Final version. Note that I recalculated ORIENT and PHASE requirements, these might interfere with previously scheduled times. The PHASE requirement is in exposure 1 of each visit. ----- Attempting Submission 1 (Thu Jun 19 15:39:08 GMT 2008) ----- ----- Attempting Submission 2 (Sat Aug 15 04:09:32 GMT 2009) ----- ----- Attempting Submission 3 (Fri Oct 29 03:36:05 GMT 2010) ----- HST Phase II Proposal 11617 (hst.apt) successfully submitted. ----- Attempting Submission 4 (Sat Oct 30 23:57:48 GMT 2010) ----- Assigned ID: 710 ----- Attempting Submission 1 (Fri Mar 07 23:04:22 GMT 2008) ----- Target 2 is in the same field of view as Target 1. The two targets are to be observed simultaneously. HAT-P-1: A Direct Glimpse into the Atmosphere of a Hot Jupiter The HATNet project has discovered a transiting planet that is an extremely valuable target for reflected light observations (Bakos et al. 2006). HAT-P-1b, with mass M_p=0.53 +/- 0.04 M_Jup, and radius R_p=1.20 +/- 0.05 R_Jup (Winn et al. 2007), has a density comparable to that of HD 209458b. However, HAT-P-1b's P=4.46536 day orbital period is longer than that of HD 209458b. It is expected that the cloud composition and particulate size distribution of HAT-P-1b will differ from that of HD 209458b, due to the larger semimajor axis and lower effective temperature of HAT-P-1b. The resulting geometric albedo for HAT-P-1b should be larger than that of HD~209458b. Furthermore, HAT-P-1 orbits one component of a wide binary (ADS 16402A and ADS 16402B are G0V stars with 11.2" at 1.39 pc), making this an ideal target for ultra-precise differential photometry. Therefore, we propose ACS/HRC slitless grism photometry near times of its secondary eclipse to make the first detection of reflected light from an extrasolar planet. Note: this program was awarded DD time in Cycle 15 but the observations were not executed before the ACS failed. Holman and Bakos are co-PIs on this proposal.
10 orbits of STIS observations are used in two 5 orbit visits. High S/N observations with the G750L grism will be obtained in time series. The third and fourth orbits will be timed to coincide with secondary eclipse, while orbits two and five will be used to establish the out of eclipse intensity as the control. We conservatively assume that the first orbit will show the characteristic incorrigible systematic errors seen in other similar high S/N HST applications. To cover first order spectra and zeroth order image of both stars separated by 11.2 arcsec we can read out the central 380 columns, in slitless mode, detecting both spectra while leaving plenty of buffer on either side. The spectra obtained will be saturated in order to overcome the low duty cycle that for these bright objects would be associated with unsaturated spectra. Adopting times of 120s for G750L exposures, with 45s readout, allows 24 exposures per orbit. The brighter (10.0) star will be used as a photometric control for the target (10.4) star resulting in a net differential (eclipse to control orbits, and target to control star) precision per visit of 2e-5. We desire that the two visits be scheduled such that complementary phases are obtained to maximize overall phase coverage of the secondary eclipse. The initial submission uses a broad phase window. After possible scheduling windows have been identified we will select the best two. We would also like to add exposures to any orbits that are not full once the final scheduling windows have been identified. Initial submission with phase = 0.454 - 0.4633. This is a one hour wide window. At the center of this range, center of secondary eclipse would be half way between HST orbits 3 and 4, and ingress and egress would be within occultations. At the extrema of these ranges ingress would be up to 30 minutes before end of orbit 3, and egress could be up to 30 minutes into orbit 4. EXTRA-SOLAR PLANETS 12 false 0.0 0.0 false false false false false false AVAILABLE EXT-STAR G V-IV Photometric reference star. Other member of the binary is exoplanetary host star ADS-16402B a.k.a. HAT-P-1, offset by 11.5 arcsec. It is a 10.4 V-magnitude G0V star. Exact coordinates: 22 57 46.8250, +38 40 29.83. J2000 22 57 46.8250 +38 40 29.83 J2000 EXT-STAR G V-IV Pseudo target at the midpoint of the binary. Pointing here allows subarray readout. J2000 00 00 0.0000 +00 00 0.00 J2000 ACS/HRC Spectroscopic No No G800L ACS/HRC Spectroscopic No No G800L Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.456/0.463. The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. /tmp/OPVisit37476.xml First of two visits. The five orbits need to be scheduled contiguously and free of SAA interupts during visibility windows. (Tic-Visit :proposal-id 11617 :visit-id "01" :proposal-version -1 :trans-version "20100505" :date "30-Oct-2010 19:56:40.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1425712 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11617 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11617 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2929 :al-overhead-at-end 101 :internal-dur-at-end 2120 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) true 5 0 We first ACQ on one of the targets, then move the telescope in the midpoint of the two so that we can make subarray readouts. After ACQ, the telescope moves to the midpoint and we take this exposure to know the exact position of the stars along AXIS2, and have a good idea about the spectrum position too. Note that subarray readout width is still large enough to accomodate large pointing errors (e.g. if one of the binary stars stayed in the center), just in case (we gain 20 s as opposed to complete CCD readout, another 3 s would not be worth the risk). Phase windows are not calculated when the period is less than 7.0 days. Assuming no scheduling restrictions for Phase 0.456/0.463. The scheduling data was generated by CASM 18.3.1. CASM was run in Phase II mode. /tmp/OPVisit37477.xml Second of two visits. The five orbits need to be scheduled contiguously and free of SAA interupts during visibility windows. (Tic-Visit :proposal-id 11617 :visit-id "02" :proposal-version -1 :trans-version "20100505" :date "30-Oct-2010 19:57:08.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1425712 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11617 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11617 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2929 :al-overhead-at-end 101 :internal-dur-at-end 2120 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 2109 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11617 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2998 :al-overhead-at-end 101 :internal-dur-at-end 677 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3301 :pcs-gap 0 ) true 5 0 We first ACQ on one of the targets, then move the telescope in the midpoint of the two so that we can make subarray readouts. After ACQ, the telescope moves to the midpoint and we take this exposure to know the exact position of the stars along AXIS2, and have a good idea about the spectrum position too. Note that subarray readout width is still large enough to accomodate large pointing errors (e.g. if one of the binary stars stayed in the center), just in case (we gain 20 s as opposed to complete CCD readout, another 3 s would not be worth the risk).