Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469

Nguyen, Dieu D.; Izumi, Teruo; Thater, Sabine; Imanishi, Masatoshi; Kawamuro, T.; Baba, Shigeo; Nakano, Suzuka; Turner, Jean L.; Kohno, Kotaro; Matsushita, Satoki; Martín, S.; Meier, David S.; Nguyen, Phuong Minh; Nguyen, Lam Tung

doi:10.1093/mnras/stab1002

Cited by 19 publications

(25 citation statements)

References 144 publications

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“…larger synthesized beams) are more susceptible to systematic biases from stellar mass uncertainties. Our ALMA observations of NGC 3593 thus belong to the majority of M BH measurements with ALMA and CARMA, that have θ FWHM 2 × θ R SOI (Davis et al 2013(Davis et al , 2017Onishi et al 2015Onishi et al , 2017Nagai et al 2019;Smith et al 2019Smith et al , 2021bThater 2019;Nguyen et al 2020Nguyen et al , 2021. This suggests our M BH estimate would benefit from observations at higher angular resolutions, to further reduce the uncertainties arising from our stellar-mass model (but see Section 5.2.1).…”

Section: Resultsmentioning

confidence: 82%

“…This kinematic PA profile varies only slightly (86 • -96 • ) across 15 arcsec, as shown in Fig. 3, but accounting for it in our dynamical model does help to reproduce the kinematic twist observed (see also Nguyen et al 2020Nguyen et al , 2021.…”

Section: Outer Mass Modelmentioning

confidence: 70%

“…The KinMS tool simulates the whole cube, then compares it to the data via a likelihood function (Davis et al 2017(Davis et al , 2018Onishi et al 2017;North et al 2019;Smith et al 2019Smith et al , 2021bNguyen et al 2020Nguyen et al , 2021Thater et al 2020). During the fit, the model, walks through parameter space using a Markov chain Monte Carlo (MCMC) method controlled by the emcee algorithm (Foreman-Mackey et al 2013) and an affine-invariant ensemble sampler (Goodman & Weare 2010) in a Bayesian framework.…”

Section: Kinms Modelmentioning

confidence: 99%

“…This rescaling approach was therefore adopted in a number of recent papers using KinMS and ALMA data (e.g. Nagai et al 2019;North et al 2019;Smith et al 2019Smith et al , 2021bDavis et al 2020;Nguyen et al 2020Nguyen et al , 2021, to yield more realistic uncertainties.…”

Section: Outer Mass Modelmentioning

confidence: 99%

“…Many recent works have used molecular gas tracers to weigh central BHs dynamically, proving this method can be applied to a variety of galaxy types and masses. The method was first pioneered with Combined Array for Research in Millimetre-wave Astronomy (CARMA) observations of the galaxy NGC 4526 (Davis et al 2013) and has now been applied to both active and non-active as well as earlytype (ETGs; Barth et al 2016a,b;Davis et al 2013Davis et al , 2017Davis et al , 2018Onishi et al 2017;Boizelle et al 2019Boizelle et al , 2021Combes et al 2019;Nagai et al 2019;North et al 2019;Smith et al 2019Smith et al , 2021aThater 2019;Cohn et al 2021;Thater et al, in preparation;Nguyen et al, in preparation) and late-type (LTGs; Onishi et al 2015;Combes et al 2019;Nguyen et al 2020Nguyen et al , 2021Boizelle et al 2021) galaxies with ALMA and CARMA. The SMBH masses have in fact now been shown to correlate with the molecular gas line widths (Smith et al 2021b) and there are thousands of potential targets (Davis 2014).…”

mentioning

confidence: 99%

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The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

Nguyen

Bureau

Thater

et al. 2021

Monthly Notices of the Royal Astronomical Society

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As part of the Measuring Black Holes in below Milky Way-mass (M⋆) galaxies (MBHBM⋆) Project, we present a dynamical measurement of the supermassive black hole (SMBH) mass in the nearby lenticular galaxy NGC 3593, using cold molecular gas 12CO(2-1) emission observed at an angular resolution of ≈0${_{.}^{\prime\prime}}$3 (≈10 pc) with the Atacama Large Millimeter/submillimeter Array (ALMA). Our ALMA observations reveal a circumnuclear molecular gas disc (CND) elongated along the galaxy major axis and rotating around the SMBH. This CND has a relatively low-velocity dispersion (≲10 km s−1) and is morphologically complex, with clumps having higher integrated intensities and velocity dispersions (≲25 km s−1). These clumps are distributed along the ridges of a two-arm/bi-symmetric spiral pattern surrounded by a larger ring-like structure (radius r ≈ 10 arcsec or ≈350 pc). This pattern likely plays an important role to bridge the molecular gas reservoirs in the CND and beyond (10 ≲ r ≲ 35 arcsec or 350 pc ≲ r ≲ 1.2 kpc). Using dynamical modelling, the molecular gas kinematics allow us to infer an SMBH mass $M_{\rm BH}=2.40_{-1.05}^{+1.87}\times 10^6$ M⊙ (only statistical uncertainties at the 3σ level). We also detect a massive core of cold molecular gas (CMC) of mass MCMC = (5.4 ± 1.2) × 106 M⊙ and effective (half-mass) radius rCMC,e = 11.2 ± 2.8 pc, co-spatial with a nuclear star cluster (NSC) of mass MNSC = (1.67 ± 0.48) × 107 M⊙ and effective radius rNSC,e = 5.0 ± 1.0 pc (or 0${_{.}^{\prime\prime}}$15 ± 0${_{.}^{\prime\prime}}$03). The mass profiles of the CMC and NSC are well described by Sérsic functions with indices 1−1.4. Our MBH and MNSC estimates for NGC 3593 agree well with the recently compiled MBH–MNSC scaling relation. Although the MNSC uncertainty is twice the inferred MBH, the rapid central rise of the rotation velocities of the CND (as the radius decreases) clearly suggests an SMBH. Indeed, our dynamical models show that even if MNSC is at the upper end of its allowed range, the evidence for a BH does not vanish, but remains with a lower limit of MBH > 3 × 105 M⊙.

