test version 1
version 2: updated team experience1695865575Assigned ID: 4030
----- Attempting Submission 1 (Mon May 22 16:38:26 GMT 2023) -----
HST Phase I Proposal 4030 successfully submitted.
Receipt: # 4030-1
----- Attempting Submission 2 (Wed May 24 16:36:44 GMT 2023) -----Version 1: test with all items in place; final if no changes identified. Target confirmation would not run.
Version 2: with target confirmation
Version 3: correction for timining links-327324114----- Attempting Submission 1 (Wed Sep 13 21:15:12 GMT 2023) -----
HST Phase II Proposal 17456 successfully submitted.
Receipt: # 17456-1
----- Attempting Submission 2 (Mon Oct 16 19:27:51 GMT 2023) -----
HST Phase II Proposal 17456 successfully submitted.
Receipt: # 17456-2
----- Attempting Submission 3 (Mon Oct 16 23:55:04 GMT 2023) -----Target confirmation would not run. However, both fixed targets were imported from a previously successful HST/STIS imaging program. No issues are expected with the targets for this reason.Travelling Through Time in the Beta Pictoris Disk: Exploring the Frequency of Protoplanet CollisionsDebris disks represent the end-stages of planet formation. Similar to the moon-forming impact and the collosion that stripped the mantle of Mercury during our own solar system's late stages of formation, major collisions between planetesimals and protoplanets shape the end products of mature planetary systems. Giant planets perturb the orbits of planetesimals, increasing the rate of collisions and the generation of micron-sized dust. These are blown out by radiation pressure to replenish the dust of the outer disk on timescales of centuries, and therefore measuring the surface density distribution of the outer disk can reveal the historical rate of collisions. There is evidence for at least one giant impact in the most nearby debris disk around Beta Pictoris having occurred in the past decades (due to the presence of CO gas which photo-dissociates within ~100 years). This suggests that such events may be even more common than previously thought. STIS images from 1997-2012 confirm the evidence of a recent impact, but only cover a quarter of the possible outer working angle. We propose to revisit the system with STIS to characterize the surface density distribution of the outer disk and thus the system's collision history over the past four centuries. By repeating the earlier observations with the optimal large outer working angle (43") orientation and occulting mask combination, we will recover surface density modulations of <20% at 200-400 au for the first time, representing collisions occurring from ~1860-1960. These observations will provide an entirely new set of constraints on the collision dynamics of the end stages of planet formation in the Beta Pictoris system.The proposed observations aim to obtain a STIS coronagraphic image of the Beta Pictoris debris disk with a goal of imaging disk structures at the furthest extent possible with HST.
Based on the comparison of the reduced 1997 and 2012 data and a set of PSF stars from other programs we identified that the following strategy provides the best quality data and best comparison to the earlier data sets:
We will observe the two targets using three single-orbit visits that are linked both in time and orientation angles (01, 02, 03) for each configuration (wedge A/B, disk NE/SW orientations). Three orbits x four configurations results in the twelve total orbits (one per visit) grouped into sets of three. Visits (04, 05, 06), (07, 08, 09), (10, 11, 12) are similarly grouped. We describe a single visit group below.
The three visits must be scheduled "back-to-back" in sequential visibility periods, each uninterrupted by Earth
occultation -- hence the AFTER scheduling requirements of 0.5 to 1.5 orbit (start-to-start) times on Visits 02 and 03.
In Visit 01 we observe our science target (Beta Pic). In Visit 02 we will observe our PSF calibration target (Alpha Pic).
The Alpha Pic visit (02) MUST be scheduled in time in between Visits 01 and 03. In Visit 03 we again observe Beta Pic,
but at an orientation angle differing from the absolute orientation specified for Visit 01.
We begin each Visit with an on-board autonomous coronagraphic target acquisition. Target acquisition exposure times
were chosen to provide SNR ~ 100 in the central pixel of the target acq images. In all cases we use the F25ND5 filter
due to the brightness of our target stars.
First orbit: We will observe Beta Pic at one of two wedge-occulted locations. We will obtain a series of identical 60 second exposures.
Absolute orientation is set such that the disk's maximum extent is visible along the line joining the occulting wedge position and the corner of the detector.
