Table 5.
Half-light radii and column densities derived from SED-fitting and X-ray analyses.
| XID | 
|
|
|
NH, ISM | NH, Xa |
|---|---|---|---|---|---|
| (1) | (2) | (3) | (4) | (5) | (6) |
| 42 | 0.28 ± 0.01 | 0.15 ± 0.07 | 1.2 ± 0.4 | 6.0 ± 5.9 |  |
| 170 | 0.16 ± 0.01 | – | 0.7 ± 0.3 | 3.2 ± 2.7 |  |
| 337 | 0.11 ± 0.01 | – | 0.4 ± 0.2 | 8.2 ± 6.9 |  |
| 539 | <0.2 | 0.13 ± 0.04 | 0.9 ± 0.3 | 9.8 ± 8.3 |  |
| 551 | 0.14 ± 0.01 | – | 0.5 ± 0.2 | 5.2 ± 4.4 |  |
| 666 | 0.38 ± 0.01 | 0.08 ± 0.02 | 0.6 ± 0.3 | 10.0 ± 7.8 |  |
| 746 | 0.14 ± 0.01 | – | 0.5 ± 0.2 | 4.2 ± 3.5 |  |
Notes. (1) X-ray source ID; (2) stellar half-light radius in arcsec as derived from HST/WFC3 H-band observations (see Chen et al. 2015a for XID42 and XID539, and van der Wel et al. 2012 for the remaining sources); (3) dust continuum half-light radius in arcsec from ALMA data (see text); and (4) ISM half-light radius in kpc. We assumed 
when ALMA data were available and 
(with ∼30% errors, similar to those on 
) otherwise (see text for details); (5) column density associated with the ISM of the host galaxy in units of 1023 cm−2; and (6) column density derived from the X-ray spectral analysis in units of 1023 cm−2.
Because the geometry adopted for the host ISM is similar to that assumed by the transmission-dominated model used to analyze X-ray spectra, we consider as fiducial results for NH, X those derived using the transmission model (see Table 3).
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