0Assigned ID: 1903
----- Attempting Submission 1 (Fri Apr 09 13:21:27 GMT 2021) -----FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browserFor the UVIS direct images, we placed a flash of 20 to mitigate CTE as guided by our contact scientist, though APT gives a warning refering to the presumably old number of 12.-863889538----- Attempting Submission 1 (Thu Jul 29 16:33:09 GMT 2021) -----UVIS flash set to 20 not 12.A Comparative Study of Planetary Atmospheres in Low-Metallicity EnvironmentsHST has completed a number of surveys for a wide range of exoplanets, enabling comparative planetology. In the dozens of planets studied thus far, clouds and hazes have been found to be prevalent, and are seen to hide spectroscopic features. The atmospheric properties of giant planets are expected to vary substantially as the compositions of their host stars change, and a host star's metallicity should be an excellent proxy for the composition of the protoplanetary disk from it formed. Giant planets which formed in sufficiently metal-poor environments should in principle show marked differences in their atmospheric properties. In particular, planets around metal-poor stars should have preferentially clearer atmospheres and stronger molecular features, as there is less refractory elements such as Mg or Fe to make condensate clouds. The gas-phase chemistry will also change as key volatile ratios like C/O change. However, to date no hot Jupiters orbiting metal-poor stars ([Fe/H] < -0.3) have been targeted by HST, with the vast majority found in metal-rich environments. Our program takes the next steps in comparative exoplanetology, targeting exoplants with reliably low stellar metallicities down to a new metal-poor extreme ([Fe/H] < -0.49). This will provide the very first comprehensive atmospheric constraints for planets around metal-poor stars, which can then be compared to the plentiful metal-rich sample. A detailed comparison of stellar abundances to the spectral features as seen in the planet could reveal correlations that provide new insights into the atmospheric chemistry of hot Jupiters, and new insights into the nature of the planet-star metallicity connection.To construct a broadband transmission spectrum, we need to observe our targets with both the WFC3 UVIS/G280 and IR/G141 grisms. That wavelength coverage provides maximum leverage to quantify the Rayleigh scattering slope, as the extinction and transit depths are expected to be very strong. The wavelength coverage provided by the instruments will be 0.2-0.8 um and 1.1- 1.7 um. Both grisms are necessary to simultaneously cover cloud scattering at short wavelengths plus Na, K, and the strongest H2O bands at longer wavelengths.
The observing strategy for transiting exoplanets consists of taking repeated exposures for the duration of each transit, plus time before and after the transits to establish the out-of-transit baseline flux. For each G141 transit, we will use the spatial scanning mode employing the strategies that have proven to be successful for past HST programs (e.g., GO-12473, 12473, 13467, and 13665). HAT-P-24 b requires five orbits per visit to optimally cover a transit event, while WASP-98 b with a shorter duration requires four orbits per visit.Prof. David Sing has significant experience and expertise in the setup and reduction of HST/WFC3 observations. 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.
Prof. Schlaufman in an expert in the use of stellar parameters to constrain planet formation and evolution, skills critical to the interpretation of these data.
Dr. Giovanni Bruno has expertise in WFC3 data reduction and and stellar spectra analysis.
Dr. Hannah Wakeford is an expert in WFC3 data reduction and in the modeling of clouds in transiting exoplanets.
Dr. Nathan Mayne and Jayesh Goyal are experts in 1D and 3D theoretical modeling of exoplanet atmospheres, skills that are needed to interpret these data.
Dr. Tom Evans and Jessica Spake are experts in WFC3 data reduction and in the interpretation of transit data.
Dr. Jeff Valenti and Henrique Reggiani are experts in stellar abundance analyses that will be needed to interpret these data.
Z. Rustamkulov and N. Allen are PhD students at JHU advised by Prof. Sing and are focusing their PhDs on the observations of transiting exoplanets.Exoplanets and Exoplanet Formation6falsefalsetruefalsefalsefalsefalseAVAILABLEEXT-STAREXTRA-SOLAR PLANETARY SYSTEMG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000J=11.691; H=11.295EXT-STAREXTRA-SOLAR PLANETARY SYSTEMF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database. F8J2000J2000J=10.797; H=10.589WFC3/UVISSpectroscopicNoNoG280WFC3/IRSpectroscopicNoNoG141WFC3/UVISSpectroscopicNoNoG280WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.(Tic-Visit
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)false40The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.
Longer wave reference image is to help detect any faint stars in the field of view, to help charaterize any contaminating spectra.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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 29.2.CASM was run in Phase II mode.(Tic-Visit
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SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.
