Table 3.
Line-flux measurements.
Quasar field | Host galaxy identifiers |
Emission-line measurements |
|||||
---|---|---|---|---|---|---|---|
θa (") | bb (kpc) | ![]() |
Transition | λ0 (Å) | FWHM (Å) | Line-flux (×10−17 erg s−1 cm−2) | |
HE 1122–1649 | 3.6c | 25.6 | 0.68249 ± 0.00003 | [O II] | 3727,3729 | 6.3 ± 0.7 | 17.7 ± 2.4 |
Hβ | 4861.39 | 6.0 ± 0.5 | 4.8 ± 0.6 | ||||
Q 0153+0009 | 4.9d | 36.6 | 0.77085 ± 0.00003 | H5 | 4340.47 | 9.5 ± 1.0 | 3.0 ± 0.4 |
Hβ | 4861.33 | 9.5 ± 0.6 | 6.3 ± 0.6 | ||||
[O III] | 5007 | 9.8 ± 0.5 | 7.5 ± 0.5 | ||||
Q 1209+107 | 7.2d | 38.3 | 0.39238 ± 0.00001 | [O II] | 3727,3729 | 6.7 ± 0.4 | 41.9 ± 1.5 |
H5 | 4340.47 | 5.0 ± 0.5 | 7.0 ± 0.7 | ||||
Hβ | 4861.33 | 5.5 ± 0.1 | 14.8 ± 0.4 | ||||
[O III] | 4958.91 | 5.6 ± 0.1 | 23.3 ± 0.8 | ||||
[O III] | 5007 | 5.8 ± 0.2 | 72.1 ± 3.0 | ||||
Q 1323–0021 | 1.4d | 10.2 | 0.71717 ± 0.00008 | [O II] | 3727,3729 | 9.6 ± 1.7 | 3.1 ± 0.4 |
Q 1436–0051 | 6.2e | 45.5 | 0.73749 ± 0.00003 | [O II] | 3727,3729 | 10.2 ± 0.7g | 11.1 ± 0.8g |
Hβ | 4861.33 | 7.9 ± 1.4 | 1.5 ± 0.3 | ||||
[O III] | 5007 | 17.8 ± 2.7 | 1.3 ± 0.3 | ||||
Q 1436–0051 | 4.4d | 34.9 | 0.92886 ± 0.00002 | [O III] | 5007 | 5.6 ± 0.4 | 7.0 ± 0.7 |
Q 2328+0022 | 1.7d | 11.9 | 0.65194 ± 0.00006 | [O II] | 3727,3729 | 5.5 ± 0.7 | 7.0 ± 0.7 |
Q 2335+1501 | 3.8f | 27.0 | 0.67989 ± 0.00002 | [O II] | 3727,3729 | 6.7 ± 0.4 | 36.3 ± 1.4 |
Hβ | 4861.33 | 6.5 ± 0.2 | 15.6 ± 6.2 |
Notes. Values for refer to the heliocentric rest-frame corrected measurement, with the quoted error reflecting the uncertainty in the profile-fit. θ is the angular separation between quasar and host, measured in arcsec. θ is translated into an impact parameter (b) measured in kpc using the the spectroscopically determined emission-line redshift and the assumed cosmology. The fluxes were integrated across the profile, and corrected for Galactic extinction assuming the Galactic EB−V values reported in Table 1. Full-width-half-maximum (FWHM) measurements have not been corrected for the instrumental resolution.
This work, based on Rao et al. (2011) K-band image (see Sect. 2.4).
This work, based on the Straka et al. (2016) spectrum (see Sects. 3.3, 3.6, and 3.8).
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