Eta Carinae is the only really observable example of structural recovery from a massive giant eruption, a "supernova imposter' event. Moreover it is the only well-observed star above 100 Msun, and its 5.5-year-recurrent spectrocopic events provide extraordinary clues to its surface instability. This truly unique combination of attributes makes it valuable for understanding the most massive stars. A fresh development arose a few years ago: The star has brightened much faster than before, and appears to have entered a rapid stage in its post-eruption recovery. A spectroscopic event will occur at 2009.0, soon after the planned HST servicing mission. Because of the recent secular trend, this event is expected to differ from its well-observed 2003.5 predecessor. The differences will be very important, because they offer clues to very-massive-star structural instabilities that can't be observed in any other known way. Some of the needed observations require HST's high spatial resolution and UV coverage. We propose an efficient, well-chosen set of STIS and ACS observations around the critical time. If the servicing mission is too late for the event, then a subset of the observations will still be merited.

Three points worth mentioning: (1) The most valuable spectroscopic diagnostics are in the STIS/CCD wavelength range. This is partly because of physics, and partly because STIS/CCD in 2003 provided the best existing record of a spectroscopic event for comparison. (2) Ground-based data now suffice for most of this problem, as explained near the end of the Scientific Justification. Here we concentrate on tasks that really need HST. (3) Our plans are based on considerable experience. In 1997 one of us (KD) planned the first STIS observations of Car. That intricate, extraordinarily efficient plan produced the highest-quality spectra of this object ever obtained, before or since. Integration times and other details for the Treasury Program evolved from that original. Meanwhile Davidson, Ishibashi, and Martin developed major improvements to the STIS IDT's reduction techniques. Hence, in this proposal we're revisiting familiar territory. Spectroscopy We propose to use the refurbished STIS/CCD for special observations before, during, and after the 2009.0 spectroscopic event (re. timing, see Fig. 1). Meanwhile we expect to get better temporal and spectral coverage with Gemini South. Spectroscopic priorities: ? H, a critical line (Fig. 3). Since it is the strongest emission feature and we need to measure its precise profile, ground-based data are still too contaminated by nearby ejecta. ? He I 6678. Very critical for interpretations; obtained with same grating tilt as H. ? UV features that can't be observed from the ground, e.g., bizarre Fe II 2507 emission. ? The crowded region near 3900A, because it includes Ca II absorption, [Ne III] emission plus diverse other features. Some of these have complex local spatial dependences that can't be disentangled in ground-based spectra. Moreover, the Gemini-South spectrograph has poor response below 4000A. ? The strange He II 4686 emission. In principle this can be done from the ground, but since it is both tricky and extremely important, we'll feel much safer with some STIS data. (The 2003 STIS data contradicted lower-quality ground-based measurements, see ref. [10].) ? [Ca II] and other features near 7300A. Anti-correlated with other features in the event,with some of the same spatial difficulties as the 3900A region. Fortunately we know the timing of Car's 5.5-year cycle with an accuracy of several days. If STIS is repaired on schedule, then at least four STIS visits are merited, preferably more. (1) A 2-orbit visit should occur as early as possible. (2) A 3-orbit visit close to 2009 Jan 1, the pre-minimum peak in Fig. 1. (3) A similar visit two or three weeks later, after the crash. This and visit 2 require two slit positions to get some information about the "Weigelt blobs" (inner ejecta). (4) At least one visit several months after the event. In addition, a one-orbit visit between 2 and 3 would be prudent, in case Car surprises us in its timing. The total is 11 orbits. Experience shows that a one-orbit STIS visit provides worthwhile information for eta Car but two orbits are more cost-effective and permit all the wavelength samples listed above. If the Weigelt ejecta must be observed separately (which depends on instrument orientation), then a third orbit gives the maximum cost-effectiveness. Integration times range from a few seconds in the red to several minutes in the UV. Eta Car has a favorable visibility length, 58 minutes in December or January, and the normal acquisition and overhead times apply. As a specific example, we cite the STIS visit that was done in March 2004 shortly before the instrument failure: http://www.stsci.edu/observing/phase2-public/9973.pro. That visit produced 33 STIS/CCD exposures in three orbits. In summary, we estimate that 11 STIS orbits gives maximum cost-effectiveness for covering the 2009.0 event. If the STIS is repaired too late for the event, then the post-event visits mentioned above will still be merited. We have heard that the STIS team may use Car as part of the re-commissioning phase. For technical reasons it is one of the best possible targets for that purpose. Note, however, that our proposed observations are carefully adjusted to the requirements of the secular-change problem, and we know the current brightness parameters from our HST photometric program. Commissioning-phase observations will not substitute for our program. HST