We request a special early execution of the first of our FGS visits, in late July or early August 2013, i.e. before the beginning of Cycle 21. This causes an error in the verification of our "Observation 5", as the observability of the object cannot be checked properly by the system. We justified carefully this special request in our proposal (Sect. "Special Requirements"). 2120833922 Assigned ID: 1204 ----- Attempting Submission 1 (Thu Feb 28 09:42:15 GMT 2013) ----- HST Phase I Proposal 1204 (V1334Cyg_v1.apt) successfully submitted. ----- Attempting Submission 2 (Thu Feb 28 17:42:39 GMT 2013) ----- HST Phase I Proposal 1204 (V1334Cyg_v2.apt) successfully submitted. ----- Attempting Submission 3 (Sat Mar 02 14:05:50 GMT 2013) ----- HST Phase I Proposal 1204 (V1334Cyg_v2.apt) successfully submitted. We request a special early execution of the first of our FGS visits, in late July or early August 2013, i.e. before the beginning of Cycle 21. This causes an error in the verification of our "Observation 5", as the observability of the object cannot be checked properly by the system. We justified carefully this special request in our proposal (Sect. "Special Requirements"). FGS visits included. As usual, please ignore warning of short exposure times. 864354896 ----- Attempting Submission 1 (Wed Jun 12 15:43:39 GMT 2013) ----- ----- Attempting Submission 2 (Fri Jun 21 03:11:13 GMT 2013) ----- Please ignore FGS warning regarding short exposure times. The parallax and mass of the binary classical Cepheid V1334 Cyg V1334 Cyg is a short-period classical Cepheid, and the primary star ("A") of a binary system. Using the CHARA interferometer, we spatially resolved its companion ("B") for the first time at an angular separation of 8 mas (Gallenne et al. 2013). Our two epochs clearly show the orbital displacement of B on its 5.3-year orbit, relative to the Cepheid, with an astrometric accuracy of 30 microas. This observation opens the exciting opportunity to determine the orbital parallax of this system. Based on the existing long-term radial velocimetry of A, and our interferometric data, we already derived the main orbital parameters of the system. However, we face a degeneracy between the mass ratio of the two stars and the distance. We miss the radial velocity of B (V1334 Cyg is still an SB1) or the orbital trajectory of the Cepheid around the center-of-mass. To waive this degeneracy, we request FGS astrometry and STIS high resolution spectroscopy. The FGS observations will trace the apparent orbital trajectory of A on the sky (to 0.1 mas accuracy), and the high-resolution STIS spectroscopy will give us the radial velocity of B (to < 1 km/s). The spectral disentangling of A and B is impossible in the visible due to the high contrast between A and B in this wavelength domain. In the UV, the companion flux dominates the Cepheid, thanks to its early spectral type (~B5V), and the disentangling is a lot easier. Combining STIS and FGS with CHARA interferometry, our goal is to obtain in 3 years the parallax and mass of the Cepheid with an unbiased accuracy of 1%. This will set a solid fiducial point for the calibration of fundamental Cepheid relations (period-luminosity, mass-period,...). The STIS observations aim at obtaining the spectrum and deriving the radial velocity of the hot companion V1334 Cyg B (hereafter "B") of the Cepheid. Contrary to the visible domain, the spectrum of B dominates the composite spectrum in the UV. The observations themselves do not present a particular technical difficulty. They will be repeated every year for 3 years, once per cycle, starting in September 2014. The minimum radial velocity will occur in 2014, and the maximum radial velocity will occur in 2016. The FGS observations are scheduled yearly in late July/early August starting in 2013 for 4 epochs. This relatively tight constraing in observing date is intended to obtain observations with always the same parallax factor. As the first observing epoch will occur shortly before the start of Cycle 21 observations, we submitted a change request (reference number 74730) that was approved. COOL STARS 12 false true false false false AVAILABLE STAR B3-B5 V-IV CEPHEID COMPOSITE SPECTRAL TYPE F0-F2 J2000 FLAM(1400)=1e-11; FLAM(1565)=8.47e-11; FLAM(2365)=4.90e-12 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 CALIBRATION ASTROMETRIC J2000 STIS/FUV-MAMA Spectroscopic No No E140H 1271 STIS/FUV-MAMA Spectroscopic No No E140H 1271 STIS/FUV-MAMA Spectroscopic No No E140H 1271 STIS/FUV-MAMA Spectroscopic No No E140H 1271 FGS POS No F5ND FGS POS No F5ND FGS POS No F5ND FGS POS No F5ND /private/var/folders/5n/j2_7w4n94ds83tmth7hz6_zm0005_1/T/OPVisit4594021625034040886.