First draft submission Detailed constraints added: soem relaxed some tightened Wrong text file uploaded, title trimmed final version -1803173200 Assigned ID: 313 ----- Attempting Submission 1 (Thu Apr 07 22:56:56 GMT 2016) ----- HST Phase I Proposal 313 (harper_zaur.apt) successfully submitted. Receipt: # 313-1 ----- Attempting Submission 2 (Fri Apr 08 16:01:23 GMT 2016) ----- HST Phase I Proposal 313 (harper_zaur.apt) successfully submitted. Receipt: # 313-2 ----- Attempting Submission 3 (Fri Apr 08 16:20:20 GMT 2016) ----- HST Phase I Proposal 313 (harper_zaur.apt) successfully submitted. Receipt: # 313-3 ----- Attempting Submission 4 (Fri Apr 08 17:48:41 GMT 2016) ----- This submission now uses the AVAILABLE (approved) mode to move the final WAVECAL to the occultation, increasing the efficiency and quality of the on-source science data. Previous: Following advice from C.Proffitt, the ACQ/PEAK on Visit 1 was close to threshold (i.e 80,000 cnt/s Source Only. So I have increased APT time from 1sec to 3 sec. 2016 Aug 29: (at request of CP) Time constraint for Visit 1 corrected to reflect Visit starts in March 2017(AFTER) -1679622294 ----- Attempting Submission 1 (Tue Jul 19 20:19:51 GMT 2016) ----- HST Phase II Proposal 14731 (zetaAur_jul19.apt) successfully submitted. Receipt: # 14731-1 ----- Attempting Submission 2 (Wed Jul 20 16:29:30 GMT 2016) ----- HST Phase II Proposal 14731 (zetaAur_jul19.apt) successfully submitted. Receipt: # 14731-2 ----- Attempting Submission 3 (Thu Jul 21 17:11:43 GMT 2016) ----- HST Phase II Proposal 14731 (zetaAur_wavecal.apt) successfully submitted. Receipt: # 14731-3 ----- Attempting Submission 4 (Mon Aug 29 15:08:08 GMT 2016) ----- 0 ----- Attempting Submission 1 (Tue Jul 19 20:15:00 GMT 2016) ----- HST Phase II Proposal 14731 (zetaAur_jul19.apt) successfully transmitted Receipt: # 14731-1 Zeta Aur eclipsing binaries provide the most detailed spatial information about the extended atmospheres of red supergiants. During chromospheric eclipse phases quantitative information about densities, temperatures, turbulence, and ionization have been obtained. However, detailed information about the atmosphere can also be obtained away from eclipse when the hemisphere illuminated by the ultraviolet continuum of the companion is visible from Earth. New Si I and C I diagnostics can provide spatially-resolved information on the velocity fields in the deepest layers yet measured for a K4 Ib star . We propose to observe the zeta Aurigae system with STIS at three orbital phases to study the velocity fields and ionization balance using the Si I and C I emission feautures. zeta Aurigae has a 972 day period and the next eclipse is in March 2017. This may be the last opportunity to study this benchmark system for studying the atmospheres of cool evolved stars. In Cycle 24 we will observe the NUV spectrum of the eclipsing binary zeta Aurigae (K4 II + B5 V) on 2 separate 1 Orbit Visits. Visit 1 is during the total eclipse of the uv-bright B star, and a Visit 2 will observe both stars, out of eclipse. NUV fluxes and Safety - This is a UV bright binary with predictable orbital variability. The BOT identifies the target as a health warning in the GSC II, and the field was too bright for a GALEX. The stars themselves are not intrinsically variable (the B star is a main sequence star, and the K supergiant is probably a low $Delta VMag < 0.03$ amplitude), but during eclipse the system flux levels are quite different with the UV flux dropping because the B star is occulted.. To estimate the system fluxes at these 2 different orbital phases we have used several flux templates: For Visit 1 (eclipse) we have used merged IUE LW HIRES and SWP LORES spectra 1650-3200 Angstroms - whose fluxes compare closely to HST/GHRS spectral segments obtained previously. We expect these are good to 10% absolute flux calibration (the limit of IUE and GHRS spectra). For Visit 2 (maximum B star irradiation - out of eclipse) we have used both a merged IUE spectrum, and a published model B star spectrum, both flux levels agree well The BOT flagged observations are either made with the MAMA E230H 0.2x0.09 or 31x0.05NDA apertures. During eclipse (0.2x0.09 aperture), at this time the high fluxes from the B star are reduced by an order of magnitude - and should not thus be a health and safety risk. The out of eclipse observations in Visit 2 use the 31x0.05ND apertures. We have used the ETC for all