0Assigned ID: 1056
----- Attempting Submission 1 (Fri Apr 07 22:56:19 GMT 2017) -----
HST Phase I Proposal 1056 (Tails_UB_25.apt) successfully submitted.
Receipt: # 1056-1
----- Attempting Submission 2 (Fri Apr 07 23:41:58 GMT 2017) -----
HST Phase I Proposal 1056 (Tails_UB_25.apt) successfully submitted.
Receipt: # 1056-2
----- Attempting Submission 3 (Fri Apr 07 23:45:59 GMT 2017) -----For the 2 visits where parallels are required, we have fit images of differing exposure times in order to get 4 images per filter for each of the two cameras.
I also wanted to thank everyone who helped with advice and technical help! (Tony, Aparna, Susana,Mario) Greatly appreciated.
8/30/2017 - removed some of the original roll angles to avoid bright stars in quadrant D in UVIS 2.
1/2/2018 - increased FLASH required for shortest (400s) ACS/WFC exposures in F435W for Visits 3 and 4. Now FLASH=10.01141216908----- Attempting Submission 1 (Wed Jul 19 22:32:47 GMT 2017) -----
----- Attempting Submission 2 (Thu Aug 31 15:17:32 GMT 2017) -----
----- Attempting Submission 3 (Wed Jan 03 14:51:11 GMT 2018) -----Star Clusters in Tidal Debris: A UV Survey of Stellar Populations, Galaxy Interactions, and EvolutionTidal tails afford us a unique window into the processes shaping star formation, offering an unobstructed view of the star formation environment in these outskirts. The latest galactic merger simulations are finding an unexpected increase of star formation in extended tidal debris, with 20 - 50% of the systems star formation rate occurring in these regions. We see this observationally in massive clusters forming in the Tadpole galaxy, occupying 30% of the system's star formation rate. At the same time, clusters suffer high rates of disruption, dispersing their material into the diffuse light of the tail and mixing with old stars drawn from the parent galaxies. We intend to break our tidal tails into their composite populations using HST and ground-based Gemini imaging. Our existing WFPC2 VI-band and HI data indicate clusters prefer to live in regions of high HI kinetic energy and low shear. However, analysis is limited to population studies, as the lack of UB-band data prevents us from age or mass estimates, permitting only a shallow understanding of the relationship between local HI properties and star clusters. Additionally, while the high resolution of HST is necessary for identifying and studying star clusters, it is unsuitable for the sensitive imaging needed to study the faint, diffuse tails. Our proposed 11 orbits of WFC3/ACS UB-band imaging will allow for precise age and mass measurements of our star clusters, while ground-based imaging searches the diffuse light for the cluster destruction history. In this manner, we will determine the present and past history of star formation in tidal tails, and the HI densities and kinematics required for cluster formation.Our program involves U/F336W and B/F438W WFC3 imaging of tidal tails in which WFPC2 V/I imaging data is already available. We are interested in photometry of faint point- and marginally-resolved sources over the entire WFC3 FOV, and we are requesting a 4 point dither pattern (where possible- see parallels below) for each filter to properly sample the PSF in our final, combined images. We do not need to cover the chip gap, as long as the ORIENT ranges (below) are OK. We needed to make sure the chip gap does not cover area where stars clusters were detected in the WFPC2 data. Our original request was to have 1.5 orbits in U, and 0.5 orbit in B; however, with the preference for a 4-dither pattern, and avoiding any observing inefficiencies with <360s exposures, our best possible observing strategy appears to be 1.3 orbits (U), the remainder of the 2nd orbit in B. Although we are interested in the highest possible S/N in our observations, we have left a few x 10s left in each orbit to allow for maximum flexibility in scheduling. Should these cuts be unnecessary, we would like to bump up the F336W observation exposure times as much as is possible to fill the orbit, while still allow for maximum schedulability
VIsits: Five of our visits are two-orbits in length, and make use of WFC3 alone, with no parallels. In those cases, we have adopted a 4 point DITHER-BOX pattern to providue the best possible PSF sampling. We do NOT need to fill in the chip gap for these observations. For the 2 single-orbit visits of NGC2992/3, we have requersted parallel observations. We have found that there appears to be no effieicnt way to get 4 equal exposures in the primary camera *and* have 4 equal exposures in the parallel obervations. For these visits I have created a manual (using POS-TARGs) 4 point dither pattern, but with unequal exposures, and unequal FLASH values (reason I did not use set DITHER-BOX pattern)
Thus we have used a 3 point sub-pixel dithering pattern to get the bast sampling for these visits only.
FLASH: We also require a post-FLASH for all WFC3 images due to the relatively short individual exposures in both of these blue filters. We used the ETC to look at the expected range of background values assuming the lowest (faintest) possible sky background for each target (our objects span a wide range in ecliptic latitudes), and assuming no Earthshine or zodiacal light. This way we have a conservative estimate for the needed FLASH to reach 12 e-/pixel in the WFC3 images. Similar, used same methodology for the ACS images - FLASH normally not required, but the shorter exposures (400s) in F435W yield a lowest possible 19 e-/pixel, so we have added FLASH=1.0 to those. However, under normal observations perahsp we do not need to add this?
Roll Angles: Our ORIENT ranges are based on the requirement to cover the WFPC2 footprint from previous observations of these galaxies, but we have found we have many months of available scheduling for each object, with the exception of the NGC 2992/3 observations (with the parallels) where we have perhaps 1-2 weeks of schedulable time due to the much more restricted roll angle requests.Galaxies and the IGMStellar Populations6falsefalsefalsefalsefalse0.01.3trueSUPPORTEDGALAXYTIDAL TAILThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYTIDAL TAILThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYTIDAL TAILThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYTIDAL TAILThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYINTERACTING GALAXYTIDAL TAILJ2000J2000GALAXYTIDAL TAILThis object was generated by the targetselector and retrieved from the NED database.J2000J2000WFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WACS/WFCImagingNoNoF435WACS/WFCImagingNoNoF435WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF438WPOS-TARGDITHER0.173LINE0.112falsefalse81.785423.884WFC3-UVIS-DITHER-BOX2falseThe scheduling data was generated by CASM 25.2.CASM was run in Phase II mode./private/var/folders/1b/yx3zlx911zl6np_bzjrqc4245gvmgy/T/OPVisit5080532772515141815.xmlE tidal tail of NGC 1487. Using 4 dithers per filter, over 2 orbits. Thin ranges in ORIENT needed to both cover previous WFPC2 observations needed to both cover WPC2 field, and minimizing chip gap covering the tidal tails. Added 8/30 - removed one ORIENT RANGE to avoid bright star in UVIS2-quad D.1511631278000358.0(Tic-Visit
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