3D-DASH: A Wide Field WFC3/IR Survey of COSMOS

This target is not used in this proposal. This target is not used in this proposal. The following visits reviewed and changes made as necessary to avoid bright stars: 5Z 6C 6J 6K 6R 6S 6U 6W 6Z 7G 7L 7O 7Q 7W 7X 7Y 7Z 8N 8R 8T 9A 9E 9O A3 AA AC AE AH AN AQ AV -137472280 ----- Attempting Submission 1 (Tue Mar 16 05:47:57 GMT 2021) ----- Has been run before, resubmission. 3D-DASH: A Wide Field WFC3/IR Survey of COSMOS The Hubble Space Telescope has enabled us to establish a broad picture of how present day galaxies came to be. We propose to extend this legacy into unprecedented new territory - degree-scale infrared imaging and spectroscopy - that will allow us for the first time to study the physical processes that shape the behemoths of the universe: the most massive, highly-star-forming, rare galaxies up to z=3.5. Using the "drift and shift" (DASH) technique, developed in Cycle 23, we propose to survey the entire 1.7 sq. deg. COSMOS field in WFC3/H(F160W) and WFC3/G141 in order to map the build up of stellar structure via >1000 resolved H-alpha maps, carry out a statistically robust census of ~450 M>10^11 M_sun galaxies, identify up to 100 massive major mergers to constrain theoretical models, determine emission line redshifts for ~37,000 z>0.7 galaxies and provide the most accurate predictions on the bias and number density of emission line galaxies prior to Euclid and WFIRST. 3D-DASH will create a wide shallow tier in the infrared "wedding cake" of extragalactic surveys, increasing the area observed with infrared grism spectroscopy by almost an order of magnitude and adding HST-resolution infrared imaging to COSMOS, one of the most actively studied fields. This program will fill in an important gap in HST extragalactic surveys in the pre-JWST era and is unlikely to be surpassed in sensitivity, area and resolution until the launch of WFIRST. This program consists of two major sets of complementary observations. Set 1 is the broad band WFC3/IR imaging in the F160W filter. The program dedicates 100 orbits to these observations which will complement existing observations from the COSMOS DASH program (GO-14114, I think). Set 2 is the grism spectroscopy using the WFC3/IR G141 optical element. There is some, but not much existing observations in this optical element so much more area needs to be covered. The grism observations have 159 orbits dedicated to them. The program follows on the COSMOS field observations done with ACS ~20 years ago but since WFC3 has a smaller field of view, there are many more pointings (green outline in the figure below). We would request that the imaging F160W observations be executed first. These observations will constitute a complete dataset on their own and the team can start on the science results with these data alone. Furthermore, the imaging is a prerequisite for analyzing the grism data. We additionally request that the imaging be executed in a sequence such that each contiguous area is completed (if possible) before starting on a new one rather than doing random visits from all over the mosaic. We suggest a sequence below. The existing F160W observations cover 3 stripes, shown in gray-scale in the image above. The planned observations are shown with colored rectangles. The large rectangles designate the different contiguous areas. The green outline is the existing ACS data we are trying to match to. We break down the remaining area into 7 columns. We tile each contiguous area at the same ORIENT so that there are no/fewer gaps between the images and the final mosaic has as few holes as possible (all interesting objects are either on the edge of the image or in the hole). Column 1 consists of a sequence of 17 visits at ORIENT = 295. V1 through V17. Column 2: top area 4 visits V68 - V71 ORIENT = 295 Column 2: bottom area 7 visits V84 - V90 ORIENT = 55 Column 3 consists of a sequence of 16 visits at ORIENT = 291. V18 through V33. 3 visits V91, V92, V93 to fill the side at ORIENT = 55 Column 4: topc area 3 visits V72 - V74 ORIENT = 291 Column 4: bottom area 3 visits V94 - V96 ORIENT = 55 Column 5 consists of a sequence of 17 visits at ORIENT = 296. V34 though V50. Column 6: top area 2 visits V75, V76 ORIENT=295 Column 6: bottom area 1 visit V83 ORIENT=295 Column 7 consists of a sequence of 17 visits at ORIENT = 296. 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