0Assigned ID: 249
----- Attempting Submission 1 (Thu Apr 04 19:38:12 GMT 2019) -----
HST Phase I Proposal 249 (epseri.apt) successfully submitted.
Receipt: # 249-1
----- Attempting Submission 2 (Thu Apr 04 20:25:18 GMT 2019) -----
HST Phase I Proposal 249 (epseri.apt) successfully submitted.
Receipt: # 249-2
----- Attempting Submission 3 (Thu Apr 04 20:33:52 GMT 2019) -----
HST Phase I Proposal 249 (epseri.apt) successfully submitted.
Receipt: # 249-3
----- Attempting Submission 4 (Fri Apr 05 16:24:35 GMT 2019) -----
HST Phase I Proposal 249 (epseri.apt) successfully submitted.
Receipt: # 249-4Unschedulable Visit
Unschedulable Visit
Unschedulable Visit
Unschedulable VisitSubmission 1 comment:
We request our PC, Beth Perillo, to schedule our observations in a way that Visit 1 and Visit 5 follow an
observation that is close in coordinates to our science target to minimize thermal slewing.
Re-planning following first epoch of observations:
We are re-planning our observations to integrate deeper and use a slightly wider coronagraphic wedge positions at WA/WB 2.5. Integration times have been adjusted accordingly.590426907----- Attempting Submission 1 (Tue Jul 16 20:49:24 GMT 2019) -----
----- Attempting Submission 2 (Fri Sep 11 16:21:19 GMT 2020) -----These visits have already been executed!Imaging planetary perturbations in the epsilon Eridani debris diskWith a Jupiter-like exoplanet in an orbit similar to that of Jupiter itself (Mawet et al. 2019) and an asteroid-analog belt just interior to it (Su et al. 2017), eps Eridani (0.8 Msun, 400-800 Myr old) has a fascinating resemblance to our expectations for a much younger Solar System. It also has an unusual intermediate debris belt, with characteristics deduced from modeling the spectral energy distribution of the entire star-plus-debris-disk system in the mid-infrared. This belt appears to extend over the region from ~ 8 to ~ 20 AU, corresponding to the orbits of Uranus and Neptune in the solar system, but it is currently unresolved. There is also an outer belt at ~ 60 AU seen in the far infrared and mm-wave. At a distance of only 3.2 pc, this system offers a unique opportunity to study an exoplanetary system at high physical resolution. We propose to image the intermediate and outer belts at high signal to noise and resolution of ~ 0.2 AU. The HST/STIS images will probe the gravitational influence of unseen planets on the intermediate and outer belts, and constrain the grain properties at these locations. The intermediate belt in particular is likely to be highly structured due to sculpting by unseen planets in orbits between that of the Jupiter-like one and the outer Kuiper-like belt. This study will test indirectly for the presence of planets far below our current limits for direct detection and substantially advance our understanding of debris disks in general, as well as revealing processes that may have shaped the early Solar System.Overview
===========================
We will observe epsilon Eridani and its PSF delta Eridani with our STIS coronagraphic program. The program uses 8 orbits, of which 6 will be used to take data of our target and 2 to observe the calibrator.
Our PSF calibrator, delta Eridani, has been used in prior programs as a calibrator for epsilon Eridani. It is a single star, without IR thermal excess, and spatially close to the star in the sky (<2.6 deg). Most importantly, the Delta(B-V) between the two stars is only around 0.04 mag. The two stars are close in stellar spectral type, therefore delta Eridani is the ideal PSF calibrator.
To minimize thermal slew at the beginning of our observing sequences (V1 and V5), we request our PC to schedule our observing sequences following an observing program relatively close in the sky (within 30 deg), ideally minimized.
Exposure details
===========================
Guide Star Acq: We require pointing and roll control with 2-FGS guiding. Single-FGS guiding does not offer sufficient target position stability for coronagraphy.
Each visit (after its Guide Star acquisition) begins with a mode-2 target acquisition and is followed by a sequence of exposures (by CR-SPLIT) at the WedgeA1.8 and WedgeB1.8 positions.
Target Acquisitions: We expose our TA images to a SNR of well over 100 using the STIS ETC. We also use the F25ND3 filtered images to photometrically obtain target:PSF template brightness ratios in the broad STIS passband. The STIS Target Acquisition ETC was used to determine the eposure times for all acquisition images. Further calculations are given in the exposure comments.
Exposure times: The exposure times are designed to reach ~80% of full-well depth (25,000 cts). The exposure times are based on GO 15217, which observed both stars at WA1.0. At 0.9'' from the star, the maximum count was ~ 5600 counts in 2.3 s for epsilon Eridani and similar count rate in 1.9 s for delta Eridani.
The orbits are filled completely. We integrate 2x7 CR-SPLIT images at both positions. The data are read-out at full frame imaging after 7 CR-SPLITS, hence the imaging methodology. To fill the orbits completely, we add an additional 3 CR-SPLIT image at the WEDGEA1.8 position.
Visits, links, and interlinked PSF observations
===========================
Epsilon Eridani and its matched PSF star (delta Eridani) is observed in two "sets" of four single-orbit visits (V1-V4 and V5-V8). Three visits are used to observe the science target in each set (V1, V2, and V4 [for the second set V5, V6, V8]), and one (each) the PSF star [V3 and V7]. These four visits within each set must be executed in sequential, contiguous orbits (i.e., back to back with no interruptions except Earth occultation).