Second Orbit: Carry out the same observing sequence as in Orbit 1 on the PSF star Alpha Pictoris.
In this visit we observe our PSF template calibration star. In order to minimize variations in PSF structure from thermal driven changes in OTA wavefront errors, we constrain the orientation of this calibration target which is nearby in the sky to our science target (similar spacecraft attitude and sun angle) to be in between the orientations of Visit 01 and 03.
Third Orbit: Repeat the observations of Beta Pic (1st orbit) but at a different spacecraft orientation.
Orientation: Visit 1 +13 degrees (13 degrees is optimal for WedgeA, while -5-10 degrees is optimal for WedgeB). Orientation restrictions for (03) are somewhat relaxed - this was necessary to enable schedulability.
The three orbits MUST be executed back-to-back to minimize the changes in the instrumental PSF and the spacecraft/instrument state.
READOUT: We require full-frame readouts in order to image the maximal extent of the disk that is possible with STIS coronagraphy.
EXPOSURE TIMES:
Individual coronagraphic exposure timesare set to 60s with CR-SPLIT=8 to enable a greater dynamic range to be extracted from sub-expsosures. We can tolerate some saturation in the inner regions, even in the first sub-exposure, but we cannot tolerate saturation of the diffraction spikes outside of a radius of 10" from the target in the first sub-exposure. Based on existing data, we expect a count rate of ~70 DN/sec in the diffraction spikes at 10" from Beta Pic (Alpha Pic is slightly brighter), which even in 60 second exposures should be will within the detector's linear regime.
ORIENTATIONS:
The observations are sensitive to the roll angles: the correct angles are necessary to ensure that the disk is optimally placed such that its furthest extent can be imaged in the corner of the detector. Separate diagrams will be emailed to our PC to assist in the verification of our approach.
DISK AND SPACECRAFT ORIENTATIONS:
The "northern" semi-major axis of the nearly-edge on Beta Pic disk is at a celestial position angle of appx 29 deg.
(The inner disk itself is warped and PAs varying by a few degrees appear in the literature, depending upon how and at what
distances measures have been made. For our observation planning we adopt 29 deg).
If a suitable GS pair cannot be found to enable this geometry, we would later suggest possible specific alternates depending upon schedualbility with more restrictive differential roll ranges with trades in science return.Our team includes expertise in high-contrast disk and exoplanet observations, as well as radiative transfer disk models. Members of our team proposed for, reduced, analyzed, and published the most recent epoch of STIS imaging on the proposed target, which we propose here to build upon by imaging the outer disk in a similar configuration.
Prof. Daniel Apai is an expert on studies of extrasolar planets and planet-forming environments. Apai led nine HST proposals as PI and has published a comprehensive paper on HST/STIS observations of the Beta Pictoris system, the target of this proposal.
Dr. Kevin Wagner is a postdoctoral researcher at the University of Arizona. Dr. Wagner's research focuses on studying exoplanets and planet formation through high-contrast imaging and spectroscopy. Dr. Wagner has experience planning, reducing, and analyzing high-contrast imaging data (e.g., Wagner et al. 2018, ApJL, 863, L8), and in interpreting planet-disk interactions (e.g., Wagner et al. 2019, ApJ, 882, 20) and disk variability (e.g., Wagner et al. 2015, ApJ, 798, 94).
Mr. Arin Avsar is a graduate student at the University of Arizona working with Prof. Apai and Dr. Wagner. Mr. Avsar has over two years of experience with STIS data reduction and analysis. This project will be a component of Mr. Avsar's Ph.D. thesis.Exoplanets and Exoplanet Formation6falsefalsefalsefalsefalsefalsetruePRIMARY0.00.0falseSUPPORTEDSTARA4-A9 V-IVBeta Pictoris, debris disk: semi-major axis P.A.: +30.8 degree (E of N)
A6VJ2000J2000B=4.03CALIBRATIONPOINT SPREAD FUNCTIONPSF calibrator for Beta PictorisHD50241J2000J2000B=3.48STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEB1.8Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days])The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/williamj/hst/work/cycle31/OP-cache/17456-v01.xmlTiming: Must be executed in sequential orbit immediately prior to Visit 02 with only intervening inter-visit Earth occultation.(Tic-Visit
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