imaging Since 2004 we have obtained about two HST imaging visits per year in order to follow eta Car's brightening trend. We used ACS, then WFPC2. HST's spatial resolution has been necessary to separate the star from its surprisingly bright ejecta, and, also, UV wavelengths are important. That program has provided the only existing data on the brightening of the central star after 2004 (Fig. 2 and ref. [11]). Similar observations should continue for all the reasons indicated in the Scientific Justification. In addition, the same images provide information about morphological changes in the ejecta through the 5.5-year cycle. They will substantially lengthen the baseline for proper motion measurements of the ejecta, an important topic because some of the ejecta ages have been controversial. If it is repaired, ACS is the best instrument for this purpose because it allows direct comparisons with earlier data, and because it has small pixels. In the past we used ACS filters 550M, 330W, and 220W, and one orbit gave an adequate set of data as can be seen from the example of program GO 10884: http://www.stsci.edu/observing/phase2-public/10884.pro. Our last WFPC2 orbit is scheduled for July 2008. A suitable plan for Cy 17 requires four visits to cover the event from December to February, and then one more visit late in 2009: five orbits in all. (See Fig. 2.) If ACS is not repaired, then WFC3 will be a good substitute. It has a satisfactory filter set, and like ACS it requires one orbit per visit. HOT STARS 12 false 0.0 0.0 false false false false false false AVAILABLE STAR CIRCUMSTELLAR MATTER EJECTA EMISSION LINE STAR ETA CARINAE STAR LUMINOUS BLUE VARIABLE Eta Car can be tricky to acquire because of the surrounding nebulosity that may affect the positions of official guide stars. Since the old GSC1 was very incomplete and very unreliable in this region, for observations of Eta Car from 1991 to 2007 we used a special catalog, ZZZQ (prepared by KD in 1989), in the GSC1 system. In dozens of acquisitions ZZZQ never failed. The improved GSC is **probably** OK, but we are nervous about it because it has not been verified for Eta Car. For some of the observations in this program, a failed acquisition would be disastrous because they sample a time-sensitive event. -- In the J2000 ICRS reference frame, the position of Eta Car A is 10h 45m 03.563s, -59deg 41' 04.14" with a rms uncertainty of roughly 0.2". F(2200) = 3.0 +/-1.5 E-12 J2000 10 45 3.5910 -59 41 4.26 J2000 STAR CIRCUMSTELLAR MATTER EJECTA ETA CARINAE STAR LUMINOUS BLUE VARIABLE WIND See comments for eta Car -A. Target position is offset abour 4 arcsec relative to eta Car-A to include two or three nearby stars for possible astrometric purposes. J2000 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA KNOT PLEASE VERIFY DEFINITION OF OFFSET. Relative to star A, object C is located at offset r = 0.235 arcsec, PA = 300 deg. In other words C is roughly WNW of A. This object is often called "Weigelt blob C." With the January spacecraft orientation, the STIS slit at this location will also partially include "Weigelt blob B" which is roughly 0.15 arcsec to the east. WEIGELT-C 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA KNOT PLEASE VERIFY OFFSET FORMAT AND DEFINITIONS... Relative to star A, target D is located at offset r = 0.275 arcsec, PA= 336 deg, i.e. D is NNW of A. This target is often called "Weigelt blob D." WEIGELT-D 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA KNOT This is a location between Weigelt blobs C and D, see separate specs for ETA-CAR-C and ETA-CAR-D. At times when the STIS slit PA is in range 14--54 deg or 194--234 deg, both C and D will be mostly in the slit at this offset location. WEIGELT-CD 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA KNOT If the STIS slit PA is close to 120 deg or 300 deg, then this position ETA-CAR-NNE gives a slit centerline that is 0.135 arcsec from the centerline for position ETA-CAR-A. 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA KNOT If the STIS slit PA is close to 120 deg or 300 deg, then this position ETA-CAR-NNE gives a slit centerline that is 0.135 arcsec from the centerline for position ETA-CAR-A. 00 00 0.0000 +00 00 0.00 J2000 UNIDENTIFIED EJECTA EMISSION LINE NEBULA If the slit PA is close to 120 or 300 deg, then this position ETA-CAR-NNE2 gives a slit centerline that is 0.27 arcsec from the centerline for position ETA-CAR-A. 00 00 0.0000 +00 00 0.00 J2000 STIS/CCD Spectroscopic No No G230MB 2557 STIS/CCD Spectroscopic No No G230MB 2697 STIS/CCD Spectroscopic No No G430M 3936 STIS/CCD Spectroscopic No No G430M 4706 STIS/CCD Spectroscopic No No G750M 6768 STIS/CCD Spectroscopic No No G750M 7283 ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F330W ACS/HRC Imaging No No F220W POS-TARG DITHER 0.15 Default pattern LINE 0.098 false false 63.5 4 19.89 ACS-HRC-DITHER-BOX 1 false POS-TARG DITHER 0.559017 LINE 0.559017 false false 143.130102 4 26.56505 WFPC2-BOX 2 false POS-TARG DITHER 0.3535 LINE false false 2 45.0 WFPC2-LINE 3 false POS-TARG DITHER 0.2282 2-point dither to improve pixel sampling. Here the spacing is 4.5 rows; is this a good choice? QUERY: WE ARE CURRENTLY UNSURE WHAT "PATTERN ORIENTATION 90deg" MEANS. 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 4 false Timing link suitability includes constraints ([41 After 40 by 10.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Roughly six weeks before Eta Car's 2009.0 spectroscopic event. Earliest spectral changes are expected to have begun before Nov 2008. 