0
Assigned ID: 7327
----- Attempting Submission 1 (Thu Apr 16 08:31:12 GMT 2026) -----
HST Phase I Proposal 7327 successfully submitted.
Receipt: # 7327-1
----- Attempting Submission 2 (Thu Apr 16 22:51:15 GMT 2026) -----
HST Phase I Proposal 7327 successfully submitted.
Receipt: # 7327-2
----- Attempting Submission 3 (Thu Apr 16 23:00:34 GMT 2026) -----
HST Phase I Proposal 7327 successfully submitted.
Receipt: # 7327-3
0
----- Attempting Submission 1 (Mon Aug 17 22:24:19 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-1
----- Attempting Submission 2 (Mon Aug 17 22:24:33 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-2
----- Attempting Submission 3 (Mon Aug 17 22:26:19 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-3
----- Attempting Submission 4 (Mon Aug 17 22:28:41 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-4
----- Attempting Submission 5 (Mon Aug 17 22:36:44 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-5
----- Attempting Submission 6 (Tue Aug 18 00:27:53 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-6
----- Attempting Submission 7 (Tue Aug 18 00:47:54 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-7
----- Attempting Submission 8 (Tue Aug 18 01:39:37 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-8
----- Attempting Submission 9 (Tue Aug 18 01:56:14 GMT 2026) -----
HST Phase II Proposal 18378 successfully submitted.
Receipt: # 18378-9
----- Attempting Submission 10 (Wed Aug 26 03:36:02 GMT 2026) -----
When Does Synchrotron Begin? A HST-COS Study of the Earliest Feedback Phase in Massive Stellar Clusters
We propose 54 orbits with the Hubble Space Telescope Cosmic Origins Spectrograph (HST/COS) to observe two nearby massive spiral galaxies hosting young massive stellar clusters with resolved 0.9 arcsec (60pc) VLA 3 GHz radio counterparts. Stellar SEDs indicate that some clusters in these two galaxies are very young (<3 Myr) and likely still in the pre-supernova phase, yet they already exhibit synchrotron emission, suggesting that cosmic-ray acceleration is already underway. This raises a fundamental question: what phase of massive-star evolution powers the earliest cosmic rays in young clusters? Cosmic rays are an important but poorly constrained form of stellar feedback, and radio synchrotron emission is one of the few direct probes of them. Stellar winds may be efficient particle accelerators, but it remains unclear whether the emission is powered by O/B-star winds, emerging Wolf-Rayet stars, or underestimated ages that already allow the first superovae. We aim to answer this question with COS far-ultraviolet spectroscopy, which provides direct constraints on the massive-star population through stellar-wind and age diagnostics, while also probing the surrounding gas through ISM absorption lines that measure kinematics, column density, and ionization state. By linking these UV diagnostics to resolved non-thermal radio emission, we will test which young stellar populations are most closely associated with the onset of synchrotron emission and place empirical constraints on the timing of early cosmic ray feedback.
We adopt COS/G140L with the 800A central-wavelength setting to avoid the detector gap near 1200A and provide continuous coverage of the principal far-UV diagnostics, including N V, Si IV, C IV, and He II. Each science target will be acquired directly using COS/NUV ACQ/IMAGE through the PSA. Our targets span NUV magnitudes of approximately 19-21 AB, with a median of 20.4 AB. Exposure times were estimated using Starburst99 spectra folded through the G140L response and normalized to the observed NUV fluxes. We adopt an exposure strategy comparable to the CLUES survey of Sirressi et al. (2022), which obtained COS FUV spectroscopy of young massive clusters out to about 13 Mpc, similar to the distance of NGC 4254, using exposures of order 8 ks for some targets.
For an 8000 s exposure and a representative 1 Myr Starburst99 spectrum normalized to the median NUV magnitude of our sample, 20.4 AB, the COS ETC predicts S/N of about 12 per resolution element at N V 1240A (ETC: COS.sp.2366495) and about 5.9 at C IV 1550A (ETC: COS.sp.2366497). Reducing the integration to about 7000 s lowers the expected S/N by only about 0.5 at both wavelengths. Because a full 8000 s integration cannot be efficiently accommodated within three HST orbits while retaining all four FP-POS positions, most targets will be observed for approximately 6.7-7.0 ks. The four G140L/800 exposures will sample FP-POS 1 through 4, with two shorter exposures sharing the second orbit.
We make two exceptions. NGC3627-3 is substantially brighter in the UV, with an NUV magnitude of 18.94 AB. An 8000 s ETC calculation produced a HARD warning and S/N = 24.9 at 1240A, so this target will be limited to 6000 s while retaining all four FP-POS positions. The three faintest NGC 4254 targets, NGC4254-6, NGC4254-8, and NGC4254-10, will instead be assigned four orbits each, allowing approximately 9 ks of FUV integration while preserving complete FP-POS coverage. For example, NGC4254-6 will receive 8985 s over four orbits. This allocation uses the full 54-orbit program, with 14 three-orbit visits and three four-orbit visits.
For bright-object safety, we performed a conservative COS ETC calculation for the brightest source in the sample, NGC3627-3, assuming an unreddened Kurucz O5V point-source spectrum normalized to its measured F275W flux of 96 microJy. For an 8000 s G140L/800 exposure, the ETC predicts a brightest-pixel count rate of 0.036 counts per second per pixel, corresponding to 289 counts in the brightest pixel, and a total detector count rate of 203 counts per second on Segment A (ETC: COS.sp.2367718). These rates are well below the COS/FUV bright-object screening limits. The ETC predicts S/N = 30.4 per resolution element at 1240 Angstrom. The only warning is that this S/N exceeds the nominal maximum achievable assuming two FP-POS positions; our observations use all four FP-POS positions, so this warning does not indicate a bright-object safety violation.
