Benchmarking early-type Wolf-Rayet stars as sources of He II ionizing flux in stellar populations

Resubmission adding Matheus as Co-I 335374803 Assigned ID: 4045 ----- Attempting Submission 1 (Mon May 22 19:59:17 GMT 2023) ----- HST Phase I Proposal 4045 successfully submitted. Receipt: # 4045-1 ----- Attempting Submission 2 (Wed May 24 20:17:00 GMT 2023) ----- Resubmission of Visits 01, 06 and 10 with adjustments as discussed with the contact scientist Christian Johnson. -1264822143 ----- Attempting Submission 1 (Mon Sep 11 18:40:30 GMT 2023) ----- HST Phase II Proposal 17426 successfully submitted. Receipt: # 17426-1 ----- Attempting Submission 2 (Mon Jan 29 09:19:25 GMT 2024) ----- Benchmarking early-type Wolf-Rayet stars as sources of He II ionizing flux in stellar populations Classical, hydrogen-depleted Wolf-Rayet (WR) stars mark an evolved stage of massive stars with major impacts to their environment. The high temperatures of WR stars, the progenitors of massive black holes, turn them into major sources of ionizing flux. In the last two decades, the discovery of strong high-ionization emission lines in both high-redshift galaxies and extremely low-metal local galaxies has raised more questions than answers about the origin of the He II ionizing radiation and its implications for the cosmic reionization and galaxy evolution. The current generation of stellar population synthesis models fails to reproduce the necessary hard ionizing fluxes. Yet, their treatment of hydrogen-depleted stars is still insufficient with regards to both theoretical insights as well as observational template material. Here, we propose a crucial observational solution by studying whether certain types of WR stars may be the missing ingredient required for stellar population synthesis models to reproduce the nebular emission line characteristics of high-redshift galaxies, enabling the inference of the properties of the first galaxies in the Universe. Most WR stars are consuming the necessary high-energy photons to drive their strong winds, but model calculations show that a subset of early-type WR stars with weaker winds can produce large amounts of He II ionizing photons. The proposed COS observations will allow us to probe the stellar and wind properties of this subset of the WR population, distinguish sources of strong He II ionizing flux, constrain pre-supernova feedback, and provide the necessary templates for a new generation of population synthesis models. We propose to observe WR stars in six different galaxies with FUV spectroscopy, aiming at a S/N of 10 or better at 1310 Angstroem. For low-reddened LMC and SMC targets, we can reach a S/N of > 50 in one orbit using the G140L grating in its 800 mode with pass band 913 - 1950. This setting covers the far UV range in one arm without any gaps. The low resolution is sufficient to resolve the wind-broadened lines of WR stars. The spectral range contains important diagnostic lines, such as the resonance lines of C IV, N V, and O VI which act as crucial indicators in order to determine accurate wind parameters and properly constrain the actual stellar temperature beneath the expanding layers of the WR wind. The presence or absence of specific lines provide major diagnostics for dense winds and follow-up spectral modelling, which will determine which stars are transparent or opaque to highly-ionizing flux below 228 Angstroem (corresponding to energies above 54 eV). A minimum S/N of ~10 is required for the total observation time of each target to resolve weaker metal line. The higher S/N targets will allow us an excellent mapping of the Fe line forest and enable us to also use the COS data in the low-sensitivity region below 1100 Angstroem, where in particular the high-ionization O VI 1038 doublet is located. For most targets, precise Gaia DR3 coordinates are available. For the remaining targets, we make use of Pan-STARRS DR1 data, which has been cross-checked with other available literature data. The resulting small-error coordinates enable a fast NUV image target acquisition. The LMC and SMC WR targets usually require the use of the bright object aperture for this procedure, while the primary science aperture can be used all further-away WR stars. For the Galactic WR target, a dispersed light acquisition is required to mitigate brightness issues. All ETC calculations are performed with dedicated atmosphere models for each target based on available optical spectra and photometry to predict the UV fluxes while taking into account the source-specific redenning. The proposing team consists