pdf left off previously?? -1699795200 Assigned ID: 6517 ----- Attempting Submission 1 (Thu Apr 10 16:23:58 GMT 2025) ----- HST Phase I Proposal 6517 successfully submitted. Receipt: # 6517-1 ----- Attempting Submission 2 (Fri Apr 11 00:06:26 GMT 2025) ----- 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. 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. 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. I have removed the Orient constraints on the WFC3 observations since these were not approved in the TTRB that I submitted 132252836 ----- Attempting Submission 1 (Wed Aug 13 04:58:04 GMT 2025) ----- ----- Attempting Submission 2 (Tue Sep 02 02:05:05 GMT 2025) ----- HST Phase II Proposal 18117 successfully submitted. Receipt: # 18117-2 ----- Attempting Submission 3 (Thu Oct 09 16:03:08 GMT 2025) ----- I can't figure why it tells me the order of the FP-POS is incorrect. The order is never specified anywhere. One of the most startling discoveries made by JWST is a population of UV-bright z > 6 galaxies that are metal-poor and extremely nitrogen-rich with N/O ratios 15 times higher than expected for their metallicity. While this unusual enrichment pattern appears to be a rare phenomenon at high-z, it is notable that the C/N/O abundance patterns match those of second generation stars in globular clusters, suggesting that this may be a common, albeit short-lived, phase associated with the formation of massive star clusters in dense environments. Only 1 local analog of the N-rich high-z galaxies is known, suggesting that the conditions that give rise to these abundance patterns are extremely rare in the local universe. Here we propose to study a second galaxy, MRK 203, which has a high density central region with an N/O ratio 5 times the solar value (comparable to the high-z galaxies) and a normal N/O ratio outside the nucleus. The galaxy has much higher metallicity and lower ionization than the N-rich high-z galaxies, but it enables us to probe the phenomenon of N-enrichment over a much wider range of galactic conditions. We propose U,B,I-band WFC3 imaging to characterize galactic conditions giving rise to the N-rich nuclear cluster(s) and H-alpha narrow band imaging to provide key constraints on the photoionization rate. We additionally propose COS FUV spectroscopy of the nuclear regions of MRK 203 to precisely constrain the cluster age and determine if the N-enrichment is due to rapid cooling of stellar wind ejecta from Wolf-Rayet stars or very massive stars (M > 150 M_sun). We seek to obain WFC3 imaging and COS FUV spectroscopy of Mrk 203, a nearby (D~100 Mpc) interacting sprial galaxy. The chief goal is to understand the stellar populations of the bright nuclear star cluster(s) to determine the cause of the unusual N/O ratio in the nucleus. WFC3 imaging: Our goal is to measure the stellar masses and approximate stellar ages of the massive star clusters in Mrk 203's nuclear region using 3 broadbands and H-alpha narrow-band photometry. We also wish to measure the ionizing photon output of the clusters via their H-alpha luminosities. At the galaxy's distance, we do not expect to resolve the sizes of the star clusters, but we will determine whether there is a single dominant central star cluster or a complex of smaller clusters. We will image the galaxy in 4 filters (F336W, F438W, F814W, F673N). Exposures are spread over 3 orbits which make up 2 Visits. Because we seek to use the F336W image as pre-imaging to define precise coordinates for COS, we have created a 1-oribt visit containing the F336W and F438W exposures to improve scheduling. The other filters make up a 2-obit Visit. We have left a minute of unscheduled time in each orbit to improve scheduling. We use the "UVIS2-FIX" position to place the galaxy's nucleus near the center of chip 2. While this is less optimal for CTE, it will enable the galaxy's merging companion to be included on the chips with only mild roll angle restrictions that would limit visibility. Using the "Roll Ranges Report" we find that the galaxy is only schedulable at ORIENTS = 200 - 335 when there are no restrictions. We restrict the ORIENT to 205-270, 300-335 to keep the companion galaxy out of the chip gap. Because of the short exposures in each filter, we have elected to use a two-point dither pattern which will cover the chip gap (WFC3-UVIS-GAP-LINE). We tried to create 3 exposures for all filters, but ran into problems with exposures being shorter than the 350 sec buffer dump. Some filters are split into 2 sub-exposures and some into 3 so we have added a third point to the default WFC3-UVIS-GAP-LINE pattern for the filters with 3 dithers. We have