0Assigned ID: 2835
----- Attempting Submission 1 (Tue Mar 22 18:11:29 GMT 2022) -----Initial submission of 17071_phase2
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----- Attempting Submission 2 (Mon Nov 28 23:15:20 GMT 2022) -----The Ionizing EUV Continua of Quasars: Minding the GapDespite several decades of UV observations, the rest-frame ionizing spectrum of QSOs remains uncertain, primarily because of insufficient wavelength coverage to identify strong absorbers and measure spectral curvature between the EUV/FUV and NUV/Optical. The primary goal of this proposal is to define the continuum of QSOs, for ionizing (Lyman continuum) wavelengths through the NUV and optical. This requires "filling the NUV gap" for intermediate-redshift AGN (z = 1.5-2.2) with existing COS/G140L (FUV) and optical (SDSS) spectra. To fit the continuum over a broad wavelength interval, with access to windows of line-free continuum, we need spectra (2000-3500A) that connect FUV and optical wavelengths. This region contains important absorption-line diagnostics, including higher Lyman lines associated with LLS and pLLS absorbers. We request 26 orbits to obtain COS/G230L near-UV spectra of 12 AGN at redshifts z = 1.51-2.12 with existing far-UV (COS/G140L) and optical spectra (SDSS/6dF). This will extend the AGN composite spectrum down to 360-420A and investigate possible spectral hardening at wavelengths below 600A. We will also derive limits on EUV turn-overs and the He I continuum edge (504A) predicted in some models of accretion disks. Our spectra will also measure higher Lyman lines associated with strong (LLS/pLLS) absorbers and prominent QSO broad emission lines in the EUV that contaminate the underlying continuum.We propose to observe 12 AGN, concentrating on UV-bright AGN at intermediate redshifts (z=1.51-2.13) that provide improvement in EUV wavelength coverage down to 360-400 Angstroms in the AGN rest-frame. Observing in the NUV gap will connect the EUV/FUV to the optical spectra available with SDSS (or 6dF), enabling us to construct a wide-band composite spectrum from 400 Angstroms into the optical band, accounting for spectral curvature and breaks. This will be useful for photoionization models of the IGM/CGM and sufficient to set physical limits on EUV turnovers, suggestive in some models of smaller inner edges of accretion disks produced by black hole spin.
We request a total of 26 orbits (COS/G230L) on 12 AGN targets (Table 1) at redshifts ranging from z = 1.51 to 2.13. These AGN all have existing COS/G140L (far-UV) spectra that probe wavelengths in the QSO rest-frame EUV down to 360-420 Ang. Eleven of the 12 have optical spectra (SDSS or 6dF). The G140L spectra become noisy at observed wavelengths lambda > 1900 Ang, which makes it difficult to anchor the continuum at longer wavelengths. This issue is especially a problem for two of our targets with LLS at 1895 Ang and 2080 Ang. The lack of NUV spectral observations is a general problem in measuring UV/EUV continua, sometimes exacerbated by the presence of LLS or pLLS near the end of G140L band or falling in the NUV gap. The absence of an NUV spectrum means that we cannot predict the continuum shape, if there are strong H I absorbers longward of 2000 Ang. The proposed observations will remove these uncertainties.
Ten of these AGN will be observed for 2 orbits each with G230L: one orbit in each of two settings (CenWaves 3000 and 3360). These observations will cover the NUV from 1700-3500 Ang, except for a gap between 2457-2801 Ang. This gap should not significantly affect the continuum fitting. This technique will allow us to extract an accurate EUV/FUV/NUV continuum, correct for strong absorbers (LLS or pLLS), and measure absorption in the higher Lyman series. Two targets, HS 0747+4259 (Fig. 2a) and SBS 1010+535 (Fig. 2b), have strong HI absorbers with Lyman continuum edges that confuse continuum fits at the long-wavelength end of the G140L band. These two QSOs will be observed in 3 settings (Cen- Waves 3000, 3360, 2635) for complete coverage of the NUV and an FUV continuum anchor between 1600-1730 Ang. In order to obtain a spectroscopic quality necessary for absorption-line measurements in the NUV, with S/N = 10-15 across the sensitive portion of the NUV, all exposures require one-orbit per G230L setting. The two bright targets with 3 settings (see Table 1 and Figure 2) will reach somewhat higher S/N.
Based on existing G140L observations, all our targets are UV-bright, with 2000 Ang fluxes listed in Table 1. We used the HST exposure time calculator to confirm that (one-orbit) exposure times (52-56-minute visibility per orbit) will yield S/N = 10-15 over most of the G230L range, particularly at wavelengths needed to fix the continuum. The existing FUV spectra have broad coverage from 1120 Ang up to 2000 Ang, where the detector noise becomes large. In the 1105 Ang setting, the existing G140L data have continuous coverage and high sensitivity with no detector gap in side-A. With the new NUV spectra, we will be able to characterize the spectral curvature, identify QSO emission lines and LLS/pLLS, and model the underlying continuum through key line-free wavelength bands. Combining the G140L data with the NUV spectra and existing optical (SDSS or 6dF) spectra, we will produce a composite rest-frame spectrum, using spline fitting over absorption lines and identifying any strong absorbers (LLS and pLLS).
