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Table 1

Properties of the outflow regions.

Region d/sinia v/cosib σ c f(CO(2−1))d log Mmol e log Eout f t dyn g FWHM h
(pc) (km s-1) (km s-1) (mJy km s-1) (M⊙) (erg) (Myr) (pc)
A 1320 −460 ± 23 70 ± 10 250 ± 10 5.5 53.8 2.8 ± 0.2 70 ± 20
B 1210 −510 ± 16 50 ± 7 374 ± 15 5.7 54.1 2.3 ± 0.1 80 ± 20
C 800 −367 ± 9 33 ± 4 474 ± 13 5.8 53.9 2.1 ± 0.1 70−110
D 90 [−530, −320]* ··· 1940 ± 30 6.4 54.6 0.2 ± 0.1 90 ± 10
E −250 370 ± 11 42 ± 5 1044 ± 15 6.1 54.2 0.7 ± 0.1 150 ± 30
F −730 [330, 750]* ··· 920 ± 40 6.1 54.5 1.4 ± 0.3 ~100
G −1100 [390, 690]* ··· 210 ± 30 5.5 53.7 2.4 ± 0.4 60 ± 20

Notes. We assume a galaxy inclination of 43° (see Sect. 3).

(a)

Deprojected distance.

(b)

Deprojected CO(2−1) velocity with respect to the nuclear velocity. When possible, we fitted with Gaussians the line profile of the outflow and the disk emission. Otherwise, we integrated the flux in the given velocity range.

(c)

Velocity dispersion derived from the Gaussian fit to the outflow component.

(d)

CO(2−1) integrated flux of the outflow component.

(e)

Logarithm of the outflowing molecular mass assuming an ULIRG-like conversion factor (αCO = 0.78 and r21 = 0.9). If we use the standard conversion factor, the molecular masses will be ~5 times (0.7 dex) higher.

(f)

Kinetic energy calculated as 1/2 × Mmol × (v/ cosi)2. For the regions without a Gaussian fit, we used the central velocity of the range. The uncertainty of the kinematic energy is dominated by the factor of ~5 uncertainty of the molecular mass estimates.

(g)

Dynamical time required for the gas to reach its current position derived using tdyn = d × coti × v-1.

(h)

FWHM of the regions measured using a 2D Gaussian fit on the outflow emission maps (Fig. 6). Region C contains several weak clumps with sizes between 70 and 110 pc. It was not possible to fit the size of region F, so we indicate the size of the aperture used to extract the spectrum.

(*)

The central velocity of the intervals for regions D, F, and G are −425, 540, and 540 km s-1, respectively.

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