0Assigned ID: 1141
----- Attempting Submission 1 (Fri Sep 27 17:38:08 GMT 2019) -----
HST Phase I Proposal 1141 (LTT1445A.apt) successfully submitted.
Receipt: # 1141-1
----- Attempting Submission 2 (Fri Sep 27 19:50:41 GMT 2019) -----
HST Phase I Proposal 1141 (LTT1445A.apt) successfully submitted.
Receipt: # 1141-2
----- Attempting Submission 3 (Fri Sep 27 20:05:50 GMT 2019) -----FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browser
FLASH level may be too low for this exposure or a short subexposure. See extended explanation in the diagnostic browserWe would like to request use of an Available mode for the UVIS G280 observations, which have been used in this submission to setup the UVIS observations.
The visits of the program are time series exoplanet transit observations, and require using a subarray such that the duty cycle and final signal-to-noise can be drastically
increased. The G141 and G102 visits use standard subarrays. For the UVIS visits, we employed sub-arrays as done in similar transit observations for GO15288 (PI Sing).
Ongoing analysis of the GO15288 data indicates that the use of the UVIS sub-arrays can produce near-photon limited precisions of 29 parts-per-million.
The subarray is specified by the SIZEAXIS and CENTERAXIS optional parameters, and we will use chip 2 as recommended in the instrument manual, which
was also used in GO15288.
01/06/2020 - ROYLE - Added technical requirement to visit 01 to better manage number of exposures
01/16/2020 - Sing - Changed all visits to schedulability 100, exposures reduced accordingly. Visit 1 which as previously four concecutive orbits was has divided into four consecutive visits (1, 2, 3, 4), which avoids buffer dumps occuring during the observation. The roll constraints on the UVIS visits (now 9 and 10) have been widened to increase scheduability.
02/10/2020 - Sing - Corrected Visits 6, 7 and 8 timing requirments. They were incorrectly linked to visits 1,2,3 but now are linked to visits 5, 6, 7. Visits 1 to 4 comparise of
one transit observations with 4 consecutive orbits in G141, while visits 5 to 8 comprise one transit observation with 4 consective orbits in G102.
10/14/2020 - Sing - Changed phase constraints for UVIS Visit 04 (10) such that the transit will occur in the second HST orbit. These phase contraints are shifted by one HST orbital period.
30/1/2023 - Sing - Swiched visits 55 to 58 to UVIS-2004191182----- Attempting Submission 1 (Thu Dec 05 14:44:32 GMT 2019) -----
----- Attempting Submission 2 (Mon Jan 06 15:25:38 GMT 2020) -----
----- Attempting Submission 3 (Thu Jan 16 16:28:41 GMT 2020) -----
----- Attempting Submission 4 (Mon Feb 10 16:44:47 GMT 2020) -----
----- Attempting Submission 5 (Wed Oct 14 19:56:09 GMT 2020) -----
----- Attempting Submission 6 (Mon Jan 30 15:40:05 GMT 2023) -----Orbit planner was run, but Visit planner didn't finnish on visit 59 after ~30 minutes, tried running a couple times.Characterizing the outstanding super-Earth LTT 1445AbTESS has recently discovered LTT 1445Ab, a small transiting exoplanet with a radius of only slightly larger than Earth. The planet orbits a mid-type M-dwarf star every 5.35 days, giving it a relatively cool equilibrium temperature of 433 K. The planet is very close to Earth, at a distance of only 6.9 pc, which makes it an extremely good target for atmospheric characterization due to the brightness of its host star and relatively large atmospheric signal. The planet is so close that it is likely the closest transiting planet that will ever be found around a mid-type M-dwarf, making it a rare case where a near-Earth size exoplanet can be characterized. Recent discoveries of water in the atmospheres around two similar planets in M-dwarf systems indicate many of these small transiting planets have hydrogen-rich atmospheres detectable with HST. Our program will measure HST/WFC3 spectroscopy of LTT 1445Ab to measure its broadband transmission spectrum from 0.3 to 1.7 microns. We will use the atmospheric information to help distinguish the exoplanet as a super-Earth with a compact secondary atmosphere from a hydrogen-rich sub-Neptune. With all three WFC3 grisms, a continuous transmission spectrum can be measured where Rayleigh scattering, CH4, and H2O can be constrained. The new, extraordinary planet LTT 1445Ab offers a rare chance to study a nearly Earth-sized exoplanet across the full optical to infrared spectrum, pushing these measurements to a largely unexplored regime of smaller, cooler exoplanets.This program uses all three UVIS and IR WFC3 slitless spectrographs to obtain an exoplanet transmission spectrum of LTT1445A covering 0.2 to 1.7 microns. Four transits observations are required, which consist of three or four consecutive HST orbits each. Phase constraints have been set in the aquisition image of each visit to observe the transit near the middle of the visits. A companion binary LTT1445BC is located 7" distant, and roll restrictions have been added such that the spectra will not overlap.
