This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
This target is not used in this proposal.
ORBITAL VISIBILITY OVERRUN
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
ORBITAL VISIBILITY OVERRUN
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIME
ORBITAL VISIBILITY OVERRUN
PARALLELS SIGNIFICANTLY EXTEND ALIGNMENT TIMEThis is resubmission fixed erroneous and inconsistent entries between the actual and subexposure entries.1019624552----- Attempting Submission 1 (Wed Jul 08 12:22:30 GMT 2015) -----
----- Attempting Submission 2 (Sun Oct 04 07:25:48 GMT 2015) -----
----- Attempting Submission 3 (Tue Oct 06 13:54:22 GMT 2015) -----
----- Attempting Submission 4 (Thu Oct 08 18:48:23 GMT 2015) -----The last subexposure of the WFC3 primary exposures has a visibility overrun by 19 seconds. We would like to keep the exposure times equal between the different subexposures and hope that this overrun can be still accepted. If not possible, you can shorten the last subexposure by 19s.The Proper Motion of Palomar 5 and its Tidal TailsThe outer-halo Milky Way globular cluster Palomar 5 (Pal 5) shows prominent tidal tails (TT) extending over tens of degrees. Published ground-based proper motion (PM) measurements of Pal 5 are inconsistent with each other, and also with predictions from our numerical modeling (PM greater than 2 mas/yr in each component). Accurate PM would allow a detailed reconstruction of Pal 5's dissolution history and provide independent constraints on the shape of the Galactic potential. We propose to measure the PM of the Pal 5 cluster and a field 5 deg (2 kpc) along its TT with an accuracy of < 0.4 mas/yr via multi-epoch WFC3 and ACS observations in Cycles 20 and 22. We have identified a large number of QSOs and galaxies in these fields, which will allow us to achieve this accuracy on a three-year baseline. Combined with the large amount of available radial velocity data and detailed numerical modeling, the proposed observations will constrain the orbit of Pal 5 to greater accuracy than any other outer-halo satellite (< 30 km/s). Hence, it will enable us to tightly constrain the Galactic circular velocity and the flattening of the Galactic potential to less than 10% uncertainty. We will further use the PM-cleaned sample of stars in Pal 5 and its TT to unambiguously probe for variations of the present-day stellar mass function down to 0.2 Msun, enabling a direct estimate of Pal 5's mass loss rate. Together with the orbital information this will provide unique insights to the complex interplay of two-body relaxation and tidal shocking, which will have direct consequence for our understanding of the build-up of galaxy field populations and the evolution of cluster mass functions.We require two epochs of observations to measure the Pal 5 and its Tidal Tail (TT) proper motion (PM). The first epoch, as early in Cycle 20 as possible, and the second epoch late in Cycle 22, to guarantee a baseline of at least 3 yrs to achieve a PM precision of ~0.4 mas/yr. Each epoch will consist of three WFC3/UVIS-F814W pointings. One pointing will be on Pal 5, the other two will cover a QSO in a dense Tidal Tail region at 5 deg (about 2 kpc) projected distance from Pal5. Observations with the ACS/WFC-F606W and F814W in parallel will increase significantly the spatial coverage of Pal5 and its TT region and allow a deep probe to its stellar mass function.
For the two TT fields a second orbit in the 1st epoch will be used with WFC3/UVIS-F606W to measure the Mass Function (MF) down to 0.2 M_sol in combination with the WFC3/UVIS-F814W 1st orbit observation. Four exposures, one short at the beginning of the orbit and three long, per epoch with WFC3/UVIS-F814W will be used to improve the PSF sampling and correct for detector imperfections (e.g. bad pixels) and cosmic rays. The first short and long exposures will have the same positions, while the dithering for the others uses a spacing of 1.302 arcsec.
The specified orientation angles for the TT and Pal5 fields are chosen to allow earliest possible scheduling (17-24 Sept 2012) as well as to include in the WFC3 fields the QSO in the TT field (RA=231.64458, DEC=2.0367500), brigth background galaxies whose brightest globular clusters can be used as background reference and spectroscopically confirmed stars in Pal5 and its TT.
For the cluster ACS field we will use F606W in the first epoch and F814W in the second epoch to probe for variations of the MF beyond Pal 5's half-light radius.RESOLVED STELLAR POPULATIONS12falsefalsefalsefalse0.00.0SUPPORTEDSTELLAR CLUSTERGLOBULAR CLUSTERTIDAL TAILThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000STELLAR CLUSTERGLOBULAR CLUSTERHALOTIDAL TAILJ2000J2000STELLAR CLUSTERGLOBULAR CLUSTERHALOTIDAL TAILJ2000J2000GALAXYQSOQSOJ2000STARK III-IJ2000STARK III-IJ2000STARK III-IJ2000WFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF606WWFC3/UVISImagingNoNoF814WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WThe scheduling data was generated by CASM 23.2.CASM was run in Phase II mode./private/var/folders/s1/jf25r68j1r18mp2km24w0s1m0000gp/T/OPVisit268024160542486441.xmlSecond epoch(Tic-Visit
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