0 Assigned ID: 893 ----- Attempting Submission 1 (Fri Apr 07 21:12:15 GMT 2017) ----- This is the Cycle 26 submission of the final three orbits in this program (Visits 07-09). Visits 01-06 were executed in Cycle 25. In this submission we deleted the ORIENT WITHIN and replaced it with a SEQUENCE in order to observe the PSF reference star in between the two science target visits (per the recommendation of John Debes). Same comments apply 12/14/18 -1652112762 ----- Attempting Submission 1 (Wed Jul 19 21:48:55 GMT 2017) ----- ----- Attempting Submission 2 (Fri Aug 18 19:02:48 GMT 2017) ----- ----- Attempting Submission 3 (Wed Aug 01 12:53:59 GMT 2018) ----- ----- Attempting Submission 4 (Tue Nov 27 19:00:10 GMT 2018) ----- ----- Attempting Submission 5 (Fri Dec 14 21:40:51 GMT 2018) ----- The target confirmation tool causes APT to hang, and it also caused my entire operating system to crash (MacOS High Sierra 10.13.6) Resolving the late planet formation stages around young M-stars Recent discoveries of earth-like planets around M-stars have highlighted the importance of understanding planet formation around late-type stars. However, this effort has been hampered by the lack of resolved observations of protoplanetary disks. In particular, scattered light images of M-star disks near the age of dispersal are critical to making further progress. The Upper Sco region provides a promising venue to remedy this situation, as it is the closest region with an age of 5-11 Myrs, commensurate with dispersal timescales. We propose to observe three M-star protoplanetary disks in the Upper Sco association using HST/STIS coronography to resolve the disks in scattered-light for the first time and to search for morphological signatures of forming planets. These three disks have been selected based on ALMA mm-dust and CO measurements that display radii within the STIS field of view and outside its inner working angle (IWA). We will use these observations to carry out a comparative study of the evolutionary state between M-star disks in Upper Sco and the younger 1-2 Myr Taurus region, leveraging both previous scattered-light images of disks in Taurus, as well as previous observations of the mm-dust and CO in both regions. All three targets are too faint to be observed using ground-based AO. Therefore, HST/STIS is the only instrument able to make these important measurements. These observations will act as critical diagnostics of the evolutionary state of nearby M-star protoplanetary disks, that will inform theories of planet formation and will further our understanding of the evolution of the planets around M-stars, such as our nearest neighbor Proxima Centauri b. Our observations seek to take advantage of the recently commissioned STIS BAR5 (i.e. the bent finger; Gaspar & Schneider, GO-12923) coronagraphic mode to achieve the 0.25" inner working angle required to image these three disks in scattered light. The expected outer radius of the scattered-light disk is unknown, as the exact relationship between the small dust and the CO at these evolved stages is unknown, but it is expected to be at least that of the CO radius (and therefore observable with STIS), but possibly extending further. Empirically measuring the relationship between these two components is one of the main goals of this proposal. The relatively small angular separations of the expected emission in these disks (~0.5") necessitates the use of PSF subtraction techniques in order to reasonably expect a detection. We therefore use three orbits per target: two orbits at different telescope ORIENT positions separated from each other by 30 degrees, and one orbit for a reference star. The first two roll-orbits allow for basic angular differential imaging PSF subtraction while building signal to noise in a given disk, and the third orbit is required to mitigate self-subtraction of the disk in order to recover its true morphology. This multi-roll-plus-reference-star PSF subtraction strategy is well established and has led to many successfully imaged disks (e.g. Schneider et al., 2014). In each case the ORIENTs are assigned using the disk's known position angle such that the disk does not fall behind either a diffraction spike or the BAR5 finger itself. The three reference stars for this program are RAVE-J161322.1-192417, UCAC2- 24134747 and 2MASS-J16150856-1851009 - one for each target. Each reference star was chosen to match the B-V color, the Vmag and the position in the sky as close as possible. Planets and Planet Formation 6 false false false false false false false SUPPORTED STAR DISK This object was generated by the targetselector and retrieved from the SIMBAD database. Position angle of disk around 2MASS J16123916-1859284 (T64-6) PA = 105 (+11 -11) 2MASS-J16123916-1859284 J2000 J2000 STAR M V-IV This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No BAR5 Timing link suitability includes constraints ([Sequence (07 09 10) within 0.2 days]) The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. /private/var/folders/xt/qjmnp0112nl6r_37xv8_kg1c0000gn/T/OPVisit7616407761177000660.xml (Tic-Visit :proposal-id 15497 :visit-id "07" :proposal-version -1 :trans-version "20181130" :date "14-Dec-2018 13:39:45.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 110832 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15497 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15497 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2806 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([Sequence (07 09 10) within 0.2 days]) The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. /private/var/folders/xt/qjmnp0112nl6r_37xv8_kg1c0000gn/T/OPVisit5202049171834343183.xml (Tic-Visit :proposal-id 15497 :visit-id "09" :proposal-version -1 :trans-version "20181130" :date "14-Dec-2018 13:39:46.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 110832 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15497 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15497 :visit-id "09" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2806 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([Sequence (07 09 10) within 0.2 days]) The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. /private/var/folders/xt/qjmnp0112nl6r_37xv8_kg1c0000gn/T/OPVisit4514738190544012646.xml (Tic-Visit :proposal-id 15497 :visit-id "10" :proposal-version -1 :trans-version "20181130" :date "14-Dec-2018 13:39:46.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 110832 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15497 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15497 :visit-id "10" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2806 :al-overhead-at-end 0 :internal-dur-at-end 419 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 1 0