1226943113000 264.5248224767689 (Tic-Visit :proposal-id 11612 :visit-id "40" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:20.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 627424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "40" :obset-id "40" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "40" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([41 After 40 by 10.0 to 90.0 days] [43 After 41 by 5.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT REMARK: We have specified "after visit 40 by at least 10 days" but this does NOT imply that visit 41 depends on visit 40. If a visit in this program fails or does not occur, then the subsequent visits should be done anyway. Operationally the point is merely that no two WFPC2 visits should be close together in time. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Visit 41 is a few weeks before the climax of the 2009.0 spectroscopic event. Odd-numbered WFPC2 visits in this program are short in order to be feasible with reduced orbit visibility times. 1228640991000 284.3777028313724 (Tic-Visit :proposal-id 11612 :visit-id "41" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:22.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 448160 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "41" :obset-id "41" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "41" :orbit-number 1 :pcs-time 355 :si-vis-utilization 1860 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([43 After 41 by 5.0 to 90.0 days] [44 After 43 by 2.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT NOTE: We have specified this visit 43 should be at least 5 days after visit 41, but this does NOT imply that visit 43 depends on visit 41. The point is simply that no two visits should be close together in time. If one of the earlier visits fails or does not occur, then the subsequent visits should be done anyway. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Climax of Eta Car's 2009.0 spectroscopic event occurs around 10 January. This odd-numbered visit is short in order to provide more scheduling opportunities. 1230937194000 308.6435968497537 (Tic-Visit :proposal-id 11612 :visit-id "43" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:24.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 358528 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "43" :obset-id "43" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "43" :orbit-number 1 :pcs-time 355 :si-vis-utilization 1440 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([44 After 43 by 2.0 to 90.0 days] [46 After 44 by 2.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT NOTE: Visit 44 should be at least 2 dqys after visit 43, but this does NOT imply that visit 44 depends on 43. The point is that no two WFPC2 visits should be close together in time. If a visit fails or does not occur, then the subsequent visits should be done anyway. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Near climax of Eta Car's 2009.0 spectroscopic event. 1231323025000 312.5515299278268 (Tic-Visit :proposal-id 11612 :visit-id "44" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:26.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 627424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "44" :obset-id "44" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "44" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([46 After 44 by 2.0 to 90.0 days] [48 After 46 by 3.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT NOTE: Visit 46 should be at least 2 days after visit 44, but this does NOT imply that visit 46 depends on 44. The point is that no two WFPC2 visits should be close together in time. If a visit fails or does not occur, then the subsequent visits should be done anyway. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Near climax of Eta Car's 2009.0 spectroscopic event. 1231582322000 315.1830738760491 (Tic-Visit :proposal-id 11612 :visit-id "46" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:28.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 627424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "46" :obset-id "46" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "46" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([48 After 46 by 3.0 to 90.0 days] [50 After 48 by 5.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT NOTE: Visit 48 should be at least 3 days after visit 46, but this does NOT imply that 48 depends on 46. The point is that no two WFPC2 visits should be close together in time. If a visit fails or does not occur, then the subsequent visits should be done anyway. ** Substituting WFPC2 for earlier-planned STIS and ACS ** Near climax of Eta Car's 2009.0 spectroscopic event. 1231927273000 318.66632724108854 (Tic-Visit :proposal-id 11612 :visit-id "48" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:42:31.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 627424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "48" :obset-id "48" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "48" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([50 After 48 by 5.0 to 90.0 days] [53 After 50 by 15.0 to 90.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** IMPORTANT NOTE: Visit 50 should be at least 4 days after visit 48, but this does NOT imply that 50 depends on 48. The point is that no two WFPC2 visits should be close together in time. If a visit fails or does not occur, then the subsequent visits should be done anyway. ** Substituting WFPC2 for earlier-planned STIS and ACS ** After climax of Eta Car's 2009.0 spectroscopic event. 