Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

Sabine Thater; Davor Krajnović; Michele Cappellari; Timothy A. Davis; P. Tim de Zeeuw; Richard M. MCdermid; Marc Sarzi

doi:10.1051/0004-6361/201834808

Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

Sabine Thater^*, Davor Krajnović, Michele Cappellari, Timothy A. Davis, P. Tim de Zeeuw, Richard M. MCdermid, Marc Sarzi

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

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Abstract

Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (M_BH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σ_e) between 170 and 245 km s⁻¹, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS^3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 10⁸ M_⊙ for NGC 584, (1.0 ± 0.6) × 10⁸ M_⊙ for NGC 2784, (7.7 ± 5) × 10⁷ M_⊙ for NGC 3640, (5.4 ± 0.8) × 10⁸ M_⊙ for NGC 4281, (6.8 ± 2.0) × 10⁷ M_⊙ for NGC 4570, and (3.2 ± 0.8) × 10⁸ M_⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent M_BH−σ_e scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

Original language	English
Article number	A62
Pages (from-to)	1-30
Number of pages	30
Journal	Astronomy and Astrophysics
Volume	625
DOIs	https://doi.org/10.1051/0004-6361/201834808
Publication status	Published - 13 May 2019

Bibliographical note

Reproduced with permission from Astronomy & Astrophysics, Copyright 2019 ESO. First published in Astronomy and Astrophysics, 625, A62, 2019, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201834808. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

Keywords

galaxies: kinematics and dynamics
quasars: supermassive black holes

Access to Document

10.1051/0004-6361/201834808

Publisher version (open access)Final published version, 11.8 MBLicence: Other

Cite this

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title = "Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations",

abstract = "Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.",

keywords = "galaxies: kinematics and dynamics, quasars: supermassive black holes",

author = "Sabine Thater and Davor Krajnovi{\'c} and Michele Cappellari and Davis, {Timothy A.} and {de Zeeuw}, {P. Tim} and MCdermid, {Richard M.} and Marc Sarzi",

note = "Reproduced with permission from Astronomy & Astrophysics, Copyright 2019 ESO. First published in Astronomy and Astrophysics, 625, A62, 2019, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201834808. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.",

year = "2019",

month = may,

day = "13",

doi = "10.1051/0004-6361/201834808",

language = "English",

volume = "625",

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journal = "Astronomy and Astrophysics",

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AU - Thater, Sabine

AU - Krajnović, Davor

AU - Cappellari, Michele

AU - Davis, Timothy A.

AU - de Zeeuw, P. Tim

AU - MCdermid, Richard M.

AU - Sarzi, Marc

N1 - Reproduced with permission from Astronomy & Astrophysics, Copyright 2019 ESO. First published in Astronomy and Astrophysics, 625, A62, 2019, published by EDP Sciences. The original publication is available at https://doi.org/10.1051/0004-6361/201834808. Version archived for private and non-commercial use with the permission of the author/s and according to publisher conditions. For further rights please contact the publisher.

PY - 2019/5/13

Y1 - 2019/5/13

N2 - Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

AB - Different massive black hole mass – host galaxy scaling relations suggest that the growth of massive black holes is entangled with the evolution of their host galaxies. The number of measured black hole masses is still limited and additional measurements are necessary to understand the underlying physics of this apparent coevolution. We add six new black hole mass (MBH) measurements of nearby fast rotating early-type galaxies to the known black hole mass sample, namely NGC 584, NGC 2784, NGC 3640, NGC 4570, NGC 4281, and NGC 7049. Our target galaxies have effective velocity dispersions (σe) between 170 and 245 km s−1, and thus this work provides additional insight into the black hole properties of intermediate-mass early-type galaxies. We combined high-resolution adaptive-optics SINFONI data with large-scale MUSE, VIMOS and SAURON data from ATLAS3D to derive two-dimensional stellar kinematics maps. We then built both Jeans Anisotropic Models and axisymmetric Schwarzschild models to measure the central black hole masses. Our Schwarzschild models provide black hole masses of (1.3 ± 0.5) × 108 M⊙ for NGC 584, (1.0 ± 0.6) × 108 M⊙ for NGC 2784, (7.7 ± 5) × 107 M⊙ for NGC 3640, (5.4 ± 0.8) × 108 M⊙ for NGC 4281, (6.8 ± 2.0) × 107 M⊙ for NGC 4570, and (3.2 ± 0.8) × 108 M⊙ for NGC 7049 at 3σ confidence level, which are consistent with recent MBH−σe scaling relations. NGC 3640 has a velocity dispersion dip and NGC 7049 a constant velocity dispersion in the center, but we can clearly constrain their lower black hole mass limit. We conclude our analysis with a test on NGC 4570 taking into account a variable mass-to-light ratio (M/L) when constructing dynamical models. When considering M/L variations linked mostly to radial changes in the stellar metallicity, we find that the dynamically determined black hole mass from NGC 4570 decreases by 30%. Further investigations are needed in the future to account for the impact of radial M/L gradients on dynamical modeling.

KW - galaxies: kinematics and dynamics

KW - quasars: supermassive black holes

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DO - 10.1051/0004-6361/201834808

M3 - Article

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JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A62

ER -

Six new supermassive black hole mass determinations from adaptive-optics assisted SINFONI observations

Abstract

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Keywords

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