Final version -2017274866 Assigned ID: 1113 ----- Attempting Submission 1 (Wed Feb 27 05:25:28 GMT 2013) ----- HST Phase I Proposal 1113 (phase1.apt) successfully submitted. ----- Attempting Submission 2 (Fri Mar 01 23:06:05 GMT 2013) ----- This is a new submission of the APT file that Amber has confirmed. Thank you! 1402663295 ----- Attempting Submission 1 (Thu Jun 27 18:46:16 GMT 2013) ----- ----- Attempting Submission 2 (Wed Feb 12 15:33:00 GMT 2014) ----- ----- Attempting Submission 3 (Fri Feb 21 20:55:58 GMT 2014) ----- We propose to use the WFC3 IR-G141 grism to measure the near-IR dayside emission spectrum of the highly inflated, hottest known Jupiter KOI-13.01 via secondary eclipses. The A-type host star of KOI-13.01 has the highest temperature among all known hot Jupiter hosts, producing extreme irradiation and making the planet's atmosphere probably quite different from others'. It is therefore an extreme and unique target to test exoplanetary atmosphere models and observed correlation between thermal inversion and irradiation. The host star of KOI-13.01 has a companion of same brightness and spectral type at 1.2 arcsec. Because the two stars will be well-resolved by WFC3, the stellar companion provides a unique advantage to calibrate the common-mode systematics of the eclipse light curves, enabling high precision and high fidelity spectroscopy of the planet's dayside emission. The WFC3 observations will definitively determine the presence or absence of a thermal inversion in the planet's upper atmosphere by probing the water bands between 1.1 - 1.7 microns. When combined with the Kepler nightside thermal emission measurement in visible light, the near-IR spectroscopy from WFC3 will also help tightly constrain its albedo and heat transport efficiency. Furthermore, resolving the binary and measuring the secondary eclipses will allow us to definitively verify whether the brigher star is indeed the host of the planet. This study can only be done with HST because of the ultra-high precision requisite and the coverage of water bands unavailable from ground. We will use the WFC3 IR camera and the G141 grism to provide slitless spectroscopy at wavelengths from 1.1 to 1.7 microns. We will use the 256x256 pixel subarray mode to reduce both readout time and data volume to minimize overhead and the time loss due to serial buffer dumps. To well separate the two stellar spectra on the detector, we will orient the roll angle of the spacecraft so that the Y axis (the direction perpendicular to the dispersion of the WFC3 IR camera) to lie within 15 degree of the maximum separation of the two stars, PA=100.45 degree. This will allow a 4-month window for scheduling each year since the +/-180 degree options will work too. We will conduct observations of KOI-13 under "staring" mode without dithering or scanning to minimize systematics caused by imperfect flat fielding. We will follow the recommendation by STScI to apply a wavelength-dependent flat field correction later on in our data analysis. Due to the constraints of available multiaccum readout modes and the nonlinearity limit of the WFC3 detector, we carefully selected SPARS10 with two sample images (NSAMP=2) per exposure (t=7.624s) to readout the detector, based on estimates from the WFC3 IR Exposure Time Calculator (ETC). This mode allows us to maximize the S/N of each exposure and the overall duty cycle of our observations. Cosmic rays will be rejected using adjacent exposures instead of the samples within each exposure - an approach widely used in CCD spectroscopy. Since the eclipse duration of KOI-13.01 is 3.1 hours, we will require 3 orbits to fully cover the ingress, full-eclipse, and the egress part of each secondary eclipse. One orbit is required to cover the pre-eclipse baseline, and another orbit is required to cover the post-eclipse baseline. Due to the nature of planetary transits and eclipses, our proposed observations are only available at certain time windows when the planet passes behind its host star (P ~ 1.76 days). To achieve our science goal, we require 1 orbit to cover the pre-eclipse baseline, and 1 orbit to cover the post-eclipse baseline. We also require 3 orbits to fully cover the ingress, full-eclipse, and the egress part of each secondary eclipse. Therefore, our observations are time critical. Each visit should consist of 5 SAA-free (or hidden) and consecutive HST orbits. To put the two stellar spectra close to their maximum separation on the detector, we will need to constrain the roll angle of the spacecraft in a +/-15 degree window relative to an ORIENT angle of 235.82 degrees. This will add additional constraints and will allow a scheduling window of 4 months each year. EXTRA-SOLAR PLANETS Default false false false false false SUPPORTED STAR A0-A3 V-IV EXTRA-SOLAR PLANET This object was generated by the target selector and retrieved from the SIMBAD database. This is a double star system, with a separation of about 1.2 arcsecond. BD+46-2629 2MASS-J19075308+4652061 J2000 J2000 WFC3/IR Spectroscopic No No G141 1393015626384 The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. Our observations are time critical. To reach our science goal, we require 1 orbit to cover the pre-eclispe baseline, and another 1 orbit to cover the post-eclipse baseline. We will need 3 orbits to fully cover both the ingress, full-eclipse, and egress part of the light curve. The eclipse duration of KOI-13.01 is 3.1 hours. Each visit must consist of 5 SAA-free (or hidden) and consecutive HST orbits. For wavelength calibration purpose, we require one direct, un-dispersed image to be taken at the beginning of each visit, followed by consecutive grism exposures throughout the visit. The position of the targets in the un-dispersed image should be the same as the grism exposures. 1398697174000 243.82 (Tic-Visit :proposal-id 13308 :visit-id "01" :proposal-version -1 :trans-version "20131031" :date "21-Feb-2014 15:46:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1818080 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13308 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 13308 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 13308 :visit-id "01" :obset-id "B1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13308 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2659 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 479 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) false 5 0 All exposures in a visit must be conducted consecutively and SAA-free (or hidden). Exposure 2 & 3 must be conducted consecutively following Exposure 1. Exposure 2 & 3 must be conducted consecutively following Exposure 1. Exposure 2 & 3 must be conducted consecutively following Exposure 1. 1393015853369 The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. Our observations are time critical. To reach our science goal, we require 1 orbit to cover the pre-eclispe baseline, and another 1 orbit to cover the post-eclipse baseline. We will need 3 orbits to fully cover both the ingress, full-eclipse, and egress part of the light curve. The the eclipse duration of KOI-13.01 is 3.1 hours. Each visit must consist of 5 SAA-free (or hidden) and consecutive HST orbits. For wavelength calibration purpose, we require one direct, un-dispersed image to be taken at the beginning of each visit, followed by consecutive grism exposures throughout the visit. The position of the targets in the un-dispersed image should be the same as the grism exposures. (Tic-Visit :proposal-id 13308 :visit-id "02" :proposal-version -1 :trans-version "20131031" :date "21-Feb-2014 15:50:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "30" :si-bright-earth-limb-angle 20.0 :data-volume 1818080 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13308 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 13308 :visit-id "02" :obset-id "A2" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 13308 :visit-id "02" :obset-id "B2" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13308 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2659 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 509 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13308 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2647 :al-overhead-at-end 0 :internal-dur-at-end 479 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3024 :pcs-gap 0 ) false 5 0 All exposures in a visit must be conducted consecutively and SAA-free (or hidden). Exposure 2 & 3 must be executed consecutively following Exposure 1. Exposure 2 & 3 must be executed consecutively following Exposure 1. Exposure 2 & 3 must be executed consecutively following Exposure 1.