Here is a summary of the CHP-II phase 2 planning which is due on Thursday July 24th. Please review. If you have any comments or suggestions please provide them as early in the week as possible. As a reminder There are four major components to CHP-II. 1. Galactic RR Lyrs using WFC3-IR F160W observations of 2 phase points. 2. Local Group Galaxies: 2a. RR Lyrs using WFC3-IR F160W observations of 12 phase points. 2b. TRGB distances using parallel observations with ACS F814W and F606W. 3. Omega Cen RR Lyrs using WFC3-IR F160W observtions of 2 phase points. 4. SN1a host galaxy TRGB distances using ACS F814W and F606W observations. The following is concise decription of the observations. 1. Galactic RR Lyrs. tbd 2. Local Group Galaxies. tbd 3. Omega Cen RR Lyrs. tbd 4. SN1a host galaxy TRGB distance. We selected these fields to sample the halo RGB population with the guiding principles of: I) Avoid disks and obvious young or tidal structures. II) Straddle WISE W1 25-26th mag isophote and Near-UV 27-28th mag isophote if applicable. III) select fields along minor axis to maximize halo stars. You can review plots of the positions in the following document: http://users.obs.carnegiescience.edu/mseibert/chp2/trgb_positions_v4.pdf These are the FOV centers and postion angles for each of the nine galaxies: NGC3627 11:20:31.48 +12:59:45.01 0 NGC3368 10:47:02.938 +11:49:28.00 0 NGC5457 14:03:18.800 +54:09:21.00 0 NGC1316 3:22:18.800 -37:20:30.00 0 NGC1365 3:33:51.428 -36:12:05.00 42 NGC1448 3:44:26.588 -44:36:14.22 45 NGC4424 12:27:09.705 +9:22:53.00 8 NGC4526 12:34:03.792 +7:45:11.71 19 NGC4536 12:34:21.123 +2:08:40.84 35 Each page of the above has 4 images of the same galaxy. On the left are WISE W1 (3.4 um) and on the right side are GALEX NUV. The only difference between the top and bottom is the stretch. Note that the two lenticular galaxies (NGC1316 and NGC4526) we replace the UV images with POSSII Red images as the UV is not instructive for them. The ellipses are 24, 25, 27 and 28th mag isophotes in green, red, blue, and white as measured in annuli. Archival ACS data with either F555W, F606W or F814W is shown in cyan. NGC1365 and NGC4424 show WFC3/UVIS fields as well. Our planned positions are shown in magenta. The first page is NGC4258 which is not a program target but is shown as an example of a well done TRGB program. Only the Madore 2003 TRGB pointing is shown for NGC4258 (see Mager et al. 2008) because there are just so many poinitngs that you would not see the galaxy if all were plotted. Some comments on specific galaxies. NGC3627/M66 and NGC3627/M96: We have opted to place the ACS fields on the opposite side of the galaxies from the Madore 2006 pointings (see Lee et al. 2013) in order to increase the sample size as opposed to increase the S/N of previous detections. NGC1316: We try to balance avoiding the tidal/shell structures and keeping close enough to maintain the halo RGB densities. The red square near this galaxy is the suggested pointing of Jang and Lee. We agree with the general region but our curretly selected pointing is a closer beacsue the surface brightness drops so rapidly at this radius and we are worried about the RGB density. A table of S/N estimates and exposure times for each band. Is availble here: http://users.obs.carnegiescience.edu/mseibert/chp2/trgb_s2n_estimates.txt The first three objects are the ETC results when applied to the archival TRGB programs of N4258, M66 and M96 and are provided as a comparison. We will achieve similar S/N with our allotted orbits for M101, M66 and M96. We are not going to be able to do as well moving further out. We tried to make sure that we obtain a S/N ~10 for the I band TRGB magnitude. The allocation of time between I and V varies between Exptime(I) / Exptime(V) = 1 to 3 . Frr the CHP-II Team, -Mutt and Jeff