0 Assigned ID: 4013 ----- Attempting Submission 1 (Mon May 22 04:37:58 GMT 2023) ----- HST Phase I Proposal 4013 successfully submitted. Receipt: # 4013-1 This target is not used in this proposal. This target is not used in this proposal. This target is not used in this proposal. Duplicated Visit 01 as Visit 12 due to failure of observations. The observing setup is identical. -597768188 ----- Attempting Submission 1 (Tue Sep 05 18:37:18 GMT 2023) ----- HST Phase II Proposal 17486 successfully submitted. Receipt: # 17486-1 ----- Attempting Submission 2 (Fri Sep 08 14:48:03 GMT 2023) ----- HST Phase II Proposal 17486 successfully submitted. Receipt: # 17486-2 ----- Attempting Submission 3 (Mon Sep 11 22:36:08 GMT 2023) ----- HST Phase II Proposal 17486 successfully submitted. Receipt: # 17486-3 ----- Attempting Submission 4 (Tue Sep 26 07:04:30 GMT 2023) ----- HST Phase II Proposal 17486 successfully submitted. Receipt: # 17486-4 ----- Attempting Submission 5 (Tue Sep 26 23:30:16 GMT 2023) ----- ----- Attempting Submission 6 (Wed Jun 19 09:52:50 GMT 2024) ----- ----- Attempting Submission 7 (Wed Feb 19 06:18:09 GMT 2025) ----- MAGPI1203, MAGPI1509, and MAGPI2304 were swapped out of the program because of limited guide stars UV-MAGPI: Sharpening our View of Dust Attenuation A description of dust attenuation curves and how they evolve with time is a critical ingredient of future precision studies of distant galaxies. The aim of the UV-MAGPI survey is to develop a revolutionary understanding of how light from galaxies is affected by dust attenuation at varying spatial scales, gas-phase metallicity, and galactic environment. This will help to inform more versatile prescriptions of dust attenuation as a function of cosmic time. We will combine UV data from HST with VLT/MUSE and VISTA, providing rest-frame UV to near-IR coverage, to perform a spatially-resolved (~3kpc-scales) study of dust attenuation at z~0.3 in 41 star-forming galaxies (SFGs) and in an integrated manner for an additional 57 SFGs (98 total). This is expected to provide fundamental insight into (1) how dust properties, most notably the 2175Ang absorption feature, and dust attenuation curves vary within galaxies and between galaxies and (2) which intrinsic galaxy properties are responsible for attenuation variation. The extensive data for these fields will also provide numerous opportunities for legacy science to study spatially-resolved and integrated properties of SFGs and early-type galaxies at low and intermediate redshifts. UV-MAGPI will obtain HST WFC3/UVIS UV imaging in 4 filters (F225W, F275W, F336W, F390W) for 11 independent fields with MUSE optical IFS spectroscopy of galaxies at 0.25<z<0.35. At z~0.3, the selected WFC3/UVIS bands provide rest-frame coverage of the 0.18-0.30um region to characterize the nature of dust attenuation in galaxies. Each field will be observed across 3 orbits: 1 orbit for F225W, 1 orbit for F275W, and 1 orbit for F336W+F390W per field (33 orbits in total). The exposure times are set by the requirement to detect (at S/N~4-5) spatially-resolved regions within star forming galaxies at z~0.3 that are experiencing moderate attenuation of their UV light due to dust (mu_R=23 AB mag with E(B-V)star=0.4). The MUSE FOV (60"x60") is smaller than the WFC3/UVIS FOV (82.04"x163.84") and our targets fit on a single UVIS chip, therefore we do not require mosaicking or have any position angle restrictions. We place the MUSE fields in the center of the more-sensitive chip (Chip 2) using the UVIS2-FIX aperture. We adopt the ACCUM readout and use a standard WFC3-UVIS-DITHER-LINE-3PT patern to subsample the PSF and to mitigate cosmic rays. This pattern choice does not fill-in the chip gap (not required). We use a post flash ranging from 17-19e- to overcome CTE issues. PI Battisti is a MAGPI team member and an expert in dust attenuation, star formation, and SED modelling. He leads the development of emission line data products for the MAGPI team. He will work on the derivation and characterization of attenuation curves and the 2175A feature and their evolution with galaxy properties, inclination, and environment. He will also lead development and distribution of the data products and their cross-matching with MAGPI data products. Co-I Wisnioski is one of the PIs of MAGPI. She specialises in studies of the interstellar medium and its evolution over cosmic time. She is a world-recognised expert on early star-forming galaxies. She is co-leading a group of 60+ researchers across Australia, Europe, Asia, and South America facilitating science across a range of key questions in galaxy evolution. Emily will assist with the analysis and dissemination of the HST products in MAGPI team publications. Co-I Mendel is one of the PIs of MAGPI. He is responsible for identifying objects and producing matched photometric catalogs for MAGPI. He is an expert on galaxy evolution and SED modelling and will aid the interpretation of the data and the production of HST object catalogs. Co-I