1) added orbital period and initial epoch under Special Requirements for Visit 01
2) added acceptable orbital phase range under Special Requirements for Exposure 01-1780351474----- Attempting Submission 2 (Thu Jul 28 14:14:21 GMT 2016) -----
HST Phase II Proposal 14476 (2016jul28_retrieved_program14476_savedAPTv23.apt) successfully submitted.
Receipt: # 14476-2
----- Attempting Submission 3 (Fri Jul 29 13:20:27 GMT 2016) -----A collision reversal in HD 5980HD 5980 provides a unique laboratory for studying the properties of wind-wind collisions. It contains one of only two binary systems having a WR-star in orbit with a LBV. The latter star has been observed to undergo major changes in its wind structure over the past 35 years, implying changes in the geometry and emitting conditions of the wind-wind collision region. Ten years ago, when the LBV wind was very strong, XMM observations revealed X-ray emission consistent with the shock cone wrapping around the WR component. Since then, the wind strength has significantly declined, implying that the collision shock cone may be inverting its orientation. The objective of this proposal is to obtain X-ray coverage of this never before observed phenomenon. We also request HST/STIS observations to determine the wind velocity of the WR-star. All recent HST observations of this system have been performed at the opposite orbital phase, when the LBV occults the WR. The WR wind speed is required for the study of the WWC region. We propose to observe HD 5980 in the 1170 - 1730 A spectral interval with STIS using the FUV- MAMA detector with the E140M grating, plus 3 short exposures with the CCD in order to complete the wavelength coverage out to 10000 A. These observations all fit into 2 orbits.We propose to observe HD 5980 in the 1170 - 1730 A spectral interval with STIS using the FUV- MAMA detector, the E140M grating and the 0.2x0.2 slit. To estimate the exposure times we used our most recent HST spectra obtained in 2013. The Exposure Time Calculator indicates that we will require an exposure of 4600 seconds to achieve S/N~50 per resolution element at 1300 A and S/N>20 in the entire spectral range. The actual exposure time entered into the Orbit Planner is 4597 seconds, split into two exposures, the first of 2569 seconds during the first orbit and the second of 2028 seconds in the second orbit. We are also requesting 3 exposures using the CCD detector and the G230BL, G430L and G750L gratings. This will provide a full spectral energy distribution for the CMFGEN model fits. The requested exposure times are 300 s, 60 s and 60 s, respectively, which will assure S/N~100. The total exposure time+overheads for the CCD spectra is less than 25 min, asuming a 5 min overhead per CCD exposure (HST Primer sec. 6.4.3). The CCD spectra will be obtained during the second orbit. The mixture of MAMA and CCD observations in the same orbit is justified by the short exposure time required for the CCD spectra (HST Primer sec. 6.2.2).
We require that the observation be scheduled to coincide with the eclipse of Star A by Star B, which occurs at orbital phase phase=0.36. The orbital period is 19.2654 days, and the initial epoch for the calculation of the eclipse phase is T0 =JD 2443158.707. The optimum results will be for an observation performed within +/-0.01 in phase of the eclipse date. This gives a tolerance of +/-0.2 days.HOT STARS12falsefalsefalsefalsefalse23falseSUPPORTEDSTAREMISSION LINE STARLUMINOUS BLUE VARIABLEWINDWOLF RAYET - WNThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG750L7751The scheduling data was generated by CASM 24.2.CASM was run in Phase II mode.Required to be scheduled for orbital phase 0.36 +/-0.01; Initial epoch T0 =JD 2443158.707 and Period P=19.2654d(Tic-Visit
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:visit-id "01"
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:trans-version "20160601"
:date "29-Jul-2016 08:15:44.0"
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