of experts from both the theoretical and the observational side with several members having long-time HST experience. A. Sander, J. Chisholm, R. Hainich, L. Oskinova, T. Shenar, and W-R. Hamann have extensive experience with HST UV data with various accepted proposals in the last decade and excellent publication records. W-R. Hamann, L. Oskinova, R. Hainich, A. Sander, V. Ramaschandran, D. Pauli, H. Todt, R. Lefever, E. Schoesser, and T. Shenar have detailed experience with non-LTE atmosphere modelling, especially in the context of analysing Wolf-Rayet (WR) stars. M. Bernini-Peron is further an expert in using the non-LTE atmosphere code CMFGEN. J. Chisholm is a known expert for the impact of massive stars on the gas within galaxies and outside of galaxies with a particular focus on the very early Universe. A. Sander, H. Todt, and W.-R. Hamann are lead developers of PoWR, one of the most advanced non-LTE expanding stellar atmosphere code, especially designed to properly cope with the complex winds of hot WR stars. Moreover, A. Sander and J.S. Vink are experts in the theoretical modelling and hydrodynamically consistent simulation of radiation-driven winds of hot stars. E.R. Higgins is an expert in stellar evolution modelling, in particular for evolved massive stars. K. Kreckel and J. E. Mendez-Delgado are experts in ISM physics, the physical conditions of ionized nebulae, and stellar feedback processes. O. Egorov has extensive experience in observational studies of the interplay between massive stars (including WR stars) and the ISM in nearby galaxies. Stellar Populations and the Interstellar Medium Stellar Physics and Stellar Types 6 false false true false false false false false SUPPORTED STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated with Gaia DR3 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated via Gaia DR3 BREY-4 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. SIMBAD Coordinates (05 26 36.8640, -68 50 59.64) replaced by closest Gaia DR3 source after original Foellmi coordinates are not confirmed by recent surverys while Gaia XP spectrum hints at WN spectral type and no other WN that close to the Foellmi coordinates is known (but would have been discovered in previous WR searches). J2000 J2000 Gaia G 14.745229 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated via Gaia DR3 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated by Gaia DR3 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated with Gaia DR3 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates from Pan-STARRS DR1 (Chambers+, 2016), agree almost perfectly with recent UVIT data (Leahy+, 2020) and still well with optical works from Massey+2016 and Maravelias+2022 LGGS-J004655.89+420015.1 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates from Pan-STARRS DR1 (Chambers+, 2016), agree almost perfectly with newer Massey photometry coordinates NM2011-J013232.07+303522.4 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates from Pan-STARRS DR1 (Chambers+, 2016), agree decently with Gaia DR3, 0.7arcsec offset to old Massey NM2011-J013232.13+303514.3 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates from Pan-STARRS DR1 (Chambers+, 2016), agree well with newer Massey+2016 photometry coordinates. NM2011-J013257.32+304418.1 J2000 J2000 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated by Gaia DR3 NM2011-J013315.55+304514.1 J2000 J2000 EXT-STAR WOLF RAYET NO This object was generated by the targetselector and retrieved from the SIMBAD database. Updated coordinates using Gaia DR3. AM85-IC-1613-6 J2000 J2000 G=19.99 EXT-STAR WOLF RAYET - WN NO This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates updated by Gaia DR3. 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(Tic-Visit :proposal-id 17426 :visit-id "12" :proposal-version -1 :trans-version "20240604" :date "20-Jun-2024 14:20:23.0" :trans-errors '(:WARNINGS 0 :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 104576 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 17426 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 17426 :visit-id "12" :orbit-number 1 :pcs-time 380 :si-vis-utilization 2625 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17426 :visit-id "12" :orbit-number 2 :pcs-time 380 :si-vis-utilization 2625 :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 3005 :pcs-gap 0 ) (Tic-Orbit :proposal-id 17426 :visit-id "12" :orbit-number 3 :pcs-time 380 :si-vis-utilization 2624 :al-overhead-at-end 0 :internal-dur-at-end 360 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3005 :pcs-gap 0 ) true 3 0