TY - JOUR
T1 - REVERBERATION MAPPING of the BROAD LINE REGION
T2 - APPLICATION to A HYDRODYNAMICAL LINE-DRIVEN DISK WIND SOLUTION
AU - Waters, Tim
AU - Kashi, Amit
AU - Proga, Daniel
AU - Eracleous, Michael
AU - Barth, Aaron J.
AU - Greene, Jenny
N1 - Publisher Copyright:
© 2016. The American Astronomical Society. All rights reserved.
PY - 2016/8/10
Y1 - 2016/8/10
N2 - The latest analysis efforts in reverberation mapping are beginning to allow reconstruction of echo images (or velocity-delay maps) that encode information about the structure and kinematics of the broad line region (BLR) in active galactic nuclei (AGNs). Such maps can constrain sophisticated physical models for the BLR. The physical picture of the BLR is often theorized to be a photoionized wind launched from the AGN accretion disk. Previously we showed that the line-driven disk wind solution found in an earlier simulation by Proga and Kallman is virialized over a large distance from the disk. This finding implies that, according to this model, black hole masses can be reliably estimated through reverberation mapping techniques. However, predictions of echo images expected from line-driven disk winds are not available. Here, after presenting the necessary radiative transfer methodology, wecarry out the first calculations of such predictions. We find that the echo images are quite similar to other virialized BLR models such as randomly orbiting clouds and thin Keplerian disks. We conduct a parameter survey exploring how echo images, line profiles, and transfer functions depend on both the inclination angle and the line opacity. We find that the line profiles are almost always single peaked, while transfer functions tend to have tails extending to large time delays. The outflow, despite being primarily equatorially directed, causes an appreciable blueshifted excess on both the echo image and line profile when seen from lower inclinations (i ≲ 45°). This effect may be observable in low ionization lines such as Hβ.
AB - The latest analysis efforts in reverberation mapping are beginning to allow reconstruction of echo images (or velocity-delay maps) that encode information about the structure and kinematics of the broad line region (BLR) in active galactic nuclei (AGNs). Such maps can constrain sophisticated physical models for the BLR. The physical picture of the BLR is often theorized to be a photoionized wind launched from the AGN accretion disk. Previously we showed that the line-driven disk wind solution found in an earlier simulation by Proga and Kallman is virialized over a large distance from the disk. This finding implies that, according to this model, black hole masses can be reliably estimated through reverberation mapping techniques. However, predictions of echo images expected from line-driven disk winds are not available. Here, after presenting the necessary radiative transfer methodology, wecarry out the first calculations of such predictions. We find that the echo images are quite similar to other virialized BLR models such as randomly orbiting clouds and thin Keplerian disks. We conduct a parameter survey exploring how echo images, line profiles, and transfer functions depend on both the inclination angle and the line opacity. We find that the line profiles are almost always single peaked, while transfer functions tend to have tails extending to large time delays. The outflow, despite being primarily equatorially directed, causes an appreciable blueshifted excess on both the echo image and line profile when seen from lower inclinations (i ≲ 45°). This effect may be observable in low ionization lines such as Hβ.
KW - galaxies: active
KW - galaxies: nuclei
KW - hydrodynamics
KW - line: profiles
KW - quasars: emission lines
UR - http://www.scopus.com/inward/record.url?scp=84982128305&partnerID=8YFLogxK
U2 - 10.3847/0004-637X/827/1/53
DO - 10.3847/0004-637X/827/1/53
M3 - ???researchoutput.researchoutputtypes.contributiontojournal.article???
AN - SCOPUS:84982128305
SN - 0004-637X
VL - 827
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 53
ER -