Zooms in towards areas of W43-MM1 with new cores and outflow detection. The CO (2−1) blue-shifted line wing is integrated over 42 – 64 km s⁻¹ (HV, blue contours) and 82 – 88 km s⁻¹ (LV, cyan contours), the red-shifted line wing over 108 – 119 km s⁻¹ (LV, orange contours) and 128 – 158 km s⁻¹ (HV, red contours). In a: For blue lobes, contours are 7, 15, 30 to 230 by steps of 40 (HV) and 7, 15 to 120 by steps of 15 (LV), in units of σ = 20 mJy beam⁻¹ km s⁻¹. For red lobes, contours are 10, 20 to 160 by steps of 20, in units of σ_LV,_R = 37 mJy beam⁻¹ km s⁻¹ (LV) and 7, 15, 30 to 280 by steps of 50, in units of σ (HV). In b: For blue lobes, contours are 5, 15, 30 by steps of 15 (HV) and 10, 20, 30 (LV), in units of σ = 20 mJy beam⁻¹ km s⁻¹. For red lobes, contours are 5, 15, 25, 35, in units of σ_LV,_R = 37 mJy beam⁻¹ km s⁻¹ (LV) and 5, 15 to 75 by steps of 15, in units of σ (HV). In a and b: Green ellipses locate protostellar cores, arrows indicate the direction of their outflows. Prestellar core candidates are represented with yellow ellipses, hatched for the high-mass core #134 in (a). The source #132 discarded from the core sample is shown with a dotted yellow ellipse. Adapted from Figs. 3 and 4 of Nony et al. (2020).