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Section: Resultsmentioning

confidence: 82%

Section: Outer Mass Modelmentioning

confidence: 70%

Section: Kinms Modelmentioning

confidence: 99%

Section: Outer Mass Modelmentioning

confidence: 99%

mentioning

confidence: 99%

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The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

Nguyen

Bureau

Thater

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Effect of the initial mass function on the dynamical SMBH mass estimate in the nucleated early-type galaxy FCC 47

Thater¹,

Lyubenova²,

Fahrion³

et al. 2023

A&A

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Supermassive black holes (SMBHs) and nuclear star clusters (NSCs) co-exist in many galaxies. While the formation history of the black hole is essentially lost, NSCs preserve their evolutionary history imprinted onto their stellar populations and kinematics. Studying SMBHs and NSCs in tandem might help us to ultimately reveal the build-up of galaxy centres. In this study, we combine large-scale VLT/MUSE and high-resolution adaptive-optics-assisted VLT/SINFONI observations of the early-type galaxy FCC 47 with the goal being to assess the effect of a spatially (non-)variable initial mass function (IMF) on the determination of the mass of the putative SMBH in this galaxy. We achieve this by performing DYNAMITE Schwarzschild orbit-superposition modelling of the galaxy and its NSC. In order to properly take account of the stellar mass contribution to the galaxy potential, we create mass maps using a varying stellar mass-to-light ratio derived from single stellar population models with fixed and with spatially varying IMFs. Using the two mass maps, we estimate black hole masses of (7.1−1.1+0.8) × 107 M⊙ and (4.4−2.1+1.2) × 107 M⊙ at 3σ signifance, respectively. Compared to models with constant stellar-mass-to-light ratio, the black hole masses decrease by 15% and 48%, respectively. Therefore, a varying IMF, both in its functional form and spatially across the galaxy, has a non-negligible effect on the SMBH mass estimate. Furthermore, we find that the SMBH in FCC 47 has probably not grown over-massive compared to its very over-massive NSC.

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Cross-checking SMBH mass estimates in NGC 6958 – I. Stellar dynamics from adaptive optics-assisted MUSE observations

Thater

Krajnović

Weilbacher

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Supermassive black hole masses (MBH) can dynamically be estimated with various methods and using different kinematic tracers. Different methods have only been cross-checked for a small number of galaxies and often show discrepancies. To understand these discrepancies, detailed cross-comparisons of additional galaxies are needed. We present the first part of our cross-comparison between stellar- and gas-based MBH estimates in the nearby fast-rotating early-type galaxy NGC 6958. The measurements presented here are based on ground-layer adaptive optics-assisted Multi-Unit Spectroscopic Explorer (MUSE) science verification data at around 0${^{\prime\prime}_{.}}$6 spatial resolution. The spatial resolution is a key ingredient for the measurement and we provide a Gaussian parametrisation of the adaptive optics-assisted point spread function (PSF) for various wavelengths. From the MUSE data, we extracted the stellar kinematics and constructed dynamical models. Using an axisymmetric Schwarzschild technique, we measured an MBH of $(3.6^{+2.7}_{-2.4}) \times 10^8\,$M⊙ at 3σ significance taking kinematical and dynamical systematics (e.g. radially-varying mass-to-light ratio) into account. We also added a dark halo, but our data does not allow to constrain the dark matter fraction. Adding dark matter with an abundance matching prior results in a 25 per cent more massive black hole. Jeans anisotropic models return MBH of $(4.6^{+2.5}_{-2.7}) \times 10^8\, \mathrm{M}_{\odot }$ and $(8.6^{+0.8}_{-0.8}) \times 10^8\, \mathrm{M}_{\odot }$ at 3σ confidence for spherical and cylindrical alignment of the velocity ellipsoid, respectively. In a follow-up study, we will compare the stellar-based MBH with those from cold and warm gas tracers, which will provide additional constraints for the MBH for NGC 6958, and insights into assumptions that lead to potential systematic uncertainty.

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Black hole mass measurement using ALMA observations of [CI] and CO emissions in the Seyfert 1 galaxy NGC 7469

Cited by 19 publications

References 144 publications

The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

The MBHBM⋆ Project – II. Molecular gas kinematics in the lenticular galaxy NGC 3593 reveal a supermassive black hole

Effect of the initial mass function on the dynamical SMBH mass estimate in the nucleated early-type galaxy FCC 47

Cross-checking SMBH mass estimates in NGC 6958 – I. Stellar dynamics from adaptive optics-assisted MUSE observations

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