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Kinematic Analysis of a Protostellar Multiple System: Measuring the Protostar Masses and Assessing Gravitational Instability in the Disks of L1448 IRS3B and L1448 IRS3A

  • Authors: Nickalas K. Reynolds, John J. Tobin, Patrick Sheehan, Sarah I. Sadavoy, Kaitlin M. Kratter, Zhi-Yun Li, Claire J. Chandler, Dominique Segura-Cox, Leslie W. Looney, and Michael M. Dunham

2021 The Astrophysical Journal Letters 907 L10.

  • Provider: AAS Journals

Caption: Figure 9.

H13CN/SO2 integrated intensity map toward IRS3B appears to trace near the outflow launch location from the tertiary, IRS3B-c. There is pretty large asymmetry in the velocity channels covered by the red- and blueshifted emission. The panels correspond to low-, medium-, and high-velocity ranges. The following panel descriptions will be noted red (blue), corresponding to the Doppler shifted emission. Low velocity: velocity ranges 5.2 ﹩\to ﹩ 7.2 km s−1 (4 ﹩\to ﹩ 4.8 km s−1), contours start at 5σ (5σ) and iterate by 2σ (5σ) with the 1σ level starting at 0.0025 (0.0021) Jy beam−1 for the red (blue) channels. Medium velocity: velocity ranges 7.2 ﹩\to ﹩ 9.2 km s−1 (3.2 ﹩\to ﹩ 4 km s−1), contours start at 5σ (5σ) and iterate by 2σ (2σ) with the 1σ level starting at 0.0016 (0.0016) Jy beam−1 for the red (blue) channels. High velocity: velocity ranges 9.2 ﹩\to ﹩ 11.2 km s−1 (1.6 ﹩\to ﹩ 3.2 km s−1), contours start at 4σ (4σ) and iterate by 3σ (3σ) with the 1σ level starting at 0.0021 (0.0021) Jy beam−1 for the red (blue) channels. The H13CN synthesized beam (0.″22 × 0.″14) is the bottom rightmost ellipse on each of the panels, and the continuum synthesized beam (0.″11 × 0.″05) is offset diagonally.

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