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13454 :visit-id "03" :proposal-version -1 :trans-version "20130502" :date "20-Jun-2013 23:09:35.0" :trans-errors '(:WARNINGS 34 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "05" :si-bright-earth-limb-angle 15.5 :data-volume 0 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13454 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13454 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2848 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0 /private/var/folders/5n/j2_7w4n94ds83tmth7hz6_zm0005_1/T/OPVisit6624861091770637968.xml The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 13454 :visit-id "04" :proposal-version -1 :trans-version "20130502" :date "20-Jun-2013 23:09:40.0" :trans-errors '(:WARNINGS 34 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "05" :si-bright-earth-limb-angle 15.5 :data-volume 0 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13454 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13454 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2844 :al-overhead-at-end 0 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0 Timing link suitability includes constraints ([02 After 01 by 1.0 to 3.0 days]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. /Users/nelan/Desktop/V1334Cyg-V2/OP-cache/13454-v02.xml Our adopted UV spectral energy distribution is based on the IUE low dispersion, large aperture observations SWP41795 and LWP20452. In the FUV, the contribution of the Cepheid itself is negligible, and the spectrum is dominated by the late-B star companion, with a flux at 1400 angstroms of about 1e-11 ergs/cm2/s/A. There are also two other SWP low dispersion, large aperture spectra, SWP08319 and SWP19267, taken at different epochs, which show essentially the same flux, so any significant FUV flux variability can be ruled out. Inserting our adopted spectral energy distribution into the ETC for the E140H 1271 with the 0.2X0.09 aperture gives a predicted global count rate of about 12500 c/s (ETC ID STIS.sp.466167). (Tic-Visit :proposal-id 13454 :visit-id "02" :proposal-version -1 :trans-version "20130502" :date "20-Jun-2013 22:52:50.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1358432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13454 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13454 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2941 :al-overhead-at-end 0 :internal-dur-at-end 808 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0 1271 (STIS.sp.466167) predicts global rate of about 12,500 Timing link suitability includes constraints ([02 After 01 by 1.0 to 3.0 days]) The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. /Users/nelan/Desktop/V1334Cyg-V2/OP-cache/13454-v01.xml Our adopted UV spectral energy distribution is based on the IUE low dispersion, large aperture observations SWP41795 and LWP20452. In the FUV, the contribution of the Cepheid itself is negligible, and the spectrum is dominated by the late-B star companion, with a flux at 1400 angstroms of about 1e-11 ergs/cm2/s/A. There are also two other SWP low dispersion, large aperture spectra, SWP08319 and SWP19267, taken at different epochs, which show essentially the same flux, so any significant FUV flux variability can be ruled out. Inserting our adopted spectral energy distribution into the ETC for the E140H 1271 with the 0.2X0.09 aperture gives a predicted global count rate of about 12500 c/s (ETC ID STIS.sp.466167). (Tic-Visit :proposal-id 13454 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "20-Jun-2013 22:52:52.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 1358432 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13454 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13454 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2941 :al-overhead-at-end 0 :internal-dur-at-end 808 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3287 :pcs-gap 0 ) true 1 0 1271 (STIS.sp.466167) predicts global rate of about 12,500