0 Assigned ID: 4749 ----- Attempting Submission 1 (Wed May 24 22:36:10 GMT 2023) ----- Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| Unsupported characters were found in Comments and replaced with |*| This target is not used in this proposal. Unsupported characters were found in Comments and replaced with |*| 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. This re-submission is to shave 100 sec from each orbit of visit 3 to make the observations schedulable in March 2024. Thanks. Ale -49926008 ----- Attempting Submission 1 (Sat Sep 16 01:47:47 GMT 2023) ----- HST Phase II Proposal 17465 successfully submitted. Receipt: # 17465-1 ----- Attempting Submission 2 (Sat Sep 16 03:58:44 GMT 2023) ----- ----- Attempting Submission 3 (Fri Oct 13 22:06:21 GMT 2023) ----- ----- Attempting Submission 4 (Wed Oct 18 20:08:58 GMT 2023) ----- ----- Attempting Submission 5 (Thu Oct 19 16:14:37 GMT 2023) ----- HST Phase II Proposal 17465 successfully submitted. Receipt: # 17465-5 ----- Attempting Submission 6 (Thu Oct 19 18:49:22 GMT 2023) ----- ----- Attempting Submission 7 (Sat Jan 06 18:41:17 GMT 2024) ----- The 23 warnings have to do with the following: 1. targets that have not been used but that are the targets with the original coordinates for comparisons with the targets defined by offsets from target 5; 2. all the COS observations are for extended targets. The escape fraction f_esc of LyC photons from star-forming galaxies (SFGs) is a topic of great interest. Leaking dwarf SFGs have been indicated as candidates for the re-ionization of the Universe at z ~ 7-10. Only a fraction of candidate LyC leakers at z > 0.5 -5 have shown enough leakage for such re-ionization (> 10-20%). Direct detections are difficult due to absorption of the LyC emission at < 912 A from the Milky Way (z ~ 0) or the IGM (z > 0). To move this field forward, indirect methods need to be spatially resolved down to the scales of individual SF regions to establish if the low detection rate is due to spatial variations and geometry within galaxies or global versus local properties. The first of a kind spatially-resolved f_esc map from HST broadband photometry indicates variations between 0-40% within NGC 4214 (~ 3 Mpc). Here we propose to use 1 archival and 6 new COS G130M pointings in NGC 4214 to probe the paths for LyC escape through analysis of the residual intensity in the core of saturated UV absorption lines (e.g., C II). We will complement these data with guaranteed simultaneous STIS G430L and G750L long-slit spectra, gaining access to another indirect indicator, O32, and emission lines critical to constrain the local physical conditions of the clumpy ISM and the ionizing photon production. Archival optical IFU data will provide the gas kinematics in the very center of NGC 4214. This wealth of data will be key to characterize the local physical processes regulating the creation and leakage of LyC photons in galaxies, and deliver to the community spatially calibrated indirect methods to measure f_esc at all redshifts in the era of JWST and ELT. We propose to perform a spatially-resolved HST COS FUV and STIS long-slit optical study of seven star-forming knots labeled as #A (or #Archival), #1, #2, #3, #4, #5 and #6 and hosted in the nearby dwarf star-forming galaxy and LyC leaker NGC 4214. Our analysis will include archival COS data for complex #A (HST PID: 11579 and 15193). COS G130M/1291 covering the 1130-1430 angstroms spectral range with a resolution of ~ 15,000 (v~20 km/sec), will be used for this purpose. The COS data will be complemented by guaranteed simultaneous and homogeneous STIS 52"x 2" G430L and G750L optical spectra (spectral resolution ~ 750) covering key emission-line diagnostics necessary to reddening correct the spectra via the Halpha/Hbeta Balmer decrement, determine electron density via the [SII] 6716, 6732 doublet, infer electron temperature via the [OIII] 5007/[O III]| 4363 emission-line ratio and consequently the direct-method metallicity indicator 12+log(O/H) and, most importantly, an accurate O32 ratio along the sightlines sampled with COS. Moreover, the combination of metallicity and O32 provides a determination of the ionization parameter, a direct measurement of the radiation field hardness which may be contributing to the escape of LyC along that sightline. With the plethora of UV and optical spectral and spatial information available, we will characterize the physical conditions of the environment (massive stars, stellar winds, multi-phase ISM, outflows) that regulate leakage of photons on the small spatial scales of individual H II regions (~40 pc). The seven SF complexes targeted in NGC 4214 with this COS/STIS program were selected as the brightest UV knots in regions with the highest fesc (> 10%) according to the map published by Choi et al. (2020; C20), sampling both small and large spatial scales within the galaxy. We used the multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5" aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes for our targets. We run the COS spectroscopic ETC calculations assuming a Single Stellar Population with a ~5 Myr age, applying the appropriate local value of reddening and normalizing to the GALEX FUV magnitudes. COS exposure times were estimated to achieve S/N~8 at rest-frame 1335 angstroms. We do not expect violations of local/global bright object limits for COS as the ETC reported no warning. This is also supported by the previous COS observations of the star-forming complex #A, the brightest of our targets. As recommended, we will use different FP-POS settings to improve S/N and minimize the effects of flat-field artifacts. We use the same COS target acquisition strategy adopted in PID 11579 for pointing #A to acquire cluster #5 which is the most isolated and point-like source, then perform an offset without target acquisition to take spectra of each cluster. The STIS calculations were performed by adding the weakest emission line that we want detected in G430L and G750L, [O II] 3727 and [N II] 6548 respectively, to the input spectra. Average fluxes for these lines were obtained from the optical spectra of Kobulnicky & Skillman (1996) and were used with a FWHM~100 km/sec (typical of HII