exposure estimates (except WAVECALS). Time Constraints- Both Visits have time constraints that relate to the phase of the binary orbit (972 period). The 2 Visits in Cycle 24 are for the eclipse of the B star (between 2017 Mar 11-25) and an epoch where the B star irradiates the visible hemisphere of the K star (2017 Aug 10 - Oct 10). Each Visit is 1 Orbit Observing strategy (Available)- STIS E240H observations will provide the high spectral resolution (R > 100,000) to fully resolve the narrowest emission lines (FWHM=9.0 km/s). In both Visits will will observe the two same E230H settings (same wavelengths: i2463, i2912) with the MAMA detectors in ACCUM mode (to save time on BUFFERing). The first WAVECAL in each Visit is required during the Orbit, but to avoid losing on-source time from the 2nd WAVECAL (i2912) we have adopted the "AVAILABLE" (but not supported mode) of explicitly specifying the wavecals. The final WAVECAL is placed at the beginning of the occultation. We have used the default expsore times for these. "Availability Mode: AVAILABLE has been approved. Visit 1: ACQ/PEAK: We ACQ the K star (V=3.90) with the STIS CCD and F25ND5. We then peak-up in a 0.2x0.09 aperture with the G230L. Science: The following MAMA E230H science observations also use 0.2x0.09 aperture. The first 2 science observations uses the i2463Ang seeting, while the 3rd and 4th science observations will be at i2912 Ang. The use of identical pairs allows for identification of artifacts resulting from the ACCUM. Visit 2: ACK/PEAK we also ACQ the K star (V=3.90) with the STIS CCD and F25ND5, but because of the higher UV flux levels, we then peakup with the 31x0.05NDC with G230L. SCIENCE: For the MAMA E230H science observations we use the 31x0.05NDA (0.4 dex) aperture+neutral density filter to keep the total count rates for the entire detector are below 70.000, below the MAMA global count rate. The first 2 science observations uses the i2463Ang seeting, while the 3rd and 4th science observations will be at i2912 Ang. The use of identical pairs allows for the identification of artifacts resulting from the ACCUM. *** Please note that a similar proposal from a previous cycle has adopted essentially the same ACQ/PEAK strategy (14070 PI P. Bennett) and has not yet been executed This will occur before the first scheduled Visit of this proposal. Stellar Physics 12 false true false false false false AVAILABLE STAR B3-B5 V-IV COMPOSITE SPECTRAL TYPE K III-I NO This object was generated by the targetselector and retrieved from the SIMBAD database.This object was generated by the targetselector and retrieved from the SIMBAD database. HR1612 J2000 J2000 NUV B star continuum [for out of eclipse observations: 1.0(-10) erg cm-2 A-1 at 1700 Ang, 4x10(-11) erg cm-2 s-1 A-1 at 2300 A, and 3.0(-11) erg cm-2 s-1 at 3000A: Star observed at proposed wavelengths with IUE in HIRES: During eclipse the NUV fluxes are significantly less STIS/NUV-MAMA Spectroscopic No No E230H 2513 STIS/NUV-MAMA Spectroscopic No No E230H 2912 STIS/NUV-MAMA Spectroscopic No No E230H 2513 STIS/NUV-MAMA Spectroscopic No No E230H 2912 STIS/NUV-MAMA Spectroscopic No No E230H 2513 STIS/NUV-MAMA Spectroscopic No No E230H 2912 /arlstorage/home/faculty/gmh/Proposals/2016/HST/zetaAur/PhaseII/OP-cache/zetaAur_wavecal-v01.xml 1469117271871 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 2 week window around central eclipse. One could make this window a little larger if an off-centrered eclipse was OK (Tic-Visit :proposal-id 14731 :visit-id "01" :proposal-version -1 :trans-version "20160601" :date "21-Jul-2016 10:07:51.0" :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 314704 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14731 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14731 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2972 :al-overhead-at-end 81 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) true 1 0 Pickles KII 3-4 model V=3.90, extinction [E(B-V)=0.08 applied before normalization. S/N=40 for 0.29 sec, elect 4 sec observation for S/N=167. [Sat occurs at 50.77 sec] Q to Charles Proffitt on how to estimate S/N for Spectral Elements (not available in ETC). Seek > 80,000 cnt/s [Source is too bright to used a non-dispersed light ACQ/PEAK] Set GAIN=4 (CProffitt) Eclipse spectrum is merge of 2 LWP HIRES and 1 SWP LORES. LWP Flux compares well with 2 GHRS regions of overlap. Exposure time (seconds) = 1.0000 at wavelength 