0 Assigned ID: 1195 ----- Attempting Submission 1 (Fri Apr 07 23:55:39 GMT 2017) ----- HST Phase I Proposal 1195 (M101.apt) successfully submitted. Receipt: # 1195-1 INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. INEFFICIENT ORDERING OF FP-POS POSITIONS INEFFICIENT ORDERING OF FP-POS POSITIONS COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. MERGING RULE VIOLATED DURING AUTOMATIC MERGING MERGING RULE VIOLATED DURING AUTOMATIC MERGING COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. MERGING RULE VIOLATED DURING AUTOMATIC MERGING MERGING RULE VIOLATED DURING AUTOMATIC MERGING COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. MERGING RULE VIOLATED DURING AUTOMATIC MERGING MERGING RULE VIOLATED DURING AUTOMATIC MERGING COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. MERGING RULE VIOLATED DURING AUTOMATIC MERGING MERGING RULE VIOLATED DURING AUTOMATIC MERGING COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. MERGING RULE VIOLATED DURING AUTOMATIC MERGING MERGING RULE VIOLATED DURING AUTOMATIC MERGING COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Updated offset coordinates to RA (sec) and Dec (arcsec) for Visit 3. Check target confirmation images and everything looks good. 730328522 ----- Attempting Submission 2 (Wed Jan 16 20:20:45 GMT 2019) ----- HST Phase II Proposal 15126 (COS15126.phaseII.newoffsets.apt) successfully submitted. Receipt: # 15126-2 ----- Attempting Submission 3 (Fri Jan 18 12:21:27 GMT 2019) ----- ----- Attempting Submission 4 (Mon Jan 28 19:38:20 GMT 2019) ----- PC and CS are aware of these. Resolving the Abundance Discrepancy with HST/COS A long-standing problem in nebular astrophysics is the discrepancy between abundances derived from collisionally-excited optical emission lines (CELs) and optical recombination emission lines (RLs). Because the optical RLs are intrinsically very faint, there is only a small collection of extragalactic HII regions for which abundances from RLs are available. C/O relative abundances are measured for a subset of these. By observing CIII] 1907,1909 and OIII] 1661,1666 in the ultraviolet, we can obtain a very secure measurement of the C/O ratio from CELs. Comparing the C/O relative abundances from UV CELs with those from optical RLs provides an independent test of the abundance discrepancy. Using the LBT, we have obtained high quality optical spectra for a large sample of HII regions in M101. We have detected the C III 4267 line in 10 of these regions. By observing these 10 regions, which span nearly a dex in oxygen abundance, we can compare the C/O and C/H abundances in these regions to provide an independent test of the abundance discrepancy. This study will also result in the most accurately measured carbon abundance gradient in a spiral galaxy. Goal: We will obtain NUV target aquisiton images of nearby stars and then use blind offsests to our targets in orde to obtain FUV COS spectroscopy of 10 H II regions in the spiral galaxy M101. We will measurement the O III] 1661,1666 and C III] 1907,1909 emission lines in these regions in order to compare the C/O gradient from optical RLs, optical CELs, and UV CELs. By measuring the C/O ratios in these metal-rich HII regions, we will extend the scale of the UV C/O relationship 0.5 dex to higher oxygen abundances. Targets: As part of the CHemical Abundances Of Spirals project (CHAOS; PIs E. Skillman & R. Pogge), we conducted a detailed study of the physical conditions and chemical abundances in the ISM of M101 using high S/N optical spectroscopy from LBT/MODS. As an extension of this project, we have examined the CHAOS spectra for the optical C II 4267 RL and have measured significant detections in 10 H II regions (Skillman et al. 2017, in prep.). These 10 H II regions are the targets we will study with this COS program. Target Acquisition: Due to the proximity of M101, the large H II regions fill the COS aperture, however, target image acquisition can be efficiently achieved using a pointing offset from a nearby bright star. In order to achieve acquistion images in a short exposure time, we require stars that are bright in the NUV, as determined by their GALXEX magnitudes. We then select stars that are near to our HII regions that