0 Assigned ID: 2052 ----- Attempting Submission 1 (Fri Apr 09 17:40:31 GMT 2021) ----- HST Phase I Proposal 2052 successfully submitted. Receipt: # 2052-1 ----- Attempting Submission 2 (Fri Apr 09 22:47:09 GMT 2021) ----- FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser We specify the ORIENT angle for 2 visits; we require a secondary galaxy to be in the image field for our science. For Visit 05, I specified two sets of ORIENT ranges: 0 to 77 deg, and 343 to 359.9 deg. The APT raises error if I put 343 to 360 deg instead, stating there would be an overlap in the ORIENT ranges. For visits 02, 04, and 08, we require imaging in 2 filters. I take 4 exposures (2 per orbit) with F390W, and 2 exposues with F814W in the 2nd orbit. In order to have the target at slightly different positions in all 4 F390W frames instead of at 2 different positions only (with the WFC3-UVIS-DITHER-LINE pattern), I apply a small offset (by stating the POS-TARG offset) before the 2nd set of Dither pattern. 33373071 ----- Attempting Submission 1 (Wed Jul 21 13:36:32 GMT 2021) ----- The 14 errors are associated with the "high" post-flash election that we entered. However, from the ETC and from the Contact Scientist, we should ignore that warning, because the APT considers the old, 12e-/pix requirement instead of the new 20e-/pix requirement. Resolving the 3D Orientation of Galactic Disks: New Constraints on Circumgalactic Gas Flow The observed growth in both the size and mass of galactic disks since redshift two requires an even larger increase in the specific angular momentum of the gas accreted from the circumgalactic medium, which is the only reservoir of gas that can sustain disk star formation for 10 billion years. The rotation of inflowing circumgalactic gas is therefore central to the development of the angular momentum of stellar disks. Observing gas accretion is complicated by the galactic outflows that feedback from massive stars drive out of the galactic plane. While the position angle and axis ratio describe the projected shape of the galactic disk, this leaves an ambiguity of which side of the galaxy minor axis tips toward the observer. This ambiguity produces degenerate solutions in modeling gas flows and identifying the origin of the observed gas, because observers do not know where the gas lies along line-of-sight. We propose new WFC3/UVIS imaging observation to map the spiral structures of 11 z=0.25 galaxies with circumgalactic Mg II absorption detected in the quasar sightlines. We will determine the 3D disk orientation using rotation curves and the wrapping direction of galaxy spiral arms. The imaging sample will be combined with 3 Mg II absorbing galaxies with spiral arms detected in archival images, bringing our sample to 14 galaxies. We collected high-resolution spectra of the quasars paired with the galaxies; these spectra resolved multiple Mg II components. The 3D orientation will constrain parameters of physical models (disks, radial inflow, and conical outflow) in individual sightlines. The measured gas flow properties will provide new constraints for models of disk growth. We aim to resolve spiral structure of eleven galactic disks at intermediate redshifts. We image all eleven galaxies (in ten fields) with the F390W bandpass, which isolates the ultraviolet flux shortward of 4000 Angstrom of the rest frame of the target galaxies and will trace the light from stars younger than roughly 100 Myr. Imaging the galaxies in two filters provides a long wavelenght baseline and optimizes the contrast between the underlying stellar disk (old stellar population) and the spiral density waves (young stellar population). So, for four galaxies (in three fields) without any existing high-resolution, HST optical images, we also image the galaxies with the F814W bandpass. The F814W images will trace the older stellar population (>1 Gyr). We place each target galaxy at the lower left of quadrant C to mimimize the charge trails due to CTE losses. We also apply post-flash, such that the image total background reaches the recommended 20e-/pix to minimize the CTE losses. We use standard dither patterns; the sub-pixel dithers optimizes the sampling of the UVIS point spread function. We set constraints on the ORIENT angle if we require the imaging of a secondary galaxy in the field. Our team is experienced in studying the circumgalactic medium and its kinematics using quasar absorption-line studies. We lead several large surveys that study circumgalactic absorption properties and gas kinematics. Crystal Martin and Stephanie Ho co-lead the Quasars Probing Galaxies Program. This project studies the kinematics of Mg II absorbers and establish the relationship between Mg II gas kinematics and the galactic disk orientation. Chris Churchill and Glenn Kacprzak co-lead the Multiphase Galaxy Halo Survey (from HST PID 13398 and from the literature) at NMSU and Swinburne, respectively. This Survey studies the warm-hot CGM kinematics and its relationship with the galactic disk. Both Churchill and Kacprzak have also