0Assigned ID: 325
----- Attempting Submission 1 (Thu Apr 06 22:48:04 GMT 2017) -----
----- Attempting Submission 2 (Sat Apr 08 05:03:26 GMT 2017) -----For the best data quality, it is strongly recommended that the maximum number of allowed FP-POS positions is used when observing at a given COS CENWAVE setting. See full description for details.First submission! We are using the FP progression that way (1,2,3,3,4,4) intentionally to maximize blue-wavelength coverage in our data.
Resubmission 12/27/17; added ACQ/SEARCH exposures on Visits 2, 4 to help with ~0.4" target coordinates on advice of STScI
Resubmitting visits 2, 4 after better coordinates (GAIA!) 2/5/18
Resubmit after partial failure of V4. HOPR 90494 was approved for a replacement orbit.-1580144362----- Attempting Submission 1 (Fri Jun 30 17:49:39 GMT 2017) -----
----- Attempting Submission 2 (Wed Dec 27 19:42:19 GMT 2017) -----
----- Attempting Submission 3 (Mon Feb 05 22:00:41 GMT 2018) -----
----- Attempting Submission 4 (Wed May 02 16:58:18 GMT 2018) -----resubmission after HOPR 90494. Should be fine.Hot Photons: Measuring the Ionizing Continuum and EUV Emission Lines of QuasarsAfter two decades of uncertainty, it is now possible to characterize the ionizing spectra of QSOs,
using HST/COS observations of intermediate-redshift AGN. To construct a reliable composite AGN
spectrum in the rest-frame EUV requires correcting for IGM absorption, identifying prominent broad
emission lines, and fitting the underlying continuum. We propose to complete the observations of
the last seven AGN (at z = 1.67 - 2.18) from a sample of 20 bright intermediate-redshift QSOs. Using
the broad-band (1120-2150 A) COS/G140L grating, we will probe the rest-frame continuum and
emission lines down to 350-450 Angstroms at these redshifts. Completing this sample will increase the
number of AGN-EUV spectra from 3 to 10 at z > 1.67 and significantly improve the statistical
reliability of the AGN composite spectrum between 400-600 A. Lyman continuum photons from
AGN dominate the metagalactic background and photoionization of hydrogen, helium, and many
metal ions. They also provide key correction factors needed to determine the baryon content and
metallicities of intergalactic and circumgalactic gas. The harder photons also have important effects
on IGM heating and for the He II epoch of reionization. Constraints on EUV spectral turnovers
below 600 Angstroms are potential diagnostics of the thermal structure of AGN accretion disks.We request a total of 21 orbits (COS/G140L) on 7 new AGN targets that will probe the shortest wavelengths in the rest-frame EUV spectra (AGN at z = 1.67 - 2.18). Each GN will be observed for 3 orbits with the G140L grating, allowing us to extract an accurate EUV continuum distribution and correct for any H I absorbers (LLS or pLLS). Three-orbit exposures are needed to reach S/N of 10-30 across the sensitive portion of the G140L band (1120-1950 Ang). Our chosen 7 targets (Table 1) are last of the 20 AGN identified in preparation for our initial COS AGN-Composite Spectrum project (Shull et al. 2012a; Stevans et al. 2014) with the G130M/G160M gratings (Figure 1). To probe to shorter rest-frame wavelengths with the G140L grating, we searched numerous AGN catalogs (Sloan-DR9, Veron-Cetty- Veron 2010). We queried SDSS DR9+DR7 (N = 32,534 objects) for QSOs, cut by redshift (z = 1.4 - 2.2) and magnitude u < 21. The VCV catalog gave N = 1903 QSOs brighter than 18th mag at z > 1.4. We looked up each FUV-bright candidate in NED to verify redshifts, classifications, and other observations, and used the SDSS spectrum catalog to double-check their AGN classification. All bright SDSS objects also appear in VCV-2010. We cross- correlated these objects with GALEX, ranked them by FUV fluxes, and selected the top 20 sources with GALEX-calibrated far-UV fluxes between (1.3 - 4.2) x 1e15 erg/cm^2/s/A. In Cycle 21, we successfully observed 11 of these targets at z = 1.5 - 2.1. Figure 2 shows three examples with a range of EUV spectral indices.
