0 Assigned ID: 385 ----- Attempting Submission 1 (Fri Mar 06 03:44:19 GMT 2020) ----- HST Phase I Proposal 385 successfully submitted. Receipt: # 385-1 The number of orbits used exceeds the number allocated FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser POS TARG & PATTERN should be used carefully with WFC3 quad filters to avoid placing the target on the vignetted part of the field of view or moving it to another quadrant. FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser This version updates the exposure times for the red/visitble filters to account for 1.5 magnitude increase in flux from the primary variable star. -946222917 ----- Attempting Submission 1 (Fri Jun 19 18:54:28 GMT 2020) ----- ----- Attempting Submission 2 (Tue Mar 16 22:04:18 GMT 2021) ----- ----- Attempting Submission 3 (Tue Apr 27 13:25:42 GMT 2021) ----- The warnings stem from setting the FLASH levels to 20 as per WFC3 Instrument team guidelines for CTE mitigation, whereas APT was based on rules stating a level of 12 was sufficient. We propose HST/WFC3 observations of the R Aqr symbiotic system, with joint Chandra and VLA observations, to carry out a high-angular resolution multiwavelength study of the binary environment and of the spatial and spectral characteristics and propagation of the ejecta resulting from the recent - earlier than expected - periastron passage of the WD accretor. The proposed observations follow up on the 2019 to early 2020 DDT/ToO HST+Chandra+VLA observations which show dramatic changes within 1" from the central binary since 2018, including newly ejected material obscuring the evolved Mira-type star and formation of a new jet. The observations are critical for studying the effects of the WD periastron passage, which include enhanced accretion and mass/jet ejections in this nearby symbiotic binary. These phenomena are observable only about twice a century, with the next periastron expected in about 40 years. We request a total of 5 orbits, in 1 visit. We plan to carry out HST WFC3/UVIS imaging of R Aqr, using the 4-point dither mode in several filters. This approach will allow us to reach the maximum resolution of 0.025''/pixel and also assist in cosmic ray removal. This will nearly double the number of pixels covering the regions of interest. Furthermore, better sampling of the PSF will allow further enhancement in the resolution using deconvolution techniques such as Richardson-Lucy or EMC2. We have selected a set of filters to separate line and continuum emission , and to distinguish shocked from photoionized emission. The high-resolution images obtained in the spectral lines e.g., CII] 2326angstroms(A), Mg II 2800A, [OII] 3726A, [OIII] 5007A, H-alpha, and [SII] 6731A, will provide information on the ionization state of the gas. The CII] line can also help determine the (dust) extinction and it is sensitive to carbonatious grain-depletion. The Mg II 2800A line is expected to have a resonant scattering component and will also provide information on the ionization state of the gas. The [OII] 3726A line is a density indicator (the line is bright when the density is low). Furthermore, the [OII] 3726A/[CII] 2326A ratio is a good indicator of temperature and density characteristics of the gas. The SII] 6731A/H-alpha ratio will allow us to identify shocked vs. ionized gas emission, e.g., the ratio will be >=0.4 for shocked gas, and smaller for photoionized gas. The exposure times are based on the online WFC3 ETC calculations as verified by the 2020 WFC3 observations of R Aqr. We optimize the efficiency of the observing time by using subarray readouts (1024x1024 readout) to minimize the overheads, while still providing a >=40''x40'' field of view. Our observations include some flash exposure in order to partially remediate the effects of charge-transfer inefficiency due to the age of the detector. The Phase II proposal was generated using the latest APT based on the desired exposure times to avoid saturation and on the use of dither patterns, and makes the most efficient use of the observing time. In the event a reduced gyro mode will need to be used for this proposal, it will not have any significant impact as long as the target is in the HST field-of-regard when the observations need to be taken in order to catch this time-sensitive behavior of the target since we have no roll constraints for our observations. We request that these observattions be coordinated with the Chandra observations. The expertise of our team is complementary (multiwavelength observations and analysis, and theoretical modeling) which will allow us to achieve the goals of our proposal. Dr. Margarita Karovska: Scientific expertise in multiwavelength observational studies and modeling of interacting binaries including symbiotic systems. High-resolution imaging expertise (including deconvolution techniques) allowing to achieve maximum resolution (e.g., previous HST, Chandra and VLA observations) including of symbiotics R Aqr, CH Cyg, Mira, and other interacting systems). Warren Hack: Expertise in HST imaging software and data processing expertise (e.g., primary developer of the Drizzlepac package). He has been applying novel dithered-images combination techniques and PSF simulations, allowing to reach the finest resolution achievable with the HST (e.g., previous HST studies of symbiotics R Aqr, CH Cyg, Mira, HM Sge). John Raymond: Extended expertise in modeling of plasma characteristics of a wide range of astrophysical sources, including symbiotics (of the central source and of the jet-structures-based on previous HST observations) Terrance Gaetz: Expertise in Chandra data analysis ,especially in spectral modeling and fitting Vinay Kashyap: Expertise in Chandra data analysis , especially in imaging and spectral fitting Amy Mioduszewski: Expertise in radio observations and analysis of JVLA data of interacting binaries Mark Claussen: Expertise in radio observations and analysis of JVLA data of evolved stars Stellar Physics and Stellar Types 6 false false true false false false 70 6.5 true SUPPORTED STAR ACCRETION DISK INTERACTING BINARY JET SYMBIOTIC STAR This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F373N WFC3/UVIS Imaging No No F280N WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No FQ437N WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No FQ232N WFC3/UVIS Imaging No No FQ243N WFC3/UVIS Imaging No No F555W POS-TARG DITHER 0.145 LINE false false 4 46.86 SPIRAL 2 false 1619531952859 The scheduling data was generated by CASM 29.0. CASM was run in Phase II mode. /private/var/folders/q9/0jb3sqc10kx2dw3wnl21b_dw000702/T/OPVisit15566714343597452814.xml (Tic-Visit :proposal-id 16312 :visit-id "01" :proposal-version -1 :trans-version "20200619" :date "27-Apr-2021 09:59:12.0" :trans-errors '(:WARNINGS 3 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1557728 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16312 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Obset :proposal-id 16312 :visit-id "01" :obset-id "A1" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16312 :visit-id "01" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2822 :al-overhead-at-end 87 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16312 :visit-id "01" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2719 :al-overhead-at-end 87 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16312 :visit-id "01" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2811 :al-overhead-at-end 87 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16312 :visit-id "01" :orbit-number 4 :pcs-time 392 :si-vis-utilization 2486 :al-overhead-at-end 178 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16312 :visit-id "01" :orbit-number 5 :pcs-time 383 :si-vis-utilization 2767 :al-overhead-at-end 178 :internal-dur-at-end 190 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3156 :pcs-gap 0 ) true 5 3