This version specifies visits 3 and 4, labeled "CCD-2" and "CCD-3" in the script. -- Visits 5--7 in this version will probably be OK, but might need to be revised after we get data from visit 3. It is also possible that we might make provision for a STIS-MAMA visit. -- [kd, 2014 Apr 8] -------- 1835024206 ----- Attempting Submission 4 (Tue Apr 08 20:05:21 GMT 2014) ----- HST Phase II Proposal 13377 (13377-visits3to7.apt) successfully submitted. The acquisition procedure for Eta Carinae is somewhat unusual, but we and Ted Gull's group have used it many times from 1998 to 2013. The target position and acquisition method in this version are exactly like those we used in September and October 2013. Essential UV Observations of Eta Carinae's Change of State Eta Carinae is now passing though a critical phase in its evolution as it recovers from its ``Great Eruption'' 170 years ago. About 12 years ago we began to see a dramatic and unpredicted change in eta Car's long-term behavior. The brightening rate suddenly accelerated, so by 2010 the central star had brightened by more than a factor of four in the near-UV. Between 2003 and 2010 the stellar-wind emission lines weakened by factors of 2 to 4(!) implying a rapid decrease in its mass loss rate. Eta Car is unsteadily returning to its pre-eruptive state, but the rapidity since 2000 has been astonishing. The recent secular changes are much stronger in the UV than at optical wavelengths, but no UV data have been obtained since 2010 and no far-UV observations since 2004. The extraordinary brightening and changes in the wind are fundamental and must indicate basic changes in the outer structure of this circa-130 Msun star. Therefore, this proposal focuses on the rapid secular changes rather than the expected 2014.6 periastron passage. This is primarily a UV problem, though longer wavelengths are also worthwhile. Fresh observations must be done early in Cycle 21 before the approaching periastron alters the system. Our highest priorities are the UV brightening and the long term changes in the wind. (1) A 2-orbit STIS/CCD visit should occur as early as possible. (2) A 1- or 2-orbit STIS/MAMA visit as early as possible in Cycle 21. (3) Additional STIS/CCD visits through and beyond the 2014.6 spectroscopic event; details TBD. (4) If possible, another STIS/MAMA orbit in 2015. The total is 11 orbits. Integration times range from a few seconds in the red to several minutes in the UV. --------- Additional Comments ---------- ============================================================ -- CLARIFICATION OF AN ORIENT RANGE -- Visit 1 has an ORIENT special requirement, to match some previous observations. If possible we would like ORIENT = exactly 197D. This appears to be feasible for a few days around September 17. The Phase 2 plan specifies ORIENT = 196.8 to 197.2 degrees. *** HOWEVER: IF THIS REQUIREMENT MAKES SCHEDULING VERY DIFFICULT, WE CAN WIDEN THE RANGE OF ORIENT ANGLES. *** ============================================================ HOT STARS Default false true false false false AVAILABLE STAR ETA CARINAE STAR J2000 J2000 F(2800) = 1.0E -11 +/- 0.4E-11, , F(2200) = 5E-12 +/- 3E-12 STIS/NUV-MAMA Spectroscopic No No E230M 1978 STIS/FUV-MAMA Spectroscopic No No E140M 1425 STIS/CCD Spectroscopic No No G230MB 2557 STIS/CCD Spectroscopic No No G230MB 2794 STIS/CCD Spectroscopic No No G430M 3680 STIS/CCD Spectroscopic No No G430M 3305 STIS/CCD Spectroscopic No No G430M 3936 STIS/CCD Spectroscopic No No G430M 4706 STIS/CCD Spectroscopic No No G230LB 2375 STIS/CCD Spectroscopic No No G230LB 2375 STIS/CCD Spectroscopic No No G430L 4300 POS-TARG DITHER 0.2282 2-point dither to improve pixel sampling. Here the spacing is 4.5 rows. Our intention is to move the pointing exactly along the STIS slit, i.e. the target must remain in the slit. LINE false false 2 90.0 STIS-ALONG-SLIT 1 false Timing link suitability includes constraints ([02 After 01 by 20.0 to 50.0 days]) The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. WE WILL USE DATA FROM THIS VISIT TO PLAN DETAILS FOR THE LATER VISITS. THIS IS ESPECIALLY CRITICAL FOR UV BRIGHTNESS LEVELS IN NEXT VISIT MAMA-1. -- A secondary purpose is to make precise spatial measurements of emission lines. -- ORIENT goal is slit PA close to -28D or +152D. PA -28D was done often before 2004 and includes the nearby ejecta Weigelt knot D. -- IMPORTANT: IF SCHEDULING IS DIFFICULT, ORIENT CAN BE RELAXED TO COVER A WIDER INTERVAL THAN 0.4. DEGREES. 