The three science target visits in each set are at different RELATIVE orientation of *NOMINALLY* -30, 0, and +30 degrees from nominal roll, with the second science target observation at nominal roll. The 3rd orbit (visit) in each 4-visit set is of the PSF template star paired with the science target. The PSF template is very close in the sky to the science target (2.59 degrees). As a result we, anticipate that with scheduling of the second science orbit at nominal roll, the PSF calibration star will also be at or close to its nominal roll and usually these two orbits will have nearly the same celestial orientation angle.
The first "repeated" orbit (V5) should be scheduled at either a +90 deg or -90 deg relative orientation from the first (V1).
APT does not have the capability to specify allowable multiple (in this case two) relative orientations. Therefore, we advise our PC that although the parity of the first orbit in the second set's (V5) relative orientation was found schedulable by APT, if for some reason it turns out not to be, our PC may freely change the sign of this relative offset range from positive to negative (or vice versa). In doing so the signs on the relative orientations (and ranges if any) on the Visit V6 and V8 Orient Froms must also be changed in concert. Either positive or negative Orients From of appx |90| are acceptable on Visit V5, with corresponding sign changes on Visits V6 and V8.
-------- Realtime Justification --------
We have no real-time requirments.
------ Calibration Justification -------
We ask for no SPECIAL calibrations for this proposal (and called none out in Phase 1). We did not because we ASSUME that STScI will acquire GAIN=4 (supported mode) bias, DARK, and flat-field frames (and derived hot/bad pixel maps) as part of their Cycle 27 calibration plan in support of approved Cycle 27 science programs. If this is NOT the case then we must obtain GAIN=4 calibration reference bias/dark data as part of our program using NON-POINTED (internal) orbits only.
--------- Additional Comments ----------
NoneOur team consists of members with multiple years of experience observing and reducing HST data.
The PI, Andras Gaspar, led the program that enabled the BAR5 coronagraphic position of STIS and has been involved with many other HST programs. Aside from working on HST observations, he has been primarily involved in modeling the collisional evolution of debris disks. As a member of the MIRI and NIRCAM/JWST instrument teams, he leads two GTO programs, one of which will observe the epsilon Eridani system with MIRI.
Co-I Glenn Schneider has been working on the HST program since the 80's. He was a project instrument scientist on the NICMOS project and has since PI-d multiple programs to observe debris disks using STIS (e.g. Schneider et al. 2014).
Co-I Ewan Douglas has observed the epsilon Eridani with STIS last year.
Co-I George Rieke was the PI of MIPS aboard Spitzer and is the US Science Team lead of MIRI/JWST. He has multiple papers on Debris Disks and is an expert in the field.
Co-I Kate Su is an expert on the epsilon Eridani system (Su et al. 2017).
Co-I Nicholas Ballering is an expert on grain optical properties and HST data analysis (e.g., Ballering et al. 2016)
Co-Is Charles Beichman and Marie Ygouf are leading a NIRCam GTO program to observe the epsilon Eridani system.
Co-I Jarron Leisenring is also a member of the NIRCam and MIRI GTO programs and has extensive experience with high contrast imaging.Planets and Planet FormationSolar System6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARDISKG V-IVNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
GAIA DR2 source ID: 5164707970261630080J2000J2000CALIBRATIONPOINT SPREAD FUNCTIONNOThis object was generated by the targetselector and retrieved from the SIMBAD database.
GAIA DR2 source 5164120762332790528DELTA-ERIDANIJ2000J2000STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8STIS/CCDImagingYesNoWEDGEB1.8STIS/CCDImagingYesNoWEDGEA1.8Timing link suitability includes constraints ([02 After 01 by 0.0 to 0.1 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.1574272235000340.62(Tic-Visit
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)false10Saturation in 0.33 seconds. Will integrate to only 0.1 s. That should be enough.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.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 28.2.CASM was run in Phase II mode.15742779550003.6200000000000045(Tic-Visit
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)true10Saturation in 0.33 seconds. Will integrate to only 0.1 s. That should be enough.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.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 28.2.CASM was run in Phase II mode.157428370300021.88148345523399(Tic-Visit
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)true10Saturation in 0.27 seconds. Will integrate to only 0.1 s. That should be enough.Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.Timing link suitability includes constraints ([04 After 03 by 0.0 to 0.1 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.157428939600026.620000000000005(Tic-Visit
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)true10Saturation in 0.33 seconds. Will integrate to only 0.1 s. That should be enough.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.Timing link suitability includes constraints ([06 After 05 by 0.0 to 0.1 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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)false10Saturation in 0.33 seconds. Will integrate to only 0.1 s. That should be enough.Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Timing 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 28.2.CASM was run in Phase II mode.(Tic-Visit
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Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Timing 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 28.2.CASM was run in Phase II mode.(Tic-Visit
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)false10Saturation in 0.27 seconds. Will integrate to only 0.1 s. That should be enough.Original: Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of delta Eridani with Program ID 15217 at 0.9" have a peak of 5690 cts in 1.9 s. Scaled to 25,000 full well, we will be using an integration time of 8.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Timing link suitability includes constraints ([08 After 07 by 0.0 to 0.1 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.(Tic-Visit
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:pcs-visibility 3145
:pcs-gap 0
)false10Saturation in 0.33 seconds. Will integrate to only 0.1 s. That should be enough.Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72Original: Observations of epsilon Eridani with Program ID 15217 at 0.9" have a peak of 5600 cts in 2.3 s. Scaled to 25,000 full well, we will be using an integration time of 10.3 seconds per exposure.
Re-planning for WA/WB2.5: increased exposure factor X2.72