0Assigned ID: 711
----- Attempting Submission 1 (Fri Apr 05 20:23:50 GMT 2019) -----1. IMPORTANT: For each timing-requirement window, the best time is near the _middle_ of the window. In the past,
we have noticed that observations tend to be scheduled near the beginning of a specified window. -- Which would
not be a good strategy for this program. Central part of the window is definitely better.
(Perhaps we should have specified narrower windows. -- But window availability is very important here.)
-----
2. Brightness limits for STIS/MAMA are worth noting for this object. See various comments for Visit 4. Here our
safety precautions are the same as we used in some previous MAMA observations.l
-----
3. The Target Confirmation Charts Tool is useless for Eta Carinae, because it's in a very crowded region with
bright nebulosity, which GSC was apparently unable to cope with. See point 5 below. BOT is also useless,
for similar reasons. See comments for visit 4.
-----
4. Like all successful HST programs on this target since 1998, the acquisition uses special catalog ZZZQ. Comparisons
with Gaia show that ZZZQ is very good except for a small number of unusually bad stars. If we can get information on
which acquisition/guide stars will be chosen, then we can confirm whether they're OK (and they probably will be).
So far, ZZZQ has never failed; but we are especially worried for this program because it concerns a one-time event.
-----383001951----- Attempting Submission 1 (Wed Jul 24 18:13:30 GMT 2019) -----``Last Call!'' Eta Carinae's Spectroscopic Event in 2020Eta Car, the only giant eruption survivor that can be studied well, has been unsteady in recovering from the 1830-1870 explosion. About 20 years ago its spectroscopic and photometric trends dramatically accelerated -- signaling a rapid decrease in the primary mass loss rate. This is a novel clue to the stellar interior's thermal and rotational disequilibrium following the eruption.
Meanwhile, "spectroscopic events" occur at 5.54-year intervals marking the companion star's periastron. HST showed that the basic nature of these events changed between 2003 and 2014 --but we do not know whether this change was temporary, or permanent, or the precursor to something more extreme. Hence the next spectroscopic event, in early 2020, is crucial.
For reasons noted in the proposal, ground-based instruments have inadequate spatial resolution for this purpose, and can't observe the UV. 2020 will be our last opportunity for HST spectroscopy, and the star will be
irreversibly changed when suitable instruments become available sometime in the future. Therefore we propose an adequate set of STIS/CCD and STIS/MAMA observations. They will be valuable for a wide range of topics including stellar instabilities, colliding-wind physics, and abnormal emission-line processes as well as eta Car's recovery from a giant eruption.Eta Car's periastron spectroscopic event will occur mainly in January-April 2020. This program samples it with STIS-CCD in 7 one-orbit visits, plus a single orbit for STIS-MAMA near the middle of the event. Much later, 2 more orbits in Cycle 28 will show the post-event state of the object.
---
Each CCD visit includes several critical wavelength intervals. Approximately in decreasing order of spectroscopic priority, these are --
(1) Interval 4570-4840 A using grating G430M. This includes the exotic HeII 4687 flash, the EUV-excited N II 4600 multiplet, a significant He I feature, and useful low-excitation features.
(2) 6490-7040 A using G750M. The H-alpha line profile changes dramatically during an event, and so does He I 6680. This also provides photometry of the red continuum.
(3) 2760-2910 A using G230MB. This includes the bright Mg II emission feature, plus necessary UV continuum photometry.
(4) 3800-4070 A using G430M. This range includes a variety of diagnostics including high-order Balmer lines, Ca H & K, and He I.
In addition, we also use low-dispersion gratings G230LB and G430L for photometry across the broad wavelength range 1700-5500 A. A secondary purpose of the low-dispersion spectrum is to detect any major unexpected changes outside the main wavelength ranges listed above.
---
Incidentally, these slit spectra also provide useful information about ejecta located 0.2 to 4 arcsec from the star. (But the star is far more important for our goals.)
---
The STIS-CCD exposure times range from 0.2 to 150 seconds (totals of CR-SPLITS). For practical reasons they are not done in order of scientific priority. In order to obtain sufficient schedulability throughout the January-April time interval, the usable time in each orbit is reduced by several minutes.
