Dynamical Modeling of Galaxies and Supermassive Black Holes: Axisymmetry in Triaxial Schwarzschild Orbit Superposition Models

Quenneville, Matthew E.; Liepold, Christopher M.; Ma, Chung‐Pei

doi:10.3847/1538-4365/abe6a0

Cited by 13 publications

(23 citation statements)

References 47 publications

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“…Using the homogeneous set of subarcsecond and wide-field IFS and photometric data as constraints, the MASSIVE collaboration is performing dynamical mass modeling of the supermassive BHs (SMBHs), stars, and dark matter components for a sample of MASSIVE galaxies (Liepold et al 2020;Quenneville et al 2021). Accurate and precise distances are essential to measuring the most fundamental properties of massive ETGs and their central BHs, including their masses.…”

Section: The Massive Surveymentioning

confidence: 99%

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Jensen

Blakeslee

et al. 2021

ApJS

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We measured high-quality surface brightness fluctuation (SBF) distances for a sample of 63 massive early-type galaxies using the WFC3/IR camera on the Hubble Space Telescope. The median uncertainty on the SBF distance measurements is 0.085 mag, or 3.9% in distance. Achieving this precision at distances of 50–100 Mpc required significant improvements to the SBF calibration and data analysis procedures for WFC3/IR data. Forty-two of the galaxies are from the MASSIVE Galaxy Survey, a complete sample of massive galaxies within ∼100 Mpc; the SBF distances for these will be used to improve the estimates of the stellar and central supermassive black hole masses in these galaxies. Twenty-four of the galaxies are Type Ia supernova hosts, useful for calibrating SN Ia distances for early-type galaxies and exploring possible systematic trends in the peak luminosities. Our results demonstrate that the SBF method is a powerful and versatile technique for measuring distances to galaxies with evolved stellar populations out to 100 Mpc and constraining the local value of the Hubble constant.

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Section: The Massive Surveymentioning

confidence: 99%

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Jensen

Blakeslee

et al. 2021

ApJS

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“…As a first application of this code, we performed triaxial orbit modeling of the massive elliptical galaxy NGC 1453 and presented the best-fit galaxy shape and mass parameters. This work complements Liepold et al (2020) and Quenneville et al (2021), in which we introduced a properly axisymmetrized version of the TriOS code.…”

Section: Discussionmentioning

confidence: 98%

“…Outside of these special cases, the orbital kinematics have significant errors. The incorrect flips were not used in our axisymmetric modelling of NGC 1453 (Liepold et al 2020;Quenneville et al 2021) since we used an axisymmetrization procedure in place of the flips in the TriOS code.…”

Section: Correct Orbital Mirroring Mistakesmentioning

confidence: 99%

“…For a triaxial model, the short-axis tubes (red points in Figure 4) and long-axis tubes (blue points) occupy two regions of the x − z start space separated by the focal curve. As derived in Appendix A of Quenneville et al (2021), the focal curve is roughly approximated by…”

Section: Resolve Issues With Insufficient Orbit Samplingmentioning

confidence: 99%

“…In the axisymmetrized TriOS code (Quenneville et al 2021), we changed the radial binning scheme above to ensure sufficient orbits are used to represent the innermost and outermost mass bins. During our subsequent tests for triaxial systems, however, we noticed occasional problems with mass misfits in which a handful mass bins would have difficulty satisfying the 1% precision and/or contribute disproportionately high values to the total χ 2 of the galaxy model under examination.…”

Section: Improve Intrinsic Mass Binning Schemementioning

confidence: 99%

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Triaxial Orbit-based Dynamical Modeling of Galaxies with Supermassive Black Holes and an Application to Massive Elliptical Galaxy NGC 1453

Quenneville,

Liepold,

2021

Preprint

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Most stellar-dynamical determinations of the masses of nearby supermassive black holes (SMBHs) have been obtained with the orbit superposition technique under the assumption of axisymmetry. However, few galaxies -in particular massive early-type galaxies -obey exact axisymmetry. Here we present a revised orbit superposition code and a new approach for dynamically determining the intrinsic shapes and mass parameters of triaxial galaxies based on spatially-resolved stellar kinematic data. The triaxial TriOS code described here corrects a major error in the original van den Bosch et al. ( 2008) code that gives rise to incorrect projections for most orbits in triaxial models and can significantly impact parameter search results. The revised code also contains significant improvements in orbit sampling, mass constraints, and run time. Furthermore, we introduce two new parameter searching strategies -a new set of triaxial shape parameters and a novel grid-free sampling technique -that together lead to a remarkable gain in efficiency in locating the best-fit model. We apply the updated code and search method to NGC 1453, a fast-rotating massive elliptical galaxy. A full 6D parameter search finds p = b/a = 0.933 +0.014 −0.015 and q = c/a = 0.779 ± 0.012 for the intrinsic axis ratios and T = 0.33±0.06 for the triaxiality parameter. Despite the deviations from axisymmetry, the best-fit SMBH mass, stellar mass-to-light ratio, and dark matter enclosed mass for NGC 1453 are consistent with the axisymmetric results. More comparisons between axisymmetric and triaxial modeling are needed before drawing general conclusions.

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Quantifying the stellar ages of dynamically separated bulges and disks of CALIFA spiral galaxies

Jin,

Zhu,

Zibetti

et al. 2024

A&A

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We employ a recently developed population-orbit superposition technique to simultaneously fit the stellar kinematic and age maps of 82 CALIFA spiral galaxies and obtain the ages of stars in different dynamical structures. We first evaluated the capabilities of this method on CALIFA-like mock data created from the Auriga simulations. The recovered mean ages of dynamically cold, warm, and hot components match the true values well, with an observational error of up to $20<!PCT!>$ in the mock age maps. For CALIFA spiral galaxies, we find that the stellar ages of the cold, warm, and hot components all increase with the stellar mass of the galaxies, from $ t_ cold Gyr, $ t_ warm Gyr, and $ t_ hot Gyr for galaxies with stellar mass odot $, to $ t_ cold Gyr, $ t_ warm Gyr, and $ t_ hot Gyr for galaxies with odot $. About $80<!PCT!>$ of the galaxies in our sample have $t_ hot >t_ cold $, and the mean values of $t_ hot -t_ cold $ also increase with stellar mass, from $0.7_ $ Gyr in low-mass galaxies ($10^ odot <M_* odot $) to $1.7_ $ Gyr in high-mass galaxies ($10^ odot <M_*<10^ odot $). The stellar age is younger in disks than in bulges, on average. This suggests that either the disks formed later and/or that they experienced a more prolonged and extensive period of star formation. Lower-mass spiral galaxies have younger bulges and younger disks, while higher-mass spiral galaxies generally have older bulges, and their disks span a wide range of ages. This is consistent with the scenario in which the bulges in more massive spirals formed earlier than those in less massive spirals.

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Dynamical Modeling of Galaxies and Supermassive Black Holes: Axisymmetry in Triaxial Schwarzschild Orbit Superposition Models

Cited by 13 publications

References 47 publications

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Infrared Surface Brightness Fluctuation Distances for MASSIVE and Type Ia Supernova Host Galaxies*

Triaxial Orbit-based Dynamical Modeling of Galaxies with Supermassive Black Holes and an Application to Massive Elliptical Galaxy NGC 1453

Quantifying the stellar ages of dynamically separated bulges and disks of CALIFA spiral galaxies

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