Image Details

Choose export citation format:

Nearby Early-type Galactic Nuclei at High Resolution: Dynamical Black Hole and Nuclear Star Cluster Mass Measurements

  • Authors: Dieu D. Nguyen, Anil C. Seth, Nadine Neumayer, Sebastian Kamann, Karina T. Voggel, Michele Cappellari, Arianna Picotti, Phuong M. Nguyen, Torsten Böker, Victor Debattista, Nelson Caldwell, Richard McDermid, Nathan Bastian, Christopher C. Ahn, and Renuka Pechetti

2018 The Astrophysical Journal 858 118.

  • Provider: AAS Journals

Caption: Figure 3.

Top panels: comparison of the mass surface density models in each galaxy. These models are created using MGEs constructed from our GALFIT models. These MGEs are then multiplied by an M/L to get a mass surface density. For the constant M/L model (blue lines), the chosen M/L is discussed in Section 4.3. For the other mass models, an M/L is assigned to each MGE based on the color of the galaxy at the radius of the MGE using the R15 or B03 color–M/L relation (red/purple lines); we use the R15 model as our default. Dashed black lines show the NSCs in the R15 model; their effective radii are shown by vertical lines. Bottom panels: to compare the relative mass distribution of the three different mass profiles for each galaxy, we plot their fractional difference relative to the R15 color–M/L relation.

Other Images in This Article

Show More

Copyright and Terms & Conditions

Additional terms of reuse