The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693
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-Objec...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2022-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ac58fd |
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| author | Jacob D. Pilawa Emily R. Liepold Silvana C. Delgado Andrade Jonelle L. Walsh Chung-Pei Ma Matthew E. Quenneville Jenny E. Greene John P. Blakeslee |
| author_facet | Jacob D. Pilawa Emily R. Liepold Silvana C. Delgado Andrade Jonelle L. Walsh Chung-Pei Ma Matthew E. Quenneville Jenny E. Greene John P. Blakeslee |
| author_sort | Jacob D. Pilawa |
| collection | DOAJ |
| description | 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 ${M}_{\mathrm{BH}}=\left(1.7\pm 0.4\right)\times {10}^{9}\ {M}_{\odot }$ 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 ${M}_{\mathrm{BH}}=\left(2.4\pm 0.6\right)\times {10}^{9}\ {M}_{\odot }$ and ${M}_{\mathrm{BH}}=\left(2.9\pm 0.3\right)\times {10}^{9}\ {M}_{\odot }$ , respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data. |
| first_indexed | 2024-03-08T15:59:02Z |
| format | Article |
| id | doaj.art-ed9462bf16994b29a51996c6d8e304db |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-08T15:59:02Z |
| publishDate | 2022-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-ed9462bf16994b29a51996c6d8e304db2024-01-08T14:40:04ZengIOP PublishingThe Astrophysical Journal1538-43572022-01-01928217810.3847/1538-4357/ac58fdThe MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693Jacob D. Pilawa0https://orcid.org/0000-0001-7040-9117Emily R. Liepold1https://orcid.org/0000-0002-7703-7077Silvana C. Delgado Andrade2Jonelle L. Walsh3https://orcid.org/0000-0002-1881-5908Chung-Pei Ma4https://orcid.org/0000-0002-4430-102XMatthew E. Quenneville5https://orcid.org/0000-0002-6148-5481Jenny E. Greene6https://orcid.org/0000-0002-5612-3427John P. Blakeslee7https://orcid.org/0000-0002-5213-3548Department of Astronomy, University of California , Berkeley, CA 94720, USA ; jacobpilawa@berkeley.eduDepartment of Astronomy, University of California , Berkeley, CA 94720, USA ; jacobpilawa@berkeley.edu; Department of Physics, University of California , Berkeley, CA 94720, USAGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University , College Station, TX 77843, USAGeorge P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, and Department of Physics and Astronomy, Texas A&M University , College Station, TX 77843, USADepartment of Astronomy, University of California , Berkeley, CA 94720, USA ; jacobpilawa@berkeley.edu; Department of Physics, University of California , Berkeley, CA 94720, USADepartment of Astronomy, University of California , Berkeley, CA 94720, USA ; jacobpilawa@berkeley.edu; Department of Physics, University of California , Berkeley, CA 94720, USADepartment of Astrophysical Sciences, Princeton University , Princeton, NJ 08544, USANSF’s NOIRLab , Tucson, AZ 85719, USAWe 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 ${M}_{\mathrm{BH}}=\left(1.7\pm 0.4\right)\times {10}^{9}\ {M}_{\odot }$ 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 ${M}_{\mathrm{BH}}=\left(2.4\pm 0.6\right)\times {10}^{9}\ {M}_{\odot }$ and ${M}_{\mathrm{BH}}=\left(2.9\pm 0.3\right)\times {10}^{9}\ {M}_{\odot }$ , respectively. Neither model can account for the non-axisymmetric stellar velocity features present in the IFS data.https://doi.org/10.3847/1538-4357/ac58fdGalaxy dynamicsGalaxy massesSupermassive black holesEarly-type galaxiesGalaxiesGalaxy dark matter halos |
| spellingShingle | Jacob D. Pilawa Emily R. Liepold Silvana C. Delgado Andrade Jonelle L. Walsh Chung-Pei Ma Matthew E. Quenneville Jenny E. Greene John P. Blakeslee The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 The Astrophysical Journal Galaxy dynamics Galaxy masses Supermassive black holes Early-type galaxies Galaxies Galaxy dark matter halos |
| title | The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 |
| title_full | The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 |
| title_fullStr | The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 |
| title_full_unstemmed | The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 |
| title_short | The MASSIVE Survey. XVII. A Triaxial Orbit-based Determination of the Black Hole Mass and Intrinsic Shape of Elliptical Galaxy NGC 2693 |
| title_sort | massive survey xvii a triaxial orbit based determination of the black hole mass and intrinsic shape of elliptical galaxy ngc 2693 |
| topic | Galaxy dynamics Galaxy masses Supermassive black holes Early-type galaxies Galaxies Galaxy dark matter halos |
| url | https://doi.org/10.3847/1538-4357/ac58fd |
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