Image Details

Choose export citation format:

Arp 220: New Observational Insights into the Structure and Kinematics of the Nuclear Molecular Disks and Surrounding Gas

  • Authors: Jordan Wheeler, Jason Glenn, Naseem Rangwala, and Adalyn Fyhrie

2020 The Astrophysical Journal 896 43.

  • Provider: AAS Journals

Caption: Figure 10.

Models for Arp 220 east (dashed lines) shown along with the observed line profiles at half-beam increments along the disk axis. 12CO J = 3 → 2 is shown on top and 13CO J = 4 → 3 is shown on the bottom of each panel. The column density of the model in the central position is 1.3 × 1025 H2 cm−2 for 12CO in all of the models. The column density of the model in the central position is 3.3 × 1024 H2 cm−2 for 13CO for both the absorber and asymmetric disk models and in the outflow model is 2.3 × 1024 H2 cm−2. Moving either to the left or right one panel at a time, the models’ column density decreases to 8.3 × 1024 H2 cm−2, 4.2 × 1024 H2 cm−2, and 2.0 × 1024 H2 cm−2 for all of the 12CO models. For 13CO, the column density decreases to 2.2 × 1024 H2 cm−2, 1.2 × 1024 H2 cm−2, and 6.5 × 1023 H2 cm−2 for both the absorber and asymmetric disk models. For the outflow model in 13CO, the column density decreases to 1.6 × 1024 H2 cm−2, 8.6 × 1023 H2 cm−2, and 4.5 × 1023 H2 cm−2 moving one panel at a time to the left or right. For 12CO J = 3 → 2, 1 Jy/beam = 248 K and for 13CO J = 4 → 3, 1 Jy/beam = 294.5 K. Used in the fitting, but not shown here, are several points perpendicular to the axis of the disk that allows for the constraint of the height of the disk. This is shown in detail for the asymmetric disk model in Figure 11.

Other Images in This Article

Show More

Copyright and Terms & Conditions