Lagos is one of the PIs of MAGPI. She is an expert on galaxy formation simulations and will be providing predictions for the effect of dust on galaxies across different environments and will aid the interpretation of the data. Co-I Foster is one of the PIs of MAGPI. She is an expert in galaxy transformation at low and intermediate redshift. She is an expert in IFS studies of the stellar dynamics and populations of early-type galaxies and will aid in the interpretation of the data. She will contribute to the production of matched MUSE/HST ancillary data and supervision of HDR students working on the legacy dataset. Co-I Harborne is one of the PIs of MAGPI. She has extensive experience working with a range of cosmological, hydrodynamical simulations of galaxy formation. Her expertise in constructing mock observables of such models will facilitate comparisons between the theory and data. Co-I Calzetti is an expert of star formation and dust obscuration. She has extensive experience with HST imaging data, and has worked on data from infrared telescopes, ISO, Spitzer, and Herschel. She has been/is the PI of multiple HST programs, including the Cycle 21 Treasury project LEGUS (Legacy ExtraGalactic UV Survey), and has been deputy PI of both Spitzer and Herschel legacy programs. She will work on the derivation and characterization of attenuation curves and the 2175A feature. Co-I Shivaei is an expert in dust attenuation, star formation, and SED modelling, particularly of high-redshift galaxies. She will work on the derivation and characterization of attenuation curves and the 2175A feature. Co-I Grasha is an expert in star formation and theoretical modeling of emission lines. She will aid in the interpretation of the data. Co-I Gupta is an expert on galaxy evolution, particularly of high-redshift galaxies. She will aid in the interpretation of the data. 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CASM was run in Phase II mode. 1715564355000 246.09000000000003 (Tic-Visit :proposal-id 17486 :visit-id "08" :proposal-version -1 :trans-version "20230626" :date "27-Sep-2023 09:25:29.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17486 :visit-id "08" :obset-id "08" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17486 :visit-id "08" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2776 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "08" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2767 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "08" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2767 :al-overhead-at-end 128 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 33.0. CASM was run in Phase II mode. 1707483411000 296.0 (Tic-Visit :proposal-id 17486 :visit-id "09" :proposal-version -1 :trans-version "20230626" :date "27-Sep-2023 09:25:31.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17486 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17486 :visit-id "09" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2753 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "09" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2744 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "09" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2744 :al-overhead-at-end 128 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3136 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 33.0. CASM was run in Phase II mode. 1719944957000 273.7412067214974 (Tic-Visit :proposal-id 17486 :visit-id "10" :proposal-version -1 :trans-version "20240604" :date "19-Jun-2024 17:45:30.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3176224 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17486 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17486 :visit-id "10" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2654 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "10" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2654 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "10" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2654 :al-overhead-at-end 125 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3034 :pcs-gap 0 ) true 3 0 The scheduling data was generated by CASM 33.0. CASM was run in Phase II mode. 1715382529000 241.9724940086444 (Tic-Visit :proposal-id 17486 :visit-id "11" :proposal-version -1 :trans-version "20230626" :date "27-Sep-2023 09:25:35.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 3464976 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17486 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17486 :visit-id "11" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2776 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "11" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2767 :al-overhead-at-end 126 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17486 :visit-id "11" :orbit-number 3 :pcs-time 392 :si-vis-utilization 2767 :al-overhead-at-end 128 :internal-dur-at-end 668 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3159 :pcs-gap 0 ) true 3 0