We will use the WFC3 G280 grism to obtain spectra covering 0.2 to 1 micron. We have estimated the exposure times using the STScI ETC, and will adopt 190 second exposures. As buffer dumps are an important issue with UVIS, we will use sub-arrays to increase duty cycle. Sub-array sizes of 590x2250 limits the overheads between exposures, and contains the entire useable spectrum as well as the binary BC pair. Using APT, we found 11 exposures-per-orbit can be obtained, and we will require 3-orbit long visits to measure both the transit and have sufficient baseline flux out of transit to characterize potential detector systematics.
The WFC3 IR uses spatial scanning to increase the SNR. The G141 uses a 5.1" scan at 0.53 arcsec/sec, with roll restrictions such that the LTT1445BC pair does not overlap the scan of target LTT1445A. The G102 uses a 6" scan at 0.2691 arcsec/sec, also with roll restrictions. The G102 was divided into four consecutive HST visits in order to force buffer dumps at the end of each orbit. For these four visits, timing requiremnts have been put in place such that they are exectued consecutively.
Impact of reduced gyro operations. Our WFC3/IR observations use spacial scanning, however the scans of both visits are less than 5 arsec/sec so reduced gyro operaion should have no effect on the ability to spactially scan. Two strategies can be employed to increase scheduablity. For both the IR and UVIS, the phase constraintes can be loosened by an additional 10 to 15 minutes with only a modest loss to SNR. Secondly, the roll constraints can be relaxed. The current roll restrictions of all visits are set to optimally separate the binary star such that the spectra do not overlap. For the UVIS, loostening up the high angle phase contraint first would be preferable as the contaminating spectra would affect primarly the -1 order, which has lower throughput. In loostening the roll restrictions in the IR observations, the binary star spectra could still be separted from the primary if the scan was shortened, or if the exposure levels and scan length was changed such that each star could be well resolved in a single Nsamp subexposure. This would likely result in a modest loss to the SNR.Prof. David Sing has significant experience and expertise in the setup and reduction of HST/WFC3 observations including both WFC3/UVIS and WFC3/IR. Prof. Sing is also an expert in exoplanet transit observations, leading many HST observing programs targeting transiting planets over the last 10 cycles. He has published 43 refereed papers over the last 12 years on HST-collected transiting exoplanet data. Prof. Sing has additional expertise in retrieval analyses of exoplanet atmosphere data.
Z. Rustamkulov is a PhD student at JHU advised by Prof. Sing and is focusing his PhD on the observations of transiting exoplanets.
Dr. Hannah Wakeford, J. Spake, and K Stevenson are experts in WFC3 data reduction in transiting exoplanets.
