0Assigned ID: 3728
----- Attempting Submission 1 (Fri Mar 25 23:41:58 GMT 2022) -----
HST Phase I Proposal 3728 successfully submitted.
Receipt: # 3728-1
----- Attempting Submission 2 (Sat Mar 26 00:37:31 GMT 2022) -----0----- Attempting Submission 1 (Wed Jul 13 21:22:04 GMT 2022) -----
HST Phase II Proposal 17124 successfully submitted.
Receipt: # 17124-1
----- Attempting Submission 2 (Wed Jul 13 21:23:27 GMT 2022) -----
HST Phase II Proposal 17124 successfully submitted.
Receipt: # 17124-2
----- Attempting Submission 3 (Thu Oct 12 16:55:14 GMT 2023) -----
----- Attempting Submission 4 (Fri Nov 17 20:52:44 GMT 2023) -----
HST Phase II Proposal 17124 successfully submitted.
Receipt: # 17124-4
----- Attempting Submission 5 (Mon Nov 20 03:23:31 GMT 2023) -----I ran the vist planner, but it keeps asking me to run it again.High Resolution Spectroscopic Mapping of Mass Loss in Luminous Blue VariablesHigh-resolution (R~110,000) HST UV spectra of the very massive LBV, eta Car, reveal interstellar-like extremely narrow, discrete absorption components with line widths ~5 km/s arising from transitions from ground configurations and metastable levels up to 40,000 cm-1 of Fe-group ions.These features, seen at high negative velocities, arise in dense gas in the near circumstellar environment of eta Car. The implied densities, at least 10^7-8 cm-3, are highly uncharacteristic of the normal ISM. They appear to have originated from clumping in mass outflow of eta Car. IUE spectra show clumping in wind features of other LBVs and has been confirmed by optical observations of Ca II and Fe II. High-resolution UV STIS spectra coupled with proper photoionization modeling offers the only means to detect these extremely narrow absoptions and determine the physical conditions, and line-of-sight distribution (distance from the star) of the ejecta producing the extremelly narrow absoptions. Knowledge of ejecta velocities and distances will permit us to construct a time history for the ejection events. We will obtain and analyze the first high-resolution HST UV spectra of three LBVs having typical masses, and perform the same analysis on archival Eta Car spectra. This information will have many implications for aspects of LBV mass loss, evolution, and wind mechanisms that are not yet understood.We have three LBV targets with a total of 13 orbits:
MR35(Visit 1 -1 0rbit & Visit 5- 4 Orbit )
AG Car ( Visit 2 - 2 orbits & Visit 3 - 3 orbits)
HD90177( Visit 4 - 3 orbits)
In our calculations, we present exposure times for the maximum fluxes seen in archival IUE spectra at each reference wavelength, where there are many spectra for AG Car & HR Car. We will use STIS E140H, E230H, and the E140M echelles.
MR35:
We request Visit 1, which is only 1 orbit, be executed well before Visit 5, our repeat visit for MR35. We may want to adjust exposures in Visit 5, based upon the fluxes in Visit 1. We expect the fluxes of MR 35 to be lower than the IUE fluxes used. The AAVSO shows MR35
in a flux decline.
HST MAMA Detector Safety: AG Car is the UV-brightest of our targets, and as the AAVSO light-curve shows it is currently at V~5.5. We approach the buffer warning limit in a few cases, The maximum global counts we obtain is for AG Car, which is ~13,000 counts globally for source plus background.
Only overexposed IUE spectra exist for Hen 3-591=MR35 (SWP39269 & LWP18410). But IUE/SWP spectra are adequate to estimate flux levels, based upon expected flux distributions of other similar stars. Strong N V 1240 and C IV 1550 in the SWP clearly indicate an O supergiant. The AAVSO light curve shows a flux decline.
In most exposures, we try to achieve S/N = 20 or better at the quoted wavelength and flux level. Because of the brightness of our targets in some bandpasses, we often must use the small 0.2"x0.09" and 0.1"x0.03"apertures. Otherwise, we use the 0.2"x0.2" aperture. The declinations of or three targets indicate that we have 57, 57, and 56 min visibility for AG Car, Hen 3-591=MR35, and HR Car=HD 90177. All exposures were calculated using the STIS ETC.
