For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. 0 Assigned ID: 4008 ----- Attempting Submission 1 (Sun May 21 21:46:55 GMT 2023) ----- HST Phase I Proposal 4008 successfully submitted. Receipt: # 4008-1 ----- Attempting Submission 2 (Mon May 22 14:36:06 GMT 2023) ----- We will use G160M at LP4. This has been mentioned in the submitted PDF file. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Added visit 51, a copy of visit 01, which failed. HOPR 92908 was submitted and approved by the TTRB for a repeat. 503752904 ----- Attempting Submission 1 (Mon Sep 04 16:37:04 GMT 2023) ----- ----- Attempting Submission 2 (Thu Aug 08 14:52:31 GMT 2024) ----- The warning is that COS FUV PSA is being used for an extended target. We are aware of the calibration limitations. The much anticipated eclipse of R Aquarii (R Aqr) in its 44 year binary orbit is underway. The hot White Dwarf (WD) and accretion disk have moved in front of the cool, dusty mass losing AGB companion giving us a direct view of the accretion flow. The system has just passed periastron, and is in a high state of binary activity, with material being injected near the base of the bipolar jet into a fast collimated flow. Fast shocks with speeds of up to, perhaps, 250 km/s are being driven into the surrounding photoionized nebula and into the pre-existing jet material. These shocks will raise the ionization levels of the gas and produce bright high-ionization emission lines in the ultraviolet (UV). We propose to use COS to obtain UV spectra (spanning 1135-3200 Ang.) of the region immediately surrounding the binary, and use the emission lines to identify and measure the various processes energizing the inner nebula during this extremely active phase. We will study the evolution of the UV emission and their causes by comparing our data with IUE spectra obtained over half an orbital period ago. During this critical phase in its binary orbit, R Aqr is being intensively monitored from the ground, and has been observed at all wavelengths from the radio to the X-ray except that no UV spectra have been obtained. This eclipse will end in a few years time, and there is an urgent imperative that COS spectra be obtained to unravel key physical processes underlying the accretion and jet formation in this nearby object. The insights gained will have wide applicability, in many astronomical systems where accretion and jets are present. The program consists of one 3-orbit visit with a single pointing centered on the R Aqr symbiotic binary. The source spectrum consists of a relatively weak continuum and a number of emission lines of varying strength as detected in several IUE observations, e.g. Kafatos et al. 1986 ApJ Supp. 62, 853; Meier and Kafatos 1995 ApJ 451, 359 (MK95). It is expected that the continuum is dominated by the central source comprising the AGB, WD and accretion disk, while the emission lines arise in an extended, yet compact, nebula surrounding the binary. Our proposed visit starts with an NUV ACQ/IM exposure. The co-ordinates are well known, and since the NUV bandpass will be dominated by the continuum we expect the target to be well centered. Following the acquisition are a series of spectroscopic exposures listed below. NUV: G185M/1913, G225M/2325, G230L/2635, G230L/2950 FUV: G130M/1291, G160M/1611 Each NUV mode will be observed at the two extreme FP-POS (1, 4) for wavelength coverage. The G160M/1611 exposures should be obtained at LP4 in order to maximize S/N without the large overheads for split wavecals. (This was requested in our Phase I proposal.) The ETC calculations used for both Phase I and Phase II use IUE fluxes reported in MK95. For Phase I, we mainly used fluxes of the weaker lines in order to estimate the required exposure times. Here, we instead use the highest observed fluxes. In Phase II calculations we have used a continuum surface brightness of 5E-14 cgs, which is five times the value used in Phase I. This is primarily to show that the count-rates are well below the bright object limits, and secondarily to estimate suitable BUFFER TIME values. In most cases the BUFFER TIMES have been chosen for maximizing efficiency. Dr. Ravi Sankrit has expertise in FUV emission line spectroscopy and the analysis of shock spectra, with a long background in the study of supernova remnants and, more recently, symbiotic Miras. He is leading the analysis of COS spectroscopy of the symbiotic system HM Sge obtained as part of an HST-SOFIA DD program. Dr. Thomas Ake is an expert in ultraviolet spectroscopy of interacting binaries, and has studied them using IUE, HST/GHRS and FUSE. He has experience in determining the physical characteristics in these complex systems where a hot companion is embedded in the circumbinary environment. Dr. Manuel Bautista is an expert in the field of atomic processes and atomic data, and their use in modeling spectra from a variety of astronomical objects. Dr. Steven Goldman's expertise is in the field of evolved stars, and is PI on the HST/SOFIA DD proposal on HM Sge. Dr. Uma Gorti has expertise in photoionization chemistry, and modeling line emission from shocks and disks in irradiated environments. She is also an expert in the theory of accretion disks