0 Assigned ID: 313 ----- Attempting Submission 1 (Thu Apr 06 22:07:17 GMT 2017) ----- HST Phase I Proposal 313 (Etaphase1-GO.apt) successfully submitted. Receipt: # 313-1 ----- Attempting Submission 2 (Thu Apr 06 22:13:45 GMT 2017) ----- STIS SCIENCE TOO FAR FROM WAVECAL STIS SCIENCE TOO FAR FROM WAVECAL (1) Special acquisition ZZZQ, see target and acquisition comments. This has been used many times before. --- (2) MAMA bright object: see comments in Visit 2. --- (3) One exposure in Visit 3 does not have a WAVECAL. It is not needed, and there is not enough time for it. --- -1655972480 ----- Attempting Submission 1 (Wed Jul 19 22:29:42 GMT 2017) ----- 1. MAMA bright object: There are 2 safeguards -- (a) This target was observed with MAMA in 2013 and 2015 (programs 13377 and 13789), and the safety limits were not approached. (b) Visit 1 will provide confirmation or warning before Visit 2. See the comments and special timing requirements for Visit 2. --- 2. One exposure in Visit 3 does not have a WAVECAL. The orbit did not allow enough time, and the WAVECAL is not needed for this particular observation. See comments for exposure "4961" in Visit 3. Eta Car is the only giant-eruption survivor that can be observed well. Hence it is genuinely unique for testing instability theories which are crucial for very massive stars. Fortuitously, a rapid change of state began about 1998. This represents an unexpected stage in the recovery following the Great Eruption ("supernova impostor event") seen 170 years ago. Now there are reasons to think that the change of state is nearly complete. HST/STIS has been the main source of information on this phenomenon, and is the only instrument that can show the final (or nearly final) state. Therefore we propose to complete this record in Cy 25. The archival value is very high, because similar observations will later be impossible; the star is changing irreversibly. HST is needed, because UV is essential and because all ground-based spectroscopy of eta Car is heavily contaminated by emission lines formed about 0.3 arcsec away. For this object each HST orbit produces many high-quality spectra. The same data apply to other problems, e.g. exotic emission processes in the ejecta, bipolar structures, and the nature of the companion star. We propose STIS observations: (1) A final update of the central star's wind spectrum at selected NUV-to-red wavelengths. (2) Brief UV spectroscopy with the MAMA echelle. This will be the only such data obtained at a time when the companion star is near apoastron. (3) Special sampling of the Homunculus ejecta-nebula using STIS/CCD with long exposure times. This was done once before, in 2000, and major changes have occurred since then. --- XXX FILLER TEXT XXX --- Will insert real description later... Stellar Physics 0 false true false false false false SUPPORTED STAR ETA CARINAE STAR IMPORTANT: Ref frame is really special catalog ZZZQ, which was used for almost all successful HST acquisitions of Eta Car in the past. ZZZQ coords differ from ICRS by about 0.2 arcsec, see etacar.umn.edu.. -- Catalog ZZZQ was prepared before 1990 because original GSC was inadequate in Carina crowded field. Later version of GSC would _probably_ be OK, but has never been verified for this target. -- See, for example, acquisitions in GO 13377 (and many other programs with this target). J2000 J2000 STAR ETA CARINAE STAR Target ETA-CAR-SR is used to duplicate pointing of 52x0.2F1 slit in Visit 2 of GO 8327, done on 2000 March 13. Name "SR" originally implied "strontium" but this has no significance now. We suspect that target SR in 2000 should have been 0.1 arcsec NW of the star, but a typo or misunderstanding put it at 0.1 arcsec N instead. Anyway, here we are trying to duplicate the earlier 52x0.2F1 observations as closely as possible. J2000 STIS/CCD Spectroscopic No No G750M 7795 STIS/CCD Spectroscopic No No G750M 6768 STIS/CCD Spectroscopic No No G750M 7283 STIS/CCD Spectroscopic No No G750M 5734 STIS/CCD Spectroscopic No No G430M 4961 STIS/CCD Spectroscopic No No G430M 4706 STIS/CCD Spectroscopic No No G430M 3680 STIS/CCD Spectroscopic No No G430M 3936 STIS/CCD Spectroscopic No No G430M 3423 STIS/CCD Spectroscopic No No G430M 3165 STIS/CCD Spectroscopic No No G230MB 2557 STIS/CCD Spectroscopic No No G230MB 2836 STIS/CCD Spectroscopic No No G230MB 2697 STIS/CCD Spectroscopic No No G230MB 2416 