TY - JOUR
T1 - Extreme-velocity quasar outflows and the role of X-ray shielding
AU - Hamann, F.
AU - Chartas, G.
AU - McGraw, S.
AU - Rodriguez Hidalgo, P.
AU - Shields, J.
AU - Capellupo, D.
AU - Charlton, J.
AU - Eracleous, M.
PY - 2013/10
Y1 - 2013/10
N2 - Quasar accretion disc winds observed via broad absorption lines (BALs) in the UV produce strong continuous absorption in X-rays. The X-ray absorber is believed to serve critically as a radiative shield to keep the outflow ionizations low enough for radiative driving. However, previous studies have shown that 'mini-BAL' and narrow absorption line (NAL) outflows have dramatically less X-ray absorption than BALs. Here, we examine X-ray and rest-frame UV spectra of eight mini-BAL quasars with outflow speeds in the range 0.1-0.2c to test the hypothesis that these extreme speeds require a strong shield.We find that theX-ray absorption is weak or moderate, with neutral-equivalent column densities NH 22 cm-2, consistent with mini-BALs at lower speeds. We use photoionization models to show that the amount of shielding consistent with our data is too weak to control the outflow ionizations and, therefore, it is not important for the acceleration. Shielding in complex geometries also seems unlikely because the alleged shield would need to extinguish the ionizing far-UV flux while avoiding detection in X-rays and the near-UV.We argue that the outflow ionizations are kept moderate, instead, by high gas densities in small clouds. If the mini-BALs form at radial distances of the order of R ~ 2 pc from the central quasar (broadly consistent with theoretical models and with the mini-BAL variabilities observed here and in previous work), and the total column densities in the mini-BAL gas are NH {less-than or approximate} 1021 cm-2, then the total radial extent of outflow clouds is only δRclouds {less-than or approximate} 3 × 1013 cm in cases of no/weak shielding or δRclouds {less-than or approximate} 3 × 1014 cm behind the maximum shield allowed by our data. This implies radial filling factorsδRclouds/R {less-than or approximate} 5 × 10-6 or {less-than or approximate}5 × 10-5 for the unshielded or maximally shielded cases, respectively. Compared to the transverse sizes {greater-than or approximate}8 × 1015 cm (based on measured line depths), the outflows have shapes like thin 'pancakes' viewed face-on, or they occupy larger volumes like a spray of many dense clouds with a small volume filling factor. These results favour models with magnetic confinement in magnetic disc winds. To the extent that BALs, mini-BALs and NALs probe the same general outflow phenomenon, our result for dense substructures should apply to all three outflow types.
AB - Quasar accretion disc winds observed via broad absorption lines (BALs) in the UV produce strong continuous absorption in X-rays. The X-ray absorber is believed to serve critically as a radiative shield to keep the outflow ionizations low enough for radiative driving. However, previous studies have shown that 'mini-BAL' and narrow absorption line (NAL) outflows have dramatically less X-ray absorption than BALs. Here, we examine X-ray and rest-frame UV spectra of eight mini-BAL quasars with outflow speeds in the range 0.1-0.2c to test the hypothesis that these extreme speeds require a strong shield.We find that theX-ray absorption is weak or moderate, with neutral-equivalent column densities NH 22 cm-2, consistent with mini-BALs at lower speeds. We use photoionization models to show that the amount of shielding consistent with our data is too weak to control the outflow ionizations and, therefore, it is not important for the acceleration. Shielding in complex geometries also seems unlikely because the alleged shield would need to extinguish the ionizing far-UV flux while avoiding detection in X-rays and the near-UV.We argue that the outflow ionizations are kept moderate, instead, by high gas densities in small clouds. If the mini-BALs form at radial distances of the order of R ~ 2 pc from the central quasar (broadly consistent with theoretical models and with the mini-BAL variabilities observed here and in previous work), and the total column densities in the mini-BAL gas are NH {less-than or approximate} 1021 cm-2, then the total radial extent of outflow clouds is only δRclouds {less-than or approximate} 3 × 1013 cm in cases of no/weak shielding or δRclouds {less-than or approximate} 3 × 1014 cm behind the maximum shield allowed by our data. This implies radial filling factorsδRclouds/R {less-than or approximate} 5 × 10-6 or {less-than or approximate}5 × 10-5 for the unshielded or maximally shielded cases, respectively. Compared to the transverse sizes {greater-than or approximate}8 × 1015 cm (based on measured line depths), the outflows have shapes like thin 'pancakes' viewed face-on, or they occupy larger volumes like a spray of many dense clouds with a small volume filling factor. These results favour models with magnetic confinement in magnetic disc winds. To the extent that BALs, mini-BALs and NALs probe the same general outflow phenomenon, our result for dense substructures should apply to all three outflow types.
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U2 - 10.1093/mnras/stt1231
DO - 10.1093/mnras/stt1231
M3 - Article
AN - SCOPUS:84885153426
SN - 0035-8711
VL - 435
SP - 133
EP - 148
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 1
ER -