As an additional safety check, we repeated the calculation for the second-brightest source, with an F275W flux of 43uJy, using an 8000 s exposure. This calculation gives S/N = 20.3 at 1240A and produces no warnings (ETC: COS.sp.2367711). Since all remaining targets have lower F275W fluxes, these calculations demonstrate that the full sample satisfies the COS bright-object safety requirements under the same conservative unreddened O5V assumption.
Our team brings together expertise in ultraviolet spectroscopy, radio continuum emission, stellar feedback, and the multiwavelength study of nearby galaxies. PI Hamid Hassani leads the project and has extensive experience combining resolved UV, infrared, optical, and radio observations to study young stellar clusters, dust, and feedback in nearby galaxies. He has led major imaging efforts in the UV and has developed tools and datasets for the analysis of star-forming galaxies across multiple wavelengths.
Erik Rosolowsky brings broad expertise in the interstellar medium and star formation in nearby galaxies, with extensive experience using JWST and other major facilities to connect resolved gas and dust structure to feedback processes. Aida Wofford contributes deep expertise in massive stars, stellar populations, and ultraviolet spectroscopy of nearby star-forming systems, which is central to interpreting the COS observations. Simon C. O. Glover adds theoretical expertise on the physics of the ISM, star formation, and feedback, providing important context for connecting the observed UV diagnostics to the surrounding gas.
Janice Lee contributes extensive experience in nearby galaxy surveys, multiwavelength star formation diagnostics, and the interpretation of resolved stellar populations and nebular emission. Sumit Sarbadhicary brings expertise in the theory of supernova remnants, synchrotron emission, and cosmic-ray production, which is essential for linking the UV properties of young clusters to their radio emission. Daniel Maschmann contributes expertise in the identification and characterization of young stellar clusters and in the analysis of resolved extragalactic stellar populations. David Thilker adds strong experience in ultraviolet studies of nearby galaxies, stellar population modeling, and SED fitting.
Galaxies
Galaxies
6
false
false
false
false
false
false
false
SUPPORTED
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W=43.55uJy (19.8AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 22.34 (20.53 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 96.33uJy (18.94 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W = 36.0 uJy (20.01 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 22.82 uJy ( 20.5 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 25.63uJy (20.38 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 29.99uJy ( 20.21 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W = 14.21uJy (21.02 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 22.44uJy (20.52 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W = 12.64uJy (21.15 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 32.13uJy ( 20.13 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 13.39 uJy (21.08 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 23.48uJy (20.47 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 13.45uJy (21.08 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 12.64 uJY ( 21.15 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 39.16uJy ( 19.92 AB mag)
EXT-CLUSTER
SPIRAL ARM
NO
J2000
F275W= 42.48uJy (19.83 mag)
The scheduling data was generated by CASM 34.0.
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COS/FUV
Spectroscopic
No
No
G140L
800
The scheduling data was generated by CASM 34.0.
CASM was run in Phase I mode.
COS/FUV
Spectroscopic
No
No
G140L
800
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With an 8000 s exposure, this source produced a HARD warning in the ETC calculation, with an S/N of 24.9 at 1240A. Therefore, we aim to detect this source using a total exposure time of 6000 s.
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With an 8000 s exposure, this source produced a HARD warning in the ETC calculation, with an S/N of 24.9 at 1240A. Therefore, we aim to detect this source using a total exposure time of 6000 s.
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(Tic-Orbit
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(Tic-Orbit
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true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v09.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Orbit
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true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v10.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
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(Tic-Obset
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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(Tic-Orbit
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true
4
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v11.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
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:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:14.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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)
(Tic-Obset
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)
(Tic-Orbit
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(Tic-Orbit
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)
(Tic-Orbit
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)
true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v12.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
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:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:15.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 4
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)
(Tic-Obset
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
true
4
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v13.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
:visit-id "13"
:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:16.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 3
:saa-model "31"
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:data-volume 78480
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:visit-id "13"
:obset-id "13"
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)
(Tic-Orbit
:proposal-id 18378
:visit-id "13"
:orbit-number 1
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:al-overhead-at-end 0
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)
(Tic-Orbit
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)
(Tic-Orbit
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)
true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v14.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
:visit-id "14"
:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:17.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 4
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:obset-id "14"
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)
(Tic-Orbit
:proposal-id 18378
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:orbit-number 1
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:al-overhead-at-end 0
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:dark-offset NIL
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)
(Tic-Orbit
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(Tic-Orbit
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)
(Tic-Orbit
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)
true
4
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v15.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
:visit-id "15"
:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:18.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 3
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:si-bright-earth-limb-angle 20.0
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
:proposal-id 18378
:visit-id "15"
:orbit-number 1
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:al-overhead-at-end 0
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:dark-offset NIL
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)
(Tic-Orbit
:proposal-id 18378
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)
(Tic-Orbit
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)
true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v16.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
:visit-id "16"
:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:19.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 3
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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:obset-id "16"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 18378
:visit-id "16"
:orbit-number 1
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:al-overhead-at-end 0
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)
(Tic-Orbit
:proposal-id 18378
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(Tic-Orbit
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)
true
3
0
/Users/hamidhassani/Desktop/OP-cache/hamid_apiII_last_phaseII-v17.xml
The scheduling data was generated by CASM 34.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 18378
:visit-id "17"
:proposal-version -1
:trans-version "20260618"
:date "25-Aug-2026 21:27:20.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
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:number-of-orbits 3
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:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
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)
(Tic-Orbit
:proposal-id 18378
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)
(Tic-Orbit
:proposal-id 18378
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:al-overhead-at-end 0
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(Tic-Orbit
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)
true
3
0