TY - JOUR
T1 - The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693
AU - Pilawa, Jacob D.
AU - Liepold, Christopher M.
AU - Delgado Andrade, Silvana C.
AU - Walsh, Jonelle L.
AU - Ma, Chung Pei
AU - Quenneville, Matthew E.
AU - Greene, Jenny E.
AU - Blakeslee, John P.
N1 - Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/4/1
Y1 - 2022/4/1
N2 - We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise ratio integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extract and model stellar kinematics of NGC 2693 from the central ∼150 pc out to ∼2.5 effective radii. Observations from Hubble Space Telescope WFC3 are used to determine the stellar light distribution. We perform fully triaxial Schwarzschild orbit modeling using the latest TriOS code and a Bayesian search in 6D galaxy model parameter space to determine NGC 2693's SMBH mass (M BH), stellar mass-to-light ratio, dark matter content, and intrinsic shape. We find MBH=1.7±0.4×109M⊙ and a triaxial intrinsic shape with axis ratios p = b/a = 0.902 ± 0.009 and q=c/a=0.721-0.010+0.011, triaxiality parameter T = 0.39 ± 0.04. In comparison, the best-fit orbit model in the axisymmetric limit and (cylindrical) Jeans anisotropic model of NGC 2693 prefer MBH=2.4±0.6×109M⊙ and MBH=2.9±0.3×109M⊙, respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data.
AB - We present a stellar dynamical mass measurement of a newly detected supermassive black hole (SMBH) at the center of the fast-rotating, massive elliptical galaxy NGC 2693 as part of the MASSIVE survey. We combine high signal-to-noise ratio integral field spectroscopy (IFS) from the Gemini Multi-Object Spectrograph with wide-field data from the Mitchell Spectrograph at McDonald Observatory to extract and model stellar kinematics of NGC 2693 from the central ∼150 pc out to ∼2.5 effective radii. Observations from Hubble Space Telescope WFC3 are used to determine the stellar light distribution. We perform fully triaxial Schwarzschild orbit modeling using the latest TriOS code and a Bayesian search in 6D galaxy model parameter space to determine NGC 2693's SMBH mass (M BH), stellar mass-to-light ratio, dark matter content, and intrinsic shape. We find MBH=1.7±0.4×109M⊙ and a triaxial intrinsic shape with axis ratios p = b/a = 0.902 ± 0.009 and q=c/a=0.721-0.010+0.011, triaxiality parameter T = 0.39 ± 0.04. In comparison, the best-fit orbit model in the axisymmetric limit and (cylindrical) Jeans anisotropic model of NGC 2693 prefer MBH=2.4±0.6×109M⊙ and MBH=2.9±0.3×109M⊙, respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data.
UR - https://www.scopus.com/pages/publications/85128706462
UR - https://www.scopus.com/pages/publications/85128706462#tab=citedBy
U2 - 10.3847/1538-4357/ac58fd
DO - 10.3847/1538-4357/ac58fd
M3 - Article
AN - SCOPUS:85128706462
SN - 0004-637X
VL - 928
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 178
ER -