0Assigned ID: 226
----- Attempting Submission 1 (Thu Apr 10 18:26:42 GMT 2014) -----Oct 2014 Post-flash of 12e- has been added to all WFC3 UVIS exposures.
Feb 2015 Pointing and ORIENT adjustment made to M104 exposures (visit 4) to avoid
issues with the very bright star near the bottom of the ACS frame.
Mar 2015 Additional pointing and OREINT adjustmnets to visits 5,6,7 to avoid
issues with bright stars.1061513080----- Attempting Submission 1 (Wed Jul 23 19:43:59 GMT 2014) -----
----- Attempting Submission 2 (Tue Oct 14 21:40:33 GMT 2014) -----
----- Attempting Submission 3 (Thu Feb 26 17:43:14 GMT 2015) -----
----- Attempting Submission 4 (Wed Mar 04 19:39:47 GMT 2015) -----Visit Planner runs include dates from September, but the tool was run and is complete.
This is a re-submission of the accepted proposal with changes made to only set of observations (M104).Important Nearby Galaxies without Accurate DistancesThe Spitzer Infrared Nearby Galaxies Survey (SINGS) and its offspring programs (e.g., THINGS, HERACLES, KINGFISH) have resulted in a fundamental change in our view of star formation and the ISM in galaxies, and together they represent the most complete multi-wavelength data set yet assembled for a large sample of nearby galaxies. These great investments of observing time have been dedicated to the goal of understanding the interstellar medium, the star formation process, and, more generally, galactic evolution at the present epoch. Nearby galaxies provide the basis for which we interpret the distant universe, and the SINGS sample represents the best studied nearby galaxies.
Accurate distances are fundamental to interpreting observations of galaxies. Surprisingly, many of the SINGS spiral galaxies have numerous distance estimates resulting in confusion. We can rectify this situation for 8 of the SINGS spiral galaxies within 10 Mpc at a very low cost through measurements of the tip of the red giant branch. The proposed observations will provide an accuracy of better than 0.1 in distance modulus. Our sample includes such well known galaxies as M51 (the Whirlpool), M63 (the Sunflower), M104 (the Sombrero), and M74 (the archetypal grand design spiral).
We are also proposing coordinated parallel WFC3 UV observations of the central regions of the galaxies, rich with high-mass UV-bright stars. As a secondary science goal we will compare the resolved UV stellar populations with integrated UV emission measurements used in calibrating star formation rates. Our observations will complement the growing HST UV atlas of high resolution images of nearby galaxies.The primary goal of this proposal is to measure the distances to 8 SINGS spiral galaxies within 10 Mpc using the tip of the red giant branch method. One of the galaxies has archival data; new observations will be obtained for the other seven systems. The secondary goal of this proposal is to compare the resolved UV stellar populations from coordinated parallel UV WFC 3 observations of the high surface brightness regions of the galaxies with integrated UV emission measurements. Orbit allocation = 14 orbits (2 orbits per galaxy).
All primary visits include 2-orbits with the ACS/WFC. The first orbit of each visit is split between the F606W filter and the F814W filter. The second orbit of each visit is also split between the F606W filter and the F814W filter with a small 2 pixel offset in pointing. The small pointing offset is implemented using the POS-TARG equivalent of X=0.099 and Y=0.107 specificed in the ACS manual as the 2-point hot pixel dither pattern number 10. We have selected this dither pattern to maximize rejection of hot pixels and cosmic rays. We do not intend to cover the chip gap with our dither pattern.
The coordinated parallel observations are to be obtained with the WFC3 UVIS camera. The first filter in each orbit is the F336W filter; the second filter in each orbit is the F275W.
The visits are requested within specific orientation ranges. The ranges have been chosen to optimize the placement of the coordinated parallels on UV-bright star forming regions, without compromising the placement of the ACS instrument needed to achieve our primary science goal.RESOLVED STELLAR POPULATIONS12falsefalse0.00.0falsefalsefalseSUPPORTEDGALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the NED database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYSPIRALThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000ACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WACS/WFCImagingNoNoF606WACS/WFCImagingNoNoF814WWFC3/UVISImagingNoNoF336WWFC3/UVISImagingNoNoF275WThe scheduling data was generated by CASM 22.2.CASM was run in Phase II mode.(Tic-Visit
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