- Timothy A. Davis
- Davor Krajnović
- Richard M. McDermid
- Martin Bureau
- Marc Sarzi
- Kristina Nyland
- Katherine Alatalo
- Estelle Bayet
- Leo Blitz
- Maxime Bois
- Frédéric Bournaud
- Michele Cappellari
- Alison Crocker
- Roger L. Davies
- P. T. de Zeeuw
- Pierre-Alain Duc
- Eric Emsellem
- Harald Kuntschner
- Pierre-Yves Lablanche
- Raffaella Morganti
- Thorsten Naab
- Tom Oosterloo
- Nicholas Scott
- Paolo Serra
- Anne-Marie Weijmans
- Lisa M. Young
Original language | English |
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Pages (from-to) | 1574-1590 |
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Journal | Monthly Notices of the Royal Astronomical Society |
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Volume | 426 |
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Issue number | 2 |
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DOIs | |
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Publication status | Published - 1 Oct 2012 |
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We use the Spectrographic Areal Unit for Research on Optical Nebulae and
Gemini Multi-Object Spectrograph integral-field spectrographs to observe
the active galactic nucleus (AGN) powered outflow in NGC 1266. This
unusualgalaxy is relatively nearby (D = 30 Mpc), allowing us to
investigate the process of AGN feedback in action. We present maps of
the kinematics and line strengths of the ionized gas emission lines
Hα, Hβ, [O III], [O I], [N II] and [S II], and report on the
detection of sodium D absorption. We use these tracers to explore the
structure of the source, derive the ionized and atomic gas kinematics,
and investigate the gas excitation and physical conditions. NGC 1266
contains two ionized gas components along most lines of sight, tracing
the ongoing outflow and a component closer to the galaxy systemic, the
origin of which is unclear. This gas appears to be disturbed by a
nascent AGN jet. We confirm that the outflow in NGC 1266 is truly
multiphase, containing radio plasma, atomic, molecular and ionized gas
and X-ray emitting plasma. The outflow has velocities of up to
±900 km s-1 away from the systemic velocity and
is very likely to remove significant amount of cold gas from the galaxy.
The low-ionization nuclear emission region-like line emission in NGC
1266 is extended, and it likely arises from fast shocks caused by the
interaction of the radio jet with the interstellar medium. These shocks
have velocities of up to 800 km s-1, which match well
with the observed velocity of the outflow. Sodium D equivalent width
profiles are used to set constraints on the size and orientation of the
outflow. The ionized gas morphology correlates with the nascent radio
jets observed in 1.4 and 5 GHz continuum emission, supporting the
suggestion that an AGN jet is providing the energy required to drive the
outflow.
- ISM: jets and outflows, galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: individual: NGC 1266, galaxies: ISM, galaxies: jets
ID: 11174778