are also visible in the PanSTARRs g-band images of M101. The excellent astrometry of PanSTARRs provides precise catalog positions of our offset stars and allows us to accurately determine offsets from the PanSTARRs images. We use the ACQ/IMAGE mode with the PSA aperture and MirrorB (due to the brightness of the offset stars) for the COS/NUV configuration. For these acquitions, we have determined integration times necessary to reach a S/N = 40. We assume a flat spectral distribution normalized by the GALEX NUV magnitudes. From our offset stars, we use the offsets determined form the PanSTARRs images to slew to our target HII regions. These offsets range between 0.75' to 2.38'. This is significantly larger than the recommended offset distance of 30", however, the exact pointing within the bright HII region is not critical. Additonally, our phase II support contact, William Januszewski, has confirmed that this acquisition plan will not cause any guide star or scheduling issues. Science Exposures: We will use COS with the G140L grating with a central wavelength of 1280 angstroms in TIMETAGE mode in order to obtain simultaneous measurements of the CIV 1548,1550, HeII 1640, OIII] 1661,1666, and CIII] 1907,1909 emission lines in Detector segment A. We used the GALEX FUV surface brightnesses to estimate the exposure time using the PSA aperture in the FUV configuration, requiring each of our targets to achieve a S/N >= 3 per resolution element in the limiting OIII] 1666 line. This results in sinlge orbits for 8/10 targets, 1 target requiring 2 orbits, and 1 target requiring 3. For the FUV G140L configuration, no flats are available and so we use FP-POS=ALL, which takes 4 images offset from one another in the dispersion direction and increases S/N. These 4 positions allow a flat to be created and cosmic rays to be eliminated. Note that while the resolution of COS spectra is degraded for non-point sources, our experience in B16 and B17 has proven that the O III] doublet can be resolved and the C III] doublet can be deblended for targets with extended nebular emission that filled the COS aperture. Galaxies and the IGM 6 false false false false false false false SUPPORTED EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 22.139 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 22.669 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.397 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.284 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.298 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.070 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.816 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.250 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 21.673 EXT-MEDIUM HII REGION YES Magnitude of M101 J2000 FUV/arcsec squared = 20.224 EXT-MEDIUM HII REGION NO J2000 NUV=17.34 EXT-MEDIUM HII REGION NO J2000 NUV=15.67 EXT-MEDIUM HII REGION NO J2000 NUV =17.6 EXT-MEDIUM HII REGION NO J2000 U=15.05 EXT-MEDIUM HII REGION NO J2000 U=15.05 EXT-MEDIUM HII REGION NO J2000 NUV=17.64 EXT-MEDIUM HII REGION NO J2000 U=15.26 EXT-MEDIUM HII REGION NO J2000 U=15.26 EXT-MEDIUM HII REGION NO J2000 NUV=17.85 EXT-MEDIUM HII REGION NO J2000 NUV=17.85 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 COS/FUV Spectroscopic No No G140L 1280 The scheduling data was generated by CASM 26.2.2. CASM was run in Phase II mode. /Users/bergda/Desktop/RESEARCH/PROPOSALS/HST/M101_CO/PHASEII/OP-cache/COS15126-v01.xml (Tic-Visit :proposal-id 15126 :visit-id "01" :proposal-version -1 :trans-version "20181130" :date "28-Jan-2019 10:53:28.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 87360 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 15126 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 15126 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2997 :al-overhead-at-end 0 :internal-dur-at-end 38 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) (Tic-Orbit :proposal-id 15126 :visit-id "01" :orbit-number 2 :pcs-time 302 :si-vis-utilization 3031 :al-overhead-at-end 0 :internal-dur-at-end 331 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3333 :pcs-gap 0 ) true 2 0 The scheduling data was generated by CASM 26.2.2. 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