regions). STIS exposure times were estimated to achieve S/N~10 at the rest-frame 3727 angstroms for G430L and 6548 angstroms for G750L. The STIS CCD observations will be executed with CR-split to get rid of cosmic rays. We will make use of small slews < 2' to observe more than one cluster per instrument configuration/orbit/visit. PI Dr. Aloisi is an expert in the analysis of UV spectroscopic observations to obtain column densities and chemical abundances of both the ISM and the stellar components in extragalactic environments. Dr. Aloisi is also an expert in resolved stellar popualtions in nearby (dwarf) star-forming galaxies with HST. One of Dr. Aloisi's primary fields of technical expertise is UV spectroscopy with space-based telescopes. For years she led the COS+STIS Team at STScI, acquiring knowledge on the strengths and weaknesses of the HST spectrographs. She is also PI and co-I of several COS and STIS programs, inlcuidng large programs. Her experience in both the scientific and technical areas is critical for the success of this project. Dr. Valentina Abril Melgarejo specialize in spatially-resolved spectroscopy over the UV-to-optical wavelength range, with ample experience in analyzing optical IFU data to derive dynamical and chemical abundance properties of galaxies from the Local Universe to intermediate/high redshifts. Dr. Choi, is an expert in stellar populations and the ISM in nearby galaxies. Dr. Choi has developed a new method to map the escape fraction of ionizing photons using resolved stellar populations, and successfully applied the method to an excellent local analog of high redshift star-forming dwarf galaxies, NGC 4214. Prof. Heckman is an expert in supermassive black holes, starbursts, and the formation and evolution of galaxies. Dr. Heckman is well-known for his work on galactic winds and on the co-evolution of galaxies and supermassive black holes. Dr. Heckman's work is observational with an emphasis on spectroscopy in the ultraviolet and visible. Dr. Heckman first proposed the CII indirect diagnostic of leaking LyC radiation, making his contributions to this program essential. Dr. Hernandez is an expert in the analysis of UV/optical/NIR spectroscopic observations of extragalactic environments, including neutral gas, star clusters, and Lyman continuum. Dr. Hernandez has served as a Research and Instrument Analyst for the COS instrument team for three years and is now an instrument scientist for STIS. She is also PI and co-I of several COS programs. Her experience in both the scientific and technical areas is critical for the success of this project. Dr. Hirschauer is currently a member of the COS Team with ample experience in data reduction of UV and optical spectroscopic observations. Additionally, Dr. Hirschauer is an expert in star-forming region abundances as it pertains to dwarf galaxies, dust and the mechanisms that facilitate star formation. Dr. James has ample experience with HST/COS spectroscopy as she is currently the deputy branch manager of the COS instrument team. Dr. James has lead several HST/COS observing campaigns to study the environments of nearby star-forming galaxies and is co-PI of the large COS treasury program CLASSY (COS Legacy Archive Spectroscopic SurveY). Dr. James is also an expert in the derivation of chemical abundances of star-forming galaxies using both UV and optical (IFU) spectroscopy. Dr. Mingozzi is an expert in interstellar medium properties (including outflows, gas-phase abundances, etc.), with ample experience analyzing COS spectroscopic observations and IFU optical nebular spectra of star-forming galaxies. Dr. Ravindranath is an expert on extreme emission-line galaxies and has used HST COS and STIS spectroscopic observations of Green Pea galaxies and local compact SFGs with exceptional O32 ratios to understand the physical conditions that produce strong nebular lines. Dr. Ravindranath is a Co-I on CLASSY and LzLCS (Low Redshift Lyman Continuum Survey) programs that use HST COS observations. Prof. Scarlata is an expert on the measurements of the escape of ionizing radiation, its evolution with redshift, its link with the escape of Lya radiation, and the study and characterization of indirect indicators from low redshift galaxies to be used at z>4. Prof. Scarlata led a number of works on constraining the escape fraction from different types of galaxies, using both HST UV (WFC3) and Galex imaging, as well as ground based imaging and spectroscopy. Stellar Populations and the Interstellar Medium 6 false false true false false false true false false false false false SUPPORTED STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 15.8 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 15.8 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 17.5 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 17.5 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 16.8 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 16.8 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 17.5 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 17.5 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 17.7 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 17.7 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 18.4 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 GALEX FUV (AB) = 18.3 +/- 0.1 mag STELLAR CLUSTER STAR FORMING REGION YES This object was generated by the targetselector, retrieved from the NED database, and updated based on HST imaging. GALEX FUV magnitudes in AB system were obtained by using multi-band photometric data and modeling from C20 to integrate the light from all the stars within the COS 2.5|*| aperture and estimate reddening and integrated GALEX FUV (AB) magnitudes. Johnson V magnitudes were obtained from the GALEX FUV magnitudes using PySynphot and same modelling information inserted into the ETC runs. J2000 J2000 GALEX FUV (AB) = 18.3 +/- 0.1 mag COS/FUV Spectroscopic No No G130M 1291 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 COS/FUV Spectroscopic No No G130M 1291 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G750L 7751 1697731880145 The scheduling data was generated by CASM 31.1. 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