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G230LB 2375 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/CCD Spectroscopic No No G750M 7795 STIS/CCD Spectroscopic No No G750M 7795 STIS/CCD Spectroscopic No No G750M 6768 STIS/CCD Spectroscopic No No G430M 4961 STIS/CCD Spectroscopic No No G430M 3936 STIS/CCD Spectroscopic No No G430M 4706 STIS/CCD Spectroscopic No No G230MB 2836 STIS/CCD Spectroscopic No No G230MB 2557 POS-TARG DITHER 0.2282 Spacing 0.2282 arcsec is intended to be 4.50 STIS/CCD pixels or rows. This dither pattern substantially improves spatial sampling along the slit, because STIS/CCD pixel size is too large re Nyquist criterion etc. LINE false false 2 90.0 STIS-ALONG-SLIT 1 false 1500496873143 /data/aps/software/APT/EtaCar/OP-cache/go15067-2017jul19-v01.xml Timing link suitability includes constraints ([Sequence (01 02) within 60.0 days] [02 After 01 by 24.0 to 75.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. This visit is adapted from Visit 01 of GO 13377 (Cy 21, 2014). --- USE SPECIAL CATALOG ZZZQ FOR ACQ --- -- ORIENT requirements: The two brightest Weigelt Knots, ejected blobs about 0.4 arcsec NW of the star, are located near PA= 302 and 332 D. Several previous STIS observations of the star have included those knots by orienting the slit accordingly. The ORIENT parameters listed below are chosen to match the most frequent earlier orientations. ORIENT = about 167.2D or 347.2D would also be OK but not as good as 17D or 197D. (Tic-Visit :proposal-id 15067 :visit-id "01" :proposal-version -1 :trans-version "20170613" :date "19-Jul-2017 15:41:12.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 471488 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15067 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15067 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3083 :al-overhead-at-end 72 :internal-dur-at-end 335 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3449 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15067 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3133 :al-overhead-at-end 75 :internal-dur-at-end 393 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3449 :pcs-gap 0 ) true 2 0 IMPORTANT: Special catalog ZZZQ must be used for acquisition, like previous obs of Eta Car. For example, see program GO 13377 (and almost all other programs on this target). --- See comments for target ETA-CAR-A. We use 7795 A becaise this wvl interval has no bright emission lines. Other wavelength ranges might be perturbed by the nearby Weigelt emission-line blobs. Very short exposure to get core of very bright H-alpha emission line. WAVE CAL=NO because we are explicitly managing the WAVECALs. Some pixels in the H-alpha emission line will be saturated in this exposure. WAVECAL=NO because we explicitly manage the WAVECALS. ' H-alpha emission line on star will be heavily exposed in this exposure. Includes UV-excited N II multiplet 5668--5712 A. Also useful for V-band photometry. -- This long exposure samples outlying ejecta. Dither and CR-SPLIT=3 to get high quality. This wvl interval includes several critical spectr features. Grating G230LB is chiefly useful for photometry. However, we use dither because some emission line structures might be omitted from our other wvl samples. We use grating G230LB primarily for photometry. However, it may also indicate NUV emission lines outside the other wvl samples. Wvls near 7283 A are useful chiefly for outlying ejecta. This FF is intended to occur at the end of orbit visibility, so it can be done in orbit non-visibility time. Low-dispersion mainly for photometry around 330 nm and 440 nm. WAVECAL is not essential. -- We use pattern to improve effective spatial resolution. Dither and CR-SPLIT=3 to get highest qual data. This wvl range includes critical spectr features. Short exposure to avoid saturation in core of H-beta line. WCAL=NO because we explicitly manage the wavecals. This wvl interval includes H-beta and other emission lines. WCAL=NO because we're explicitly managing the wavecals. This wvl range includes the Fe II 2507 quasi-laser lines. Short exposure because they may be bright. 