0Assigned ID: 393
----- Attempting Submission 1 (Fri Apr 07 04:26:21 GMT 2017) -----
HST Phase I Proposal 393 (RSGs.apt) successfully submitted.
Receipt: # 393-1
----- Attempting Submission 2 (Fri Apr 07 19:00:57 GMT 2017) -----
HST Phase I Proposal 393 (RSGs.apt) successfully submitted.
Receipt: # 393-2
----- Attempting Submission 3 (Fri Apr 07 19:11:00 GMT 2017) -----
HST Phase I Proposal 393 (RSGs.apt) successfully submitted.
Receipt: # 393-3
----- Attempting Submission 4 (Fri Apr 07 21:08:35 GMT 2017) -----I have updated this Phase II so that all of my exposure for a given visit are in non-interruptible seq. containers, as suggested by John Debes. This ensures that the breathing and focus behavior within the linked visits are roughly similar from visit to visit, which should help to give optimal contrast.1087309670----- Attempting Submission 1 (Wed Jul 19 22:45:12 GMT 2017) -----
----- Attempting Submission 2 (Tue Sep 26 03:43:09 GMT 2017) -----High Fidelity Imaging of a Red Supergiant's Circumstellar MaterialIn young and low mass environments, where ABG stars have yet to form and WC stars are intrinsically rare, red supergiants (RSGs) are thought to be the main source of circumstellar dust due to their dusty winds. A recent discovery of large grains around VY CMa that will escape from the system before its central star becomes a SN has further strengthened this idea. At the same time, it is unclear what physical scenario is responsible for the large mass-loss rates of RSGs. Characterizing the morphologies of circumstellar material close to RSGs is likely the only way to distinguish between these scenarios. We have recently obtained high-contrast coronagraphic imagery of material around a RSG that appears to be viewed at a low inclination angle. Because of the observing techniques used by ground-based extreme adaptive optics systems to remove PSF residuals, much of the dust signal has likely been self-subtracted from our dataset. The only way to fully characterize the morphology of this material is to use the coronagraphic capabilities HST/STIS. Therefore, we ask for 8 orbits to obtain new imagery of this system using a previously proven high-fidelity coronagraphic imaging technique.In this porgram we plan to observe one red supergiant star (V-V384-PUP, spectral type of M2.5 I) in order to search for and image any dust forming in its stellar wind using STIS coronagraphy. Specifically, we plan to use the STIS BAR5 occulting apperature. In order to accomplish this, we also plan to observe one B-V color matching PSF star that is within ~15 degrees of our red supergiant science target.
Visit Structure
--------------------
Our observing strategy is to uses two sets of four consecutive visit each to observe V-V384-PUP at three different roll angles and our PSF star. There is no set timing between our two sets of visits, although there are relative orient constraints between them that affect when they can be scheduled. In particular, the first set of four consecutive visits can occur at any time and will include three visits of V-V384-PUP at three different orient angles: the nominal roll angle, the nominal roll angle +30 deg, and the nominal roll angle -30 deg. The fourth visit will be to collect data on a PSF star, which can be done at any orient. We will then repeat those four visits at additional orient angles such that a final mosaiced image of the entire area around V-V384-PUP can be created.
The optimal orient break down of our visits are as follows:
Visits 1 - 4 in Back-to-Back Orbits
------------------------------------------------------------------------------------
1 V-V384-PUP Orient from Visit 2 by -30 deg
2 V-V384-PUP Nominal (or other) Roll as Scheduled by STScI
3 PSF-STAR Nominal (or other) Roll as Scheduled by STScI
4 V-V384-PUP Orient from Visit 2 by +30 deg
Visits 5 - 8 in Back-to-Back Orbits
-------------------------------------------------------------------------------------
5 V-V384-PUP Orient from Visit 1 by +90 deg *OR* -90 deg*
6 V-V384-PUP Orient from Visit 5 by +30 deg
7 PSF-STAR Nominal (or other) Roll as Scheduled by STScI
8 V-V384-PUP Orient from Visit 5 by +60 deg
*We note that for Visit 5 both +90 deg and -90 deg orient angles relative to the orient of Visit 1 are acceptable, but we are unable to specify this in the current version of the APT. We have used +90 deg when linking the constraints of the observations to each other, but the PC is free to change this to -90 deg if needed for schedulling purposes.
