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. 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. 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. 0 ----- Attempting Submission 1 (Mon Jul 04 22:23:23 GMT 2022) ----- These observations with the quad filters replicate the same observations from previous proposals that worked successfully. The title needed to be corrected slightly. 1555625659 Assigned ID: 3221 ----- Attempting Submission 1 (Fri Mar 25 13:34:52 GMT 2022) ----- HST Phase I Proposal 3221 successfully submitted. Receipt: # 3221-1 ----- Attempting Submission 2 (Fri Mar 25 17:32:17 GMT 2022) ----- HST Phase I Proposal 3221 successfully submitted. Receipt: # 3221-2 We propose HST observations of the R Aqr symbiotic binary system, jointly with Chandra and VLA, as a follow up on the 2020 and 2021 archival observations which show dramatic changes within 1" from the central binary resulting from the enhanced accretion during the recent periastron passage of the white dwarf (WD) accretor. These phenomena are observable in R Aqr only about twice a century, with the next periastron expected in about 40 years. Our goal is to carry out a timely high-angular resolution multi-wavelength study of this event by zooming in on the central 3" radius circumbinary region. This will allow us to determine the spatial/spectral evolution of the distribution and the characteristics of the new ejecta and jet, and to gain a unique insight into jet formation and early propagation in symbiotic and other accretion-powered systems. We request a total of 6 orbits, in 1 visit (if not possible, then in two visits within a couple of weeks from each other). The HST high-angular resolution in the spectral regions (filters) that we selected is critical for achieving the science goals of this project. It is very important to have the images at different filters obtained close in time because the R Aqr outburst and jet structures are evolving rapidly, To avoid spatial/spectral confusion of the information in the lines and the continuum we would prefer that the observations are carried in one visit. We prefer that the observations are scheduled during late Autumn 2022 to Spring 2023 when the Mira is in the vicinity of (or at) its optical minimum. The primary should have a magnitude of V less than 10.5 mag based on the 2020, 2021 and 2022 light curves. This period around minimum starts roughly 15-Nov-2022 and goes through late-June/mid-July 2023 during which time the target visibility becomes very good. The emission from R Aqr is variable, and we will be monitoring closely the light curve and spectra using ground based hotometry/spectroscopy. Depending on when the observations are scheduled, we may need to adjust the exposures accordingly - in the time frame of about a month before the actual observations. 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 0.025''/pixel, and will also assist in cosmic ray removal. Combining the dithered images will result in improvement of the sampling of the PSF and will allow us to further enhance the (nominal 0.04'') resolution using deconvolution techniques such as Richardson-Lucy or EMC2 reaching 0.025''. This will nearly double the number of pixels covering the regions of interest. We also plan several long exposures to image the fainter outer lobes and determine their morphology and evolution when compared to the archival HST observations in the past decade. Most of the selected filters were used in the 2020 and 2021 archival observations, and will allow direct comparison and study of the dynamical evolution and proper motions of individual structures (inner jet, knots and blobs). The images obtained in the spectral lines will provide information on the ionization state, temperature, and density of the gas. The [CII] line will help determine the (dust) extinction and it is sensitive to carbonaceous grain-depletion. The [Ne IV] line is a good indicator of emission from a high temperature material in the system and its surrounding environment. The F343N filter will provide the [NeV] line intensity, which will indicate whether temperatures significantly higher than $10^5$ K are present. The Mg II$\lambda$2800\AA\ line has a resonant scattering component and will provide information on the ionization state of the gas. The [OII]$\lambda$3726\AA\ line is a density indicator. Furthermore, the [OII]$\lambda$3726\AA/CII]$\lambda$2326\AA\ ratio is a good indicator of temperature and density characteristics of the gas. The [SII]$\lambda$6731\AA/H$\alpha$ ratio will allow us to identify shocked vs. ionized gas emission.The [O III]4363\AA/5007\AA\ ratio gives the temperature which further constrains the shock speed and the ionizing spectrum. The F658N filter will provide an estimate the [NII] emission and also allow us to calculate the [S II]/[N II] ratio. The ratio would be suppressed in the inner regions of R Aqr, providing a density diagnostics. The H$\alpha$/H$\beta$ ratio will map the reddening along the jet and counter-jet, and perpendicularly to the jet (e.g., orbital plane). The exposure times are based on the online WFC3 ETC calculations as verified by the 2021 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''x 40'' 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. 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 Nicholas Lee: Expertise in high-angular resolution data analysis, including PSF and data characterization and modeling. Stellar Physics and Stellar Types 6 false false true false false false 80 16 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 FQ232N WFC3/UVIS Imaging No No FQ243N WFC3/UVIS Imaging No No F275W WFC3/UVIS Imaging No No F280N WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F343N WFC3/UVIS Imaging No No F373N WFC3/UVIS Imaging No No FQ437N WFC3/UVIS Imaging No No F487N WFC3/UVIS Imaging No No F502N WFC3/UVIS Imaging No No F547M WFC3/UVIS Imaging No No F656N WFC3/UVIS Imaging No No F658N WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F763M POS-TARG DITHER 0.145 LINE false false 4 46.86 SPIRAL 2 false 1656966312746 The scheduling data was generated by CASM 30.3. CASM was run in Phase II mode. 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