2600.00 Ang. gives: SNR = 17.9390 (per resolution element) gives: Time to Saturation (for a single exposure) = 167.64 seconds Source only 94,375.812 cnt/s Exposure time calculation HAD WARNINGS. WARNING MESSAGE: "Electrons per pixel due to background (0.0095) is less than the recommended threshold of 20 electrons to avoid poor charge transfer efficiency (CTE). We suggest you consider CTE mitigation strategies described in the STIS Instrument Handbook." Mode: spectroscopic Detector: CCD Central Wavelength: Grating: [G230LB] R ~ 700 Aperture: 0.2X0.09 Gain: 4.0 # Frames: 2 Binning: dispersion: 1, spatial: 1 Observe Si I 2438, 2478., 2515, 2582 + scattered light spectrum Exposure time (seconds) = 790.0000 at wavelength 2582.90 Ang. gives: SNR = 15.5768 (per resolution element) Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2463 Grating: [E230H] R ~ 114000 Aperture: 0.2X0.09 Observe Si I 2438, 2478., 2515, 2582 + scattered light spectrum Exposure time (seconds) = 790.0000 at wavelength 2582.90 Ang. gives: SNR = 15.5768 (per resolution element) Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2463 Grating: [E230H] R ~ 114000 Aperture: 0.2X0.09 Exposure time (seconds) = 790.0000 at wavelength 2881.00 Ang.` gives: SNR = 8.0749 (per resolution element) Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2912 Grating: [E230H] R ~ 114000 Aperture: 0.2X0.09 Exposure time (seconds) = 790.0000 at wavelength 2881.00 Ang.` gives: SNR = 8.0749 (per resolution element) Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2912 Grating: [E230H] R ~ 114000 Aperture: 0.2X0.09 Exposure time based on AUTO WAVECAL /arlstorage/home/faculty/gmh/Proposals/2016/HST/zetaAur/PhaseII/OP-cache/zetaAur_wavecal-v02.xml 1469117178372 The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 14731 :visit-id "02" :proposal-version -1 :trans-version "20160601" :date "21-Jul-2016 10:06:18.0" :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 314144 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 14731 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 14731 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2971 :al-overhead-at-end 132 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3307 :pcs-gap 0 ) true 1 0 Pickles KII 3-4 model V=3.90, extinction [E(B-V)=0.08 applied before normalization. S/N=40 for 0.29 sec, elect 4 sec observation for S/N=167. [Sat occurs at 50.77 sec] Q to Charles Proffitt on how to estimate S/N for Spectral Elements (not available in ETC). Seek cnt/s > 80,000 Source is too bright to used a non-dispersed light ACQ/PEAK Input spectrum B star model + K4 II contribution (small) from lambda Velorom Exposure time (seconds) = 1.0000 at wavelength 2600.00 Ang. Source only 205,100.357 cnt/s gives: SNR = 7.1371 (per resolution element) gives: Time to Saturation (for a single exposure) = 648.14 seconds Exposure time calculation HAD WARNINGS. WARNING MESSAGE: "Electrons per pixel due to background (0.0095) is less than the recommended threshold of 20 electrons to avoid poor charge transfer efficiency (CTE). We suggest you consider CTE mitigation strategies described in the STIS Instrument Handbook." Note we are using a smaller aperture than for the science observations (31x0.03NDA) Observe Si I 2438, 2478., 2515, 2582 + scattered light spectrum Exposure time (seconds) = 700.0000 at wavelength 2478.50 A gives: SNR = 48.6805 (per resolution element) Count rate entire detector 68,740.468 Exposure time calculation HAD WARNINGS. WARNING MESSAGE: Buffer time 29.0949 is less than minimum 99 seconds. Observe Si I 2438, 2478., 2515, 2582 + scattered light spectrum Exposure time (seconds) = 700.0000 at wavelength 2478.50 A gives: SNR = 48.6805 (per resolution element) Count rate entire detector 68,740.468 Exposure time calculation HAD WARNINGS. WARNING MESSAGE: Buffer time 29.0949 is less than minimum 99 seconds. Exposure time (seconds) = 275.0000 at wavelength 2987.60 Ang gives: SNR = 26.0580 (per resolution element) Count rate entire detector 42,040.578 Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2912 Grating: [E230H] R ~ 114000 Aperture: 31X0.05NDA Exposure time (seconds) = 275.0000 at wavelength 2987.60 Ang gives: SNR = 26.0580 (per resolution element) Count rate entire detector 42,040.578 Mode: spectroscopic Detector: NUVMAMA Central Wavelength: 2912 Grating: [E230H] R ~ 114000 Aperture: 31X0.05NDA Using the 0.2x0.09 aperture (while science observations use the 31x0.05 NDA)