0Assigned ID: 4741
----- Attempting Submission 1 (Wed May 24 22:30:51 GMT 2023) -----ORBITAL VISIBILITY OVERRUN
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ORBITAL VISIBILITY OVERRUNAdded Visit 05, a redo of the failed Visit 04. Scan angles on all the scans in visit 05 changed to the correct values of 90 deg.-1086407132----- Attempting Submission 1 (Wed Sep 13 00:55:13 GMT 2023) -----
----- Attempting Submission 2 (Fri Nov 10 22:04:18 GMT 2023) -----
HST Phase II Proposal 17505 successfully submitted.
Receipt: # 17505-2
----- Attempting Submission 3 (Mon Feb 12 22:18:36 GMT 2024) -----
HST Phase II Proposal 17505 successfully submitted.
Receipt: # 17505-3
----- Attempting Submission 4 (Tue Feb 13 17:46:13 GMT 2024) -----
----- Attempting Submission 5 (Wed Jun 12 16:17:42 GMT 2024) -----
----- Attempting Submission 6 (Fri Jun 14 18:27:34 GMT 2024) -----
----- Attempting Submission 7 (Tue Sep 17 02:32:02 GMT 2024) -----This is fine.Constraining dark matter near the Galactic plane with precisely timed eclipsing binary starsMeasuring the accelerations of stars that live within the gravitational potential of the Galaxy using precise, time-series observations gives the most precise probe of the mass distribution, including the dark matter. For more than a century, astronomers have estimated the accelerations of stars in the Galaxy, assuming equilibrium. Evidence that our Galaxy is out of equilibrium has snowballed in recent years. Acceleration measurements have recently become possible from analysis of pulsar timing observations. These very small accelerations (~ few cm/s/decade) hold the key to mapping the spatial density of dark matter on sub-galactic scales, thereby constraining the nature of dark matter, including the possibility of a dark matter disk. Our observations will effectively double the sample of acceleration measurements and extend them to a new kind of clock - eclipsing binaries (EBs).
Acceleration mechanisms induce a period drift for EBs, manifesting as a deviation in the eclipse mid-point time from a linear ephemeris. Mid-eclipse times of EBs observed by the Kepler mission have been measured so precisely that we can now measure the shift in the eclipse mid-point time induced by the Galactic potential in the last decade. We request HST observations to measure the eclipses of four EBs from the Kepler field, which will provide the first eclipse timing measurement of the mid-plane density (also known as the Oort limit) to 3-sigma. Together with the pulsar observations, we should obtain a 4-5 sigma measurement of the Oort limit, and a meaningful constraint on the local dark matter density.The goal of these observations is to measure super precise (<0.2sec) eclipse times for four binary stars. They are designed similar to spectroscopic exoplanet transit observations using WFC3 in scanning mode, with the main differences being that the targets here are generally fainter than a typical exoplanet system, and since we don't care about the eclipe depth per se, we're using less out-of-eclipse baseline than the usual for an exoplanet transit.
For each orbit within a visit I've set it to take a direct image -- for a wavelength solution -- followed by a set of round-trip WFC3/G141 scans. When necessary I've added on one more forward scan at the very end to try and fill out the entire orbit duration.This is a highly inter-disciplinary group with expertise ranging from galactic dynamics to transit timing. PI S. Chakrabarti has extensive experience in Galactic dynamics, and lead the development of direct acceleration techniques (including EPRV and pulsar timing and now eclipse timing); she has earlier worked on analysis of lightcurves of stars from VVV and OGLE. Together with collaborators listed here (Stevens, Wright, Beatty, Huber), she also helped to develop the technique to measure accelerations with eclipse timing. Co-I D. Stevens has significant expertise in studies of eclipsing binaries and transiting exoplanets, and in studies of fundamental stellar parameters. He has made significant contributions to the KELT survey, and is an expert in precision analyses of eclipsing binary and transiting planet light curves. Co-I T. Beatty is an expert in working with spectroscopic timeseries observations of exoplanet and eclipsing binary lightcurves using WFC3, including the data reduction and analysis of spatially-scanned WFC3 observations. Co-I Jason Wright has made many contributions to exoplanet detection techniques. He is the project scientist for NEID and Wright and Chakrabarti have worked together earlier in developing a framework for EPRV observations to measure Galactic accelerations. Daniel Huber is a leading expert on asteroseismology and is the co-Chair of the Kepler Star Properties Working Group, and has worked broadly on many observational aspects of stellar astronomy and exoplanet detection and characterization. A. Quillen, E. D'Onghia and N. Garavito-Camargo are experts on dynamics of galaxies, stars, and galaxies. Co-I J. MacKenty is an expert on WFC3 observations, and Senior Scientist and HST Mission Scientist. Co-I Co-I P. Craig is a Ph.d. student who is working on comparisons of kinematic methods to direct acceleration measurements. Co-I Mtthew Walker is an expert on dark matter and galactic dynamics.GalaxiesLarge Scale Structure of the Universe6falsefalsefalsefalsefalsefalsefalseSUPPORTEDSTARG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.KIC6131659J2000J2000STARG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.KIC5986209J2000J2000STARK V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.KIC9284741J2000J2000STARG V-IVThis object was generated by the targetselector and retrieved from the SIMBAD database.KIC4847832J2000WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141WFC3/IRSpectroscopicNoNoG141The scheduling data was generated by CASM 33.0.CASM was run in Phase II mode./System/Volumes/Data/solaris/user1/royle/OP-cache/17505-v01.xml8 orbits1740003649000316.4629048874324(Tic-Visit
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:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3039
:pcs-gap 0
)false95