Outflows in Active Galactic Nucleus/Starburst-Composite Ultraluminous Infrared Galaxies

By D. Rupke, Sylvain Veilleux, D. Sanders. 2005

204 citations recorded by the source corpus.

Galactic superwinds occur in almost all infrared-luminous galaxies with star formation rates (SFRs) above 10 M☉ yr-1, as shown by studies of the Na I D interstellar absorption line. We demonstrate that this result also applies to ultraluminous infrared galaxies (ULIRGs) that host an active galactic nucleus (AGN) embedded in a strong starburst (SFR ≳ 100 M☉ yr-1) by studying a sample of 26 Seyfert ULIRGs in Na I D. The infrared luminosity of these galaxies is powered jointly by the AGN and starburst. We find that there are hints of the influence of the AGN on outflows in Seyfert 2/starburst composites, but the evidence is not yet statistically conclusive. The evidence we find is lower wind detection rates (i.e., wind opening angles) in Seyfert 2 ULIRGs than in galaxies of comparable LIR, higher velocities than in galaxies of comparable SFR, and correlations between the neutral gas and the ionized gas in the extended narrow-line region. Although the AGN probably contributes to the outflows in Seyfert 2 ULIRGs, its momentum and energy injection is equal to or less than that of the starburst. Similarly, the outflow mechanical luminosity (energy outflow rate) per unit radiative luminosity is the same for starburst and Seyfert 2 ULIRGs. In the nuclei of Seyfert 1 ULIRGs, we observe small-scale outflows that are powered solely by the AGN. However, in Mrk 231, we observe both a high-velocity, small-scale and low-velocity, extended outflow. The latter may be powered by a starburst or radio jet. These large-scale, lower velocity outflows certainly exist in other Seyfert 1 ULIRGs, but they are washed out by the light of the nucleus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/056ff45484b814dde348d74734efba5b65e6aa6e

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Citations in the corpus

SPITZER QUASAR AND ULIRG EVOLUTION STUDY (QUEST). IV. COMPARISON OF 1 Jy ULTRALUMINOUS INFRARED GALAXIES WITH PALOMAR-GREEN QUASARS (2009, background): “Optical spectral types, which are referred to extensively in this paper, are taken from Veilleux et al. 1999a and Rupke et al. 2005a for the 1 Jy sample, and Veilleux et al. 1995 for the 5 RBGS objects.”
EXTREME FEEDBACK AND THE EPOCH OF REIONIZATION: CLUES IN THE LOCAL UNIVERSE (2011, background): “Very high outflow speeds (many thousands of km s−1) are commonly observed in unobscured (Type 1) AGN (e.g. Rupke et al. 2005; Krug et al. 2010).”
THE MULTIPHASE STRUCTURE AND POWER SOURCES OF GALACTIC WINDS IN MAJOR MERGERS (2013, methodology): “Outflowing ionized gas is also observed away from the minor axis, particularly in the cases of Mrk 273 and F10565+2448.”
INTEGRAL FIELD SPECTROSCOPY OF MASSIVE, KILOPARSEC-SCALE OUTFLOWS IN THE INFRARED-LUMINOUS QSO Mrk 231 (2011, methodology): “However, evidence has remained elusive for largescale outflows that are clearly AGN-driven in LIRGs or ULIRGs (Rupke et al. 2005a).”
Ionized gas outflows and global kinematics of low-z luminous star-forming galaxies (2014, methodology): “These results compare relatively well with those obtained by Rupke et al. (2005) for the neutral gas component, who found average maximum velocities of 301 and 408 kms−1 for their sample of LIRGs and ULIRGs, respectively.”
Quasar feedback revealed by giant molecular outflows (2010, result): “We note that the extended blue-shifted emission is consistent with the result on Na I D by Rupke et al. (2005).”
On the Nature of Seyfert Galaxies with High [O III] λ5007 Blueshifts (2008, background): “In AGN with strong starburst activity winds could also be starburst driven (e.g., Rupke et al. 2005).”
FEEDBACK IN LUMINOUS OBSCURED QUASARS (2011, background): “There is a jet in this galaxy (as well as a starburst) but the jet is not likely the source of acceleration of the neutral outflow (Rupke et al. 2005).”
The SAMI Galaxy Survey: shocks and outflows in a normal star-forming galaxy (2014, background): “Studies of blue-shifted absorption by neutral gas entrained in outflows have reached sample sizes on the order of tens to a hundred and provided constraints on the mass, momentum, and energy of outflows (Heckman et al. 2000; Rupke et al. 2005b,c; Rubin et al. 2013, and references therein).”
FAST MOLECULAR OUTFLOWS IN LUMINOUS GALAXY MERGERS: EVIDENCE FOR QUASAR FEEDBACK FROM HERSCHEL (2013, background): “– 14 – Rupke et al. (2005b) refer to starburst dominated LIRGs, which are not adequately sampled by our set of objects, so we cannot verify if the dependence of the wind detection rate on star formation rate seen in the neutral gas is also present in the molecular gas.”
Fueling Low-Level AGN Activity through Stochastic Accretion of Cold Gas (2006, background): “…indicatethat even Seyfert II ULIRGs in which large-scale winds may be driven by star formation have central, AGN-driven outflows (Cecil et al. 2001; Rupke et al. 2005), and observations at optical, X-ray, and radio wavelengths (Colbert et al. 1996a,b, 1998; Whittle & Wilson 2004) identify a number…”
Direct Cosmological Simulations of the Growth of Black Holes and Galaxies (2007, background): “These include Seyfert II ULIRGs (e.g., Rupke et al. 2005), the ‘‘warm absorbers’’ seen in soft X-rays that show evidence of outflow (e.g., Laor et al. 1997), and broad absorption line (BAL) systems with intense winds with velocities up to 104 km s 1 (e.g., Pounds et al. 2003a, 2003b).”
Formation of z~6 Quasars from Hierarchical Galaxy Mergers (2006, background): “…to prevail in both local star-forming galaxies as indicated by blueshifted optical absorption lines (e.g., Martin 1999, 2005; Heckman et al. 2000; Rupke et al. 2002, 2005) and Lyman break galaxies at z 3 as indicated by blueshifted interstellar absorption lines and redshifted Ly emission lines…”
A Cosmological Framework for the Co-Evolution of Quasars, Supermassive Black Holes, and Elliptical Galaxies. II. Formation of Red Ellipticals (2007, background): “—Quasars are known to often exhibit strong outflows (for a review, see Veilleux et al. 2005) and to have a large effect on the ionization and temperature state of the inner regions of their host galaxies (e.g., Laor et al. 1997; Krongold et al. 2007; Rupke et al. 2005 and references therein).”