0 Assigned ID: 6916 ----- Attempting Submission 1 (Wed Aug 27 23:13:44 GMT 2025) ----- HST Phase I Proposal 6916 successfully submitted. Receipt: # 6916-1 Unsupported characters were found in Observing Description and replaced with |*| Changed TA filter from 50CCD to F28X50LP 2098757188 ----- Attempting Submission 1 (Tue Sep 09 22:20:17 GMT 2025) ----- HST Phase II Proposal 18192 successfully submitted. Receipt: # 18192-1 ----- Attempting Submission 2 (Wed Dec 03 00:32:27 GMT 2025) ----- Removed unsupported characters but warning flag persists ACIS imaging of the nearby Seyfert MCG-03-34-64 has revealed two spatially-resolved peaks of luminous Fe Ka line emission, coincident with radio peaks, comprising a candidate dual AGN. If confirmed, this merger pair - at a separation of just 100 pc - would be the closest dual nuclei detected in multi waveband analysis to date. Establishment of close nuclear pairs offers critical model constraints for galaxy/AGN co-evolution. However, a single nucleus plus shocked gas provides an alternative model for the data. We request 200 ks of ACIS-S time (4x the existing exposure), supported by 2 orbits of HST STIS, to confirm the statistical significance and origin of the Fe Ka peaks and confidently parameterize this important system. In order to map the spatially-resolved kinematics of the NLR emission-line gas, we request a STIS G430M spectrum of [O III] 5007|*| through the 0:200 - 5200 slit. With this, we will achieve a velocity resolution of |*| 60 km/, which is ideal for separating distinct kinematic components and measuring accurate velocity dispersions for each component. The slit will be oriented to cover the bright knots of [O III] present in the archival ACS narrow-band image, with a |*|20 deg tolerance. Based on the [OIII] image, the peak [OIII] fluxes are similar corresponding to a surface brightness of 2|*|10|*|13 erg s|*|1 cm|*|2 arcsec|*|2, while the wings have surface brightness 5|*|10|*|14 erg s|*|1 cm|*|2 arcsec|*|2 and the fainter regions have surface brightness 3|*|10|*|15 erg s|*|1 cm|*|2 arcsec|*|2. Using the STIS ETC, and the NGC 1068 spectrum (to represent a Seyfert 2) normalized to the [O III] line with an integration of 40 minutes and the 0:200 |*| 5200 slit, we will achieve a SNR = 75, 33, 3.5 for the 3 regions defined by the 3 [O III] knots. Therefore, we require one orbit for the G430M spectrum. In order to constrain the ionization mechanisms for the optical emission-line gas, we request a G430L spectrum with the same slit and orientation used for the G430M. We base our exposure request on the need to obtain useful S/N for [Ne V] 3426|*|, which, based on the archival ESO-VLT X-Shooter spectra, has a flux 10% that of the integrated [O III] emission, corresponding to a surface brightness of |*| 4 |*| 10|*|13 erg s|*|1 cm|*|2 arcsec|*|2. Using the ETC, we determine that in a 40 minute exposure we will obtain a SNR |*| 7.5 at the average surface brightness, and SNR |*| 3 at 1:5 |*| 10|*|13 erg s|*|1 cm|*|2 arcsec|*|2. The [O II] 3727|*| , [Ne III] 3869|*| , and [O III] 5007 |*| lines are all su|*|ciently bright to map the ionization structure of the NLR with the proposed data, at a slightly lower S/N than that detailed for [O III], above. We require one orbit for the G430L spectrum. For each spectrum, we will obtain three sub exposures at slightly di|*|erent positions along the slit to facilitate the removal of cosmic rays and hot pixels on the CCD images. We will obtain these exposures near the top of the chip (the E1 position) to minimize CTE loss. Our team have extensive experience in the analysis, interpretation and publication of X-ray spectral data (Turner,Reeves, Braito, Trindade Falcao) and UV and optical data (Kraemer, Schmitt, Trindade Falcao, Feullit) and radio data (Schmitt, Feullit). The PI has authored 200 publications in refereed journals. For the proposed project we will use publicly available models with ftools, CIAO and XSPEC software for the data analysis. All co-investigators will be involved in the interpretation and publication of the results. Supermassive Black Holes and Active Galaxies 6 false false false false false false true SECONDARY CHANDRA 27700028 200 true SUPPORTED GALAXY ACCRETION DISK SEYFERT YES This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 STIS/CCD Spectroscopic No No G430L 4300 STIS/CCD Spectroscopic No No G430M 5093 POS-TARG DITHER 0.567 LINE false false 3 90.0 STIS-ALONG-SLIT 1 false 1757455823763 /Users/turner/Documents/Proposals/Chandra/C27/MCG-03/MCG-03_Sep9APTPhaseII/OP-cache/tempAPTSep9v3apt-v01.xml The scheduling data was generated by CASM 33.1. CASM was run in Phase II mode. 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