We recognize that our relative 30 deg orientation differences might not always be possible, even though they are optimal for our science. We ask that our visits be scheduled with as close to the relative orientations that we outlined above, but have the following loose tolerances:
Loose tolerances in orient break down of our visits are as follows:
Visits 1 - 4 in Back-to-Back Orbits
------------------------------------------------------------------------------------
1 V-V384-PUP Orient from Visit 2 by -30 deg to -15 deg
2 V-V384-PUP Nominal (or other) Roll as Scheduled by STScI
3 PSF-STAR Nominal (or other) Roll as Scheduled by STScI
4 V-V384-PUP Orient from Visit 2 by +15 deg to +30 deg
Visits 5 - 8 in Back-to-Back Orbits
-------------------------------------------------------------------------------------
5 V-V384-PUP Orient from Visit 1 by +75 deg to +105 deg *OR* -105 deg* to -75 deg
6 V-V384-PUP Orient from Visit 5 by +15 to +30 deg
7 PSF-STAR Nominal (or other) Roll as Scheduled by STScI
8 V-V384-PUP Orient from Visit 5 by +45 deg to +60 deg
For each orbit we observe either our PSF star or V-V384-PUP and perform:
1) a cogronagraphic imaging target acquisition
2) a series of short exposure with BAR5
We dither by +/- 1/4 pixel above and below the mid-line of the BAR5 finger in sets of eight short images for most of the Visit. In order to fill as much observable time as possible during a Visit, a few of these dithers have only 3 or 4 subexposures.
BAR5 WITH POS TARGS for dithering
---------------------------------------------------------------------------------------------------------------------------------------------------
For BAR5 we use the following for dithering:
POS TARGs to effect a +/- 3 point dither centered on the bar as follows:
BAR10 with POSTARG 0.0024921, -0.0122491 (below mid-line of BAR5)
BAR10 with POSTARG 0.0, 0.0 (on mid-line of BAR5)
BAR10 with POSTARG 0.0024921, 0.0122491 (above mid-line of BAR5)Stellar Physics6falsefalsefalsefalsefalsefalseAVAILABLEEXT-STARCIRCUMSTELLAR MATTERM III-IThis object was generated by the targetselector and retrieved from the SIMBAD database.
B-V Color: 2.04J2000J2000STARUNDESIGNATEDThis object was generated by the targetselector and retrieved from the SIMBAD database.
PSF was chosen to be close in color to V-V384-PUP. This star's B-V is 2.05.
Magnitudes from Simbad are:
B 12.31 [0.23]
V 10.26 [0.04]
J 6.764 [0.024]
H 5.901 [0.042]
K 5.620 [0.027]
The spectral type for this star is unknown.J2000J2000STIS/CCDImagingYesNoBAR5STIS/CCDImagingYesNoBAR5STIS/CCDImagingYesNoBAR5STIS/CCDImagingYesNoBAR5Timing 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.This is the first visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient constraints: The optimal relative orient for this visit is -30 deg from Visit 2 and we ask that this visit is scheduled as close to that orient as possible. However, we allow for a relative orientation tolerance of -15 deg to -30 deg to assist in guide star selection and scheduleing.
Timing constraints: There is no specific timing constraint except that it needs to immediately preceed Visit 2. They should be scheduled in back-to-back orbits.1511607236000285.32477(Tic-Visit
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)true10V384 Pup: M2.5 I; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)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.This is the second visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).1511613045000301.5(Tic-Visit
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)true10V384 Pup: M2.5 I; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)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.This is the third visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient Constraints: NOTE TO OUR PC: Our PSF star visits (#3 and #7) have no absolute or relative orientation constraints. However, all other things being equal, when scheduled, we would request that both be observed with roll angles as close to Visit 2 as possible. This is not a hard requirement and we do not constrain, but a request this if possible to optimize the science return through likely better PSF calibration.
Timing Constraints: This visit should immediately proceed Visit 2. They should be in back-to-back orbits.1511618712000307.86280465367713(Tic-Visit
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)true10TYC 6551-975-1: unknown spectral type; assumed spectral type of M2V for exposure time calculation because SED appears to be M type like; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1010701
Exposure time created by exposure time calculator is consistent with scaling exposure time of V-V384-PUP to TYC 6551-975-1's brightness in V band.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of no CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)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.This is the fourth visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient Constraints: The optimal relative orient for this visit is +30 deg from Visit 2 and ask that this visit is scheduled as close to that orient as possible. However, we allow for a relative orientation tolerance of +15 deg to +30 deg to assist in guide star selection and scheduleing.
Timing Constraints: This visit should immediately proceed Visit 3. They should be in back-to-back orbits.1511624666000326.32477(Tic-Visit
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(Tic-Obset
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)true10V384 Pup: M2.5 I; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.This is the first visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient constraints: The optimal telative orient for this visit is +90 deg *or* -90 deg from Visit 1 and ask that this visit is scheduled as close to one of those orients as possible. However, we allow for a relative orientation tolerance of +75 deg to +105 deg or -75 deg to -105 deg to assist in guide star selection and scheduleing. We note that there is no way to specify that both relative orientaitons are acceptable.