Longer wave reference image is to help detect any faint stars in the field of view, to help charaterize any contaminating spectra.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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.Timing link suitability includes constraints ([04 After 03 by 0.1 to 0.1 days])Hst Same orient constraint links visits (03 04 05 06)The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.WFC3/G141 time series transit observations consisiting of four consecutive HST orbits. Visits WASP-98 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.1659662485000249.07999999999998(Tic-Visit
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)false10Direct filter image to assist with wavelength calibration. Image is only used to find the reference detctor possition. Filter chosen to be in G141 wavelength range and give high SNR in a short exposure.Timing link suitability includes constraints ([04 After 03 by 0.1 to 0.1 days] [05 After 04 by 0.1 to 0.1 days])Hst Same orient constraint links visits (03 04 05 06)The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.Second orbit of G102 transit. Must be scheduled directly after WASP-98 WFC3/G102 Orbit 1 (03).1659668198000249.07999999999998(Tic-Visit
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)true10The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.period updated from Literature with TESS transits164836933500095.74768563615089(Tic-Visit
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)false50The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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.period updated from Literature with TESS transits(Tic-Visit
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:date "29-Jul-2021 12:27:06.0"
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(Tic-Orbit
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(Tic-Orbit
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)false50The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.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=2100 and SIZEAXIS2=800 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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 29.2.CASM was run in Phase II mode.164923802500097.14927244146611(Tic-Visit
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:date "29-Jul-2021 12:27:10.0"
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:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 5
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 698016
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:coron NIL
)
(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
:proposal-id 16736
:visit-id "15"
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)false50The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.The 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, at an approximate XY position of (2048,1024).
SIZEAXIS1=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS1 and CENTERAXIS2 are used to center the subarray readout on the target spectrum, which will be displaced from the direct image of the target. The zeroth order is expected to be about 175 pixels above the target in Y, and about 100 pixels to the right of the target in X. Therefore we set CENTERAXIS1 = 2048+100 = 2148 and CENTERAXIS2 = 1024 + 176 = 1200.
We use FLASH=12 to meet the nominal count level. These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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=1500 and SIZEAXIS2=500 are used to minimize data volume, while CENTERAXIS2 is used to center the subarray readout on the target location. The latter is set to 1026, to place the vertical center of the subarray on chip 2 where the target is positioned at (2048,1026) -50" in y below the nominal aperture (assuming each pixel = 0.04"). \These parameters are based upon similar observations obtained successfully in proposal 13574.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.Timing link suitability includes constraints ([11 After 10 by 0.1 to 0.1 days])Hst Same orient constraint links visits (10 11 12 13 14)The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode./private/var/folders/8t/mg1bkfyj20xf2vfc_9vyhfs80006z1/T/OPVisit724561903190370508.xmlWFC3/G141 time series transit observations consisiting of four consecutive HST orbits. Visits HAT-P-24 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.
Orientation requirements are placed to avoid a nearby fainter red companion, located about 5" south of the target and visible in a SDSS image. PA of the comanion is 189.45 degrees.(Tic-Visit
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:date "23-Aug-2022 15:15:50.0"
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)true10Direct filter image to assist with wavelength calibration. Image is only used to find the reference detctor possition. Filter chosen to be in G141 wavelength range and give high SNR in a short exposure.Timing link suitability includes constraints ([11 After 10 by 0.1 to 0.1 days] [12 After 11 by 0.1 to 0.1 days])Hst Same orient constraint links visits (10 11 12 13 14)The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Second orbit of G141 transit. Must be scheduled directly after HAT-P-24 WFC3/G102 Orbit 1 (10).(Tic-Visit
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(Tic-Obset
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)true10Timing link suitability includes constraints ([12 After 11 by 0.1 to 0.1 days] [13 After 12 by 0.1 to 0.1 days])Hst Same orient constraint links visits (10 11 12 13 14)The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Third orbit of G141 transit. Must be scheduled directly after HAT-P-24 WFC3/G102 Orbit 2 (12).(Tic-Visit
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:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 134416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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(Tic-Orbit
:proposal-id 16736
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:low-sky "N"
:pcs-visibility 2927
:pcs-gap 0
)true10Timing link suitability includes constraints ([13 After 12 by 0.1 to 0.1 days] [14 After 13 by 0.1 to 0.1 days])Hst Same orient constraint links visits (10 11 12 13 14)The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Fourth orbit of G141 transit. Must be scheduled directly after WASP-98 WFC3/G102 Orbit 3 (13).(Tic-Visit
:proposal-id 16736
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:proposal-version -1
:trans-version "20210514"
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 134416
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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(Tic-Orbit
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:pcs-gap 0
)true10Timing link suitability includes constraints ([14 After 13 by 0.1 to 0.1 days])Hst Same orient constraint links visits (10 11 12 13 14)The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.Fifth orbit of G141 transit. Must be scheduled directly after HAT-P-24 WFC3/G102 Orbit 3 (14).(Tic-Visit
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:trans-version "20210514"
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:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:saa-model "30"
:si-bright-earth-limb-angle 20.0
:data-volume 134416
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:coron NIL
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(Tic-Obset
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(Tic-Orbit
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)true10