0 Assigned ID: 96 ----- Attempting Submission 1 (Tue Apr 05 11:02:49 GMT 2016) ----- 0 ----- Attempting Submission 1 (Mon Jul 11 10:27:07 GMT 2016) ----- A Definitive UV-Optical Template for Iron Emission in Active Galactic Nuclei The spectra of broad-line AGNs typically show strong blends of Fe II emission that form a pseudo-continuum covering much of the UV/optical range. However, the complex Fe II emission is difficult to model theoretically, and current models still struggle to match the details and diversity of observed Fe II emission in quasars. Accurate measurements of the emission lines and continuum in quasar spectra require the use of empirically derived iron templates based on observations of narrow-line Seyfert 1 galaxies. Fitting Fe II emission and separating it from the Balmer lines and Mg II is required for deriving accurate virial black hole masses in quasars, for investigating broad-line region structure and dynamics via reverberation mapping, and for probing quasar metal enrichment over cosmic time. The existing templates, however, suffer from low S/N and non-contemporaneous data with limited wavelength coverage, which consequently limits the accuracy of almost all spectroscopic measurements of continuum and emission lines in AGNs. Thus, it is critically important to derive a new empirical iron template having high S/N and complete UV/optical coverage simultaneously observed with a consistent aperture. To achieve this goal, we propose to obtain new STIS spectra covering 1150-10270 A for a new and better identified Fe II template galaxy, Mrk 493, which will yield the first consistent and complete UV/optical iron template. Our new Fe II template will provide the best practical tool to enable accurate modeling and fitting of the iron emission blends in AGN spectra, thus improving the understanding of black hole masses, broad-line region physics, and the cosmic evolution of AGNs. The goal of our proposed observations is to obtain high-S/N, quasi-simultaneous UV and optical spectra with a consistent slit width and aperture size for the new template galaxy Mrk 493, in order to construct new iron emission template of broader wavelength coverage and higher quality than was previously possible with any HST or ground-based dataset. We will use the G140L (1150-1730 A), G230L (1570-3180 A), G430L (2900-5700 A), and G750L (5240-10270 A) gratings to cover the full available wavelength range, and use the 52x0.2 slit, whose narrow width will minimize the host-galaxy and narrow-line region contributions to the data. The spectral resolution for G140L is R ~ 2400, which is higher than the previous HST FOS resolution (i.e., R ~ 1300), and the resolution for G230L/G430L/G750L is R ~ 1500. For the CCD G430L observations, we will use the E1 aperture position to minimize the CTE losses. For optimal fringe subtraction, the E2 aperture location for the CCD G750L grating will be used, along with CCDFLAT exposures observed immediately afterward. We will place the G750L science exposures at the end of an orbit so that the CCDFLAT exposures can be taken during the occultation period to optimize the efficiency. The D1 aperture position for the FUV-MAMA G140L grating will be used for low FUV dark current. Our goal is to achieve a minimum S/N per pixel of 40 at the rest wavelength of 1350 A in the G140L setting, 70 at the rest wavelength of 2650 A in G230L, and 100 at the rest wavelengths of 5100 A and 6200 A in G430L and G750L, in order to be able to construct iron templates of significantly higher quality and S/N than have ever been previously possible. Using the STIS exposure time calculator, a total of ~8.0 hours on-source are required (10609 sec with G140L, 12578 sec with G230L, 3498 sec with G430L, and 2566 sec with G750L). Multiple dithered exposures (between 5 and 7) will be taken in each of the optical CCD and UV MAMA grating settings for cleaning of cosmic-ray hits and bad pixels and reduction of small-scale detector nonuniformity. To ensure SAA-free orbits, a MAMA visit should be restricted up to five orbits as recommended in the STIS Instrument Handbook. Thus we split observations into three visits. We set the SAME ORIENT requirement so that every visit will be done with same orientation to minimize the possible biases from the variable host galaxy and narrow-line contribution. Since our observations require three separate visits for the target, we request the separate visits to be done as close in time as possible to minimize possible systematic biases due to AGN variability. Massive Black Holes and their Hosts 12 false true false false false false SUPPORTED GALAXY BLR NLR NUCLEUS SEYFERT This object was generated by the targetselector and retrieved from the SIMBAD database. J2000 J2000 FUV (GALEX) AB = 16.270, NUV (GALEX) AB = 15.745, F330W (HST/ACS) = 14.43, r (SDSS PSF) AB = 15.52 STIS/CCD Spectroscopic No No G750L 7751 STIS/CCD Spectroscopic No No G430L 4300 STIS/NUV-MAMA Spectroscopic No No G230L 2376 STIS/FUV-MAMA Spectroscopic No No G140L 1425 POS-TARG DITHER 0.15 LINE false false 7 90.0 STIS-ALONG-SLIT 1 false POS-TARG DITHER 0.15 LINE false false 5 90.0 STIS-ALONG-SLIT 2 false Timing link suitability includes constraints ([Sequence (01 02 03) within 1.0 days]) Hst Same orient constraint links visits (01 02 03) The scheduling data was generated by CASM 24.2. CASM was run in Phase II mode. 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