COS Spectra of High-Redshift AGN: Probing Deep into the Rest-Frame Ionizing Continuum and Broad Emission Lines
The order-of-magnitude improvement in sensitivity of COS over previous spectrographs has increased the number of AGN available for far-UV spectroscopy covering the rest-frame EUV. In archival work, we have enlarged our composite spectrum from 22 to 150 AGN, but the maximum redshift is z_max = 1.47. We request COS/G140L observations of 11 bright AGN (z = 1.45 to 2.13) to extend the composite below 400 A and greatly improve the statistics. At these redshifts, the G140L (1105 A setting) covers 1120-2000 A, probing the rest-frame continuum and emission lines down to 360-450 A. We will observe the Lyman continuum (LyC) below the He I edge (504 A) as it approaches the He II Lya break (304 A). Obtaining 11 well-exposed QSO spectra will greatly increase our knowledge in the EUV beyond the few AGN currently observed in this band. These LyC photons are responsible for ionizing hydrogen, helium, and many metal ions, for ionizing QSO broad emission-line regions (BELR), and for heating the IGM. Characterizing the AGN spectrum in the far-UV and ionizing EUV is also a crucial ingredient for studies of accretion disk structure and QSO outflows. We will also measure (or limit) the He I continuum edge (504 A) expected in some models of accretion disks, and will identify and characterize the key QSO broad emission lines in the FUV and EUV (Ne II, Ne III, Ne V, Ne VI, Ne VIII, O II, O III, O IV, O V, O VI). Detecting multiple ions from the same element (Ne and O) will yield more accurate diagnostics of BELR temperatures and metallicities.
Our targets were chosen by searching numerous AGN catalogs (Sloan-DR9, Veron) and cross- correlating them with GALEX fluxes. We found over 2000 AGN with redshifts 1.3<z<2.2, from which we drew a short list of 15 bright targets with GALEX-calibrated far-UV fluxes between (1.7-4.2)x10-15 erg cm-2 s-1 A-1. Our final list chose the 11 brightest targets with redshifts z=1.45 to z=2.13 that provide EUV wavelength coverage illustrated in Figure 4. We selected the G140L grating, which provides good sensitivity in 2 orbits (5 ksec per target) sufficient to measure the QSO continuum with S/N=10-30 and identify the expected EUV emission lines. We used the HST exposure time calculator to show that these 2-orbit exposure times yield S/N=10-20 over most of the G140L range (1120-2000A). Dropping the two brightest targets to just one orbit reduced the S/N at several important wavelengths needed to fix the continuum (line-free bands) and probe the EUV at lambda<600A .
The main advantage of G140L is its broad continuum coverage from 1120-2000A, rather than making two exposures with G130M (1133-1468A) and G160M (1383-1796A) and matching fluxes. In the 1105 setting, G140L gives broader continuous coverage and high sensitivity from 1120-2000A, with no detector gap in side-A. This broad range allows us to fit the underlying continuum through the key line-free wavelength bands. The G130M and G160M spectra do not cover those wavelengths for many of our high-z AGN. We chose a single exposure with G140L rather than two much longer exposures with the native resolution of medium-resolution (G130M+G160M) gratings.
Although we could bin up the M-grating spectra to achieve S/N comparable to G140L, we found that this would require 50% extra observing time (3 orbits per target). Our preparatory studies of G140L archival data show that we can characterize the QSO continuum and broad emission lines with high-S/N, but lower spectral resolution, of G140L. We are also able to correct for Lyman-limit systems (LLS) and Lyalpha forest line-blanketing.
AGN/QUASARS
Default
false
true
false
false
false
SUPPORTED
GALAXY
BLR
QSO
QUASAR
This object was generated by the targetselector and retrieved from the NED database. Coordinates refined with GSC2 search (match to object S35Q003409).
6DFJ0250552-361636
1RXSJ025055.4-361640
J2000
J2000
F(1530) = 4.2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
This object was generated by the targetselector and retrieved from the SIMBAD database. One of four images of lensed quasar. Coordinates checked in GSC23. GSC2 HSTID=N6H3003164
HB89-1115+080A1
J2000
J2000
F(1530) = 2.9e-15 ergs/s/cm^2/Ang
GALAXY
QSO
QUASAR
This object was generated by the targetselector and retrieved from the SIMBAD database. Coords checked in GSC2; hstID=N10H009447
1RXSJ180437.4+542524
J2000
J2000
F(1530) = 2.8e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
This object was generated by the targetselector and retrieved from the SIMBAD database. Checked in GSC2; hstID=N6CI002224
UM425
HB89-1120+019
J2000
J2000
F(1530) = 2.7e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
This object was generated by the targetselector and retrieved from the NED database. Checked in NED. N4TA002824
GALEX2696857944295739378
J2000
J2000
F(1530) = 2.2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
This object was generated by the targetselector and retrieved from the SIMBAD database. Coordinates checked in GSC2 (hstID=N956002270)
1RXSJ094210.0+520739
J2000
J2000
F(1530) = 2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
Checked in GSC2, hstID=N5K9000415
HS1307+4617
H1307+462
J2000
J2000
F(1530) = 2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
Checked in GSC2: hstID=N95Y004607
J2000
J2000
F(1530) = 2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
GSC2 hstID=N9EL004710
J2000
J2000
F(1530) = 2e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
Coordinates checked in GSC2, hstID=N6NE005334
FBQSJ112950.1+265253
SDSSJ112950.17+265254.0
J2000
J2000
F(1530) = 1.8e-15 ergs/s/cm^2/Ang
GALAXY
BLR
QSO
QUASAR
Coordinates checked in GSC2. hstID=N648010106
BZQJ1623+3909
RXJ1623.1+3909
J2000
J2000
F(1530) = 1.8e-15 ergs/s/cm^2/Ang
COS/FUV
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No
G140L
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No
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COS/FUV
Spectroscopic
No
No
G140L
1105
COS/FUV
Spectroscopic
No
No
G140L
1105
COS/FUV
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No
No
G140L
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The scheduling data was generated by CASM 21.2.
CASM was run in Phase II mode.
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