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tokens: arise from a multiphase ISM. This is also supported by the maximum velocity of the CO (2–1) emission (FWZI/2 ∼ 1000 km s −1 ; Fig. 1 b), which is consistent with the maximum velocity of a warm molecular outflow traced by blueshifted OH absorption (∼1200 km s −1 ; Veilleux et al. 2013 ) and H α emission (≥1000 km s −1 ; Heckman, Armus Miley 1990 ). As seen in other LIRGs (e.g. NGC 1068; García-Burillo et al. 2014 , NGC 3256; Sakamoto et al. 2014 , and NGC 1614; Saito et al. 2017 ), molecular outflows are often spatially extended (a few kpc) and concomitant with (or entrained by) ionized gas outflow. Considering all pieces of evidence described above and some similarities with other LIRGs, we suggest that the four peaks of the broad CO (2–1) components trace molecular outflows in NGC 6240. We derive physical parameters of the molecular outflows found in NGC 6240. The spatially resolved map (Fig. 3 c) allows us to estimate the mass and projected distance of the line width peaks from the launching points. We assume the launching points are the double nuclei, that is, the northern and eastern (southern and western) components of the molecular outflow come from the northern (southern) nucleus (see grey arrows in Fig. 4 ). This spatial configuration is supported by radio continuum observations with very long baseline interferometers (Gallimore Beswick 2004 ; Hagiwara, Baan Klöckner 2011 ), showing that the northern nucleus has an east–west bipolar structure. The direction of those bipolar structures is similar to our assumed morphology of the molecular outflows. We also assume that the inclination (α), CO (2–1)/CO (1–0) line intensity ratio, and CO (1–0) luminosity to H 2 mass conversion factor of the molecular outflows in NGC 6240 are 45°, unity, and 0.8 M ⊙ (K km s −1 pc 2 ) −1 , respectively, for the sake of simplicity. Figure 4. Peak velocity map of the broad component. The velocity field in colour scale ranges from 6850 to 7350 km s −1 . Data points around the four peaks in Fig. 3 c are shown. To estimate the mass outflow rate (), we employ the expression, where v out, proj is the projected velocity of the outflow, is the gas mass of the outflow, R out, proj is the distance from the launching point to the outflowing gas, and α is the inclination of the outflow. This equation assumes a uniformly filled cone geometry (Maiolino et al. 2012 ). All derived parameters related to are listed in Table 1 . v out, proj of the northern and eastern (southern and western) outflows is derived by using the projected velocity of the outflowing gas (Fig. 4 ) and the systemic velocity of the northern (southern) nucleus of 7122 (7164) km s −1 in the radio LSRK velocity frame (Hagiwara 2010 ). Table 1. NGC 6240 molecular outflow properties. The derived mass of each broad component is ∼10 7.9–8.2 M ⊙ (∼10 8.7 M ⊙ in total, which is consistent with the value derived from unresolved CO data; Cicone et al. 2014 ). Since the ionized gas mass of the butterfly