published extensive amount of work related to the Mg II gas properties, especially the gas kinematics. Nikki Nielsen leads the MAGIICAT project (Mg II Absorber-Galaxy Catalog). She complied this catalog and used it to study the properties of Mg II absorption, including the absorption strength, the kinematics, and the effect of group environment. She is also a key member of the Multiphase Galaxy Halo Survey. Rob Kennicutt is an expert in star formation and chemical evolution of galaxies. He has led and co-led a number of collaborations that conduct comprehensive multi-wavelength studies of nearby galaxies (e.g., SINGS, KINGFISH, etc.). The PI (Ho) has published the following papers directly related to the scientific goals of this proposal: Ho, S. H., Martin, C. L. & Schaye, J. 2020, ApJ, 904, 76 Ho, S. H. & Martin, C. L. 2020, ApJ, 888, 14 Martin, C. L., Ho, S. H. et al. 2019, ApJ, 878, 84 Ho, S. H., Martin, C. L. & Turner, M. L. 2019, ApJ, 875, 54 Ho, S. H. et al. 2017, ApJ, 835, 267 Kacprzak, G. G. et al. (including Stephanie Ho) 2017, ApJ, 792, L12 The PI (Ho) has the following HST programs related to this proposal: * GO-15866: This COS program obtained the FUV spectra of OVI 1032,1038 absorption around low-z galaxies. The project also focuses on gas kinematics; the analysis is ongoing, and the new spectra will determine whether the OVI gas kinematics correlates with disk rotation. * GO-14754: As a Co-I of this WFC3 program, she redrizzled the images, processed the images to identify spiral structures of galaxies, and used the inferred 3D disk orientation to develop analytical models for explaining the kinematics of absorption-line systems (PI: Crystal Martin). This program is directly related to the current proposal. Intergalactic Medium and the Circumgalactic Medium 6 false false false false false false false false SUPPORTED GALAXY SPIRAL YES J2000 J2000 AB mag [F702W] = 20.7 GALAXY SPIRAL YES J2000 J2000 u=22.47, r=20.62, i=20.32 GALAXY SPIRAL YES J2000 J2000 u=25.11, r=21.01, i=20.32 GALAXY SPIRAL YES J2000 J2000 u=21.43, r=19.46, i=19.11 GALAXY SPIRAL YES J2000 J2000 u=22.10, r=20.16, i=19.76 GALAXY SPIRAL YES J2000 J2000 u=21.66, r=19.09, i=18.62 GALAXY SPIRAL YES J2000 J2000 AB mag [F702W] = 20.18 GALAXY SPIRAL YES J2000 J2000 u=24.30, r=20.26, i=19.99 GALAXY SPIRAL YES J2000 J2000 u=20.33, r=18.79, i=18.45 GALAXY SPIRAL J2000 J2000 u=23.64, r=20.40, i=19.84 WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F814W WFC3/UVIS Imaging No No F390W WFC3/UVIS Imaging No No F390W POS-TARG DITHER 0.173 LINE 0.112 false false 81.785 4 23.884 WFC3-UVIS-DITHER-BOX 1 false POS-TARG DITHER 0.135 LINE false false 3 46.84 WFC3-UVIS-DITHER-LINE-3PT 2 false POS-TARG DITHER 0.145 LINE false false 2 46.84 WFC3-UVIS-DITHER-LINE 3 false /Users/stephaniehho/Dropbox/Proposals/observing_proposal/hst/2021_cycle29_imaging/phase2/OP-cache/qpg_imaging_phase2-v01.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 16742 :visit-id "05" :proposal-version -1 :trans-version "20210514" :date "19-Jul-2021 18:58:35.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 866240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16742 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16742 :visit-id "05" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3006 :al-overhead-at-end 122 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3389 :pcs-gap 0 ) true 1 0 /Users/stephaniehho/Dropbox/Proposals/observing_proposal/hst/2021_cycle29_imaging/phase2/OP-cache/qpg_imaging_phase2-v06.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. (Tic-Visit :proposal-id 16742 :visit-id "06" :proposal-version -1 :trans-version "20210514" :date "16-Jul-2021 12:37:43.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 866240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16742 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16742 :visit-id "06" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2900 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3285 :pcs-gap 0 ) true 1 0 /Users/stephaniehho/Dropbox/Proposals/observing_proposal/hst/2021_cycle29_imaging/phase2/OP-cache/qpg_imaging_phase2-v07.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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CASM was run in Phase II mode. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 16742 :visit-id "09" :proposal-version -1 :trans-version "20210514" :date "16-Jul-2021 12:45:30.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 866240 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16742 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16742 :visit-id "09" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2816 :al-overhead-at-end 123 :internal-dur-at-end 352 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3200 :pcs-gap 0 ) true 1 0 /Users/stephaniehho/Dropbox/Proposals/observing_proposal/hst/2021_cycle29_imaging/phase2/OP-cache/qpg_imaging_phase2-v10.xml The scheduling data was generated by CASM 29.2. CASM was run in Phase II mode. 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