We describe our exposures and time overhead for all three targets. These targets have pronounced extinction which is notable by extreme decreased flux near 2200A and shorter wavelengthd. Exposure times vary dramatically across the UV spectrum.P.I. Frederick C. Bruhweiler has more than 40 years of experience working with stellar ultraviolet spectra. He has been a PI or co-I on several HST and IUE proposals, and has been first author or co-author on more than one hundred refereed papers, mostly pertaining to stellar astronomy and interstellar absorption features. Bruce McCollum has more than 30 years of experience working with stellar UV spectra and has been first author or co-author on 21 refereed papers. He has been a P.I or Co-I on several HST and IUE proposals about stellar astronomyStellar Physics and Stellar TypesIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalsefalseAVAILABLESTARLUMINOUS BLUE VARIABLENOCoordinates are from Gaia.J2000J20005E-12 @ 1400A; 5.5E-12 @ 1650A; 2E-12 @ 2000A; 4E-12 @ 2400A; 1E-11 @ 2900A : LBVSTARLUMINOUS BLUE VARIABLENOCoordinates are from Gaia.J2000J20007E-12 @ 1300A; 6.5E-12 @ 1700A; 3.8E-12 @ 2000A; 3.8E-12 @ 2600A; 3.8E-12 @ 3000A : LBV- IUE fluxesSTARLUMINOUS BLUE VARIABLENOCoordinates are from Gaia.J2000J20004E-14@1305A; 7E-14@1400A; 1.5E-13@1600A; 2E-13@2400: 4E-13@2600A; 7E-13@2800A; 1E-12@3000ASTIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H2513STIS/NUV-MAMASpectroscopicNoNoE230H2013STIS/NUV-MAMASpectroscopicNoNoE230H2513STIS/NUV-MAMASpectroscopicNoNoE230H2013STIS/NUV-MAMASpectroscopicNoNoE230H3012STIS/FUV-MAMASpectroscopicNoNoE140H1598STIS/FUV-MAMASpectroscopicNoNoE140H1416STIS/FUV-MAMASpectroscopicNoNoE140H1234STIS/FUV-MAMASpectroscopicNoNoE140M1425STIS/NUV-MAMASpectroscopicNoNoE230H2762STIS/NUV-MAMASpectroscopicNoNoE230H3012Timing link suitability includes constraints ([05 After 01 by 30.0 to 365.0 days])The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.1699095610000242.67745684201338(Tic-Visit
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)true10We request Visit 1, which is only 1 orbit, be executed well before Visit 5, our repeat visit for MR35. We may want to adjuxt exposures in Visit 5, based upon the fluxes in Visit 1. We expect the fluxes of MR 35 to be lower than the IUE fluxes used. The AAVSO shows MR35 in a flux decline. on 24 Sep 23, the V-mag=12.5A 02x0.05ND is required becasue of the small aperture that we are using for the spectral exposures.Buffer-Time is 4/5 of the calculated Buffer-Time.Buffer-Time is 4/5 of that given in the ETC. NOTE: THE ADJUSTED BUFFER-TIME IS EXACTLY THE LIMIT.The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.1699240496000246.75(Tic-Visit
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)true304/5 of ETC Buffer-time is 62 sec, which is below the 99s minimum. Thus, I have split exposuure times into smll 45s segments in an attempt to get around this.Adjusted Buffer-Time=48s, which is 4/5 of that given by the ETC. i've adopted short, repeated ACCUM exposuresThe scheduling data was generated by CASM 31.1.CASM was run in Phase II mode.1699331591000257.3084198317709(Tic-Visit
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)true30Buffer-Time is 4/5 of that given in the ETC.Buffer-Time given above is 4/5 that given in ETCBuffer-Time is 4/5 of tht given in ETC.The buffer-time given bove is 4/5 tht given by the ETC.Timing link suitability includes constraints ([05 After 01 by 30.0 to 365.0 days])The scheduling data was generated by CASM 31.1.CASM was run in Phase II mode./private/var/folders/t3/4tqb59yj1252_fcp2d3vcs4r0000gp/T/OPVisit3632555812987847779.xml(Tic-Visit
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)true40on hold for data analysis in visit 014/5 the ETC buffer-time=115ss