In Cycle 25 we will observe seven more AGN, concentrating on bright AGN at the highest redshifts (z = 1.67 -| 2.18) that provide EUV wavelength coverage down to 350-400 A in the AGN rest-frame, sufficient to limit any EUV turnovers indicative of smaller inner edges of accretion disks produced by black hole spin. We used the HST exposure time calculator to show that these exposure times will yield S/N = 15-20 over most of the G140L range (1120-1950 A), particularly at important wavelengths needed to fix the continuum (line-free bands) and probe the EUV at lambda < 600 A. We chose a single exposure with G140L rather than two much longer exposures with the native resolu- tion of medium resolution (G130M+G160M) gratings. The advantage of G140L is its broad coverage from 1120-2150 A, rather than making two exposures with G130M (1133-1468 A) and G160M (1383-1796 A) and matching fluxes. In its 1105 A setting, G140L gives contin- uous coverage and high sensitivity with no detector gap in side-A. This allows us to fit the underlying continuum through key line-free wavelength bands (red squares along the bottom of Figure 1). The G130M and G160M spectra do not cover those wavelengths for many of our high-z AGN.
Tilton et al. (2016) described our moderate-resolution (G140L) observations of 11 AGN observed in Cycle 21. Those AGN produced a composite rest-frame EUV spectrum using spline fitting over narrow lines and identifying the strong absorbers (LLS and pLLS). We have therefore demonstrated an ability to characterize the QSO continuum, fit the broad emission lines, and restore the continuum from LLS and pLLS absorbers in high-S/N G140L data. Figure 2 illustrates this technique for 3 of the 11 AGN observed in Cycle-21.Massive Black Holes And Their Host GalaxiesCosmology6falsetruefalsefalsefalsefalseSUPPORTEDGALAXYQSOQUASARNOHE0025-4047J2000J2000F(1530A)=1.6e-15GALAXYQSOQUASARNOCoordinates (with very small uncertainty) courtesy of GAIA dr1. Source ID: 925602973122608768SDSSJ075054.64+425219.2J2000J2000F(1530A)=1.4e-15GALAXYQSOQUASARNOSMASSJ23401574-4726356J2000J2000F(1530A)=1.3e-15GALAXYQSOQUASARNOCoordinates (with very small uncertainty) courtesy of GAIA dr1. Source ID: 632123356664406912J2000J2000F(1530A)=1.4e-15GALAXYQSOQUASARNO2MASSJ02045766-1701200J2000J2000F(1530A)=1.9e-15GALAXYQSOQUASARNO2MASSJ15485478+1211200J2000J2000F(1530A)=1.9e-15GALAXYQSOQUASARNOQSO lensed by z=0.408 galaxy.2MASSJ00502782-1740092J2000J2000F(1530A)=1.9e-15COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105COS/FUVSpectroscopicNoNoG140L1105The scheduling data was generated by CASM 25.2.CASM was run in Phase II mode./private/var/folders/28/q7n1k9mx06q9bdhm39kq5pn80000gn/T/OPVisit6743222117704183597.xml151631433700088.65298079881649(Tic-Visit
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:pcs-visibility 3216
:pcs-gap 0
)true30F(1530A)=1.9e-15, MIRRORA=4.0 sec.S/N for 1ks exp=8.5
S/N for 7ks=22S/N for 1ks exp=8.5
S/N for 7ks=22S/N for 1ks exp=8.5
S/N for 7ks=22S/N for 1ks exp=8.5
S/N for 7ks=22S/N for 1ks exp=8.5
S/N for 7ks=22S/N for 1ks exp=8.5
S/N for 7ks=22