The number of orbits used exceeds the number allocated
Unschedulable VisitPlease process all the three visits (6,7 and 8) as I discussed (with Denise).
However, we have only 2 orbits left, so only 2 of these visits can be executed.
By tomorrow morning I will inform which of these 3 visits should actually execute.
For info:
Visit 6 is identical to visit 2,
Visit 7 is identical to visit 5, and
Visit 8 is identical to visit 4, except that the exposure times have been reduced to fit within the orbits.
Thanks.-307976040----- Attempting Submission 6 (Wed Oct 01 13:07:36 GMT 2014) -----
----- Attempting Submission 7 (Wed Oct 08 15:32:59 GMT 2014) -----See above comments.Detecting Isolated Black Holes through Astrometric MicrolensingA significant fraction of the mass of an old stellar population should be in the form of non-luminous, isolated black holes (BHs). Yet there has never been a unambiguous detection of a solitary BH---not surprisingly, since the expected accretion rate from the ISM is extremely low, and thus they emit essentially no radiation.
The only technique available to detect such isolated BHs is astrometric microlensing---the relativistic deflection of light from background stars. HST is the only instrument currently capable of detecting such tiny deflections.
We have underway a multi-year program of HST high-precision astrometry of long-duration microlensing events in the Galactic bulge, using the WFC3 camera. Our aim is the first detection of stellar-mass black holes, by monitoring five optimally selected events.
Our program has met with success, with clear detections of motions during microlensing, indicative of non-luminous massive lenses. However, proper motions of the stars in the Galactic bulge can be of similar magnitude as the deflections due to microlensing. Fortunately, the proper motions are linear whereas the deflections due to microlensing are not, but it is clearly important to accurately subtract the proper motions. The time baseline of our observations is inadequate for 4 of the 5 microlensing events that we are monitoring, since the expected lensing signal was substantial until now. We have completed observations for one, but need 2 additional observations each for the 4 remaining events in order to accurately determine their proper motions. This will lead to a robust determination of the lens masses, thus completing the original objectives of the program.We will continue our observations of long-duration events which do not show any light contribution from the lens (continuation of 11707/12322/12670). We will take most images in a single filter, but also take a small number of images in a different filter to check the color dependenacy, if any, of the astrometric shift.
We will try to take as many images as possible in a single ORIENT for better astrometric accuracy. However, maintaining a single ORIENT may not be possible for all the observations. Since almost all of our targets are close to the ecliptic, we plan to use the same orient for nearly half of the year, and then flip it by 180 deg.HOT STARS12falsefalse0.00.0falsefalsefalseSUPPORTEDSTARBULGEGRAVITATIONAL LENSJ2000J2000STARBULGEJ2000J2000STARBULGEJ2000J2000STARBULGEJ2000J2000STARBULGEJ2000J2000WFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WThe scheduling data was generated by CASM 21.2.CASM was run in Phase II mode.1371469597000285.5(Tic-Visit
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