Mass Loss from the Nuclei of Active Galaxies

By D. Crenshaw, S. Kraemer, I. George. 2003

418 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f44c35f8b9f03b956dd3610c3b2ae1745ad4fc1a

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In Astronomy and Astrophysics

Citations in the corpus

NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. III. REVISITING WIND PROPERTIES USING THE TRAJECTORY APPROACH (2015, background): “…(RN); xbai@cfa.harvard.edu (XNB) 3 MIT Kavli Institute for Astrophysics and Space Rsearch; asadowsk@mit.edu 4 NASA Einstein Fellow 5 NASA Hubble Fellow and perhaps even some direct observations on outflow (e.g., Crenshaw et al. 2003; Crenshaw & Kraemer 2012; Yuan, Bu & Wu 2012).”
INTEGRAL FIELD SPECTROSCOPY OF MASSIVE, KILOPARSEC-SCALE OUTFLOWS IN THE INFRARED-LUMINOUS QSO Mrk 231 (2011, background): “Either (1) wide-angle winds from the AGN accretion disk or broad line region or (2) coupling of the AGN radiation to the dust in the wind are possible explanations (e.g., Crenshaw et al. 2003; Hopkins & Elvis 2010).”
Outflows in Infrared-Luminous Starbursts at z < 0.5. II. Analysis and Discussion (2005, methodology): “The global covering factor is then given by /4 ¼C hCf i ¼ DhCf i (see x 2.6.2 and Crenshaw et al. 2003).”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, background): “Nuclear activity is known to drive outflows on small scales (Crenshaw et al. 2003; Ganguly & Brotherton 2008), perhaps via the radiation pressure of the quasar (Murray et al. 1995; Proga et al. 2000).”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “…direct spectroscopic evidence for discrete absorption lines and photoelectric edges in their soft-band (E < 3 keV) spectra (e.g. Reynolds 1997; Crenshaw et al. 2003; Blustin et al. 2005), with typical lineof-sight velocities ranging from a few hundred to around a thousand km s−1 (Blustin et…”
The Coevolution of Galaxies and Supermassive Black Holes: Insights from Surveys of the Contemporary Universe (2014, background): “This is primarily based on the frequent presence of blue-shifted absorption-lines in the optical, ultraviolet, and soft X-ray spectra of Type 1 AGN (see Crenshaw et al. 2003 and references therein).”
The Blast Wave Model for AGN Feedback: Effects on AGN Obscuration (2008, background): “219 scales, the observed X-ray absorption lines indicate the presence of outward winds with velocities up to some 104 km s 1 (Weymann 1981; Turnshek et al. 1988; Crenshaw et al. 2003; Chartas et al. 2002; Pounds et al. 2003; Pounds & Page 2006; Risaliti et al. 2005a).”
NUMERICAL SIMULATION OF HOT ACCRETION FLOWS. II. NATURE, ORIGIN, AND PROPERTIES OF OUTFLOWS AND THEIR POSSIBLE OBSERVATIONAL APPLICATIONS (2012, background): “Outflow has been directly detected in AGNs such as broad absorption lines quasars (e.g., Crenshaw et al. 2003; Tombesi et al. 2010; 2011a; 2012).”
Emission-line diagnostics of low-metallicity active galactic nuclei (2006, background): “The models are all truncated at a column density of log(N(H )) = 21, which is reasonable for NLR clouds (e.g. Crenshaw et al. 2003).”
Outflows in Active Galactic Nucleus/Starburst-Composite Ultraluminous Infrared Galaxies (2005, methodology): “Our detection rate is similar to that of intrinsic UV and X-ray absorbers in local Seyfert 1 galaxies (50%–70%; Crenshaw et al. 2003).”
Quasar feedback and the origin of radio emission in radio-quiet quasars (2014, background): “If an outflow has non-zero optical depth, then its presence can be inferred by its absorption of the background light at wavelengths blue-shifted relative to the quasar rest-frame, as happens in quasar absorption-line systems (Crenshaw et al. 2003; Arav et al. 2008), but this is not our case.”