0Assigned ID: 123
----- Attempting Submission 1 (Wed Apr 08 17:35:23 GMT 2015) -----
HST Phase I Proposal 123 (cep.mass.pdf.apt) successfully submitted.
Receipt: # 123-1
----- Attempting Submission 2 (Fri Apr 10 15:08:40 GMT 2015) -----Shortened lamp exposure times to 50 s for 1416 WAVECALS and 100 s for 1271 WAVECALS.
Adjusted buffer time in exposure 3 of visit 1 to allow a bit more margin.563302008----- Attempting Submission 1 (Mon Jul 20 16:24:04 GMT 2015) -----
HST Phase II Proposal 14194 (14194_phase2_draft2.apt) successfully submitted.
Receipt: # 14194-1
----- Attempting Submission 2 (Mon Jul 20 16:27:19 GMT 2015) -----
----- Attempting Submission 3 (Wed Sep 02 19:33:07 GMT 2015) -----Precision Masses and Distances of Classical CepheidsAn important HST UV legacy is the measurement of the masses of Cepheids. Recently optical interferometry with the Very Large Telescope Interferometer (VLTI) and CHARA has resolved a number of Cepheid binary systems, providing combined spectroscopic and visual orbits. In order to fully exploit this data, we are requesting HST high resolution E140H spectra of 4 Cepheid systems (AX Cir, AW Per, Y Car, and V636 Sco) to measure the orbital velocity amplitude of the hot companion, and thereby determine the mass ratio for the Cepheid--companion system (using the ground-based orbit of the Cepheid). The anticipated velocity accuracy from the STIS spectra will result in masses with uncertainties of 5 to 11\%. This will provide a definitive test of evolutionary track physics (specifically main sequence core convective overshoot), and also a comparison of the mass-luminosity relation at two metallicities (the Milky Way and the Large Magellanic cloud).Auto-wavecals will be turned off and replaced with deep wavecals at the beginning and end of each orbit. All but the first wavecal hide in the occultations and or guide-star re-acquisitions.
ACQ and ACQ/PEAK exposures will center on the Cepheid. Offset targets are defined for the expected position of the blue companions based on inteferemetric measurements by CoI A Gallenne.
Other than the initial ACQ, the exposures for each orbit are put into a non-interruptable sequence to ensure that the wavecals stay close in time to each bracketed science exposure.
AX CIR:
1 visit of 1 orbit
(1) Acquire target with 0.6s F28X52OIII ACQ exposure
(2) 0.2 s ACQ/PEAK with G430L and 0.2X0.09 aperture
(3) 120 s WAVE
(4) 2014 s E140H 1271
(5) 250 s WAVE
AW PER:
Two identical visits of 3 orbits each
First orbit:
(1) Acquire target with 0.2s F28X52OIII ACQ exposure
(2) 0.2 s ACQ/PEAK with G430L and 0.2X0.09 aperture
(3) 120 s WAVE
(4) 1800 s E140H 1416
(5) 250 s WAVE
Each of two subsquent orbits:
(6) 250 s WAVE
(7) 3015 s E140H 1416
(8) 250 s WAVE
--------- Additional Comments ----------
Notes to schedulers:
The STIS FUV detector background rate increases with time after detector HV turn-on. Since AW Per is rather faint, please SCHEDULE VISITS B1 & B2 AS THE FIRST FUV MAMA VISIT IN EACH DAY'S SAA FREE BLOCK, and START EACH VISIT AS SOON AS POSSIBLE AFTER THAT DAY'S FUV HV RAMPUP. Please do NOT schedule B1 and B2 together in the same SAA free blockCOOL STARS12falsetruefalsefalseAVAILABLESTARB6-B9.5 V-IVCEPHEIDCOMPOSITE SPECTRAL TYPEF3-F9This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000Spec=F8II+B6STARB6-B9.5 V-IVCEPHEIDCOMPOSITE SPECTRAL TYPEF0-F2This object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STARB6-B9.5 V-IVBased on inteferemetric data plus what is known about the orbit, the companion to AX Cir has a predicted position for 2016-03-01 of 2016-03-01: rho = 29.746 mas, theta = -168.594 degSTARB6-B9.5 V-IVBased on inteferemetric data plus what is known about the orbit, the companion to AW Per has a predicted position for 2015-10-01 of rho = 32.952 mas, theta = 80.286 deg (A. Gallenne)STIS/FUV-MAMASpectroscopicNoNoE140H1271STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1416/user/proffitt/research/14194/OP-cache/14194_phase2_revised_24aug2015-v01.xmlThe scheduling data was generated by CASM 23.2.CASM was run in Phase II mode.ACQ and peakup are done on the Cepheid and an offset is done to the expected location of the blue companion based on inteferometric observations.(Tic-Visit
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Note to schedulers: The STIS FUV detector background rate increases with time after detector HV turn-on. Since our target is rather faint (about 5X average background), please schedule each visit as the first FUV MAMA visit in that day's SAA free block of orbits, and start the visits as soon as possible after the HV is turned on for the day.(Tic-Visit
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