Timing constraints: There is no specific timing constraint except that it needs to immediately preceed Visit 6. They should be scheduled in back-to-back orbits.(Tic-Visit
:proposal-id 15314
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:trans-version "20170613"
:date "25-Sep-2017 20:40:15.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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(Tic-Obset
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)false10V384 Pup: M2.5; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days] [07 After 06 by 0.0 to 0.1 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.This is the second visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient constraints: The optimal relative orient for this visit is +30 deg from Visit 5 and ask that this visit is scheduled as close to that orient as possible. However, we allow for a relative orientation tolerance of +15 deg to +30 deg to assist in guide star selection and scheduleing.
Timing constraints: There is no specific timing constraint except that it needs to immediately proceed Visit 5. They should be scheduled in back-to-back orbits.(Tic-Visit
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:trans-version "20170613"
:date "25-Sep-2017 20:40:20.0"
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(Tic-Obset
:proposal-id 15314
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)true10V384 Pup: M2.5; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)Timing link suitability includes constraints ([07 After 06 by 0.0 to 0.1 days] [08 After 07 by 0.0 to 0.1 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.This is the third visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient Constraints: NOTE TO OUR PC: Our PSF star visits (#3 and #7) have no absolute or relative orientation constraints. However, all other things being equal, when scheduled, we would request that both be observed with roll angles as close to Visit 6 as possible. This is not a hard requirement and we do not constrain, but a request this if possible to optimize the science return through likely better PSF calibration.
Timing constraints: There is no specific timing constraint except that it needs to immediately proceed Visit 6. They should be scheduled in back-to-back orbits.(Tic-Visit
:proposal-id 15314
:visit-id "07"
:proposal-version -1
:trans-version "20170613"
:date "25-Sep-2017 20:40:24.0"
: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 44832
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15314
:visit-id "07"
:obset-id "07"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15314
:visit-id "07"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2808
:al-overhead-at-end 0
:internal-dur-at-end 349
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3225
:pcs-gap 0
)true10TYC 6551-975-1: unknown spectral type; assumed spectral type of M2V for exposure time calculation because SED appears to be M type like; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1010701
Exposure time created by exposure time calculator is consistent with scaling exposure time of V-V384-PUP to TYC 6551-975-1's brightness in V band.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491).. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 73.5 seconds per exposure will yield 75% to saturation in the brightest pixel of TYC-6551-957-1. Our exposures are thus comprised of no CR-SPLITS in integral units of 73.5 second exposures. (Note: AU Mic is approximately 4.5 times brighter TYC-6551-957-1.)Timing link suitability includes constraints ([08 After 07 by 0.0 to 0.1 days])The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode.This is the fourth visit in a set of four that must all be conducted back to back (the four visits within each set must be executed sequentally in contiguous orbits interrupeted only by Earth occultation).
Orient constraints: The optimal relative orient for this visit is +60 deg from Visit 5 and ask that this visit is scheduled as close to that orient as possible. However, we allow for a relative orientation tolerance of +45 deg to +60 deg to assist in guide star selection and scheduleing.
Timing constraints: There is no specific timing constraint except that it needs to immediately proceed Visit 7. They should be scheduled in back-to-back orbits.(Tic-Visit
:proposal-id 15314
:visit-id "08"
:proposal-version -1
:trans-version "20170613"
:date "25-Sep-2017 20:40:27.0"
: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 105232
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 15314
:visit-id "08"
:obset-id "08"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 15314
:visit-id "08"
:orbit-number 1
:pcs-time 333
:si-vis-utilization 2880
:al-overhead-at-end 0
:internal-dur-at-end 339
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3240
:pcs-gap 0
)false10V384 Pup: M2.5; SNR+100; exposure time from STIS AQC ETC; ETC Request ID: STIS.ta.1009352NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target on the mid-line of BAR5. We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 3 CR-SPLITS in integral units of 18.4 second exposures.NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly above the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = 0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 8 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)NOTE TO PC/CS: Here we use the BAR5 occulter (Aperture) that was comissioned in GO program 12923. Here we attempt to place the target slightly below the mid-line of BAR5, using a 0.25 pixel dither perpendicular to the BAR5 long-axis (via POS TARG offsets of x = 0.0024921 arcsec and y = -0.0122491). We then use a subarray readout of CENTYERAXIS2 = 700 appopriate for BAR5 with a SIZEAXIS2 = 100 (the same that was used for GO program 13786)
SCALABLE BENCHMARK: We scale our exposure times from the end product result of the AU Mic observations in GO-12923. We expect that 18.4 seconds per exposure will yield 75% to saturation in the brightest pixel of V-V384-PUP. Our exposures are thus comprised of 4 CR-SPLITS in integral units of 18.4 second exposures. (Note: V-V384-PUP is approximately 10% dimmer than AU Mic.)