---
In the MAMA visit, echelles E140M and E230M cover the entire attainable UV range 1300-3100 A,, using the FUV and NUV detectors respectively. Exposures of several hundred seconds give high S/N, so the combination fits well into one orbit. Regarding detector brightness limits, we apply a double test: specific count rates were found in earlier observations of the same type, and CCD visits 1 and 2 will give information about the current UV brightness level. See comments in Visit 4..
---
Concerning HST's gyro issue: 1-gyro operation would most likely cause a shortage of visibility windows during the 4-month event. In that case we would need to heavily revise the plan -- for instance, reducing the number of observations per visit might allow more time-windows, and/or we might need to accept sparser temporal sampling.. Meanwhile, depending on gyro performance and jitter amounts, we might need to use the 52x0.2 slit instead of 52x0.1. This would be acceptable for the main science goals.
---The PI, Dr. Kris Davidson has more than 20 years experience with HST data. He has led the numerous STIS proposals on eta Car since 1998 and the HST Treasury Program on eta Car, one of the first three treasury programs in 2003. He is responsible for program oversight and leads the analysis of the stellar wind from the CCD spectra. Dr John Marin has been a co-I on the eta Car programs since 2003. He is responsible for resonstruction of the multi-wavelength photometry and light curves. Co-I Dr. Kazunori Ishibashi is experienced with observations from X-ray through near-IR. He is primarily responsible for reduction of the STIS CCD and MAMA data and focuses on the analysis of UV spectra. Co-I Dr. Roberta Humphreys is an experienced HST user on this program as well as other HST programs on massive stars. This team has over 30 refereed publications on eta Car, most based on HST observations.Stellar Physics0falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARETA CARINAE STARSpecial catalog ZZZQ was prepared in 1989 because the original HST GSC was very poor in this crowded nebular region. Later GSC, and especially GAIA, would _probably_ be OK for Eta Car acquisition. However, ZZZQ was used for nearly every successful Eta Car HST observation 1991--2018, and it never failed. Absolute position of Eta Car is still uncertain at the 0.2 arcsec level, even with GAIA, because this object has asymmetric structure at every size scale. The RA and dec listed here were used for successful programs in 2014 and 2018.J2000J2000STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430M3936STIS/CCDSpectroscopicNoNoG430M4706STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230MB2836STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG750M6768STIS/CCDSpectroscopicNoNoG430M3936STIS/CCDSpectroscopicNoNoG430M4706STIS/CCDSpectroscopicNoNoG430L4300STIS/CCDSpectroscopicNoNoG230LB2375STIS/CCDSpectroscopicNoNoG230MB2836STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230M1978The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The MOST DESIRABLE date for this visit is 22-JAN-2020. This is in the first obvious stage of eta Car's spectroscopic event. Dates near the beginning and end of the timing requirement are not as good as Jan 22.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day orbit cycle: 22 Jan 2020 = MJD 58870 has phase = -0.0178 = -36 days in the standard "Treasury Program" system. (Periastron is most likely t = -15 days +/- 10 days.)1579444678000322.4879187476653(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicit WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this might help to force a WCAL into the occultation period after last science exposure. (At least these were the reasons in earlier HST cycles.)Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.CR-SPLIT=3 because the long-wavelength end of this low-dispersion spectrum will be saturated. If we use 3 subexposures instead of 2, then useful data extends to slightly longer wavelength.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The most desirable time for this visit is as early as possible after Feb 7. According to the Visit Planner, it is very difficult to schedule a visit in the days before Feb 8. Since we do not know exactly why this is true, this one-orbit visit uses an unusually short amount of time within the orbit. --
Phase in the 2023-day orbit cycle: 8 Feb 2020 = MJD 58887 has phase = -0.0094 = -19 days in the "Treasury Program" system.--1581470381000343.50609275398983(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.WAVECA:L after orbit visibility time.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The most desirable date for this visit is 22-FEB-2020. This represents a particular stage in eta Car's spectroscopic event.. Dates near the beginning and end of the timing requirement are not as good as Feb 22.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day orbit cycle: 22 Feb 2020 = MJD 58901 has cycle phase = -0.0025 = -5 days.1582471124000354.5754724657075(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicit WAVECALs for reasons noted in the Visit 1 comments.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.(1) Note about timing limits: The DESIRED time is close to 8 March, the middle of the specified timing requirements. Dates near the beginning or end of this interval are not as good. ---
(2) In order to allow a wide enough observing window (i.e., a large enough range of possible dates), this plan has 8 minutes of unused orbital visibility. ---
(3) MAMA brightness limits: This target is not suitable for an ETC run, but it has been observed with STIS/MAMA several times in the past. Also we can use preceding CCD visits to verify safety. See comments for the observations.
