0Assigned ID: 1200
----- Attempting Submission 1 (Fri Apr 07 23:56:45 GMT 2017) -----
HST Phase I Proposal 1200 (bh_long_prop.apt) successfully submitted.
Receipt: # 1200-1
----- Attempting Submission 2 (Sat Apr 08 17:43:36 GMT 2017) -----The number of orbits used exceeds the number allocatedVisit 81 is a revised version of visit 8. If possible, please schedule visit 81 instead of visit 8.-1519638924----- Attempting Submission 1 (Tue Jul 18 20:53:05 GMT 2017) -----
HST Phase II Proposal 15318 (15318_phase2.apt) successfully submitted.
Receipt: # 15318-1
----- Attempting Submission 2 (Wed Jul 19 15:21:58 GMT 2017) -----
HST Phase II Proposal 15318 (15318_phase2.apt) successfully submitted.
Receipt: # 15318-2
----- Attempting Submission 3 (Wed Jul 19 15:43:47 GMT 2017) -----
----- Attempting Submission 4 (Fri Aug 04 21:38:57 GMT 2017) -----
----- Attempting Submission 5 (Wed Sep 13 19:31:24 GMT 2017) -----
----- Attempting Submission 6 (Thu Sep 28 12:20:25 GMT 2017) -----
----- Attempting Submission 7 (Fri Sep 29 20:59:28 GMT 2017) -----
----- Attempting Submission 8 (Thu Oct 05 17:08:29 GMT 2017) -----
----- Attempting Submission 10 (Wed Oct 11 19:39:14 GMT 2017) -----
----- Attempting Submission 11 (Tue Mar 06 18:17:03 GMT 2018) -----
HST Phase II Proposal 15318 (15318_p2.apt) successfully submitted.
Receipt: # 15318-11
----- Attempting Submission 12 (Tue Mar 06 21:27:09 GMT 2018) -----
----- Attempting Submission 13 (Mon Mar 12 17:34:02 GMT 2018) -----
----- Attempting Submission 14 (Wed Apr 24 15:32:02 GMT 2019) -----
----- Attempting Submission 15 (Wed Jul 03 14:25:25 GMT 2019) -----
HST Phase II Proposal 15513 (15513.apt) successfully submitted.
Receipt: # 15513-15
----- Attempting Submission 16 (Tue Jul 09 12:46:29 GMT 2019) -----
----- Attempting Submission 17 (Mon Jul 15 13:14:45 GMT 2019) -----
----- Attempting Submission 18 (Thu Oct 10 15:28:56 GMT 2019) -----
----- Attempting Submission 19 (Mon Oct 14 15:17:33 GMT 2019) -----
HST Phase II Proposal 15513 (15513_vis8.apt) successfully submitted.
Receipt: # 15513-19
----- Attempting Submission 20 (Tue Oct 15 17:13:21 GMT 2019) -----Denise, I'm assuming that your answer would be yes, and submitting accorddingly! Thanks!!Detecting Isolated Black Holes through Astrometric MicrolensingA significant fraction of the mass of an old stellar population should be in the form of isolated black holes (BHs). Yet there has never been an unambiguous detection of a solitary BH. The only technique available to detect isolated BHs is astrometric microlensing--relativistic deflection of light from background stars.
We have carried out 2 HST programs aimed at the first detection of isolated BHs through astrometric microlensing. Our first program was a multi-year program where we monitored 5 microlensing events with T>100 days in the Galactic bulge. We detected astometric deflections, but the inferered masses for all these events are <0.5 Msun, indicating that these lenses are low-mass stars with small relative proper motions. Our second program was a large multi-cycle program where we monitored ~3 million stars in the Galactic bulge for 3 years to simultaneously detect microlensing events and deterimne their astrometric shifts. We have detected a large number of microlensing events. However, once again, none of them show appreciable astrometric deflections indicative of massive BHs.
Our results imply that either isolated BHs are more massive (>10 Msun), or T~100 day events are dominated by low-mass stars moving more slowly, or BHs are much rarer. BHs with mass > 10 Msun are expected to have T>300 days, and such very-long duration events are extremely unlikely to be caused by low-mass stars. Monitoring a few T>300-day events thus offers the last but most promising opportunity to detect isolated BHs, and distinguish between the above possibilities. After the recent upgrades, OGLE detects six T>300 days events each year, here we propose to monitor 4 such events.We will employ the same observational strategy we have followed earlier. Basically, we will image each field using WFC3, primarily with the F814W filter, but also with F606W. We will employ a 6-point dithering pattern, where we will observe the target star and the reference stars at a variety of pixel phases, thereby allowing us to construct an exquisite model of the PSF, and also randomize any remaining (small) systematic errors related to pixelization. Our dithers will also involve offsets of ~100 pixels, so that we will observe the target star at different places on the detector, so that any remaining distortion errors will average out. We expect such errors to be small (< 0.01 pixel), but randomizing them will be worthwhile. The procedure described here does not require the observations at different epochs to be taken in the same ORIENT, which makes the scheduling easier.
In a rich stellar field such as the Galactic bulge, there is always a large number of reference stars available in an WFC3 field, making it possible to achieve the highest possible astrometric accuracy. We will also image the field in the F606W and F814W filters. If there is blending, then the centroid shift is expected to be color dependent; V -band observations will provide additional help in evaluating the possible color-dependent blending contribution. The combined V and I-band observations will require one orbit per target at each epoch. We will observe at 5 different epochs which will be adequate to separate the proper motions from the deflections caused by lensing. For each event, we will obtain 2 observations in cycle 25, 2 observations in cycle 26, and 1 observation in cycle 27.
These observations need to be considered as ToO since the targets will be chosen after we find suitable candidates from OGLE alerts.Stellar Physics6falsefalsefalsefalsefalsefalsefalseSUPPORTEDEXT-STARA0-A3 III-IJ2000J2000EXT-STARA0-A3 III-IJ2000J2000EXT-STARA0-A3 III-IJ2000J2000EXT-STARA0-A3 III-IJ2000J2000EXT-STARA0-A3 III-IJ2000J2000WFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WThe scheduling data was generated by CASM 27.0.CASM was run in Phase II mode.1557360739000277.72459241424394(Tic-Visit
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