critical requirement for building accurate PSF models to aid primary star subtraction. It is achieved through a nine-point 0.02arcsec spiral dithering strategy. At each of the nine pointing positions, we will take one F336W exposure and one F656N exposure. This dithering strategy will allow us to reconstruct Nyquist-sampled PSFs (0.02arcsec/pixel resolution) in both the F336W filter and the F656N filter in each orbit. To ensure pointing accuracy, we choose "Fine" guiding mode with 0.005 arcsec guiding tolerance. The gyro mode is 3GOBAD
Telescope roll angle: For angular differential imaging, we require each orbit to have 10-20 degrees roll angle difference from its previous orbit. We schedule the roll angle constraints through a "orient from" chain. With the possible range of schedulable observations, we request the roll angle difference between two orbits to be as close to 20 degrees as possible. This request mitigates self-subtraction in angular differential imaging reduciton.
Schedulability: We group our 18 orbits observations into 6 epochs. Each epoch has three orbits that are connected through Timing Requirements "after visit" chain. We do not place timing constraint for each epoch to increase flexibility. However, we prefer pairs of epochs (Epoch one and two, three and four, five and six) can be executed back-to-back to increase temproal coherence of the PSFs, if such observations can be scheduled.
High-Contrast Direct-Imaging Observations with WFC3/UVIS: Direct-imaging observations in the optical and UV wavelengths have an intrinsic advantage over direct-imaging observations in the near-infrared due to the sharper PSFs. In the proposed observations, the 0.18 arcsec separation between PDS70A and b corresponds to 9-10 resolution elements in the reconstructed and up-sampled images. In the observations of HR8799 with WFC3/IR (Rajan et al. 2015), the $5-\sigma$ contrast curve reached ~11.5 magnitudes at 0.5 arcsec separation corresponded to ~8 resolution elements (0.64 arcsec/resolution element). We therefore expect our proposed observation to achieve at least comparable contrast (11.5 mag) to Rajan et al. (2015), as we exceed the requirement of ~10 magnitude at 0.18 arcsec separation. Importantly, unlike the observations of HR8799, PDS70 (V ~12.2) will not saturate the detector and will not limit the inner working angle of the observation. This advantage further aids the success of this observation.Mr. Yifan Zhou is an expert on HST/WFC3 high-contrast direct imaging observations, and has led three first-author paper on this topic: Zhou et al. (2014), (2016), and (2019). Zhou et al. (2014) used HST/WFC3/UVIS to study the accretion processes of planetary-mass companions. Mr. Zhou is a 5th year graduate student at the University of Arizona and is going to be a McDonald Fellow at UT Austin.
Dr. Daniel Apai is an expert on high-contrast imaging observations and giant exoplanets. Dr. Apai was involved in multiple discoveries of directly-imaged giant young planets. Dr. Apai is an associate professor at the Unversity of Arizona and the academic adivosr of Mr. Zhou.
Dr. Glenn Schneider is an expert on high-contrast imaging observations with HST. Dr. Schneider has numerous works of using HST images to study giant planets and circumstellar disks. Dr. Schneider involved in the discovery of the first directly imaged planetary mass compnion 2M1207b using HST angular differential imaging. Dr. Schneider is an astronomer at the University of Arizona.
Mr. Kevin Wagner is an expert on ground based high-contrast imaging observations and data reductions. Mr. Wagner led the discovery of H alpha emission from PDS70b using MagAO observations. Mr Wagner is a 4th year graduate student at the University of Arizona.
Dr. Min Fang is an expert on low-mass star formation. Dr. Fang has published many high-impact works on using H alpha emissions to study the formation of low mass stars. Dr. Fang is a postdoc at the University of Arizona.
Dr. Adam Kraus is an expert on high-contrast direct imaging observations, low mass star formation, and giant planet formation. Dr. Kraus has published a large number of works on these topics. Dr. Kraus is an assistant professor at UT Austin.
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.
Dr. Greg Herczeg is an expert on low-mass star and giant planet formation. Dr. Herczeg developed the methodology of using UV excess emission to measure the accretion luminosity of low mass stars and brown dwarfs. Dr. Herczeg is a professor at Kavli Institute of Astronomy and Astrophysics (KIAA), Peking 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 involved in multiple ground-based discoveries of H alpha emissions from accreting young giant planets. Dr. Close is a professor at the University of Arizona.Planets and Planet Formation6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTAREXTRA-SOLAR PLANETSTAR FORMING REGIONThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000WFC3/UVISImagingNoNoF656NWFC3/UVISImagingNoNoF336WPOS-TARGDITHER0.02LINEfalsefalse90.0SPIRAL2falseTiming link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
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:data-volume 86960
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(Tic-Obset
:proposal-id 15830
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([14 After 13 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 13-15 are chained by Time Requirement constraint.
We do not place timing constraint between Visit 12 and Visit 13 for flexibility. However, it is preferrable that these two visits are scheduled as close as possible159256706100069.03999999999999(Tic-Visit
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:data-volume 86960
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(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([14 After 13 by 0.0 to 0.1 days] [15 After 14 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 13-15 are chained by Time Requirement constraint.159257277900079.04000000000002(Tic-Visit
:proposal-id 15830
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:date "23-Jul-2019 11:59:11.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:data-volume 86960
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(Tic-Obset
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)true10Timing link suitability includes constraints ([15 After 14 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 13-15 are chained by Time Requirement constraint.159257849700089.04000000000002(Tic-Visit
:proposal-id 15830
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([17 After 16 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 16-18 are chained by Time Requirement constraint.
We do not place timing constraint between Visit 15 and Visit 16 for flexibility. However, it is preferrable that these two visits are scheduled as close as possible(Tic-Visit
:proposal-id 15830
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([17 After 16 by 0.0 to 0.1 days] [18 After 17 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 16-18 are chained by Time Requirement constraint.(Tic-Visit
:proposal-id 15830
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:data-volume 86960
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(Tic-Obset
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(Tic-Orbit
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)true10Timing link suitability includes constraints ([18 After 17 by 0.0 to 0.1 days])The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.We choose to ignore the warning of low fresh level for the last exposure in each orbit and do not schedule pre-flash for these exposures. These exposures will be taken at the same pointing as their previous adjacent exposures.
Visit 16-18 are chained by Time Requirement constraint.(Tic-Visit
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:data-volume 86960
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15830
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)
(Tic-Orbit
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:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3238
:pcs-gap 0
)false10