adjusted the flash to reach the recommended minimum of 20 e- in each sub-exposure using the WFC3 ETC. Given that our target is at the center of a fairly extended bright galaxy, we are not as concerned about CTE issues; therefore we did not add extra FLASH to account for spatial variations. COS spectroscopy: Our goal is to obtain a UV spectrum of the of the most massive nuclear star cluster to look for spectral signatures of Very Massive Stars (M > 150 M_sun). Acquisition: We request that our COS Visits take place at least 30 days after our WFC3 imaging (we have submitted a TTRB request). The nuclear region of the galaxy is not well resolved in available ground based imaging and therefore we wish to use our F336W images to update the coordinates of our COS visits to focus on the brightest cluster. Because COS peak-up may not work in the crowded center of the galaxy, we have opted to target a nearby bright star for acquisition and then do an offset to Mrk 203. The star is g=16 and NUV=20.89 mag and is 105 arcseconds away. Using the ETC and the GALEX NUV mag, we estimate that we can achieve S/N = 20 in 10 seconds. We opt for a 30 second ACQ/IMAGE exposure to be on the safe side, yielding S/N=34. After the first acquisition and move to MRK 203, we take a 60 second NUV IMAGE to confirm the target centering and provide additional NUV photometry for our SED fitting. We have assumed that the 3"-diameter nuclear region has a flux of 18.5 mag AB in the GALEX FUV filter. Assuming 1/3 of that flux is in the central star cluster gives m=19.7 mag. For a NUV image the ETC reaches S/N = 20 in 17.5 seconds. We adopt an exposure time of 60 seconds (COS.ta.2027085) in case the central star cluster is fainter. We will use the G140L grating centered at 1105 to obtain R~3000 spectra from 1120- 2000 A. This will enable us to measure several key diagnostics of massive stars: NV 1240, Si IV 1440, C IV 1550, He II 1640. Following standard recommendations to reduce fixed pattern noise, we chose FP-POS=ALL. We have used the magnitude estimated for the 3" diameter nuclear region (m_FUV = 18.5) to estimate our Buffer time of 7580 seconds. We assume a point source for our calculations, but recognize that some of the flux may be more diffusely distributed. A total exposure time of 16,320 seconds meets our requirement of S/N=15 per resolution element at 1550 A. (ETC =COS.sp.2027092). We require 8 orbits for our COS exposures which we split into 3 Visits for ease of scheduling. Dr. Christy Tremonti is an expert on starburst galaxies, chemcial enrichment, and stellar feedback. She has authored a widely cited paper on the stellar mass-metallicity relation. She spent the early part of her career working on UV stellar populations in local galaxies using HST/FOS, GHRS, STIS, and COS spectra and the STARBURST99 models. She will lead the UV data analysis and supervise the the UV stellar population modeling portion of the project. Dr. Ralf Kotulla has a background in observational astronomy and data processing, with particular expertise in stellar population modeling and SED fitting. He's the lead author of the GALEV stellar population synthesis models. He will lead the processing and analysis of all imaging data used in this project. Dr. Adam Schaefer was a postdoc at the Max Plack Institute for Astronomy before recently moving to industry. Adam wrote several seminal papers metallicity gradients in the SDSSIV/MaNGA galaxies, and identified the galaxy Mrk 203 as an interesting outlier. Adam will assist with analyzing the MaNGA data and with the interpretaion of the findings from this proposal. Dr. Marsha Wolf is a research scientist at the University of Wisconsin-Madison. She has expertise in stellar population modeling and radio astronomy. She will contribute to the analysis and interpretation of the data. Mr. Owen Matthews Acuna is a graduate student working under the supervision of Prof. Tremonti. Owen is an expert on modeling optical stellar populations using stellar population synthesis models. He will lead the effort to model the UV stellar populations under the guidance of PI Tremonti. Galaxies 6 false true false false false false SUPPORTED GALAXY SPIRAL STARBURST YES The galaxy is fairly nearby (D~111 Mpc) spiral galaxy with a diameter of about 30". Our coordinates are from GAIA. For our WFC3 imaging, coordinate uncertainties are not a concern. We will be targeting the bright nuclear star cluster for our COS observations. We will update the coordiates of our COS pointings based on our WFC3 imaging. UGC07340 J2000 J2000 M_FUV = 16.75 STAR G V-IV NO Star to be used for COS Offset targeting J121803+441051 J2000 SDSS