1232709928000 326.5980824770271 (Tic-Visit :proposal-id 11612 :visit-id "50" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:27:39.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 627424 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "50" :obset-id "50" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "50" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([53 After 50 by 15.0 to 90.0 days] [54 After 53 by 30.0 to 180.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** Substituting WFPC2 for earlier-planned STIS and ACS ** 4 to 8 weeks after climax of 2009.0 event. Observations in this visit are curtailed to increase scheduling opportunities. 1234257830000 342.71038081771553 (Tic-Visit :proposal-id 11612 :visit-id "53" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 18:48:03.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 313712 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "53" :obset-id "53" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "53" :orbit-number 1 :pcs-time 355 :si-vis-utilization 1380 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. Timing link suitability includes constraints ([54 After 53 by 30.0 to 180.0 days]) The scheduling data was generated by CASM 17.2. CASM was run in Phase II mode. ** Substituting WFPC2 for earlier-planned STIS and ACS ** IMPORTANT NOTE: If servicing mission is scheduled early enough so ACS and/or STIS is likely to be repaired, then this visit should be deleted. In that case some of the originally-planned ACS and/or STIS observations should be done instead. 1240894778000 65.11880257556811 (Tic-Visit :proposal-id 11612 :visit-id "54" :proposal-version -1 :trans-version "20080624" :date "02-Nov-2008 19:21:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 537792 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "54" :obset-id "54" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "54" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2520 :al-overhead-at-end 120 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 1 0 Gain 15 because very high count rate in central object. Birightest pixel may saturate at some of the dither points but probably not at all of them. Gain 15 because very high count rate in central object. We used 2 diff exposure times to get high dynamic range in surrounding ejecta. (1) This visit is URGENT because Eta Car is recovering from its January 2009 event. --- (2) The plan for this visit assumes that slit PA = about 300 deg so it includes both the star A and Weigelt blob C. This occurs if ORIENT = about 165 deg, suitable for late August 2009. 1250632714000 166.67682200664763 (Tic-Visit :proposal-id 11612 :visit-id "62" :proposal-version -1 :trans-version "20090702" :date "03-Aug-2009 14:53:19.0" :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 458352 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "62" :obset-id "62" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "62" :orbit-number 1 :pcs-time 333 :si-vis-utilization 3091 :al-overhead-at-end 301 :internal-dur-at-end 84 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11612 :visit-id "62" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3278 :al-overhead-at-end 72 :internal-dur-at-end 852 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3517 :pcs-gap 0 ) false 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. Very short integration time because H-alpha emission at 6564 AA is tremendously bright in this object. WAVECAL=NO because we are managing WAVECALS explicitly in this plan -- partly to delete some that are definitely not needed for the program goals, and partly to force some of them into the occultation period. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. WAVECAL=NO because we manage WAVECALS explicitly, see comment for exposure 62.003. 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. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. Normally we would use CR-SPLIT=3 for this long an exposure, but in this case the critical feature will be restricted to only a small region, a few hundred pixels. The longer individual subexposure allows time for a buffer dump, to save time for the rest of the observing sequence. WAVECAL is not needed for this wavelength interval, for several reasons. This exposure is for photometric purposes. Its exposure time is too short to produce a high-quality spectrum. WAVECAL is not needed (and not even very useful) for this exposure. This exposure is for photometric purposes. Its exposure time is too short to produce a high-quality spectrum. WAVECAL is not needed (and not even very useful) for this exposure. In this program we explicitly manage the WAVECALS that are needed. Some other WAVECALS are omitted because they are not useful for the program's scientific goals. This wvl range includes He II 4687, [Fe III] emission, etc. Mainly for photometric purposes, no WAVECAL is needed. Mainly for photometric purposes, no WAVECAL is needed. Mainly for photometric purposes, no WAVECAL is needed. Mainly for photometric purposes, no WAVECAL is needed. Short exposure to get bright peak of H-beta, only a few pixels. No CR-SPLIT or WAVECAL is needed. H-beta; no WAVECAL is needed and we don't have time for one. Accurate wavelengths can be gotten from the 4706 exposures, using Eta Car's forest of narrow well-known emission lines. Short exposure in case some of the bright features saturate in the regular exposure A 3936. Hope to see faint extended [Ne III]. Hope to see faint extended [Ne III]. This long exposure is intended to occur during buffer readout. Short exposure in case some of the bright