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Please specify your scheduling constraints or 'No Constraints' on all Observation forms.0Assigned ID: 1046
----- Attempting Submission 1 (Fri Aug 09 11:34:59 GMT 2019) -----
HST Phase I Proposal 1046 (corcoran.apt) successfully submitted.
Receipt: # 1046-1Joint Chandra/HSTThis is a close duplicate of proposal 15611 and requires permission for an additional wavecal at E140H 1234A given the very faint
nominal wavecal encountered in 15611 visits. We note that visibility of Eta Car appears to be much more constrained than in past visits
and that there seems to be no difference between CVZ window and 100% schedulability window. i.e. the display for visibilities behaves
peculiarly. Is the lessened visibility due to precession of the HST orbit?
We will be reviewing this plan over the next few weeks paying close attention to changes seen in ongoing CHANDRA/HST-STIS
observations, from the ground-based high dispersion monitoring with the intent to fine-tune these visits should such be deemed
necessary.
Revision#1 Special WAVECAL exposure for E140H 1234A setting revised to 100 seconds as per advise of Dan Welty email of 20190909
REvision#2 Given that WAVECAL=No, we have manually inserted wavecals for each spectrum, but with the wavecal after the exposure.
This increases the observing time by 68 seconds. However, there is deadtime during readout, which might still be used to increase
exposure times?
Revision#3 Attempts to minimize the dump overheads via 1598:Source-lamp 1416:lamp-source 1234 source-lamp in earth occultation.
Revision#4 Due to flares in NICER observations and upcoming CHANDRA spectrum visit on 27-29 January, we are moving visit 4
forward to January 20-28, having shortened exposure times to accommodate decreased visibility. Concurrent observations with NICER
and ground-based spectroscopy are ongoing. Note visit 2 remains as in declining X-ray flux domain just before periastron.
Submission 5: Shortened visit 3 so it could be scheduled close to the CHANDRA visit.
Submission 6: Adjusted window on vist 3 to be 1-15 March and added 100 seconds backinto exposures (3 and 7).
Window for visit 4 is now 1 to 30 April 16 to 46 days after visit 3
Submission 6: adjusted window to accommodate changing gyro restrictions to obtain 1 Mar window.838268865----- Attempting Submission 1 (Wed Aug 21 19:07:31 GMT 2019) -----
----- Attempting Submission 2 (Mon Sep 09 19:08:42 GMT 2019) -----
----- Attempting Submission 3 (Thu Sep 26 11:35:33 GMT 2019) -----
----- Attempting Submission 4 (Sat Jan 11 16:46:47 GMT 2020) -----
----- Attempting Submission 5 (Wed Feb 12 01:27:51 GMT 2020) -----
----- Attempting Submission 6 (Wed Feb 12 22:01:05 GMT 2020) -----
----- Attempting Submission 7 (Mon Feb 17 19:46:10 GMT 2020) -----Eta Carinae: Taking the PlungeEta Carinae is the nearest superluminous binary system we can easily study. Over the past 20 years the HETGS has been a key to unlocking the dynamics of the wind-wind collision and the nature of the hidden companion star. The AO 21 interval includes the next periastron passage, offering us a view of the hot gas in the wind-wind bow shock as it plunges towards the primary. We request Chandra and HST imaging spectrometry to uniquely probe the wind-wind shock on scales from the stellar separation to 100s of AU. These observations and our approved AO20 HETG Eta Car observations (not yet obtained),with new imaging with VLTI/MATISSE, and previous X-ray spectra from Chandra and other instruments will provide a detailed view of the colliding wind shock structure and the nature of the companion.
The four HST/STIS orbits are committed to monitor the FUV spectral changes as the X-ray flux peaks, then drops through the minimum.The four orbits will be dedicated to single orbit visits recording the FUV spectra in coordination with the X-ray spectroscopic visits by CHANDRA. Visibiilty has evolved for Eta Carinae. Previously it has been accessible for nominal orbits throughout the year, but apparently is less accessible. The projected windos, 19-Dec-31 Dec-2019, 8-Feb- to 24 Feb-2020 and 20-Mar-13-Apr-2020 do not align as well as anticipated during the proposal cycle. The best match appears to beas follow:
CHANDRA visit WINDOW HST VISIT APT PLANNING HST/STIS WINDOW
1-3 5 Jan to 5 Feb-2020 1 28 to 31-DEC-2019 (two or three visits planned for CHANDRA grating)
4 18 to 25 Feb-2020 2 8 to 24-FEB-2020 Visit with CHANDRA/ACIS
5 29-Feb to 8-MAR-2020 3 20 to 31-MAR-2020 2nd visit with CHANDRA/ACIS
4 1 to 18-APR-2020 Followup during late portion of low stateThe proposal team has devoted much effort to the study of Eta Carinae across the past four 5.5 year cycles with well over 60 refreed papers demonstrating results.
Drs Corcoran, Hamaguchi, Petre and Espinoza are experts in the behaviour of the X-ray spectral changes as the binary system approaches periastron.
Dr. Gull is expert on the application of the HST/STIS to studies of Eta Carinae especiallly in the ultraviolet and spatial mapping of the fossil wind structures.
Dr. Weigelt leads a team of experts studying the near infrared changes in the massive binary utilizing the VLTI with approaching milliarcsecond angular resolution.
Dr. Damineli originally discovered the binarity of Eta Carinae and continues to lead studies of the pectrophotometric changes, both long term and cyclic, over the past four decades.
Dr. Hillier is expert on the extended stellar atmospheres of massive stars and has spearheaded several studies of Eta Carinae from Uv to infrared.
Drs. Madura, Pittard and Russell have pioneered the 3-D hydrodynamical modelings of Eta Carinae and will apply their expertise to modleling of the X-ray and UV spectra.
Dr. Richardson leads an extended ground-based study of changes in stellar line profiles, especially of He I and correlations with the FUV spectra.
Dr. Moffat is expert in the properties of massive stars, especially Wolf-Rayets in binary systems.Stellar Physics6falsefalsefalsefalsefalsefalsefalseAVAILABLESTARETA CARINAE STARWOLF RAYET - WNNOThis utilizes special astrometry that has been accurate for observations from 2000 to 2019.
The stated flux is an upper limit as historically Eta Car begins to fade in the UV a few months before periastron.
However, being very cautious of the MAMA global count rate, we shift from E140M to E140H.J2000J20002e-11 erg cm2 s at 1400ASTIS/FUV-MAMASpectroscopicNoNoE140MSTIS/NUV-MAMASpectroscopicNoNoE230H1863STIS/FUV-MAMASpectroscopicNoNoE140MSTIS/NUV-MAMASpectroscopicNoNoE230H1863STIS/FUV-MAMASpectroscopicNoNoE140MSTIS/NUV-MAMASpectroscopicNoNoE230H1863STIS/FUV-MAMASpectroscopicNoNoE140MSTIS/NUV-MAMASpectroscopicNoNoE230H1863Timing link suitability includes constraints ([02 After 01])The scheduling data was generated by CASM 28.0.CASM was run in Phase II mode.This visit is to be within the first CHANDRA window in January 20201577569033000303.43799210667703(Tic-Visit
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