1500322163999 /data/aps/software/APT/EtaCar/OP-cache/go15067-2017jul19-v02.xml Timing link suitability includes constraints ([Sequence (01 02) within 60.0 days] [02 After 01 by 24.0 to 75.0 days]) The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. This is practically a copy of Visit 3 in program GO 13389, which occurred in Sept 2015. Also Visit 2 iin GO 13377, Oct 2013. ` It is highly desirable for this visit to occur within about 2 months of visit 1. -- IEta Car was safely below the allowed brightness limits during 2013-2015. In this program, we can use STIS/CCD data from Visit 1 to verify that this is still true. -- Note that acquisition uses special catalog ZZZQ, see comments on target and on Visit 1. (Tic-Visit :proposal-id 15067 :visit-id "02" :proposal-version -1 :trans-version "20170613" :date "17-Jul-2017 15:09:23.0" :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 174976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15067 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15067 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3109 :al-overhead-at-end 0 :internal-dur-at-end 394 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3449 :pcs-gap 0 ) true 1 0 This ACQ has the same parameters as Visit 3 in program GO 13389. Again, just like Visit 3 in program 13389. We use wavelength 7795 because that interval has no strong emission lines. Therefore the peakup will not be perturbed by the nearby Weigelt Knots which are emission-line sources. We omit an ETC run, because observations like this have already been done on Eta Car: 2013 Oct 26 in program 13377, and 2015 Sept 2 in program 13789. Observed MAMA count rates were far below the allowed limits, see below. We will use STIS/CCD Visit 1 to verify that the star has not brightened by a large factor.in the UV. --- (In any case, Eta Car's UV spectrum is too complicated for a realistic ETC run.) --- ** Count rates observed in 2013-2015: 0.5 ct/s in peak pixel, global rate 55 thousand cts/s in entire detector. ** We omit an ETC run number for reasons explained in previous exposure. Target was far below allowed brightness limits in MAMA obs 2013 and 2015. --- ** Observed count rates in 2013--2015: Maximum pixel 4.8 cts/s, global 100 thousand cts/s in entire detector. ** 1500497038492 /data/aps/software/APT/EtaCar/OP-cache/go15067-2017jul19-v03.xml The scheduling data was generated by CASM 25.2. CASM was run in Phase II mode. Here we are trying to duplicate some earlier observations as closely as possible. Those obs occurred in Visit 2 of program GO 8327, done on 2000 March 13. The goal is to use wider slit 52x0.2F1 across Eta Car's Homunculus nebula. The slit must have the same orientation as in 2000, and the star plus Weigelt Knots must be blocked by the slit's occulting bar ("fiducial"). --- The ORIENT angle is simply copied from the GO 8327 plan, with +180D alternative; if STIS definitions or slit orientation parameters have been revised since 2000, then we should alter the ORIENT angle accordingly. -- We omit a WAVECAL for grating tilt 4961, because there is not enough orbit time; see comment for that exposure. -- Note that acquisition uses special catalog ZZZQ, see comments for target ETA-CAR-A and for Visit 1. (Tic-Visit :proposal-id 15067 :visit-id "03" :proposal-version -1 :trans-version "20170613" :date "19-Jul-2017 15:43:57.0" :trans-errors '(:WARNINGS 2 :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 255056 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15067 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15067 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3102 :al-overhead-at-end 84 :internal-dur-at-end 690 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3449 :pcs-gap 0 ) true 1 0 We use wvl 7795 A for peakfup, see comments for Visits 1 and 2. -- Note that slit 52x0.1 is used for this peakup, but the main observations in this visit will use slit 52x0.2F1. -- WAVECAL=NO because we are managing WAVECALS explicitly. Automatic wavecal is assumed for this exposure, not for the preceding one. No WAVECAL for this grating tilt, because the orbit does not allow enough time. We will estimate an approximate wvl calibration by combining information from known features in the object, plus wavecals for 4961 at other times, plus the 6768 and 3936 data in this orbit. Precise wavelengths and velocities ae not needed for the 4961 grating tilt. Exposures with wvl 7283 A should be at end of orbit, so FFLATs can be done after visibility time ends. This exposure should occur at end of orbit, so FFLAT's can be done after orbit visibility time. FFLATS should occur after end of visi bility period