For a sample of 13 star-forming galaxies at 1 < z < 1.4, selected from an ongoing IRAM/PdBI CO survey that measures molecular gas masses, we propose HST/WFC3-IR G141 grism spectroscopy to measure Halpha fluxes and sizes. The spatial resolution of HST combined with the sensitivity of Halpha as a star-formation indicator afford the ability to precisely trace the current amount and extent of star formation in galaxies at z > 1, physical properties that are poorly constrained with ground-based or Spitzer IR observations. Together, the HST and radio data will create the first sample of relatively typical star-forming galaxies at high redshift that have measurements of both molecular gas and star formation rate (SFR) surface densities. Combined with existing HST grism observations of 3 additional galaxies from our CO survey (for a total of 16 sources), this dataset will provide unprecedented insight into what fueled the high level of global star formation at z > 1 and what drove its decline over the last 7 Gyr. The precise measurements of current SFR and its spatial extent, derived from WFC3 spectroscopy, will enable us to determine if the higher SFRs at high redshift are due to greater supplies of cold gas or greater star formation efficiencies. Furthermore, the proposed observations will allow us to test the applicability of the Kennicutt-Schmidt relation for star formation rate versus gas surface density at high redshift, where the bulk of star formation occurs. This relation, which is a critical component of galaxy formation models, remains poorly constrained beyond the local Universe. Observation Description HST GO Program 12547 PI Michael Cooper This program involves targeted observations of 13 star-forming galaxies at at 1 < z < 1.4 using the WFC3-IR G141 grism to obtain slitless spectroscopy. The chief aims of the program are to (i) measure Halpha luminosities and sizes for the 13 target galaxies and (ii) conduct a blind redshift survey in each of the target fields. The visits are subject to position angle/ORIENT constraints in order to ensure that spectral observations of the primary target (one of the 13 star-forming galaxies) are not negatively impacted by overlap from a nearby bright object. A wide range of ORIENTs are allowed for each object, allowing flexibility in scheduling and finding guide stars. Two of our proposed targets are separated by 116'', such that they are able to be observed in a single WFC3 pointing. As a result, we are able to observe 13 targets with a total of 24 orbits (2 orbits per pointing/visit). Orbit/Visit Strategy: ---------------- In each visit (2 orbits per visit), we observe 1 target field at 4 dither positions. At each position in the dither pattern, we take a short direct F140W exposure and a long grism G141 exposure, using the GRSIM1024 aperture. The direct exposures are necessary as a reference for the object locations in order to extract and wavelength-calibrate the slitless spectra. Taking a direct exposure at each dither costs little time, will make the data easier to reduce, and allows making a combined direct HST image of the field (excellent resolution albeit not very deep). The direct exposures are ~200 sec (SPARS25 x NSAMP=9 or NSAMP=10) and the grism exposures are ~1300 sec (SPARS100 x NSAMP=14 or NSAMP=13). The longer grism exposures result from less overhead in orbit 2 for guide star (re-)acquisition. The order of exposures within an orbit is: direct, grism, grism, direct. This saves a wheel move over direct, grism, direct, grism, and seems to be a better order for timing buffer dumps. Dithering Strategy: --------------- We use POS-TARG offsets to make the dithers. Each direct/grism pair has the same set of POS-TARG offsets. The dither pattern is one that we designed (as part of separate Cycle-17 program -- PID 11600; PI Weiner), using the following offsets in x,y: WFC3 pix ACS pix arcsec (POS-TARG) 0.0 0.0 0.0 0.0 0.0 0.0 4.5 1.5 6.41 11.46 0.6075 0.1815 2.0 5.5 -5.13 10.0 0.2700 0.6655 -2.5 4.0 -11.54 -1.46 -0.3375 0.4840 The point of this dither pattern is to produce half-pixel steps in both the WFC3-IR and parallel ACS data. The half-pixel steps are necessary for WFC3-IR since it is somewhat undersampled, and also highly desirable for ACS data. We have assumed that the POS-TARG x and y axes are parallel to the WFC3-IR x and y axes, as shown in the Phase 2 instructions. This dither pattern is just a tiny bit larger than the standard WFC3-IR-DITHER-BOX-MIN pattern. Orient Constraints: --------------- The visits are subject to position angle/ORIENT constraints in order to ensure that spectral observations of the primary target (one of the 13 star-forming galaxies) are not negatively impacted by overlap from a nearby bright object. Each 1st-order grism spectral trace is 20′′ long, and bright objects also have a visible 0th-order image. We searched catalogs for nearby objects and have specified ORIENT constraints on each target to avoid contamination from nearby galaxies in either 0th or 1st order. We avoid 0th-order contaminants 2 mag brighter than the primary, and 1st-order contaminants down to 1 mag fainter. 2nd-order spectra are too faint to be of concern. A wide range of ORIENTs are allowed for each object, allowing flexibility in scheduling and finding guide stars. Parallels: ------- We have requested parallel exposures with ACS using the F814W I-band filter. For each dither position, with a WFC3 direct+grism exposure pair, we configured an ACS CR-SPLIT=2 exposure. The resulting exposures are of order 650 seconds long. We are doing 4 dithers at each target, so the CR-SPLIT is not relied on for cosmic ray removal; pairing the exposures keeps them to a reasonable length. The reasonably long WFC3 grism and ACS F814W exposures allow efficient buffer dumping during an orbit so that little time is lost to overheads. The total exposure time in ACS F814W is about 5000 sec per 2-orbit visit. Since the ORIENT constraints are only limited by the effort to ensure clean grism spectra are collected for the primary science targets (see summary above), the ACS parallels will often (but not always) overlap existing ACS imaging from previous programs (e.g., PID 10134, PI Davis and PID 12063, PIs Faber & Ferugson) --- either outcome will yield additional scientific value. When overlap occurs, the addition to the net ACS/F814W exposure time in the field will be considerable. In other cases, the parellel field will expand the area with existing ACS imaging (reaching a depth deeper than that of PID 10134) and will still fall within the area covered by many ground- and space-based programs (e.g., Spitzer FIDEL, DEEP2 and DEEP3 surveys) that will benefit from the additional areal coverage. Special Requirements: ----------------- We have requested a bright limb avoidance limit of 35 degrees. Previous observations (e.g., from PID 11600 and PID 11719) have shown that WFC3-IR suffers from significant scattered light near the Earth's bright limb --- see HOPR #1757 for further details. We note that all of the visits in our program have been designed with default settings (i.e., BRIGHT LIMB AVOID = 20) since visibility tables do not exist within APT for BRIGHT LIMB AVOID = 35. STAR FORMATION 0 false 0.0 0.0 false false false false AVAILABLE GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 20.4 (AB), z=1.12 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.9 (AB), z=1.19 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.7 (AB), z=1.28 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.8 (AB), z=1.10 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 22.3 (AB), z=1.17 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.9 (AB), z=1.17 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 22.7 (AB), z=1.37 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 22.1 (AB), z=1.38 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.2 (AB), z=1.03 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.7 (AB), z=1.00 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 21.8 (AB), z=1.02 GALAXY HIGH REDSHIFT GALAXY J2000 J2000 I = 20.9 (AB), z=1.16 and I = 21.5 (AB), z=1.12 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 WFC3/IR Spectroscopic No No G141 ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W ACS/WFC Imaging No No F814W The scheduling data was generated by CASM 19.3. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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