Kavli Affiliate: Erin Kara
| First 5 Authors: , , , ,
| Summary:
We present our study of the XRISM observation of the Seyfert-1 galaxy NGC
3783. XRISM’s Resolve microcalorimeter has enabled, for the first time, a
detailed characterization of the highly ionized outflows in this active
galactic nucleus. Our analysis constrains their outflow and turbulent
velocities, along with their ionization parameter ($xi$) and column density
($N_rm H$). The high-resolution Resolve spectrum reveals a distinct series
of Fe absorption lines between 6.4 and 7.8 keV, ranging from Fe XVIII to Fe
XXVI. At lower energies, absorption features from Si, S, and Ar are also
detected. Our spectroscopy and photoionization modeling of the time-averaged
Resolve spectrum uncovers six outflow components, five of which exhibit
relatively narrow absorption lines with outflow velocities ranging from 560 to
1170 km/s. In addition, a broad absorption feature is detected, which is
consistent with Fe XXVI outflowing at 14,300 km/s (0.05 $c$). The kinetic
luminosity of this component is 0.8-3% of the bolometric luminosity. Our
analysis of the Resolve spectrum shows that more highly ionized absorption
lines are intrinsically broader than those of lower-ionization species,
indicating that the turbulent velocity of the six outflow components (ranging
from 0 to 3500 km/s) increases with $xi$. Furthermore, we find that the
$N_rm H$ of the outflows generally declines with $xi$ up to $log xi =
3.2$ but rises beyond this point, suggesting a complex ionization structure.
The absorption profile of the Fe XXV resonance line is intriguingly similar to
UV absorption lines (Ly$alpha$ and C IV) observed by the HST, from which we
infer that the outflows are clumpy in nature. Our XRISM/Resolve results support
a "hybrid wind" scenario in which the observed outflows have multiple origins
and driving mechanisms. We explore various interpretations of our findings
within AGN wind models.
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