0 Assigned ID: 5662 ----- Attempting Submission 1 (Tue Mar 26 21:13:04 GMT 2024) ----- SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE SAME POS MAY NOT BE APPROPRIATE The 12 warnings refer to the SAME POS requirement, which we set between the short direct image and grism exposures for each visit to make sure that they are at the same position. There are no other warnings. -811834294 ----- Attempting Submission 1 (Fri Aug 16 16:43:39 GMT 2024) ----- The 12 warnings refer to the SAME POS requirement, which we set between the short direct image and grism exposures for each visit to make sure that they are at the same position. There are no other errors or warnings. Gravitational-arc tomography of the circumgalactic medium at z~0.7: Identifying the host galaxies of three MgII absorbers The dynamic circumgalactic medium (CGM) is the site of gas flows into, out of, and around galaxies, and thus plays a central role in regulating star formation over cosmic time. Many of its properties remain unconstrained, however, particularly on a spatially resolved basis. Extensive statistical studies of the gas around galaxies have been performed using the absorption it produces in background sources, usually quasars that probe a single line of sight. In particular, absorption from singly-ionized magnesium (MgII) has been shown to trace the outflow and accretion of cool, enriched gas surrounding galaxies. More recently, a handful of MgII-absorbing galaxies have been studied with gravitational-arc tomography, which uses the fortuitous alignment of an intermediate redshift galaxy and a background lensed arc to probe the gas around the foreground galaxy in unprecedented detail over tens of kpc. We here propose to use WFC3/IR grism spectroscopy to identify the galaxies responsible for spatially varying foreground MgII and FeII absorption observed at z~0.7-0.8 in Keck Cosmic Web Imager (KCWI) integral field spectroscopy of three gravitationally lensed galaxies. The proposed observations will provide spectroscopy at high spatial resolution of the entire field surrounding each arc, targeting H-alpha emission at the redshifts of the absorbers. Identification of the absorbing galaxies will enable measurement of the impact parameters of the absorption and the correlation of the strength, structure and kinematics of the absorption lines with the morphologies, star formation rates, and star formation rate surface densities of the absorbing galaxies. The three target absorption systems are at z = 0.69, z = 0.83 and z = 0.65 for J1206+5142, J1514+3636 and J0918+5104 respectively, placing Halpha emission at 1.109, 1.201 and 1.083 um. We will therefore use the G102 grism with F098M direct images for the two lower redshift targets, J1206+5142 and J0918+5104, and the G141 grism with F140W direct images for J1514+3636. Orbits and exposures: ----------------- We observe each target for two orbits, and each visit consists of one orbit. In each orbit 2 dithered exposures with the grism will be obtained, along with short direct images taken at the same position, which are necessary for the wavelength calibration. We schedule the two orbits on each target as two different visits, with the roll angle of the second visit set to differ from that of the first visit by at least 20 degrees. We set ORIENT 20 TO 160 from the previous visit to the target, but ORIENT -20 to -160 is also acceptable. The purpose of using different roll angles for the two orbits is to improve our ability to account for contamination by overlapping spectra. This offset in the roll angle between visits to the same target will produce two sets of data with differing contamination properties, making the overall contamination for individual spectra easier to determine. We follow the simple pattern: direct, grism, offset, direct, grism Dithering strategy: --------------- We use POS-TARG offsets to enable rejection of hot/bad pixels and to improve sampling of the PSF. The pattern is: POS-TARG: (0, 0) (1.355, 0.424) pixels: (0, 0) (10.0, 3.5) This is a larger version of the standard WFC3-IR-DITHER-BOX-MIN pattern, which has only 1-2 pixel offsets between