1379133449000 196.8 (Tic-Visit :proposal-id 13377 :visit-id "01" :proposal-version -1 :trans-version "20131031" :date "31-Mar-2014 13:46:17.0" :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 479360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3105 :al-overhead-at-end 75 :internal-dur-at-end 182 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13377 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3239 :al-overhead-at-end 72 :internal-dur-at-end 780 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) true 2 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. H-alpha will be heavily overexposed with this exposure time. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Quick look at far UV, for photometry and also for planning later MAMA obs. With this exposure time, the longest wavelengths covered by this grating will be saturated. Compare shorter exposures. --- There are two reasons for the long exposure time: (1) good S/N below 2400 AA, and (2) make use of the time during a buffer dump. This exposure is intended to coincide with a buffer dump. Quick look at UV, for photometry and for planning later MAMA obs. Compare preceding long exposure. Important spectral region includes diverse emission features. For photometry, WAVECAL is not essdential. Mainly for photometry, S/N inadequate for spectroscopy, hence no WAVECAL needed. Observing plan doesn't have enough time for this WAVECAL. For photometry, WAVECAL is not essential. This exposure is intended to coincide with a buffer dump. For photometry, no WAVECAL needed. For photometry, no WAVECAL needed. This grating will be used for synthetic photometry in future brief visits. Included here in order to calibrate those visits, by comparison with higer-dispersion data obtained this visit. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Timing link suitability includes constraints ([02 After 01 by 20.0 to 50.0 days]) The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. UV spectra with E140M, E230M. Brightness levels were checked based on the preceeding CCD visit. 1382810709000 239.7849635716422 (Tic-Visit :proposal-id 13377 :visit-id "02" :proposal-version -1 :trans-version "20131031" :date "31-Mar-2014 13:46:21.0" :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 13377 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3158 :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 3491 :pcs-gap 0 ) true 1 0 The wavelength interval 7795AA has no strong emission lines. Therefore peakup leads to the star A and not to ejecta blobs like C and D. Preceding STIS/CCD visit will be used to assure that this exposure does not violate brightness limits for NUV-MAMA. The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. 2014.6 spectroscopic event. This visit occurs near t = -30 d, expected max NUV and max HeII 4687. - Visits CCD-2 to CCD-5 do not use the maximum possible orbit visibility time, because the timing of each visit is critical. Shortened visibility time increases the schedulability. 1405226552000 135.488796492279 (Tic-Visit :proposal-id 13377 :visit-id "03" :proposal-version -1 :trans-version "20131031" :date "08-Apr-2014 14:33:13.0" :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 153952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2723 :al-overhead-at-end 258 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) true 1 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Mainly for photometry around 330 nm, also good for blue photometry. Quick look at UV, for photometry and features 250-300 nm. Compare following long exposure. Long exposure for UV 170--250 nm. CR-SPLIT = 3 instead of 2, because this observation is critical and one c.r. hit could ruin an entire spectral line at low dispersion. Extremely important wavelength interval for HeII 4687 and other varying emission features. Important spectral region includes diverse emission features. The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. 2014.6 spectroscopic event. This sample is centered near t = -13 d, which in 2009 was near midpoint of NUV decline and minimum of HeII 4687 emission. There are reasons to suspect that this phase in the cycle may appear quite different from the 2009 event. 