A low upper mass limit for the central black hole in the late-type galaxy NGC 4414

Thater, Sabine; Krajnović, Davor; Bourne, Martin A.; Cappellari, Michele; Zeeuw, Tim de; Emsellem, Éric; Magorrian, John; McDermid, Richard M.; Sarzi, Marc; Ven, Glenn van de

doi:10.1051/0004-6361/201629480

Cited by 23 publications

(34 citation statements)

References 104 publications

(160 reference statements)

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“…A careful dust correction is necessary to optimize the reproducibility from the model and the actual shape of the galaxy. We used the same method as in Cappellari et al (2002) and Scott et al (2013) to dust-correct the SDSS and CGS images and the dust-masking method outlined in Thater et al (2017) to mask dust-rings visible in the HST images, which had only a single image available (for details see Appendix A). We also visually inspected the HST images of our galaxies for nuclear star clusters, but could not find any evidence.…”

Section: The Mass Modelmentioning

confidence: 99%

“…Therefore, including a nearly constant dynamical M/L must not always be a bad assumption in dynamical modeling (e.g. Thater et al 2017) in particular, when modeling the stellar kinematics observed over a wide range of radial scales.…”

Section: Variations In Stellar Populationsmentioning

confidence: 99%

“…The smoothing is applied by adding a linear regularization to the pPXF fit which is chosen such that the difference in χ 2 between regularised and non-regularised fit equals √ 2N, where N is the number of good pixels in the spectrum. We then calculated the mass-weighted stellar M/L for each radial bin using the tracked stellar mass and r-band luminosity from the SSP models and using equation (5) from Thater et al (2017).…”

Section: Variations In Stellar Populationsmentioning

confidence: 99%

“…Furthermore, we found a small dust ring in the HST image of NGC 2784. As carefully tested in Thater et al (2017) we applied a dust mask for the HST small scale images for all three galaxies and a dust correction for the SDSS large scale image of NGC 4281.…”

Section: Appendix A: Dust Correction and Maskingmentioning

confidence: 99%

“…The careful dust correction in the HST images is crucial as we probe the direct vicinity of the black hole with them. However, due to the lack of HST images in different bands, we applied the dust masking method which was developed in Thater et al (2017). The method is based on the assumptions 1) that the presence of dust attenuates the light emitted within the galaxy and 2) the major part of the galaxy surface brightness is not significantly affected by dust.…”

Section: Appendix A1: Hst Imagesmentioning

confidence: 99%

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

Thater

Krajnović

Cappellari

et al. 2019

A&A

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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 co-evolution. 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 combine 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 build 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) × 10 8 M for NGC 584, (1.0 ± 0.6) × 10 8 M for NGC 2784, (7.7 ± 5) × 10 7 M for NGC 3640, (5.4 ± 0.8) × 10 8 M for NGC 4281, (6.8 ± 2.0) × 10 7 M for NGC 4570 and (3.2 ± 0.8) × 10 8 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.

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Section: The Mass Modelmentioning

confidence: 99%

Section: Variations In Stellar Populationsmentioning

confidence: 99%

Section: Variations In Stellar Populationsmentioning

confidence: 99%

Section: Appendix A: Dust Correction and Maskingmentioning

confidence: 99%

Section: Appendix A1: Hst Imagesmentioning

confidence: 99%

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

Thater

Krajnović

Cappellari

et al. 2019

A&A

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Testing the robustness of DYNAMITE triaxial Schwarzschild modelling: The effects of correcting the orbit mirroring

Thater

Jethwa

Tahmasebzadeh

et al. 2022

A&A

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In the past 15 years, the triaxial Schwarzschild orbit-superposition code developed by van den Bosch and van de Ven in Leiden has been widely applied to study the dynamics of galaxies. Recently, a bug was reported in the orbit calculation of this code, specifically in the mirroring procedure that is used to speed up the computation. We have fixed the incorrect mirroring in the DYNAMITE code, which is the publicly-released successor of the Leiden triaxial Schwarzschild code. In this study, we provide a thorough quantification of how this bug has affected the results of dynamical analyses performed with this code. We compare results obtained with the original and corrected versions of DYNAMITE, and discuss the differences in the phase-space distribution of a single orbit and in the global stellar orbit distribution, in the mass estimate of the central black hole in the highly triaxial galaxy PGC 46832, and in the measurement of intrinsic shape and enclosed mass for more than 50 galaxies. Focusing on the typical scientific applications of the Schwarzschild method, in all our tests we find that differences are negligible with respect to the statistical and systematic uncertainties. We conclude that previous results with the Leiden triaxial Schwarzschild code are not significantly affected by the incorrect mirroring.

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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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A low upper mass limit for the central black hole in the late-type galaxy NGC 4414

Cited by 23 publications

References 104 publications

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

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

Testing the robustness of DYNAMITE triaxial Schwarzschild modelling: The effects of correcting the orbit mirroring

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

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