Selection of Targets. Our goal was to make a significant improvement in the COS com- posite spectrum at lambda < 600 Ang, where fewer than 10 AGN contributed (Stevans et al. 2014). Only 2 targets probed to 500 Ang. We also wanted AGN with previous COS/G140L data, in order to connect FUV and NUV spectra. We looked for AGN with optical spectra, mostly from SDSS. We examined the 11 AGN observed by Tilton et al. (2016) and 5 others from the G140L archives (z = 1.5-2.2). We dropped 4 from 11 with z < 1.5 from the first group. The UVBQ survey (Monroe et al. 2016) found 217 AGN with with FUV mag < 18.5, but only three were at z = 1.5-1.9, and they lacked G140L data. Our final sample was 12 AGN, eight at redshifts z > 1.7. The requested 26 orbits form a reasonably sized request for a sizable increase (from 3 to 11) in AGN that probe below 500 Ang.
Summary: The order-of-magnitude improvement in sensitivity of COS over previous UV spectrographs has increased the number of AGN covering the rest-frame EUV. We request 26 orbits to obtain COS/G230L near-UV spectra of 12 AGN at z = 1.51-2.13. This will extend the AGN composite spectrum down to 360-420 Ang and statistically confirm (or refute) the spectral hardening at lambda < 600 Ang seen by Tilton et al. (2016). We will also derive better limits on the He I continuum edge (504 Ang) expected in some models of accretion disks. Our spectra will also measure higher Lyman lines associated with LLS and pLLS absorbers and prominent QSO broad emission lines in the EUV that contaminate the underlying continuum.Michael Shull (PI) - Professor of Astrophysics, University of Colorado,
Adjunct Professor of Physics & Astronomy, University of North Carolina.
PhD 1976 (Physics, Princeton). Research interests in theoretical astrophysics and UV/X-ray space astronomy. Shull has worked on ultraviolet spectroscopic data from four space missions (Copernicus, IUE, FUSE, and Hubble) on topics including ISM, IGM, quasars, SNRs, and Galactic high-velocity clouds. He was a member of the COS-GTO team that designed and built the Cosmic Origins Spectrograph and a member of the FUSE science team. Recent studies include surveys of interstellar H2, distances to OB-stars (Gaia) in the Milky Way, COS surveys of missing baryons, O VI and other metals, He II reionization epoch, Galactic halo gas, high-redshift galaxies, and quasars (composite ionizing continuum and emission lines). Theoretical interests include galactic halo gas, ISM/IGM, interstellar radiative shocks, supernovae, ionizing photons from massive stars, reionization epochs of H and He, and the baryon census of the universe.
Charles Danforth (CoI) - Senior Research Associate, University of Colorado.
PhD 2003 (Physics & Astrophysics, Johns Hopkins University). Also working in remote sensing at Maxar Technologies, Colorado. Research expertise in spectroscopic observations and data analysis of interstellar matter, supernova remnants, intergalactic medium, metal transport into the circumgalactic and intergalactic medium around galaxies. Lead author on major surveys of the low-redshift IGM (Lya, O VI) and expert on HST/COS spectroscopic data calibration and co-addition methods. Danforth and Shull have worked together for 19 years on UV spectroscopic studies of interstellar and intergalactic matter, with 44 refereed papers published (ApJ, Nature) since 2005. Their HST and FUSE projects include surveys of the low-redshift Lya forest, Lyman-limit systems, O VI tracers of warm-hot IGM, galaxy/quasar interactions, IGM baryon census, QSO spectra, and interstellar high-velocity clouds.
Rongmon Bodoloi (CoI) - Asst. Professor, North Carolina State University.
PhD 2013 (ETH Zurich). Postdoc at STScI and MIT (Hubble Fellow). Observational astrophysicist studying galaxy formation and evolution, and the cycling of baryons into and out of galaxies. He uses multi-wavelength spectroscopy and imaging (ground and space) to study the galaxy baryon cycle that regulates star formation in galaxies and the evolution of a galaxy. He has extensively used HST/COS observations to study the CGM of nearby galaxies and the Milky Way. He has also introduced new numerical deep-learning methods to characterize the quasar continua using HST/COS spectra. His research over the years have led to tens of publications using HST/COS spectra, which led to several NASA press releases.Supermassive Black Holes and Active GalaxiesIntergalactic Medium and the Circumgalactic Medium6falsefalsetruefalsefalsefalsefalseSUPPORTEDGALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=3.0E-15 (z=1.509)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.4E-15 (z=1.600)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.5E-15 (z=1.614)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000F(2000)=1.0E-15 (z=1.648)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.2E-15 (z=1.733)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the SIMBAD database.J2000J2000F(2000)=1.5E-15 (z=1.737)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.2E-15 (z=1.743)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=0.8E-15 (z=1.739)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=3.1E-15 (z=1.899)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.0E-15 (z=1.96)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=0.8E-15 (z=1.978)GALAXYACCRETION DISKQSOQUASARNOThis object was generated by the targetselector and retrieved from the NED database.J2000J2000F(2000)=1.2E-15 (z=2.133)COS/NUVSpectroscopicNoNoG230L2635COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L2635COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360COS/NUVSpectroscopicNoNoG230L3000COS/NUVSpectroscopicNoNoG230L3360The scheduling data was generated by CASM 30.3.CASM was run in Phase II mode.(Tic-Visit
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(Tic-Orbit
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