1406681599000 149.3223310177505 (Tic-Visit :proposal-id 13377 :visit-id "04" :proposal-version -1 :trans-version "20131031" :date "08-Apr-2014 14:34:22.0" :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 153952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "04" :obset-id "04" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "04" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2723 :al-overhead-at-end 258 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) true 1 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Photometry around 330 nm and also in blue. Photometry 250--300 nm, also good for spectral features in same range. Long exposure for features at short wavelengths 1650--2500 AA. Critical HeII 4687 and other emission features in this interval. Important spectral region includes diverse emission features. The scheduling data was generated by CASM 22.0. CASM was run in Phase II mode. 2014.6 spectroscopic event. This interval is centered near t = +4 d, which in 2009 was NUV minimum and beginning of 2nd HeII 4687 flash. ** THIS VISIT MIGHT NEED TO BE REVISED BASED ON RESULTS OF VISIT CCD-2 A MONTH EARLIER. ** -- ORIENT requirement samples Weigelt Knot C with same slit PA as obs in March 2010. This opportunity is fortuitous, because the timing requirement is based on other reasons. If the ORIENT requirement makes any trouble in scheduling, it can be widened or even deleted. (Tic-Visit :proposal-id 13377 :visit-id "05" :proposal-version -1 :trans-version "20131031" :date "08-Apr-2014 14:39:30.0" :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 153952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "05" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2723 :al-overhead-at-end 258 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3491 :pcs-gap 0 ) true 1 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Photometry around 330 nm, and emission features at longer wavelengths. Short exposure, features 250-300 nm. Long exposure for short wavelengths 170-250 nm. Critical HeII 4687 and other varying emission features. Important spectral region includes diverse emission features. The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. -- REVISED 2014 JULY 22 (kd) -- 2014.6 spectroscopic event. This interval is centered near t = +16 d, which in 2009 was just before peak of 2nd HeII 4687 flash. -- Earlier version had an ORIENT requirement. This has been deleted because the timing requirement has been revised forward several days. (kd, July 22) (Tic-Visit :proposal-id 13377 :visit-id "06" :proposal-version -1 :trans-version "20140605" :date "21-Jul-2014 13:29:31.0" :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 153952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "06" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2723 :al-overhead-at-end 258 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) true 1 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Photometry around 330 nm, and broad coverage of longer wavelengths. Photometry and NUV features 250-300 nm. Long exposure for UV 165-250 nm. HeII 4687 and other varying emission features. Important spectral region includes diverse emission features. The scheduling data was generated by CASM 22.2. CASM was run in Phase II mode. -- REVISED 22 JULY 2014 (kd) -- the timing is now several weeks earlier than in the original version. The new time is about t = 35 days in event, when He II 4686 will either be declining or absent. -- ORIENT requirement can be deleted if it makes trouble. It is intended to match many observations made in 1998-2004. (Tic-Visit :proposal-id 13377 :visit-id "07" :proposal-version -1 :trans-version "20140605" :date "21-Jul-2014 14:17:42.0" :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 153952 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13377 :visit-id "07" :obset-id "07" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13377 :visit-id "07" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2723 :al-overhead-at-end 258 :internal-dur-at-end 320 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3470 :pcs-gap 0 ) true 1 0 Target Acquisition for STIS CCD longslit This wavelength interval 7795AA has no strong emision lines. Therefore peakup really leads to the star A and not to ejecta blobs like C and D. Ultra-short exposure to get extremely bright H-alpha emission line profile. WAVECAL=NO because we are explicitly managing the WCALs. Some H-alpha pixels will be saturated in this exposure; H-alpha is extremely bright. NOTE: In past several years Eta Car has been brightening 0.1--0.2 magn per year. In this program we include WAVECALS explicitly so we can omit some that are definitely not needed for the program goals, and partly to force some of them into occultation periods. Synthetic photometry around 330 nm, plus varying features at longer wvl. Coverage of 250-300 nm varying features, and synthetic photometry. Long exposure for UV 165-250 nm. Important spectral region includes diverse emission features.