First Submission
April 16 - Second Submission (revised text)
April 16 - Third Submission (revised text)-36723257Assigned ID: 7232
----- Attempting Submission 1 (Wed Apr 15 22:59:19 GMT 2026) -----
HST Phase I Proposal 7232 successfully submitted.
Receipt: # 7232-1
----- Attempting Submission 2 (Thu Apr 16 19:09:34 GMT 2026) -----
HST Phase I Proposal 7232 successfully submitted.
Receipt: # 7232-2
----- Attempting Submission 3 (Thu Apr 16 23:53:00 GMT 2026) -----Could not connect to APT Status Server
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.First submission - Aug 12 20261406775645----- Attempting Submission 1 (Wed Aug 12 22:31:03 GMT 2026) -----I'm not sure about the first warning "Warning (Form): Could not connect to APT Status Server". I retrieved the Phase I from APT, converted in Phase II and then worked on it.
My target are not point sources (they are not stars), but they are very compact nearby galaxies; as such, I considered them extended, despite I except their UV emission to be compact enough to be mostly covered by the COS aperture.
Please, let me know if there are any issues.CLASSY AGaiN: A COS Atlas of Low-Metallicity AGN for Rest-Frame UV Diagnostics in the JWST EraIn the JWST era, the UV spectroscopic frontier has been pushed to higher redshifts than ever before to finally reveal the distant Universe. Thus, rest-frame UV spectra have now become crucial to interpret the properties of the first galaxies in the epoch of reionization (EoR, z>6). Recent studies have been revealing an increasing number of high-z active galactic nuclei (AGN) candidates, suggesting that we are still underestimating the black hole accretion rate of the early universe, which is directly connected to the production rate of ionizing photons. In order to shed light on the impact of AGN on the EoR, we have to take a step back: have we really understood how to identify AGN activity in metal-poor conditions? Indeed, UV spectral features of AGN and extreme metal-poor star-forming galaxies can look extremely similar and a powerful diagnostic toolkit is needed to disentangle them. This proposal aims to observe with COS G140L the UV spectra of 17 low-mass low-metallicity (LMLZ) AGN, selected in detail with optical diagnostics to span a range of galaxy properties. Thus, we will create for the first time a reliable dataset of UV+Optical spectra of EoR AGN analogs to recognize the AGN signatures in metal-poor environments and to understand how to use them to interpret the high-z universe.We will obtain COS/FUV spectroscopy of 15 (+2 archival datasets) nearby low-mass, low-metallicity AGN to establish the first empirical UV benchmark for accretion-powered ionization in metal-poor environments. The observations will provide coverage of the main UV emission lines from Ly-alpha to CIII], enabling us to characterize the UV signatures and ISM conditions of these systems and calibrate UV+optical diagnostics for distinguishing AGN from stellar and composite excitation.
Observations:
COS/FUV G140L/1105 TIME-TAG spectroscopy will be obtained for each target, covering the main UV emission lines from Ly-alpha through CIII]. Targets will be acquired with ACQ/IMAGE using MIRRORA and the PSA. Science exposures will be distributed among multiple FP-POS positions to mitigate fixed-pattern noise and are designed to achieve S/N~3-5 per resolution element on one of the expected faintest emission lines, OIII]1666.Our team includes experts in observational studies of AGN and starburst galaxies, both in the nearby universe and at high-z, as well as experts on UV and optical spectroscopy. Scientifically, the team is uniquely qualified to explore the properties and diagnostics diagrams of the interstellar medium and pursue the science goals of the proposed study.
Our team contains forefront leaders in UV spectroscopy (Abril Melgarejo, Berg, Hayes, Fischer, James, Mingozzi, Ravrindranath, Revalski, Scarlata, Hernandez), each having significant experience with HST/COS spectroscopy in particular. The team has led several UV-centric observing campaigns, with more than 15 papers published in the past 5 years on data carried out with COS observations. Dr Fischer is a current member of the HST/COS team, Dr Hernandez is the current HST/COS team lead, Dr James was the deputy lead of the HST/COS team in 2020-2023 and Dr Mingozzi is a current member of the HST/STIS team. As such they are intimately familiar with all aspects of the HST/UV spectroscopy in general, its data reduction, analysis and observations.
Drs Carniani, Cresci, Fischer, Heckman, Marconi, Revalski, Mr Ceci and Ms Zucchi are experts in the field of galaxy evolution, focusing on studies of active galactic nuclei (AGN) and the impact of AGN feedback, both in the nearby and high-z universe.
Drs Berg, Cresci, Hayes, Heckman, James, Marconi, Mingozzi, Ravrindranath, Revalski, Vaught, del Valle-Espinosa, Hernandez, and Mr Ceci and Ms Moreschini are experts in determining chemical abundances and physical conditions from UV-to-optical emission lines. Their expertise are complementary, gathering knowledge on both low-metallicity star-forming galaxies and galaxies hosting an AGN.
Drs Berg, Feltre, Marconi, Ravindranath, Revalski, Scarlata, Ms Moreschini and Mr Ceci are experts in photoionization modeling of the ISM. Dr Cannarozzo is expert in statistical analysis and zoom-in simulations. Overall, these models will be crucial in interpreting the data from this proposal.
The team is also anchored at both low-redshift and high-redshift such that we will calibrate the proposed UV emission-line diagnostics with an eye towards what is observable by JWST.Galaxies6falsetruefalsefalsefalsefalsefalseSUPPORTEDGALAXYDWARF COMPACTSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000NUV=20.5GALAXYDWARF COMPACTSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
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SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000NUV~19.2GALAXYDWARF COMPACTSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000NUV~20GALAXYDWARF COMPACTSEYFERTSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000NUV~19.5GALAXYDWARF COMPACTSEYFERTSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000GALAXYDWARF COMPACTSEYFERTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.
SIMBAD listed proper motion for this target. When retrieving targets with PM from SIMBAD, APT requests the coordinates be calculated with an epoch of the year 2000. Do not modify this epoch. Always review coordinates using the Target Confirmation tool, which graphically displays the PM.J2000J2000GALAXYDWARF COMPACTSEYFERTSTARBURSTYESThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000B~16, NUV~18.8COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105/Users/mmingozzi/Desktop/classy-agn-c34/OP-cache/almost-ready-v01.xmlThe scheduling data was generated by CASM 34.2.CASM was run in Phase II mode.(Tic-Visit
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