0 Assigned ID: 68 ----- Attempting Submission 1 (Tue Apr 08 13:21:58 GMT 2014) ----- INEFFICIENT ORDERING OF FP-POS POSITIONS For the best data quality, it is strongly recommended that all four FP-POS positions be used when observing at a given COS CENWAVE setting. Re-submission after a relaxation of the time constraints for the observations of WASP-13. The orbital period for WASP-13 has been only very slightly updated as well. -482069042 ----- Attempting Submission 1 (Tue Jul 15 12:21:43 GMT 2014) ----- ----- Attempting Submission 2 (Thu Sep 18 15:02:15 GMT 2014) ----- ----- Attempting Submission 3 (Tue Jan 06 14:07:19 GMT 2015) ----- - Warning concerning the WASP-18 observation cannot be currently solved - Warning concerning the FP-POS of the WASP-13 observation: due to the aim of the observations (measure of the planet transit) we have to use only one FP-POS. Ultraviolet HST observations have shown that atmospheric evaporation is a common feature of hot-Jupiters: highly irradiated (short-period) Jupiter-like planets. Models show that hot-Jupiters lose only a small fraction of their mass to evaporation but this may not be the case for extreme hot-Jupiters such as WASP-12b, which orbit very close to their host stars. Our Cycle 17 observations of WASP-12b showed that the planet atmosphere is evaporating and that gas escaping from the heavily irradiated planet may form a stable and thick circumstellar disk, causing an anomalously low stellar activity index. This anomaly does not allow us to correctly estimate the stellar UV flux, which drives the evaporation, from the available observational material. We request 6 HST orbits to obtain far-UV spectra of WASP-18 and WASP-13. Both stars host extreme hot-Jupiters, show an anomalously low activity index, and are much brighter than WASP-12, allowing one to obtain the necessary high quality far-UV spectra; WASP-12 is too faint at far-UV wavelengths to be measured by the instruments on-board HST. The data will allow us to improve the mass loss rates estimated for the most extreme hot-Jupiters as well as to resolve the ambiguity about the activity of the host stars in these systems. These data are necessary to correctly interpret the Cycle 17 HST observations, as well as observations of WASP-12b which have recently been obtained in Cycle-21. We will observe WASP-18 for 2 consecutive HST orbits and WASP-13 for 4 consecutive HST orbits to obtain FUV spectra of WASP-18 and WASP-13, respectively. The WASP-13 observations are timed with the planet transit: the hot-Jupiter WASP-13b passing in front of its parent star. The transit happens every 4.353 days and lasts about 4.08 hours. The WASP-13 observations aim at almost completely covering the planet transit. For the WASP-13 observations the timing requirements are set as phase constraints on the first acquisition (ACQ) exposure. The given phase is specified so that the first science exposure (1 science exposure is done during each orbit) falls integrally just before the ingress, the second and third science exposures occur during the transit, while the last science exposure occurs integrally just after the planet transit. Having the last exposure integrally after the transit is critical for the success of the program. The phase constraints given for the first orbit authorize a margin of about 4 minutes. Due to the fact that we aim at measuring the planet transit, we have set FP-POS=3, rather than equal to ALL. We submitted a Program Change Request for this (timed observations and use of one single FP-POS) which has been accepted (PCR 78372). No ACQ/PEAK is set because the coordinates of both targets are extremely precise. We will take two FUV spectra of WASP-18 and four FUV spectra of WASP-13 with the COS/FUV TIME-TAG mode using the G140L grating and the 1105 setting. WASP-18 is a late F-type main sequence star hosting a massive hot-Jupiter, while WASP-13 is an early G-type main sequence star hosting an extremely bloated and hot Saturn-mass planet. The spectrum will cover the 1118-2251 A spectral region with a spectral resolution R~2000. To calculate the exposure times of the science exposures we considered the CII lines at lambda~1335 A. We then considered the flux density of this multiplet as observed on the spectrum of alpha Cen and rescaled it to the distance of WASP-18 (100 pc) and WASP-13 (156 pc). EXTRA-SOLAR PLANETS Default false true false false false SUPPORTED STAR CIRCUMSTELLAR MATTER EXTRA-SOLAR PLANET F3-F9 This object was generated by the target selector and retrieved from the SIMBAD database. HD10069 HIP7562 J2000 J2000 CII emission line at 1334 A: estimated peak flux of 10^-15 erg A^-1 s^-1; GALEX FUV flux: 2.16x10^-15 erg A^-1 s^-1; GALEX NUV flux: saturated STAR CIRCUMSTELLAR MATTER EXTRA-SOLAR PLANET F3-F9 This object was generated by the target selector and retrieved from the SIMBAD database. TYC2496-1114-1 2MASSJ09202471+3352567 J2000 J2000 CII emission line at 1334 A: estimated peak flux of 4.3*10^-16 erg A^-1 s^-1; GALEX FUV flux: 1.9x10^-16 erg A^-1 s^-1; GALEX NUV flux: 5.0x10^-14 erg A^-1 s^-1 COS/FUV Spectroscopic No No G140L 1105 COS/FUV Spectroscopic No No G140L 1105 1420553219403 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. /tmp/OPVisit4718053335673128989.xml Two-orbit exposure on WASP-18 (Tic-Visit :proposal-id 13859 :visit-id "01" :proposal-version -1 :trans-version "20140605" :date "06-Jan-2015 15:06:59.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 87360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13859 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13859 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3015 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3358 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13859 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3135 :al-overhead-at-end 0 :internal-dur-at-end 366 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3358 :pcs-gap 0 ) true 2 0 Using the PSA aperture I got a total count rate which largely exceeds the bright limit: ETC Run # COS.ta.620288 /export/data2/lfossati/proposal/hst/cos_GO_apr14/Phase2/OP-cache/phase2-v02.xml 1420551842373 The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. Four-orbit exposure of WASP-13 timed with the planet transit. (Tic-Visit :proposal-id 13859 :visit-id "02" :proposal-version -1 :trans-version "20140605" :date "06-Jan-2015 14:44:01.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 156736 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13859 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13859 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2890 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13859 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13859 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13859 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3035 :al-overhead-at-end 0 :internal-dur-at-end 395 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) false 4 0 The exposure time is based on the GALEX magnitude of NUV_mag=15.57 HST Orbit 1 HST Orbit 2 HST Orbit 3 HST Orbit 4