A Race Against the Clock: Too Much Nitrogen, Too Early?

For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. For G160M observations, please consult Chapter 9 of the COS Instrument Handbook to estimate overheads and the number of exposures per orbit, and consequently the correct lifetime position. Use of LP4 with G160M requires justification in the "Special Requirements" section of the Phase I PDF. Use of the default LP6 with G160M requires no justification. Proposals can be submitted with the warning present. 0 Assigned ID: 5402 ----- Attempting Submission 1 (Tue Mar 26 13:08:35 GMT 2024) ----- HST Phase I Proposal 5402 successfully submitted. Receipt: # 5402-1 ----- Attempting Submission 2 (Tue Mar 26 17:55:32 GMT 2024) ----- G160M LP warning - LP6 is fine as far as I can tell. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN 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. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN ORBITAL VISIBILITY OVERRUN 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. 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. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. For the best data quality, it is generally required to use all four FP-POS positions at a given COS cenwave (or 2 positions for certain exception cases). See extended explanation in the diagnostic browser. 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. COS FUV PSA science exposures with extended targets have special calibration limitations. See "Errors and Warnings" for more details. Repeat observations for partially approved HOPR 93487. 225958432 ----- Attempting Submission 1 (Tue Aug 06 22:29:25 GMT 2024) ----- Your proposal could not be saved. Submission aborted. ----- Attempting Submission 2 (Mon Jun 08 21:47:58 GMT 2026) ----- There are two errors/warnings that occur multiple times: - warning about PSA wiht extended targets - this is noted and fine. - warning about inefficient ordering of FP-POS positons - happy to consult with my contact scientits about this. A Race Against the Clock: Too Much Nitrogen, Too Early? Chemical abundances encode the integrated star formation over the lifetimes of galaxies. Since stars produce different metals, e.g., nitrogen and oxygen, at different times, the relative abundance of N/O acts as a clock to determine the star formation history. Specifically, N/O describes the relative ratio of moderately old stars(>100 Myr) to very young stars (<10 Myr). Recently, JWST observations of an extreme star-forming galaxy only 440 Myr after the big bang have found extremely high-energy N IV] and N III emission lines. These lines suggest that the galaxy has a super-solar N/O ratio, implying a contradiction: this galaxy has existed for < 440 Myr but still has a substantial older stellar population that is responsible for the N enrichment. This galaxy has too much N too early in the universe. However, few galaxies at any redshift have similar high-ionization N emisison. Unearthing the mechanism that produces these emission lines is required to reveal the chemical enrichment of the first galaxies. We propose 26 orbits of COS G160M + G185M spectroscopic observations of 7 local high-ionization galaxies. We will measure the FUV high-ionization emission lines (NIV], NIII, CIV, HeII, OIII], OIV), as well as describe their stellar populations. This will test the ionizing source within these galaxies and determine if the strong high-ionization emission arises from exotic non-stellar sources. These observations will map out the ionization structure of these galaxies to accurately determine their N/O values. Combined, these observations will construct a blueprint to interpret observations of the most extreme early galaxies to reveal the primitive relative abundance patterns. Goal: The observational goal of our program is to use the high-resolution G160M and G185M gratings on COS to obtain measurements of the N IV] 1483,1486 and N III] 1747,1749,1750,1752,1750 emission lines in 7 extreme N emission line candidates. Target Acquisition: We have excellent input coordinates for our sample from the previous optical spectroscopy studies, allowing us to utilize the ACQ/IMAGE mode for target acquisition with the PSA aperture and MirrorA for the COS/NUV configuration. For these acquitions, we have determined integration times necessary to reach a S/N >= 20. We assume a flat spectral distribution normalized by the GALEX FUV or SDSS u-band surface brightnesses, where each galaxy is compact in its optical imaging with a FWHM PSF diameter of ~2". Science Exposures: We will use the COS G160M and G185M gratings with central wavelengths determined by the redshifted location of the NIII] and NIV] emission lines in TIMETAG mode with the PSA aperture. Since not much is yet known about the behavior of the UV N III] and N IV] emission, we use the COS ETC with predicted UV line fluxes to determine the time necessary to achieve a S/N per resolution element of > 3 for the strongest lines in the NIII] multiplet. The total number of orbits necessary were determined considering the length of target visibility per orbit (APT) plus the approximate overheads: i.e., guide star acquisition (6 min), reacquisition (4 min), ACQ/IMAGE target acquisition (3 min), and science exposures (11 min for 4 exposures). We use a minimum of 2 FP-POS positions for each grating. All investigators are experts in observational studies of extreme emission line galaxies, particularly focusing on nebular gas, its diagnostics, N emission, and stellar populations. The