Shock Excited Molecules in NGC 1266 : ULIRG Conditions at the Center of a Bulge-dominated Galaxy
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Author
Pellegrini, E.W.
Smith, J.D.
Wolfire, M.G.
Draine, B.T.
Crocker, A.F.
Croxall, K.V.
van der Werf, P.
Dale, D.A.
Rigopoulou, D.
Wilson, C.D.
Schinnerer, E.
Groves, B.A.
Kreckel, K.
Sandstrom, K.M.
Armus, L.
Calzetti, D.
Murphy, E. J.
Walter, F.
Koda, J.
Bayet, E.
Beirao, P.
Bolatto, A. D.
Bradford, M.
Brinks, E.
Hunt, L.
Kennicutt, R.
Knapen, J.H.
Leroy, A.K.
Rosolowsky, E.
Vigroux, L.
Hopwood, R.H.B.
Attention
2299/13053
Abstract
We investigate the far infrared (IR) spectrum of NGC 1266, a S0 galaxy that contains a massive reservoir of highly excited molecular gas. Using the Herschel Fourier Transform Spectrometer, we detect the 12CO ladder up to J = (13-12), [C I] and [N II] lines, and also strong water lines more characteristic of UltraLuminous IR Galaxies (ULIRGs). The 12CO line emission is modeled with a combination of a low-velocity C-shock and a photodissociation region. Shocks are required to produce the H2O and most of the high-J CO emission. Despite having an IR luminosity 30 times less than a typical ULIRG, the spectral characteristics and physical conditions of the interstellar medium of NGC 1266 closely resemble those of ULIRGs, which often harbor strong shocks and large-scale outflows