Three-color composite image of the Serpens filament (Berschel 70 µm: blue, Berschel 250 µm: green, Berschel 500 µm: red). The three green pluses indicate the positions of the three embedded YSOs, emb10 (also knupown as IRAS 18262+0050), emb16, and emb28 (Enoch et al. 2009), while the crosses mark the positions of 1.1 mm dust cores (Enoch et al. 2007). The beam size (36″.3) for the 500 µm emission is shown in the lower right corner. The regions mapped with the IRAM-30 m and APEX telescopes are indicated by the red and white dashed boxes, respectively.

Outflow driven by Ser-emb 10. Left: same as Fig. 2e in Gong et al. (2021). Right: (a) Observed ¹³CO (2−1) spectra of the two positions indicated by the blue and red pluses in panel b overlaid with the C¹⁸O spectrum of the position indicated by the yellow star in panel b. (b) ¹³CO (2−1) outflow map of Ser-emb 10. The blueshifted emission integrated from 2.0 to 5.5 kms⁻¹ is shown in blue dashed contours which start at 0.20 K km s⁻¹ (5σ) and increase by 0.20 K km s⁻¹. The redshifted emission integrated from 9.4 to 12 km s⁻¹ is shown in red dashed contours which start at 0.20 K km s⁻¹ and increase by 0.20 K km s⁻¹. The yellow star marks the position of Ser-emb 10. The beam size is shown in the lower left corner. (c) Position-velocity diagram of the ¹³CO (2−1) emission along the cut indicated by the black line in panel b. The contours start at 0.18 K (3σ) and increase by 0.36 K. The horizontal dashed line indicates the position of Ser-emb 10, and the vertical dashed line marks its systemic velocity of 7.87 km s⁻¹. The resolution element is shown in the lower left corner.

(a) Local velocity gradient magnitude map overlaid with the H₂ column density contours. (b) Herschel H₂ column density map overlaid with the normalized velocity vector maps. The arrows represent the estimated local velocity gradients which are rotated by 180° in order to better visualize the accretion directions in SE. The polarized angle of the Planck 353 GHz thermal dust emission has been rotated by 90° to trace the magnetic field direction which is indicated by the red line. In both panels, the contours correspond to H₂ column densities from 1×10²¹ cm⁻² to 1.6×10²² cm⁻² with a step of 3×10²¹ cm⁻², and the beam sizes for the H₂ column density and velocity gradient maps are shown as the gray and blue circles in the lower right corner. The three green pluses give the positions of the three embedded YSOs, emb10, emb16, and Ser-emb 28 (Enoch et al. 2009), and the white crosses mark the positions of the seven dust cores (Enoch et al. 2007).

Physical and chemical parameters (from top to bottom: position angle of local velocity gradient, magnitude of local velocity gradient, C¹⁸O rotational temperature, C¹⁸O column density, C¹⁸O fractional abundance, dust temperature, H₂ column density, nonthermal velocity dispersion, and velocity centroid) along the crest of the Serpens filament indicated by the blue line in Fig. 2d of Gong et al. (2021). The origin of the offsets corresponds to the southern end of the blue line in Fig. 2d of Gong et al. (2021). The offset increases from south to north. The positions which are close to the seven 1.1 mm dust cores and the three YSOs are indicated by the cyan and orange vertical lines, respectively. In the two lowest panels, the data derived from C¹⁸O (1−0) and C¹⁸O (2−1) are indicated by blue and red symbols, respectively.

Three-color composite image of the Serpens filament (Berschel 70 µm: blue, Berschel 250 µm: green, Berschel 500 µm: red). The three green pluses indicate the positions of the three embedded YSOs, emb10 (also knupown as IRAS 18262+0050), emb16, and emb28 (Enoch et al. 2009), while the crosses mark the positions of 1.1 mm dust cores (Enoch et al. 2007). The beam size (36″.3) for the 500 µm emission is shown in the lower right corner. The regions mapped with the IRAM-30 m and APEX telescopes are indicated by the red and white dashed boxes, respectively.

Outflow driven by Ser-emb 10. Left: same as Fig. 2e in Gong et al. (2021). Right: (a) Observed ¹³CO (2−1) spectra of the two positions indicated by the blue and red pluses in panel b overlaid with the C¹⁸O spectrum of the position indicated by the yellow star in panel b. (b) ¹³CO (2−1) outflow map of Ser-emb 10. The blueshifted emission integrated from 2.0 to 5.5 kms⁻¹ is shown in blue dashed contours which start at 0.20 K km s⁻¹ (5σ) and increase by 0.20 K km s⁻¹. The redshifted emission integrated from 9.4 to 12 km s⁻¹ is shown in red dashed contours which start at 0.20 K km s⁻¹ and increase by 0.20 K km s⁻¹. The yellow star marks the position of Ser-emb 10. The beam size is shown in the lower left corner. (c) Position-velocity diagram of the ¹³CO (2−1) emission along the cut indicated by the black line in panel b. The contours start at 0.18 K (3σ) and increase by 0.36 K. The horizontal dashed line indicates the position of Ser-emb 10, and the vertical dashed line marks its systemic velocity of 7.87 km s⁻¹. The resolution element is shown in the lower left corner.

(a) Local velocity gradient magnitude map overlaid with the H₂ column density contours. (b) Herschel H₂ column density map overlaid with the normalized velocity vector maps. The arrows represent the estimated local velocity gradients which are rotated by 180° in order to better visualize the accretion directions in SE. The polarized angle of the Planck 353 GHz thermal dust emission has been rotated by 90° to trace the magnetic field direction which is indicated by the red line. In both panels, the contours correspond to H₂ column densities from 1×10²¹ cm⁻² to 1.6×10²² cm⁻² with a step of 3×10²¹ cm⁻², and the beam sizes for the H₂ column density and velocity gradient maps are shown as the gray and blue circles in the lower right corner. The three green pluses give the positions of the three embedded YSOs, emb10, emb16, and Ser-emb 28 (Enoch et al. 2009), and the white crosses mark the positions of the seven dust cores (Enoch et al. 2007).

Physical and chemical parameters (from top to bottom: position angle of local velocity gradient, magnitude of local velocity gradient, C¹⁸O rotational temperature, C¹⁸O column density, C¹⁸O fractional abundance, dust temperature, H₂ column density, nonthermal velocity dispersion, and velocity centroid) along the crest of the Serpens filament indicated by the blue line in Fig. 2d of Gong et al. (2021). The origin of the offsets corresponds to the southern end of the blue line in Fig. 2d of Gong et al. (2021). The offset increases from south to north. The positions which are close to the seven 1.1 mm dust cores and the three YSOs are indicated by the cyan and orange vertical lines, respectively. In the two lowest panels, the data derived from C¹⁸O (1−0) and C¹⁸O (2−1) are indicated by blue and red symbols, respectively.