Saved in:
| Main Authors: | , , , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2023
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2310.00497 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866916381283319808 |
|---|---|
| author | Tahmasebzadeh, Behzad Zhu, Ling Shen, Juntai Gadotti, Dimitri A. Valluri, Monica Thater, Sabine van de Ven, Glenn Jin, Yunpeng Gerhard, Ortwin Erwin, Peter Jethwa, Prashin Zocchi, Alice Lilley, Edward J. Fragkoudi, Francesca de Lorenzo-Cáceres, Adriana Méndez-Abreu, Jairo Neumann, Justus Guo, Rui |
| author_facet | Tahmasebzadeh, Behzad Zhu, Ling Shen, Juntai Gadotti, Dimitri A. Valluri, Monica Thater, Sabine van de Ven, Glenn Jin, Yunpeng Gerhard, Ortwin Erwin, Peter Jethwa, Prashin Zocchi, Alice Lilley, Edward J. Fragkoudi, Francesca de Lorenzo-Cáceres, Adriana Méndez-Abreu, Jairo Neumann, Justus Guo, Rui |
| contents | We apply the barred Schwarzschild method developed by Tahmasebzadeh et al. (2022) to a barred S0 galaxy, NGC 4371, observed by IFU instruments from the TIMER and ATLAS3D projects. We construct the gravitational potential by combining a fixed black hole mass, a spherical dark matter halo, and stellar mass distribution deprojected from $3.6$ $μ$m S$^4$G image considering an axisymmetric disk and a triaxial bar. We independently modelled kinematic data from TIMER and ATLAS3D. Both models fit the data remarkably well. We find a consistent bar pattern speed from the two sets of models with $Ω_{\rm p} = 23.6 \pm 2.8 \hspace{.08cm} \mathrm{km \hspace{.04cm} s^{-1} \hspace{.04cm} kpc^{-1} }$ and $Ω_{\rm p} = 22.4 \pm 3.5 \hspace{.08cm} \mathrm{km \hspace{.04cm} s^{-1} \hspace{.04cm} kpc^{-1} }$, respectively. The dimensionless bar rotation parameter is determined to be $ 1.88 \pm 0.37$, indicating a likely slow bar in NGC 4371. Additionally, our model predicts a high amount of dark matter within the bar region ($M_{\rm DM}/ M_{\rm total}$ $\sim 0.51 \pm 0.06$), which, aligned with the predictions of cosmological simulations, indicates that fast bars are generally found in baryon-dominated disks. Based on the best-fitting model, we further decompose the galaxy into multiple 3D orbital structures, including a BP/X bar, a classical bulge, a nuclear disk, and a main disk. The BP/X bar is not perfectly included in the input 3D density model, but BP/X-supporting orbits are picked through the fitting to the kinematic data. This is the first time a real barred galaxy has been modelled utilizing the Schwarzschild method including a 3D bar. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2310_00497 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Schwarzschild Modeling of Barred S0 Galaxy NGC 4371 Tahmasebzadeh, Behzad Zhu, Ling Shen, Juntai Gadotti, Dimitri A. Valluri, Monica Thater, Sabine van de Ven, Glenn Jin, Yunpeng Gerhard, Ortwin Erwin, Peter Jethwa, Prashin Zocchi, Alice Lilley, Edward J. Fragkoudi, Francesca de Lorenzo-Cáceres, Adriana Méndez-Abreu, Jairo Neumann, Justus Guo, Rui Astrophysics of Galaxies We apply the barred Schwarzschild method developed by Tahmasebzadeh et al. (2022) to a barred S0 galaxy, NGC 4371, observed by IFU instruments from the TIMER and ATLAS3D projects. We construct the gravitational potential by combining a fixed black hole mass, a spherical dark matter halo, and stellar mass distribution deprojected from $3.6$ $μ$m S$^4$G image considering an axisymmetric disk and a triaxial bar. We independently modelled kinematic data from TIMER and ATLAS3D. Both models fit the data remarkably well. We find a consistent bar pattern speed from the two sets of models with $Ω_{\rm p} = 23.6 \pm 2.8 \hspace{.08cm} \mathrm{km \hspace{.04cm} s^{-1} \hspace{.04cm} kpc^{-1} }$ and $Ω_{\rm p} = 22.4 \pm 3.5 \hspace{.08cm} \mathrm{km \hspace{.04cm} s^{-1} \hspace{.04cm} kpc^{-1} }$, respectively. The dimensionless bar rotation parameter is determined to be $ 1.88 \pm 0.37$, indicating a likely slow bar in NGC 4371. Additionally, our model predicts a high amount of dark matter within the bar region ($M_{\rm DM}/ M_{\rm total}$ $\sim 0.51 \pm 0.06$), which, aligned with the predictions of cosmological simulations, indicates that fast bars are generally found in baryon-dominated disks. Based on the best-fitting model, we further decompose the galaxy into multiple 3D orbital structures, including a BP/X bar, a classical bulge, a nuclear disk, and a main disk. The BP/X bar is not perfectly included in the input 3D density model, but BP/X-supporting orbits are picked through the fitting to the kinematic data. This is the first time a real barred galaxy has been modelled utilizing the Schwarzschild method including a 3D bar. |
| title | Schwarzschild Modeling of Barred S0 Galaxy NGC 4371 |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2310.00497 |