and their physical and chemical evolution. Prof. Shazrene Mohamed is an expert on hydrodynamic modeling of mass-transfer and outflows in evolved binary star systems, and their interactions with the circumstellar surroundings. Mr. Eric Omelian has expertise in 3D radiative transfer modeling of circumstellar shells, and has been PI on the SOFIA proposals from Cycles 4 through 9 monitoring R Aqr in the mid-infrared. Stellar Physics and Stellar Types 6 false true false false false false false AVAILABLE STAR SYMBIOTIC STAR YES Co-ordinates and propermotions obtained from SIMBAD, which uses Gaia DR3. J2000 J2000 COS/NUV Imaging No No MIRRORA COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G160M 1611 COS/NUV Spectroscopic No No G185M 1913 COS/NUV Spectroscopic No No G225M 2325 COS/NUV Spectroscopic No No G230L 2635 COS/NUV Spectroscopic No No G230L 2950 1723128569064 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1719432839000 229.8613273759538 (Tic-Visit :proposal-id 17451 :visit-id "01" :proposal-version -1 :trans-version "20240604" :date "08-Aug-2024 10:49:28.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1843760 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17451 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17451 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2643 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "01" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2615 :al-overhead-at-end 0 :internal-dur-at-end 95 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "01" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2637 :al-overhead-at-end 0 :internal-dur-at-end 455 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) false 3 0 Used December 1991 IUE spectrum to estimate exposure time. Increased the exposure time from the calculation result by a factor of 4 in order to get a higher S/N image of the field, and also to guard against the flux having decreased. The C III] line is described as saturated in MK95; we use twice their reported flux in our calculation and show it is still safe. The ETC run includes the total CIV 1548,1552 doublet flux as a single line, and both OIII] 1663 and NIII] 1750. Calculation COS.sp.1888995 includes the CIV lines separately and the OIII]. 1723128571020 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. Repeat of failed visit 01. 1751019534000 229.8633460916226 (Tic-Visit :proposal-id 17451 :visit-id "51" :proposal-version -1 :trans-version "20240604" :date "08-Aug-2024 10:49:30.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1843760 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17451 :visit-id "51" :obset-id "51" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17451 :visit-id "51" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2643 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "51" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2615 :al-overhead-at-end 0 :internal-dur-at-end 95 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "51" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2637 :al-overhead-at-end 0 :internal-dur-at-end 455 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3023 :pcs-gap 0 ) false 3 0 Used December 1991 IUE spectrum to estimate exposure time. Increased the exposure time from the calculation result by a factor of 4 in order to get a higher S/N image of the field, and also to guard against the flux having decreased. The C III] line is described as saturated in MK95; we use twice their reported flux in our calculation and show it is still safe. The ETC run includes the total CIV 1548,1552 doublet flux as a single line, and both OIII] 1663 and NIII] 1750. Calculation COS.sp.1888995 includes the CIV lines separately and the OIII]. 1767102503647 /System/Volumes/Data/solaris/user1/williamj/hst/work/cycle31/OP-cache/17451-v52.xml Repeat of failed visit 51. (Tic-Visit :proposal-id 17451 :visit-id "52" :proposal-version -1 :trans-version "20250929" :date "30-Dec-2025 08:48:23.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1843760 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17451 :visit-id "52" :obset-id "52" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17451 :visit-id "52" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2642 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "52" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2615 :al-overhead-at-end 0 :internal-dur-at-end 95 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17451 :visit-id "52" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2637 :al-overhead-at-end 0 :internal-dur-at-end 453 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 2976 :pcs-gap 0 ) false 3 3 Used December 1991 IUE spectrum to estimate exposure time. Increased the exposure time from the calculation result by a factor of 4 in order to get a higher S/N image of the field, and also to guard against the flux having decreased. The C III] line is described as saturated in MK95; we use twice their reported flux in our calculation and show it is still safe. The ETC run includes the total CIV 1548,1552 doublet flux as a single line, and both OIII] 1663 and NIII] 1750. Calculation COS.sp.1888995 includes the CIV lines separately and the OIII].