Abstract
We present up to two decades of spectroscopic monitoring of the double-peaked broad Hα emission lines of seven broad-line radio galaxies. These extremely broad, double-peaked lines are successfully modeled by emission from gas in the outer accretion disk, and their profiles vary on timescales of months to years. This variability is a valuable probe for understanding the structure and dynamics of the accretion disk. We characterize the long-term broad-line profile variability in detail and compare the evolution of the line profiles with predictions from a few simple physical models for dynamical processes in the accretion disk. We find no evidence for persistent, periodic variability that would be indicative of a precessing elliptical disk, or a circular disk with a long-lived, single-armed spiral or warp. We do find transient, periodic variability on the orbital timescale, possibly resulting from shocks induced by tidal perturbations, and variability in the wings of the profile, which suggests changes in the emissivity of the inner accretion flow. Dramatic but localized profile changes are observed during flares and high states of broad-line flux. In 3C 332, these changes can be explained by a slow, smooth, secular change in disk illumination. In Arp 102B and 3C 390.3, however, a simple disk model cannot explain the asymmetric profile changes, suggesting a need for more sophisticated models. We also observe sharp, transient features that appear in the blue peak of the objects, which require a well-organized velocity field.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 167-212 |
| Number of pages | 46 |
| Journal | Astrophysical Journal, Supplement Series |
| Volume | 169 |
| Issue number | 2 |
| DOIs | |
| State | Published - Apr 1 2007 |
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All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science
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Long-term profile variability of double-peaked emission lines in active galactic nuclei. / Gezari, S.; Halpern, J. P.; Eracleous, M.
In: Astrophysical Journal, Supplement Series, Vol. 169, No. 2, 01.04.2007, p. 167-212.Research output: Contribution to journal › Article
TY - JOUR
T1 - Long-term profile variability of double-peaked emission lines in active galactic nuclei
AU - Gezari, S.
AU - Halpern, J. P.
AU - Eracleous, M.
PY - 2007/4/1
Y1 - 2007/4/1
N2 - We present up to two decades of spectroscopic monitoring of the double-peaked broad Hα emission lines of seven broad-line radio galaxies. These extremely broad, double-peaked lines are successfully modeled by emission from gas in the outer accretion disk, and their profiles vary on timescales of months to years. This variability is a valuable probe for understanding the structure and dynamics of the accretion disk. We characterize the long-term broad-line profile variability in detail and compare the evolution of the line profiles with predictions from a few simple physical models for dynamical processes in the accretion disk. We find no evidence for persistent, periodic variability that would be indicative of a precessing elliptical disk, or a circular disk with a long-lived, single-armed spiral or warp. We do find transient, periodic variability on the orbital timescale, possibly resulting from shocks induced by tidal perturbations, and variability in the wings of the profile, which suggests changes in the emissivity of the inner accretion flow. Dramatic but localized profile changes are observed during flares and high states of broad-line flux. In 3C 332, these changes can be explained by a slow, smooth, secular change in disk illumination. In Arp 102B and 3C 390.3, however, a simple disk model cannot explain the asymmetric profile changes, suggesting a need for more sophisticated models. We also observe sharp, transient features that appear in the blue peak of the objects, which require a well-organized velocity field.
AB - We present up to two decades of spectroscopic monitoring of the double-peaked broad Hα emission lines of seven broad-line radio galaxies. These extremely broad, double-peaked lines are successfully modeled by emission from gas in the outer accretion disk, and their profiles vary on timescales of months to years. This variability is a valuable probe for understanding the structure and dynamics of the accretion disk. We characterize the long-term broad-line profile variability in detail and compare the evolution of the line profiles with predictions from a few simple physical models for dynamical processes in the accretion disk. We find no evidence for persistent, periodic variability that would be indicative of a precessing elliptical disk, or a circular disk with a long-lived, single-armed spiral or warp. We do find transient, periodic variability on the orbital timescale, possibly resulting from shocks induced by tidal perturbations, and variability in the wings of the profile, which suggests changes in the emissivity of the inner accretion flow. Dramatic but localized profile changes are observed during flares and high states of broad-line flux. In 3C 332, these changes can be explained by a slow, smooth, secular change in disk illumination. In Arp 102B and 3C 390.3, however, a simple disk model cannot explain the asymmetric profile changes, suggesting a need for more sophisticated models. We also observe sharp, transient features that appear in the blue peak of the objects, which require a well-organized velocity field.
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U2 - 10.1086/511032
DO - 10.1086/511032
M3 - Article
AN - SCOPUS:34248379678
VL - 169
SP - 167
EP - 212
JO - Astrophysical Journal, Supplement Series
JF - Astrophysical Journal, Supplement Series
SN - 0067-0049
IS - 2
ER -