0Assigned ID: 753
----- Attempting Submission 1 (Fri Mar 06 20:40:19 GMT 2020) -----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
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
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 browserWe have removed postflash parameter from ACS parallels.-132977574----- Attempting Submission 1 (Mon Jun 29 06:22:42 GMT 2020) -----
----- Attempting Submission 2 (Sat Oct 10 05:03:49 GMT 2020) -----
HST Phase II Proposal 16217 successfully submitted.
Receipt: # 16217-2
----- Attempting Submission 3 (Thu Oct 15 04:16:20 GMT 2020) -----The APT seems to warn about a post flash larger than 12.Identifying Double White Dwarf Binaries in Globular ClustersDouble white dwarf binaries (aka AM CVns) are systems with orbital periods ~5-65 mins. Because of their short orbits, they are important sources of low-frequency gravitational waves. They are also candidates for progenitors of SN Ia through the double degenerate path. In globular clusters (GCs) they are predicted to exist in large amounts due to stellar interactions. However, no single AM CVn has yet been confirmed in any GC. We propose to carry out the first multi-epoch UV study of the low extinction, relatively massive Galactic GC 47 Tuc to identify the missing population of AM CVns through their outbursts. Using this novel technique we will test dynamical formation and evolutionary models of these binaries in clusters. We will also refine predictions of AM CVns as potential gravitational wave sources to be detected with LISA. Finding an upper limit on the rate of identifications that is lower than expected would change the current paradigm of GCs as efficient factories of compact binaries, especially those harboring white dwarfs. That would mean that the double degenerate path for SN Ia is negligible, which ultimately has cosmological implications.Our goal is to identify blue transients in the cluster. We have 9 visits of 1 orbit each. For the primaries we use the F225W and F275W filters on the UVIS channel of WFC3 in order to overcome the stellar crowding. We point at the center of the cluster. In order to remove cosmic rays and other artifacts we obtain 2 images per filter for a total of 4 per orbit. Each F225W observation has an exposure of approximately 715s and the F275W observations have 600s, optimazed to obtain the same signal-to-noise. For the primaries, the strategy is the same for each of the 9 visits.
We simultaneously obtain parallel observations with the WFC on the ACS. We are using 3 filters: F435W, F635W and F658N. Due to dumping and maneuver times to cover the chip gaps, we accomodate 4 parallel images per orbit. Our statrategy is to obtain 2 images in 2 different filters every orbit, alternating between the F435W and F658N filters between visits. This help us to remove cosmic rays and other artifacts each orbit, giving us reliable colors of the sources identified. For the first parallel visit we use the combination F625W and F435W, with longer exposures in F435W because it is the bluer filters. The total exposure times per orbit are 873s for F625W and 1150s for F435W, each divided in 2 observations.
For the second parallel visit we use the combination F625W and F658N. In this case we give more weight to the narrow filter. Total exposure times are 474s in F625W and 1240s in F658N, divided in 2 observations each. Our third and fouth observations are similar to our first and second one, respectively. The rest repeat the pattern.
We set up our dithers as POS-TARGS. We use similar values to the ones given by the WFC3-UVIS-MOSAIC-LINE strategy, which according to the documentation (section "C.2 WFC3 Patterns" of the WFC3 handbook) steps the gap on both detectors and it is used for full-frame WFC3-UVIS with ACS-WFC in parallel. The values used are X=1.446 arcsec, Y=2.926 arcsec and were set after the second primary observation in each visit.
No timing restrictions for the first visit are placed. However, subsequent visits must be scheduled between 10-30 days from the previous one.
We give a post flash of 20 e-/pix for each WFC3-UVIS images to account for the increasing CTE looses on the detector, as was recommended by our CS and the documentaion (ISR 2020-08: Strategies for Mitigation of CTE Losses in WFC3/UVIS) . We give similar post flash values to our ACS observations to ensure good detections in the narrow and wide filters.The team members of this proposal are experts on the study of compact binaries in globular clusters (GCs). They have made important contributions to the field using data taken at different wavelengths. All of them have several published papers on compact binaries in GCs, including several papers based on HST data.
Dr. L.E. Rivera Sandoval has expertise reducing and analyzing UV HST WFC3 data, the prime instrument and wavelengths requested in this proposal. She has carried out NUV studies of compact binaries in 47 Tuc, leading to the discovery of the first AM CVn candidate in that cluster as well as doubled the number of cataclysmic variables known there. She has 3 first-author papers published between 2015-2018 on UV data taken with HST data.
Prof. T. J. Maccarone has expertise in X-ray observations for understanding the populations of X-ray binaries in the field and in star clusters, and in correlating X-ray source properties with multiwavelength properties.
Prof. C. O. Heinke is an expert on X-ray observations of GCs. He has also been PI and Co-I of several succesful HST proposals.
Dr. A. Dieball has expertise in stellar populations in GCs, and extensive knowledge of HST ACS and WFC3 data reduction and analysis. She has led a previous HST far-UV survey on the GC M30 (GO-10561).
Prof. C. Knigge is an expert on cataclysmic variable stars and was involved in several further HST observing campaigns of GCs (e.g. M80 - GO-10183, M15 - GO-9792, 47 Tuc - GO-8219).
Dr. D. R. Zurek is an expert in the reduction of data taken with all HST instruments. He has expertise on imaging and spectroscopy, and has been involved in various HST observing campaigns, both as a PI and Co-I. He has led the far-UV observations on the GC NGC 1851 (GO-10184 and GO-13394), where he identified the first AM CVn candidate in a GC.Stellar Populations and the Interstellar MediumStellar Physics and Stellar Types6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTELLAR CLUSTERGLOBULAR CLUSTERJ2000J2000WFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WWFC3/UVISImagingNoNoF225WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF625WACS/WFCImagingNoNoF658NTiming link suitability includes constraints ([02 After 01 by 10.0 to 30.0 days])The scheduling data was generated by CASM 28.2.CASM was run in Phase II mode.1658407757000286.5(Tic-Visit
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