u=17.35, g=16.0, GALEX NUV = 20.89 COS/FUV Spectroscopic No No G140L 1105 WFC3/UVIS Imaging No No F336W WFC3/UVIS Imaging No No F475W WFC3/UVIS Imaging No No F673N WFC3/UVIS Imaging No No F814W POS-TARG MOSAIC DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 3 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 5 false POS-TARG MOSAIC DITHER 4 2.414 WFC3-UVIS-DITHER-BOX false 81.785 true 0.112 0.173 2 85.759 POS-TARG WFC3-UVIS-GAP-LINE 23.884 6 false 1760025464646 Timing link suitability includes constraints ([03 After 01 by 30.0 to 365.0 days] [04 After 01 by 30.0 to 365.0 days] [05 After 01 by 30.0 to 365.0 days]) The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. /private/var/folders/1s/jbw8fdfn7g32s505cypm2_4h0000gn/T/OPVisit8310783360010851148.xml (Tic-Visit :proposal-id 18117 :visit-id "01" :proposal-version -1 :trans-version "20250624" :date "09-Oct-2025 10:57:44.0" :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 1443744 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18117 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18117 :visit-id "01" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2561 :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 3001 :pcs-gap 0 ) true 1 0 1760025762174 The scheduling data was generated by CASM 33.1. 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CASM was run in Phase II mode. (Tic-Visit :proposal-id 18117 :visit-id "03" :proposal-version -1 :trans-version "20250624" :date "01-Sep-2025 20:37:03.0" :trans-errors '(:WARNINGS 2 :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 139712 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 18117 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18117 :visit-id "03" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2565 :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 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18117 :visit-id "03" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2559 :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 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18117 :visit-id "03" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2559 :al-overhead-at-end 0 :internal-dur-at-end 348 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 3 0 We require the WFC3 imaging in Visit 1 to happen first in order to center the COS aperture on our target. The target is the brightest UV cluster in a crowded region at the center of the galaxy. We will use our WFC3 F336W imaging to select the cluster for COS spectroscopy and update the target coordinates. Image to help us understand which clusters in the crowded nuclear region are observed in the COS aperture. We have assumed that the 3"-diameter nuclear region has a flux of 18.5 mag AB in the GALEX FUV filter. Assuming 1/3 of that flux is in the central star cluster gives m=19.7 mag. For a NUV image the ETC reaches S/N = 20 in 17.5 seconds. We adopt an exposure time of 60 seconds. 1756776908872 Timing link suitability includes constraints ([04 After 01 by 30.0 to 365.0 days]) The scheduling data was generated by CASM 33.1. 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The target is the brightest UV cluster in a crowded region at the center of the galaxy. We will use our WFC3 F336W imaging to select the cluster for COS spectroscopy and update the target coordinates. 1756776965453 Timing link suitability includes constraints ([05 After 01 by 30.0 to 365.0 days]) The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. /Users/tremonti/Desktop/HST_Cy33_PhaseII/OP-cache/HST_Cy33_Phase2_Version2-v05.xml (Tic-Visit :proposal-id 18117 :visit-id "05" :proposal-version -1 :trans-version "20250624" :date "01-Sep-2025 20:36:05.0" :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 18117 :visit-id "05" :obset-id "05" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 18117 :visit-id "05" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2561 :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 3001 :pcs-gap 0 ) (Tic-Orbit :proposal-id 18117 :visit-id "05" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2559 :al-overhead-at-end 0 :internal-dur-at-end 348 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3001 :pcs-gap 0 ) true 2 0 We require the WFC3 imaging in Visit 1 to happen first in order to center the COS aperture on our target. The target is the brightest UV cluster in a crowded region at the center of the galaxy. We will use our WFC3 F336W imaging to select the cluster for COS spectroscopy and update the target coordinates. We will use the coordintates from our WFC3 F336W image to update the COS pointing coordinates to center on the brightest nuclear star cluster.