pointings. As some bad pixels come in clumps we prefer a slightly larger pattern. No attempt is made to dither over the "dead spot", as large dithers introduce large differential distortion. We use the same dither pattern for both visits to each field, since the differing orientations will ensure that spectra of the same objects fall on different pixels. Additional requirements: ------------------- For J1206+5142, we additionally specify an ORIENT range of 117 to 28 degrees for the first visit, based on avoiding spectral contamination from the lens and arc for the most likely host galaxy. We place no ORIENT constraints on the first visit for the other two targets. PI Prof. Dawn Erb has extensive experience in the imaging and spectroscopy of high redshift galaxies, including UV absorption line spectroscopy (Erb et al. 2010, 2012), the study of lensed galaxies (Erb et al. 2019), and integral field spectroscopy with KCWI (Erb et al. 2023). Prof. Britt Lundgren specializes in studying gaseous halos probed by MgII absorption, and led a Cycle 21 HST program that used the WFC3/IR grism to identify the host galaxies of MgII absorbers (Lundgren et al 2021). Dr. Matthew Auger is an expert on gravitational lensing, and has constructed lens models for large numbers of high redshift galaxies; those recently studied by our team include Berg et al 2018, Erb et al 2019, and Citro et al 2021, 2024. Dr. Lindsay Oldham specializes in the precise modeling of gravitational lenses in order to constrain the structure of galaxies (Oldham et al 2018a, 2019b). Prof. Max Pettini is one of the leading experts on both the study of absorption line systems (e.g. Pettini et al 2003, 2002, 1999) and gravitationally lensed galaxies (Pettini et al 2001, 2002, Quider et al 2009, 2010). Dr. Annalisa Citro is an expert in the spectroscopy of galaxies, with particular experience in the analysis of the UV spectra of gravitationally lensed sources (Citro et al 2021, Citro et al 2024, submitted). Dr. Bethan James is a leader in spectroscopic studies of both local galaxies and more distant lensed sources, specializing in the spatial variations of metallicity and gas flows with both UV and optical spectra (James et al. 2014, 2016, 2018, 2020). Prof. Danielle Berg is a leader in spectroscopic surveys of galaxies, with particular expertise in the analysis of both UV and optical spectra (Berg et al 2018, 2019, 2021, 2022). References: Berg, D. A., Chisholm, J., Erb, D. K., et al. 2019, ApJ, 878, L3 Berg, D. A., Chisholm, J., Erb, D. K., et al. 2021, ApJ, 922, 170 Berg, D. A., Erb, D. K., Auger, M. W., et al. 2018, ApJ, 859, 164 Berg, D. A., James, B. L., King, T., et al. 2022, ApJS, 261, 31 Citro, A., Erb, D. K., Pettini, M., et al. 2021, ApJ, 922, 187 Erb, D. K. 2008, ApJ, 674, 151 Erb, D. K., Berg, D. A., Auger, M. W., et al. 2019, ApJ, 884, 7 Erb, D. K., Li, Z., Steidel, C. C., et al. 2023, ApJ 953, 118 Erb, D. K., Pettini, M., Shapley, A. E., et al. 2010, ApJ, 719, 1168 Erb, D. K., Quider, A. M., Henry, A. L., & Martin, C. L. 2012, ApJ, 759, 26 James, B. L., Auger, M., Aloisi, A., et al. 2016, ApJ, 816, 40 James, B. L., Auger, M., Pettini, M., et al. 2018, MNRAS, 476, 1726 James, B. L., Kumari, N., Emerick, A., et al. 2020, MNRAS, 495, 2564 James, B. L., Pettini, M., Christensen, L., et al. 2014, MNRAS, 440, 1794 Lundgren, B. F., Creech, S., Brammer, G., et al. 2021, ApJ, 913, 50 Oldham, L. J., Auger, M. W.. 2018a, Monthly Notices of the Royal Astronomical Society, 476, 133 Oldham, L., Auger, M.. 2018b, Monthly Notices of the Royal Astronomical Society, 474, 4169 Pettini, M., Madau, P., Bolte, M., et al.. 2003, The Astrophysical Journal, 594, 695 Pettini, M., Ellison, S. L., Bergeron, J., et al.. 2002, Astronomy and Astrophysics, 391, 21 Pettini, M., Ellison, S. L., Steidel, C. C., et al.. 1999, The Astrophysical Journal, 510, 576 Pettini, M., Rix, S. A., Steidel, C. C., et al. 2002, ApJ, 569, 742 Pettini, M., Steidel, C. C., Adelberger, K. L., et al. 2000, ApJ, 528, 96 Quider, A. M., Pettini, M., Shapley, A. E., & Steidel, C. C. 2009, MNRAS, 398, 1263 Quider, A. M., Shapley, A. 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