SDSS-IV MaNGA: Stellar rotational support in disk galaxies vs. central surface density and stellar population age
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| Main Authors: | , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866912009774170112 |
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| author | Wang, Xiaohan Luo, Yifei Faber, S. M. Koo, David C. Mao, Shude Westfall, Kyle B. Lu, Shengdong Wang, Weichen Bundy, Kevin Boardman, N. Avila-Reese, Vladimir Fernández-Trincado, José G. Lane, Richard R. |
| author_facet | Wang, Xiaohan Luo, Yifei Faber, S. M. Koo, David C. Mao, Shude Westfall, Kyle B. Lu, Shengdong Wang, Weichen Bundy, Kevin Boardman, N. Avila-Reese, Vladimir Fernández-Trincado, José G. Lane, Richard R. |
| contents | We investigate how the stellar rotational support changes as a function of spatially resolved stellar population age ($\rm D_n4000$) and relative central stellar surface density ($ΔΣ_1$) for MaNGA isolated/central disk galaxies. We find that the galaxy rotational support $λ_{R_\mathrm{e}}$ varies smoothly as a function of $ΔΣ_1$ and $\rm D_n4000$. $\rm D_n4000$ vs. $ΔΣ_1$ follows a "J-shape", with $λ_{R_\mathrm{e}}$ contributing to the scatters. In this "J-shaped" pattern rotational support increases with central $\rm D_n4000$ when $ΔΣ_1$ is low but decreases with $ΔΣ_1$ when $ΔΣ_1$ is high. Restricting attention to low-$ΔΣ_1$ (i.e, large-radius) galaxies, we suggest that the trend of increasing rotational support with $\rm D_n4000$ for these objects is produced by a mix of two different processes, a primary trend characterized by growth in $λ_{R_\mathrm{e}}$ along with mass through gas accretion, on top of which disturbance episodes are overlaid, which reduce rotational support and trigger increased star formation. An additional finding is that star forming galaxies with low $ΔΣ_1$ have relatively larger radii than galaxies with higher $ΔΣ_1$ at fixed stellar mass. Assuming that these relative radii rankings are preserved while galaxies are star forming then implies clear evolutionary paths in central $\rm D_n4000$ vs. $ΔΣ_1$. The paper closes with comments on the implications that these paths have for the evolution of pseudo-bulges vs. classical-bulges. The utility of using $\rm D_n4000$-$ΔΣ_1$ to study $λ_{R_\mathrm{e}}$ reinforces the notion that galaxy kinematics correlate both with structure and with stellar-population state, and indicates the importance of a multi-dimensional description for understanding bulge and galaxy evolution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_02669 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | SDSS-IV MaNGA: Stellar rotational support in disk galaxies vs. central surface density and stellar population age Wang, Xiaohan Luo, Yifei Faber, S. M. Koo, David C. Mao, Shude Westfall, Kyle B. Lu, Shengdong Wang, Weichen Bundy, Kevin Boardman, N. Avila-Reese, Vladimir Fernández-Trincado, José G. Lane, Richard R. Astrophysics of Galaxies We investigate how the stellar rotational support changes as a function of spatially resolved stellar population age ($\rm D_n4000$) and relative central stellar surface density ($ΔΣ_1$) for MaNGA isolated/central disk galaxies. We find that the galaxy rotational support $λ_{R_\mathrm{e}}$ varies smoothly as a function of $ΔΣ_1$ and $\rm D_n4000$. $\rm D_n4000$ vs. $ΔΣ_1$ follows a "J-shape", with $λ_{R_\mathrm{e}}$ contributing to the scatters. In this "J-shaped" pattern rotational support increases with central $\rm D_n4000$ when $ΔΣ_1$ is low but decreases with $ΔΣ_1$ when $ΔΣ_1$ is high. Restricting attention to low-$ΔΣ_1$ (i.e, large-radius) galaxies, we suggest that the trend of increasing rotational support with $\rm D_n4000$ for these objects is produced by a mix of two different processes, a primary trend characterized by growth in $λ_{R_\mathrm{e}}$ along with mass through gas accretion, on top of which disturbance episodes are overlaid, which reduce rotational support and trigger increased star formation. An additional finding is that star forming galaxies with low $ΔΣ_1$ have relatively larger radii than galaxies with higher $ΔΣ_1$ at fixed stellar mass. Assuming that these relative radii rankings are preserved while galaxies are star forming then implies clear evolutionary paths in central $\rm D_n4000$ vs. $ΔΣ_1$. The paper closes with comments on the implications that these paths have for the evolution of pseudo-bulges vs. classical-bulges. The utility of using $\rm D_n4000$-$ΔΣ_1$ to study $λ_{R_\mathrm{e}}$ reinforces the notion that galaxy kinematics correlate both with structure and with stellar-population state, and indicates the importance of a multi-dimensional description for understanding bulge and galaxy evolution. |
| title | SDSS-IV MaNGA: Stellar rotational support in disk galaxies vs. central surface density and stellar population age |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.02669 |