0 Assigned ID: 15 ----- Attempting Submission 1 (Tue Mar 14 00:17:25 GMT 2017) ----- position of source HIZSS-021 revised -1770400652 ----- Attempting Submission 1 (Tue Jul 18 20:32:15 GMT 2017) ----- HST Phase II Proposal 15150 (antivoid25_ph2.apt) successfully submitted. Receipt: # 15150-1 ----- Attempting Submission 2 (Wed Jul 19 21:43:29 GMT 2017) ----- Local Void Reflex: IR TRGB Distances to Obscured Galaxies at the South Supergalactic Pole Our galaxy lies in a thin sheet that is part of a wall of the Local Void. It is now evident that our `Local Sheet' has a peculiar velocity of several hundred km/s away from the void. Further, it is evident that there is a compression onto the Local Sheet, with galaxies above and below the sheet exhibiting peculiar velocities toward us. This trend was confirmed with HST observations of a lonely galaxy toward the void center. Galaxies in the opposite direction also have peculiar velocities toward us. However, galaxies with good distances in the sector opposed to the void lie at sufficient angles that only moderate fractions of their anomalous radial motions are directed away from the void. There are good nearby candidates to test the hypothesis of compression toward the Local Sheet but they lie in the zone of obscuration, requiring observations in the infrared. Experience has shown that the measurements are possible with the tip of the red giant branch method, now well calibrated. The experiment is important because the measurement in the void anti-apex coupled with an existing sample of distances to significant redshifts will give the absolute amplitude of expansion of the Local Void. The expansion velocity of a void depends on the size and emptiness of the void and on cosmological parameters. The measurement can only realistically be carried out at this boundary of the Local Void and requires a foundation in the motions of galaxies in the anti-void direction. We propose to observe 4 high priority obscured galaxies; each for 3 orbits. The exposures times will be divided between F110W and F160W filters with variations that account for relative obscuration; the relative exposure times in the F110W filter will be greater for more obscured sources. We are guided by the exposure times used in the course of the cycle 17 SNAP program 11719 (PI Dalcanton) and our own cycle 20 program 12877 with galaxies at similar distances. We follow dithering procedures demonstrated to be optimal for psf reconstruction. The photometry is carried out with the software DOLPHOT, the successor to HSTPHOT (Dolphin 2000), enhanced to be used with WFC3 data (http://purcell.as.arizona.edu/dolphot). Calibration of the TRGB in the F110W and F160W filters (Wu et al. 2014) is carried out using archival data from program 11719, involving observations of well studied nearby high latitude galaxies using the same F110W and F160W filters, then applied to 3 major obscured galaxies in the Maffei group. The analysis follows procedures developed by Makarov et al. (2006) and Rizzi et al. (2007) with optical band material. With both ACS and WFC3/IR data our pipeline is now sufficiently well established that the photometry leading to CMD can be carried out within 24 hours of receipt of data from HST and within another 24 hours the TRGB and a distance can be established with a maximum likelihood method that involves recovery tests with artificial stars. The tests establish the fractional recovery as a function of magnitude and color and the associated errors. The products, both tabular and graphical, are made available through the Extragalactic Distance Database (http://edd.ifa.hawaii.edu) by selecting the catalog CMDs/TRGB (Tully et al. 2009; Jacobs et al. 2009). Reddening in the line-of-sight can be determined from the color displacement of the zero age main sequence. It is seen in the comparisons of the IC 342 and NGC 300 CMD that suitable information will be available to determine the reddening in the immediate field of the IR observations. All our candidates are gas-rich and likely to have prominent population I components. For comparison, foreground reddening can be estimated from the colors of galactic main sequence stars projected across the entire field of view with simulations generated by the TRILEGAL code (Girardi et al. 2012). Even in the infrared, reddening is the largest source of error for low latitude targets. For the relatively nearby objects that will be observed, the TRGB can be established to +-5% in distance, modulo obscuration. An uncertainty of +-0.1 mag in absorption at F110W, roughly what might be expected for the more obscured candidates, adds in quadrature another 5% uncertainty in distance (Wu et al. 2014). Presently, there is no information on the distances of any of the targets beyond inferences from redshifts. Cosmology 6 false false false false false false SUPPORTED GALAXY LSB MAGELLANIC IRREGULAR This object was generated by the targetselector and retrieved from the SIMBAD database. PGC17716 J2000 J2000 GALAXY LSB MAGELLANIC IRREGULAR This object was generated by the targetselector and retrieved from the NED database. PGC2807061 J2000 J2000 GALAXY LSB MAGELLANIC IRREGULAR This object was generated by the targetselector and retrieved from the NED database. 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