0Assigned ID: 1057
----- Attempting Submission 1 (Sat Mar 07 00:53:24 GMT 2020) -----We have planned observations for the failed visit 3654237784----- Attempting Submission 1 (Fri Jun 26 21:38:24 GMT 2020) -----
----- Attempting Submission 2 (Mon Mar 01 07:47:29 GMT 2021) -----
----- Attempting Submission 3 (Mon Mar 08 17:02:14 GMT 2021) -----
----- Attempting Submission 4 (Tue Mar 09 20:33:20 GMT 2021) -----
----- Attempting Submission 5 (Fri Apr 16 00:06:47 GMT 2021) -----
----- Attempting Submission 6 (Thu Apr 29 16:39:02 GMT 2021) -----
----- Attempting Submission 7 (Wed Oct 06 00:36:29 GMT 2021) -----
HST Phase II Proposal 16218 successfully submitted.
Receipt: # 16218-7
----- Attempting Submission 8 (Wed Oct 06 03:50:41 GMT 2021) -----
----- Attempting Submission 9 (Fri May 13 07:27:40 GMT 2022) ------Confirming the first double degenerates in globular clustersThe first 3 good candidates to AM CVn (double degenerate binaries) binaries in a globular cluster were recently identified with HST photometry. One of them is N1851-FUV1 which was identified as a short
period (18 minutes) far-ultraviolet variable near the center of the globular cluster NGC 1851
(Zurek et al 2016). The other 2 candidates have been identified in the globular cluster 47 Tuc
(Rivera Sandoval et al 2018) based on a combination of the their X-ray and optical/near-ultraviolet properties.
A far-ultraviolet spectrum of each of these candidates will confirm or refute these candidates as AM CVn. Their confirmation will establish globular clusters as factories of compact binaries that emit gravitational waves and which are expected to be detected with LISA. The characterization of these systems is crucial to be performed while HST is still working, as it is the only telescope capable to resolve the stars in the cores of globular clusters. If confirmed, the first comparison to AM CVns in the Galactic field will be possible, giving direct evidence of the impact of stellar interactions in their formation and evolution. This program may enable follow-up studies to set important constraints on double degenerate binary models.We will acquire a bright red giant and offset to our target.
For NGC 1851 we will make a second peak up on the target before obtaining the science exposures.
For NGC 104 the offset star is relatively isolated, a peak up on the target previous to science data is not feasible considering its faintness.
The main observations will be with the G140L grating and the FUV-MAMA.Dr. L.E. Rivera Sandoval has expertise reducing and analyzing UV HST WFC3 data. 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.
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.
Dr. M. van den Berg is an expert on the study of compact binaries in open clusters and in GCs at different
wavelengths. She also has experience reducing and analyzing HST ACS data.
Drs. Pooley, Shara and Long are experts on binaries in globular clusters. They have performed optical an X-ray observations, including those with HST.Stellar Physics and Stellar TypesStellar Populations and the Interstellar Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDSTARINTERACTING BINARYWe used the WFPC2 image (PC chip), because saturation isn't an issue, to measure the positions of this offset star and the intended source FUV1. The F555W WFPC2 frame used is U2VO0301T. We have also made calculations using a FUV image of the cluster (STIS/FUV-MAMA and the F25QTZ filter) and none of the sources exceed the bright limits. The brightest sources have about 11 cnts/ second. This corresponds (using the photflam of 1.0388894E-16) to a flux of about 1.13446722E-15. If we put this value into the ETC with our setup (using a black body model of 50,000K to mimic a hot source) the bright limits are never in danger of being exceeded. The ETC calculation done is STIS.sp.1479536. We have also sent images to our HST program coordinator.J2000J2000F140LP = 18.7 +/- 0.06STARINTERACTING BINARYWe used the ACS/WFC image j9l960a7q_flc.fits (exptime=3s in F606W) which is under the J9L960010 data set to select the offset star. We have also used a 3.6 sec STIS/F28X50LP image (o48c0100r0_crj.fits under o48c010r0) and the stars in the cluster did not exceed the brightness limits, we sent finding chart to our HST program coordinator. The cluster has previously been observed in FUV slitless spectroscopy with no problems, so the current configuration will not be an issue. The current coordinates are based on precise absolute astrometry performed by our group (epoch J2000), not on the above mentioned archival reference HST image.J2000J2000STARM III-IWe used the WFPC2 image (PC chip), because saturation isn't an issue, to measure the positions of this offset star and the intended source FUV1. The F555W WFPC2 frame used is U2VO0301T.J2000STARK III-IWe used the ACS/WFC image j9l960a7q_flc.fits (exptime=3s in F606W) which is under the J9L960010 data set to identify a suitable, isolated, bright offset-star. The current coordinates are based on precise absolute astrometry performed by our group (epoch J2000), not on the above mentioned archival reference HST image.J2000F606W = 12.8, F814W=11.8STIS/FUV-MAMASpectroscopicNoNoG140L1425STIS/FUV-MAMASpectroscopicNoNoG140L1425The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.It would be very convenient to have visits 1 and 2 for this target scheduled very close to each other.1617850543000118.88(Tic-Visit
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)true20The scheduling data was generated by CASM 29.2.CASM was run in Phase II mode.It would be very convenient to have visits 1 and 2 for this target scheduled very close to each other.
We have given 6 orbits to the target in 47 Tuc, the faintest one, to recover some of the time lost in the visit's split.1645681438000149.47000000000003(Tic-Visit
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)true30The scheduling data was generated by CASM 30.1.CASM was run in Phase II mode./private/var/folders/4z/t_bqgcq137j8sd4xmqs9vq0w0000gn/T/OPVisit10381565429600190737.xmlIt would be very convenient to have visits 1 and 2 for this target scheduled very close to each other.
We have given 6 orbits to the target in 47 Tuc, the faintest one, to recover some of the time lost in the visit's split.
Repeat of failed visit 03.(Tic-Visit
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