TY - JOUR
T1 - JWST Q3D Program
T2 - Active Galactic Nucleus Photoionization and Shock Ionization in a Red Quasar at z = 0.4
AU - Sankar, Swetha
AU - Zakamska, Nadia L.
AU - Rupke, David S.N.
AU - Liu, Weizhe
AU - Wylezalek, Dominika
AU - Veilleux, Sylvain
AU - Bertemes, Caroline
AU - Diachenko, Nadiia
AU - Chen, Yu Ching
AU - Ishikawa, Yuzo
AU - Vayner, Andrey
AU - Nesvadba, Nicole P.H.
AU - Liu, Guilin
AU - Goulding, Andy D.
AU - Lutz, Dieter
N1 - Publisher Copyright:
© 2025. The Author(s). Published by the American Astronomical Society.
PY - 2025/10/1
Y1 - 2025/10/1
N2 - Red quasars, often associated with potent [O iii] outflows on both galactic and circumgalactic scales, may play a pivotal role in galactic evolution and black hole feedback. In this work, we explore the [Fe ii] emission in one such quasar at z = 0.4352-F2M J110648.32+480712.3 using the integral field unit mode of the Near Infrared Spectrograph aboard the JWST. Our observations reveal clumpy [Fe ii] gas located to the south of the quasar. By comparing the kinematics of [Fe ii] and [O iii], we find that the clumpy [Fe ii] gas in the southeast and southwest aligns with the outflow, exhibiting similar median velocities up to v50 = 1200 km s−1 and high velocity widths W80 > 1000 km s−1. In contrast, the [Fe ii] gas to the south shows kinematics inconsistent with the outflow, with W80 ∼ 500 km s−1, significantly smaller than the [O iii] at the same location, suggesting that the [Fe ii] may be confined within the host galaxy. Utilizing standard emission-line diagnostic ratios, we map the ionization sources of the gas. According to the MAPPINGS III shock models for [Fe ii]/Paβ, the regions to the southwest and southeast of the quasar are primarily photoionized. Conversely, the [Fe ii] emission to the south is likely excited by shocks generated by the back-pressure of the outflow on the galaxy disk, a direct signature of the impact of the quasar on its host.
AB - Red quasars, often associated with potent [O iii] outflows on both galactic and circumgalactic scales, may play a pivotal role in galactic evolution and black hole feedback. In this work, we explore the [Fe ii] emission in one such quasar at z = 0.4352-F2M J110648.32+480712.3 using the integral field unit mode of the Near Infrared Spectrograph aboard the JWST. Our observations reveal clumpy [Fe ii] gas located to the south of the quasar. By comparing the kinematics of [Fe ii] and [O iii], we find that the clumpy [Fe ii] gas in the southeast and southwest aligns with the outflow, exhibiting similar median velocities up to v50 = 1200 km s−1 and high velocity widths W80 > 1000 km s−1. In contrast, the [Fe ii] gas to the south shows kinematics inconsistent with the outflow, with W80 ∼ 500 km s−1, significantly smaller than the [O iii] at the same location, suggesting that the [Fe ii] may be confined within the host galaxy. Utilizing standard emission-line diagnostic ratios, we map the ionization sources of the gas. According to the MAPPINGS III shock models for [Fe ii]/Paβ, the regions to the southwest and southeast of the quasar are primarily photoionized. Conversely, the [Fe ii] emission to the south is likely excited by shocks generated by the back-pressure of the outflow on the galaxy disk, a direct signature of the impact of the quasar on its host.
UR - https://www.scopus.com/pages/publications/105017511083
UR - https://www.scopus.com/inward/citedby.url?scp=105017511083&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/adf967
DO - 10.3847/1538-4357/adf967
M3 - Article
AN - SCOPUS:105017511083
SN - 0004-637X
VL - 991
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 227
ER -