0 Assigned ID: 703 ----- Attempting Submission 1 (Fri Apr 07 18:23:18 GMT 2017) ----- HST Phase I Proposal 703 (APT_HD34700.apt) successfully submitted. Receipt: # 703-1 ----- Attempting Submission 2 (Fri Apr 07 21:57:41 GMT 2017) ----- Modifications in this new submission: - HD 34700 acquisition image with ND3 filter 1.8 sec exposure time to avoid saturation - HD 34135 acquisition image with ND3 filter 0.9 sec exposure time to avoid saturation - HD 34700 science image with BAR5 36 sec exposure time (instead of 42 sec) to avoid saturation - HD 34135 science image with BAR5 18 sec exposure time (instead of 21 sec) to avoid saturation - Decreasing exposure time of science images with the wedgeA1.0 to compensate for the time increase -712991104 ----- Attempting Submission 1 (Thu Jul 20 00:28:20 GMT 2017) ----- HST Phase II Proposal 15295 (HD34700_PHASE2_JHD_V6.apt) successfully submitted. Receipt: # 15295-1 ----- Attempting Submission 2 (Thu Jul 20 10:09:51 GMT 2017) ----- HST Phase II Proposal 15295 (HD34700_PHASE2_JHD_V7.apt) successfully submitted. Receipt: # 15295-2 ----- Attempting Submission 3 (Thu Jul 20 13:15:34 GMT 2017) ----- HST Phase II Proposal 15295 (HD34700_PHASE2_JHD_V8.pdf.apt) successfully submitted. Receipt: # 15295-3 ----- Attempting Submission 4 (Thu Jul 20 20:01:24 GMT 2017) ----- ----- Attempting Submission 5 (Fri Nov 03 04:48:43 GMT 2017) ----- We propose to use four orbits of HST/STIS coronagraphy with the bent finger occulter (BAR5) to image the circumbinary disk around the spectroscopic binary HD 34700. This disk was recently discovered by our team both with NICMOS and Keck-NIRC2 in the IR. We propose to probe it, for the first time in visible scattered light, down to as close as 0.2'' (65 AU). HD 34700 has an eccentric 23-day orbit and may resemble the birth environment of circumbinary planets like the ones discovered by the Kepler mission. The eccentricity of the binary and the possible presence of additional companions make HD 34700 a unique testbed for studies of perturbed disk evolution. Previous observations by our team in the infrared show evidence for asymmetric features in both the inner and outer part of the disk. Possible interpretation is the presence of streamers and at least one spiral arm. New observations of this disk are required to confirm the nature and the cause of these features. Are they the result of stellar interactions, forming planets, or gravitational instabilities? We will probe the disk at high fidelity, with the goal of discriminating between these possibilities. We will look for signs of planet-disk interaction, with the aim to better understand the birth environment of dynamically extreme planetary systems. These observations are essential to unveil the very nature of this disk and will provide an anchor for future exploration with JWST and ALMA. We propose to follow the same overall strategy that has been successfully implemented in other programs that have dealt with the high-contrast imaging of circumstellar disks, namely a series of four total orbits that images the disk at three separate spacecraft orientations while also using a spectrally matched PSF reference star. We emphasize that the spectroscopic binary will not be resolved and thus for all practical coronagraphic considerations, the system is effectively a single star. Multiple orientations are required to realize the full potential of STIS high-contrast imaging. As demonstrated for previous STIS observations, a non-negligible fraction of azimuthal coverage in the disk is blocked by the stellar diffraction spikes and occulting wedges. The near face-on nature of the system does require 3 orients for full azimuthal coverage. We plan observations at 3 orientations oriented at 0 degree, +30 degrees, -30 degrees in roll. Relatively loose absolute orientation constraints will be specified to position the outer disks faint features near orthogonal to the STIS occulting wedge in the 0 degree visit. We will also obtain contemporaneously color-matched reference star observed in the same manner at one orientation for speckle calibration. The 3 observations of the target plus the reference star require 4 orbits total. Planets and Planet Formation 6 false false false false false false AVAILABLE STAR CIRCUMSTELLAR MATTER DISK PRE-MAIN SEQUENCE STAR PROTOPLANETARY DISK SPIRAL ARM NO This object was generated by the target selector and retrieved from the SIMBAD database. Manual update of coordinates precision values using Simbad. Manual entry of Proper Motion values using Simbad. Manual entry of Annual Parallax