features saturate in the regular exposure A 3936. Duplicate of an exposure in orbit 1, to check on photometric repeatability. No WAVECAL is needed. Duplicates an earlier exposure, to test photometric repeatability (or rather, pointing drift and jitter). No WAVECAL is needed for this purpose. WAVECAL=NO because we explicitly do the WAVECAL at the end of the orbit. WAVECAL=NO because we explicitly do the WAVECAL at the end of the orbit. WAVECAL=NO because we explicitly do the WAVECAL at the end of the orbit. WAVECAL=NO because we explicitly do the WAVECAL at the end of the orbit. WAVECAL=NO because we explicitly do the WAVECAL at the end of the orbit. ORIENT goal is to get observations with approx same slit coverage as in Aug 2009. ORIENT = 346.6 deg would match those obs. ...We can widen the acceptable range somewhat if this is operationally necessary. 1267624447000 347.3 (Tic-Visit :proposal-id 11612 :visit-id "64" :proposal-version -1 :trans-version "20091209" :date "04-Feb-2010 06:48:37.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "24" :si-bright-earth-limb-angle 20.0 :data-volume 566240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "64" :obset-id "64" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "64" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2739 :al-overhead-at-end 72 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11612 :visit-id "64" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2849 :al-overhead-at-end 75 :internal-dur-at-end 185 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11612 :visit-id "64" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2857 :al-overhead-at-end 72 :internal-dur-at-end 847 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) true 3 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. H-alpha is very bright even in the ejecta. H-alpha is very bright even in the ejecta. THIS LONG EXPOSURE IS INTENDED TO MAKE USE OF THE TIME REQUIRED FOR A BUFFER DUMP. The precise exposure time is not important, provided that it occurs DURING the buffer readout, not before or after. If this trick is not feasible, then this long exposure should be omitted. 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. WAVECAL=NO because we are managing WCALs explicitly. This long exposure is intended to coincide with a buffer dump. For photometry, no WCAL needed. For photometry, no WAVECAL needed. For photometry, no WAVECAL needed. For photometry, no WAVECAL needed. Primary goal photometry, WAVECAL not needed and we don't have enough time for WAVECAL. Primary prupose photometry, WAVECAL not needed. Primary purpose photometry, WAVECAL not needed. ORIENT is intended to duplicate slit orientation used for previous Aug 2009 and Mar 2010 observations. Optimum value is 166.6 deg. -- -- **Two comments about possible calendar dates for this visit: *** 1. According to APT Visit Planner, dates between 9 Aug and 28 Aug 2010 are feasible. If convenient, we prefer the last part of that interval, preferably after 20 August. 2. The Visit Planner shows a gap (not-feasible) in 10--16 August. However, if we reduce the exposure list by a small amount, this gap disappears and the entire period 9--28 Aug 2010 becomes OK with Visit Planner. (Tic-Visit :proposal-id 11612 :visit-id "67" :proposal-version -1 :trans-version "20100505" :date "16-Jun-2010 18:24:40.0" :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 481312 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11612 :visit-id "67" :obset-id "67" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11612 :visit-id "67" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2784 :al-overhead-at-end 75 :internal-dur-at-end 130 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11612 :visit-id "67" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2961 :al-overhead-at-end 72 :internal-dur-at-end 779 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3511 :pcs-gap 0 ) false 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. Very short integration time because H-alpha emission at 6564 AA is tremendously bright in this object. WAVECAL=NO because we are managing WAVECALS explicitly in this plan -- partly to delete some that are definitely not needed for the program goals, and partly to force some of them into the occultation period. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; CR-SPLIT=3 instead of 2, to somewhat reduce the saturated area. WAVECAL=NO because we manage WAVECALS explicitly, see comment for exposure 003. 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. Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; - Includes HeI 6680 line, and wings of H-alpha. Central part of H-alpha will saturate heavily in this exposure; WCAL=NO because we manage wavecals explicitly. Extra exposure, very long, to take advantage of buffer-readout that APT Orbit Planner (v 18.2) puts at this time. This exposure has low priority and perhaps it can be deleted if it CANNOT be done during buffer readout. 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. This long exposure is intended to coincide with a buffer dump that APT Orbit Planner puts at this time. Same story as for exposure 67.009. Intended to get quick look at entire UV. Intended to get quick look at far UV. With this exposure time, the longer wavelengths covered by this grating will be saturated. Compare preceding shorter exposure. Intended only to take advantage of a STIS buffer dump that APT Orbit Planner puts at this time. Same story as for exposures 67.009 and 67.015. Some pixels on the star will be saturated in this triple exposure.