--
Phase in the 2023-day orbit cycle: 8 Mar 2020 = MJD 58916 has phase = +0.0049 = +10 days.158391779400011.672501038211095(Tic-Visit
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)true10This ACQ plan is copied from program 15067, done in 2018.This ACQ plan is copied from program 15067, done in 2018.Re. BRIGHTNESS LIMITS: ETC is only a rough guide for this object, because the spectrum is extremely complex and changes during the spectroscopic event. Real observed count rates are better. On 21 April 2018, E230M produced 6.6 cts/s in the maximum pixel, and 143,000 cts/s in the entire detector. On average, Eta Car is brightening about 12 percent per year in the UV -- EXCEPT that it has always become temporarily fainter during each spectroscopic event.
--- In order to verify that Eta Car has not brightened by a dangerous amount, we will examine CCD-G230LB and CCD-G230MB data from visits 1 and 2.
--- Note that this object is not a strong irregular variable in the sense used for brightness limits. Absorption lines have caused rapid UV _decreases_ in previous spectroscopic events, but there have been no strong rapid increases in UV emission.Re. BRIGHTNESS LIMITS: ETC is only a rough guide for this object, because the spectrum is extremely complex and changes during the spectroscopic event. Real observed count rates are better. On 21 April 2018, E140M produced 0.5 cts/s in the maximum pixel, and 75,000 cts/s in the entire detector. On average, Eta Car is brightening about 12 percent per year in the UV -- EXCEPT that it has always become temporarily fainter during each spectroscopic event.
--- In order to verify that Eta Car has not brightened by a dangerous amount, we will examine CCD-G230LB and CCD-G230MB data from visits 1 and 2.
--- Note that this object is not a strong irregular variable in the sense used for brightness limits. Absorption lines have caused rapid UV _decreases_ in previous spectroscopic events, but there have been no strong rapid increases in UV emission.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The most desirable date for this visit is 08-MAR-2020. Dates near the beginning and end of the timing requirement are not as good as Mar 8.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day cycle:: 8 March 2020 = MJD 58916 has phase +0.0049 = +10 days.15837519980009.64295067866371(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.The most desirable date for this visit is 08-MAR-2020. Dates near the beginning and end of the timing requirement are not as good as Mar 8.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day cycle:: 8 March 2020 = MJD 58916 has phase +0.0049 = +10 days.(Tic-Visit
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)false10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The most desirable date for this visit is 23-MAR-2020. Dates near the beginning and end of the timing requirement are not as good as Mar 23.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day cycle: 23 Mar 2020 = MJD 58931 has phase = +0.0124 = +25 days.158471243000021.641317425553012(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.The most desirable date for this visit is 10-APR-2020. Dates near the beginning and end of the timing requirement are not as good as Apr 10.
In order to allow a scheduling window of several days, this one-orbit visit has about 6 minutes of unused orbital visibility. --
Phase in the 2023-day cycle: 10 Apr 2020 = MJD 58949 has phase = +0.0213 = +43 days.(Tic-Visit
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)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.The scheduling data was generated by CASM 27.2.CASM was run in Phase II mode.Timing requirement is not as strict as the earlier visits. --
Phase in the 2023-day cycle: 15 May 2020 = MJD 58984 has phase = +0.0385 = +78 days.(Tic-Visit
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:pcs-visibility 3389
:pcs-gap 0
)true10We use wavelength interval 7795 because it is relatively free of narrow emission lines produced in blobs at r = 0.2 arcsec. Shorter wavelengths would be better in other respects, but they can be perturbed by the extraneous off-center emission lines.Ultra-short exposure for bright H-alpha emission profile. WAVECAL=NO because we are explicitly managing the WCALs. Throughout this program we restrict SIZEAXIS2 to avoid buffer dump.Some H-alpha pixels will be saturated in this exposure. WAVECAL=NO because we are explicitly managing the WCALs.We use explicity WCALs for two reasons: (1) Some may be omitted if not needed for program goals, and (2) this may help to force a WCAL into the occultation period after last science exposure.Extremely important wvl interval for He II 4687 and rad-exc N II features. WAVECAL=NO because we manage the WCALs explicitly.