value using Gaia catalog. Manual entry of V-Magnitude error. Changed Reference Frame from Simbad to ICRS. HIP-24855 J2000 J2000 STAR F3-F9 NO This object was generated by the targetselector and retrieved from the SIMBAD database. Manual entry Proper Motion values using Simbad. Manual entry of Epoch. Manual entry of Annual Parallax Manual entry of V Magnitude error Changed Reference Frame from Simbad to ICRS HIP-24510-CALIB J2000 J2000 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No WEDGEA1.0 STIS/CCD Imaging Yes No BAR5 STIS/CCD Imaging Yes No WEDGEA1.0 Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1509683951764 /Users/mygouf/Documents/6-Caltech/2-Travail/3-Proposals/2017_HST/PhaseII/APT/APT_file_John_Version/Second_Submission_updated_exposure_times/OP-cache/HD34700_PHASE2_JHD_V11-v01.xml HD 34700 (V=9.15, B-V=0.638) First of three visits of HD 34700. Each of the three visits will be done at different relative orientations with one PSF calibration observation interleaved. This is the first HD 34700 visit. The four visits (HD 34700 + PSF calibration) must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (1) at a relative angle of -30 from visit (2). We allow a relative orientation tolerence from -30 deg to -15 deg to assist in guide star selection and scheduling. Relative Timing: This visit (1) should immediately preceed visit (2). I.e., They should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 15295 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "02-Nov-2017 21:39:10.0" :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 46992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15295 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15295 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2700 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 1 0 F25ND3 Aperture Exposure time needed to obtain a S/N ratio of 100 Kurucz Model G2V 5860 4.4 vegamag = 9.15 Requested Signal/Noise Ratio = 100.000 gives: Time = 1.78 seconds Time to Saturation (for a single exposure) = 49.55 seconds => so to get signal to noise ratio of 100, need 1.8 seconds exposure time Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 36s. Here we use the WEDGE1.0 occulter (Aperture). We then use a SIZEAXIS2 = 427. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 396s. Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days] [03 After 02 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1509683956204 /Users/mygouf/Documents/6-Caltech/2-Travail/3-Proposals/2017_HST/PhaseII/APT/APT_file_John_Version/Second_Submission_updated_exposure_times/OP-cache/HD34700_PHASE2_JHD_V11-v02.xml HD 34700 (V=9.15, B-V=0.638) Second of three visits of HD 34700. Each of the three visits will be done at different relative orientations with one PSF calibration observation interleaved. This is the second HD 34700 visit. The four visits (HD 34700 + PSF calibration) must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (2) at an absolute orientation 5 deg. We allow an absolute orientation tolerance from 330 deg to 30 deg to assist in guide star selection and scheduling. The orientation is constrained by the program goal which is to confirm the presence of spiral arms in the disk. With this absolute constraint, we ensure that the features previously identified with NICMOS don't fall under the wedge or the diffraction pattern. Relative Timing: This visit (2) should immediately follow Visit 1 and immediately preceed Visit 3 in back-to-back orbits. (Tic-Visit :proposal-id 15295 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "02-Nov-2017 21:39:15.0" :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 46992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15295 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15295 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2700 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 1 0 F25ND3 Aperture Exposure time needed to obtain a S/N ratio of 100 Kurucz Model G2V 5860 4.4 vegamag = 9.15 Requested Signal/Noise Ratio = 100.000 gives: Time = 1.78 seconds Time to Saturation (for a single exposure) = 49.55 seconds => so to get signal to noise ratio of 100, need 1.8 seconds exposure time Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 36s. Here we use the WEDGE1.0 occulter (Aperture). We then use a SIZEAXIS2 = 427. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 396s. Timing link suitability includes constraints ([03 After 02 by 0.0 to 0.1 days] [04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1509683963020 /Users/mygouf/Documents/6-Caltech/2-Travail/3-Proposals/2017_HST/PhaseII/APT/APT_file_John_Version/Second_Submission_updated_exposure_times/OP-cache/HD34700_PHASE2_JHD_V11-v03.xml PSF (HD 34135). PSF calibration target for HD 34700. V = 8.37 B - V = +0.5 Spec Type F5 This is the PSF star calibrator for the flanking visits (1-4). We levy no orientation constraints on this visit (3). However, we choose this target since it has been used in the past for our HD 34700 observations with Keck. So as Visits 2 and 3 must be scheduled in sequential contiguous orbits, if scheduled at nominal roll (as we expect also Visit 2 will be) then we expect absolute orientations of Visits 2 and 3 to be very similar (within a few degrees). This is important so we maintain similar Sun and Beta angles for the science target and its PSF calibrator. Relative Timing: This visit (3) should immediately follow visit 2 and immediately precede visit 4. I.e., they should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 15295 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "02-Nov-2017 21:39:21.0" :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 76704 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15295 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15295 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2645 :al-overhead-at-end 0 :internal-dur-at-end 383 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 1 0 F25ND3 Aperture Exposure time needed to obtain a S/N ratio of 100 Kurucz Model F5V 6440 4.3 vegamag = 8.37 Requested Signal/Noise Ratio = 100.000 gives: Time = 0.92 seconds Time to Saturation (for a single exposure) = 24.65 seconds => so to get signal to noise ratio of 100, need 0.9 seconds exposure time Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. Reference psf is V=8.37. We expect to hit 80% full well in 18s. We choose 3x1 dither pattern perpendicular to BAR5 position to mitigate centering mismatches. Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. Reference psf is V=8.37. We expect to hit 80% full well in 18s. We choose 3x1 dither pattern perpendicular to BAR5 position to mitigate centering mismatches. Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. Reference psf is V=8.37. We expect to hit 80% full well in 18s. We choose 3x1 dither pattern perpendicular to BAR5 position to mitigate centering mismatches. Here we use the WEDGE1.0 occulter (Aperture). We then use a SIZEAXIS2 = 427. We expect to hit 80% full well in 198 sec for the reference PSF. Timing link suitability includes constraints ([04 After 03 by 0.0 to 0.1 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. 1509683967163 /Users/mygouf/Documents/6-Caltech/2-Travail/3-Proposals/2017_HST/PhaseII/APT/APT_file_John_Version/Second_Submission_updated_exposure_times/OP-cache/HD34700_PHASE2_JHD_V11-v04.xml HD 34700 (V=9.15, B-V=0.638) Third of three visits of HD 34700. Each of the three visits will be done at different relative orientations with one PSF calibration observation interleaved. This is the third HD 34700 visit. The four visits (HD 34700 + PSF calibration) must be executed sequentally in contiguous orbits interrupted only for Earth occultation. Orientation: We wish to schedule this visit (4) at a relative angle of 30 from visit (2). We allow a relative orientation tolerence from 15 deg to 30 deg to assist in guide star selection and scheduling. Relative Timing: This visit (4) should immediately follow Visit 3. I.e., They should be executed sequentially in "back-to-back" orbits. (Tic-Visit :proposal-id 15295 :visit-id "04" :proposal-version -1 :trans-version "20170613" :date "02-Nov-2017 21:39:26.0" :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 46992 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15295 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15295 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2700 :al-overhead-at-end 0 :internal-dur-at-end 351 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 1 0 F25ND3 Aperture Exposure time needed to obtain a S/N ratio of 100 Kurucz Model G2V 5860 4.4 vegamag = 9.15 Requested Signal/Noise Ratio = 100.000 gives: Time = 1.78 seconds Time to Saturation (for a single exposure) = 49.55 seconds => so to get signal to noise ratio of 100, need 1.8 seconds exposure time Here we use the BAR5 occulter (Aperture). He we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 36s. Here we use the WEDGE1.0 occulter (Aperture). We then use a SIZEAXIS2 = 427. SCALABLE BENCHMARK: 14426 reached ~80% full well in 0.2s for a V=3.6 F star. G0V is close in SED to this, and target is V=9.15. We expect to hit 80% full well in 396s.