Prof. Nathan Mayne is an expert in 1D and 3D theoretical modeling of exoplanet atmospheres, skills that are needed to interpret these data.Planets and Planet Formation6falsefalsetruefalsefalsefalsefalseAVAILABLEEXT-STAREXTRA-SOLAR PLANETARY SYSTEMM V-IVWinters et al 2019 and Gaia DR2J2000J2000Ic = 8.66WFC3/UVISSpectroscopicNoNoG280WFC3/IRSpectroscopicNoNoG102WFC3/IRSpectroscopicNoNoG141Timing link suitability includes constraints ([02 After 01 by 0.1 to 0.1 days])Hst Same orient constraint links visits (01 02 03 04)The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.WFC3/G141 time series transit observations consisiting of four consecutive HST orbits. Visits LTT1145A WFC3/G141 1, 2, 3 and 4 must be scheduled consecutively. The visits have been broken up in APT to force a buffer dump at the end of each orbit, which drastically increases the duty cycle, which is important for time-series observations.
-7" offset has been applied such that the target spatial scan is near the middle of the 256 subarray. This provides room for a companion star to appear either above or below the target, depending on the roll angle.160999765200074.69402(Tic-Visit
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)false10Filter image to assist with wavelength calibration. Saturated, but the image is only used to find the reference detctor possition.For the target star, the Brightest Pixel (single exposure) is at 1.09 um with 50,192.06. BC binary pair together is slightly dimmer at G102 wavelengths, so the max counts will be slightly less. The scan of 6" will provideTiming link suitability includes constraints ([06 After 05 by 0.1 to 0.1 days] [07 After 06 by 0.1 to 0.1 days])Hst Same orient constraint links visits (05 06 07 08)The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.Second orbit of G102 transit. Must be scheduled directly after LTT1445A WFC3/G102 Orbit 1 (05).161092971500074.69402(Tic-Visit
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)true10The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.The optional parameters SIZEAXIS1=2250 and SIZEAXIS2=590 are used for all exposures to minimize the data volume and hence time lost to buffer dumps. This is fine for the data that needs to be obtained because the spectum of LTT1445A will occupy only a narrow swath of pixel rows within the field. This also requires the use of optional parameters CENTERAXIS1 and CENTERAXIS2 in order to "steer" the location of the subarray readout so that it is centered on the target spectrum. If we were positioning on chip 1 we could set CENTERAXIS2=TARGET. However, for the field center (nominal "UVIS" aperture) location on chip 2, we cannot center the subarray on the target because this would cause the subarray to extend into the chip gap, so we hardwire CENTERAXIS1=2136 and CENTERAXIS2=1216, which is intende to put the vertical center of the subarray on the zeroth order of the target spectrum.
Chip 2 biases are taken at the end of the visit because the grism exposures use custom subarrays, which will not have matching biases from the WFC3 bias calibration program.
For each visit we have phase constraints around the event of the planetary transit, both the orbital period of the planet and the phasing needed are placed on the first exposure in the sequence for each visit.
As this target has a potential binary star companion 7" away which can contaminate the spectra, we have placed Orient Ranges for the observations to reach our science goals.1601200794000290.2813466564468(Tic-Visit
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)false32Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration.The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.Idential to vist 3160768734800040.308059877962904(Tic-Visit
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)false32Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration.Copied from Visit 3, replaces G102 visits 55-58(Tic-Visit
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)false40Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.Nominal "UVIS" aperture is ~10" above the chip gap on chip 1; a Y-postarg of about -50" places the target near the center of subarray on chip 2.
SIZEAXIS1=2250 and SIZEAXIS2=590 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the zeroth order of G280 spectrum. These parameters are based upon similar observations obtained successfully in GOs 13574 & 15288 but have been adjusted to better center the zeroth order spectrum on the sub-array.
Exposure times of 191 seconds have been chosen to expose the region of interest (0.2 to 0.7 microns) to ~2/3 well depth. The ETC predicts that the star will saturate over four or five pixels of the spectra near 0.74 microns. As linearity for photometry holds to levels better than 1% generally for UVIS2 to well beyond saturation, we will simply sum over the few pixels that have been bled into as a result of over-saturation, as recomended in ISR-WFC3-2010-10. These longer integration times are prefereable over shorter exposure times, as the overall duty cycle and final SNR levels are higher.We set up the bias frames based on previously sucessful program 11934 and are using the same Aperture and subarray size and position as the observations for direct calibration.