team has significant experience of stellar modeling (Chisholm), photoionization modeling (Berg, James, Mingozzi, Arellano-Cordova), and the measurement on N abundances (Berg, Skillman, Rogers, James, Arellano-Cordova) that will be required for the interpretation of the data. Several of our investigators have also pioneered observational campaigns of the weak UV emission lines, in both the local universe and at the highest redshifts (Berg, Mingozzi, James, Skillman, Rogers). All also have significant expertise in imaging and spectroscopy with Hubble, having led more than 41 programs over the last decade. In particular, co-PIs D. Berg, B. James, and J. Chisholm have been leading the field in detecting and characterizing extreme emission line galaxies and co-PIed the CLASSY Treasury Survey. Galaxies Stellar Populations and the Interstellar Medium 6 false true false false false false false SUPPORTED GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u = 20.5; FUV = 21.04; NUV = 20.58 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u=22.8; FUV = 19.14 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u=19.4 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u = 20.32 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u=20.3; FUV = 19.8 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u=17.9 GALAXY DWARF COMPACT EMISSION LINE NEBULA STAR FORMING REGION YES J2000 J2000 u=20.31 COS/NUV Spectroscopic No No G185M 1864 COS/FUV Spectroscopic No No G160M 1611 COS/NUV Spectroscopic No No G185M 1817 COS/FUV Spectroscopic No No G160M 1589 COS/NUV Spectroscopic No No G185M 1890 COS/FUV Spectroscopic No No G160M 1577 COS/NUV Spectroscopic No No G185M 1864 COS/FUV Spectroscopic No No G160M 1577 COS/NUV Spectroscopic No No G185M 1900 COS/FUV Spectroscopic No No G160M 1533 COS/NUV Spectroscopic No No G185M 1864 COS/FUV Spectroscopic No No G160M 1533 COS/NUV Spectroscopic No No G185M 1900 COS/FUV Spectroscopic No No G160M 1577 1780955026600 /private/var/folders/3v/3pp29g8x19vfh3bt22hd2cfh0000gp/T/OPVisit8508446077496964608.xml The scheduling data was generated by CASM 32.1.1. 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CASM was run in Phase II mode. 1755773743000 260.4580734823685 (Tic-Visit :proposal-id 17791 :visit-id "09" :proposal-version -1 :trans-version "20240604" :date "06-Aug-2024 17:21:47.0" :trans-errors '(:WARNINGS 0 :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 296160 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17791 :visit-id "09" :obset-id "09" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17791 :visit-id "09" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2629 :al-overhead-at-end 0 :internal-dur-at-end 2296 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "09" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2630 :al-overhead-at-end 0 :internal-dur-at-end 527 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3010 :pcs-gap 0 ) true 2 0 1722982909693 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1755953928000 206.08961470243474 (Tic-Visit :proposal-id 17791 :visit-id "06" :proposal-version -1 :trans-version "20240604" :date "06-Aug-2024 17:21:49.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 357072 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17791 :visit-id "06" :obset-id "06" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17791 :visit-id "06" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2635 :al-overhead-at-end 0 :internal-dur-at-end 2290 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "06" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2634 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "06" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2632 :al-overhead-at-end 0 :internal-dur-at-end 369 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 3 0 1722982911094 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1758756383000 302.8744308750622 (Tic-Visit :proposal-id 17791 :visit-id "10" :proposal-version -1 :trans-version "20240604" :date "06-Aug-2024 17:21:51.0" :trans-errors '(:WARNINGS 1 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "32" :si-bright-earth-limb-angle 20.0 :data-volume 295872 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17791 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17791 :visit-id "10" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2660 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "10" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2669 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "10" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2669 :al-overhead-at-end 0 :internal-dur-at-end 398 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) true 3 0 1722982912459 The scheduling data was generated by CASM 32.1.1. CASM was run in Phase II mode. 1763386678000 273.14885387304594 (Tic-Visit :proposal-id 17791 :visit-id "11" :proposal-version -1 :trans-version "20240604" :date "06-Aug-2024 17:21:52.0" :trans-errors '(:WARNINGS 0 :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 296160 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17791 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17791 :visit-id "11" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2668 :al-overhead-at-end 0 :internal-dur-at-end 2257 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17791 :visit-id "11" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2668 :al-overhead-at-end 0 :internal-dur-at-end 527 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3049 :pcs-gap 0 ) true 2 0