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| Main Authors: | , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| Online Access: | https://arxiv.org/abs/2504.02755 |
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| _version_ | 1866909563490402304 |
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| author | Cano-DÍaz, M. Rodríguez-Puebla, A. Robleto-Orús, A. C. Ávila-Reese, V. Hernández-Toledo, H. M. Vázquez-Mata, J. A. Valenzuela, O. González, J. J. Ibarra-Medel, H. J. Clemente-González, J. C. Pavón-Alvarez, L. |
| author_facet | Cano-DÍaz, M. Rodríguez-Puebla, A. Robleto-Orús, A. C. Ávila-Reese, V. Hernández-Toledo, H. M. Vázquez-Mata, J. A. Valenzuela, O. González, J. J. Ibarra-Medel, H. J. Clemente-González, J. C. Pavón-Alvarez, L. |
| contents | We derived radial profiles and inner/outer gradients of various stellar population (SP) properties for 124 bright dwarf galaxies, $10^{7.53}\leq M_*/M_\odot\leq 10^{9.06}$, from the MaNDala sample, using integral field spectroscopy observations. Given the complex structure of dwarf galaxies, we used four different methods to derive SP radial profiles: two based on concentric elliptical rings, and two exploiting the spatially resolved data. For each method, we applied four approaches to calculate the inner ($0 \leq R/R_e \leq 1$) and outer ($0.75 \leq R/R_e \leq 1.5$) gradients of: luminosity- and mass-weighted age and stellar metallicity, dust attenuation, $D_{n4000}$ index, stellar mass and star formation rate (SFR) surface densities, and specific SFR. While the PSF has a minor impact on the SP gradients, the methodology for characterizing radial profiles significantly affects them. At fixed property, differences in inner gradients from concentric rings methods are $\sim0.05\text{-}0.1 \text{ dex/}R_e$, while outer gradients can reach $0.5\text{-}1 \text{ dex/}R_e$, relative to the median of all gradients of that property, $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$. Spatially resolved methods yield smaller differences, $\lesssim0.1 \text{ dex/}R_e$. For some SP gradients, e.g. $\nabla_\text{SFR}$, the dispersion among the methods is comparable to $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$. While it is not possible to select a single preferred method for determining SP gradients, we suggest to use $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$ for each SP property. The resulting median age and metallicity suggest that, overall, bright dwarfs experienced moderate inside-out formation, and significant early SF from low-metallicity gas with outward radial migration of old SPs. The derived SP gradients provide strong constraints on feedback mechanisms in dwarf galaxies. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_02755 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The MaNGA Dwarf Galaxy Sample (MaNDala): stellar profiles and gradients characterization Cano-DÍaz, M. Rodríguez-Puebla, A. Robleto-Orús, A. C. Ávila-Reese, V. Hernández-Toledo, H. M. Vázquez-Mata, J. A. Valenzuela, O. González, J. J. Ibarra-Medel, H. J. Clemente-González, J. C. Pavón-Alvarez, L. Astrophysics of Galaxies We derived radial profiles and inner/outer gradients of various stellar population (SP) properties for 124 bright dwarf galaxies, $10^{7.53}\leq M_*/M_\odot\leq 10^{9.06}$, from the MaNDala sample, using integral field spectroscopy observations. Given the complex structure of dwarf galaxies, we used four different methods to derive SP radial profiles: two based on concentric elliptical rings, and two exploiting the spatially resolved data. For each method, we applied four approaches to calculate the inner ($0 \leq R/R_e \leq 1$) and outer ($0.75 \leq R/R_e \leq 1.5$) gradients of: luminosity- and mass-weighted age and stellar metallicity, dust attenuation, $D_{n4000}$ index, stellar mass and star formation rate (SFR) surface densities, and specific SFR. While the PSF has a minor impact on the SP gradients, the methodology for characterizing radial profiles significantly affects them. At fixed property, differences in inner gradients from concentric rings methods are $\sim0.05\text{-}0.1 \text{ dex/}R_e$, while outer gradients can reach $0.5\text{-}1 \text{ dex/}R_e$, relative to the median of all gradients of that property, $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$. Spatially resolved methods yield smaller differences, $\lesssim0.1 \text{ dex/}R_e$. For some SP gradients, e.g. $\nabla_\text{SFR}$, the dispersion among the methods is comparable to $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$. While it is not possible to select a single preferred method for determining SP gradients, we suggest to use $\text{med}\left(\{\nabla \mathcal{G}\}_i\right)$ for each SP property. The resulting median age and metallicity suggest that, overall, bright dwarfs experienced moderate inside-out formation, and significant early SF from low-metallicity gas with outward radial migration of old SPs. The derived SP gradients provide strong constraints on feedback mechanisms in dwarf galaxies. |
| title | The MaNGA Dwarf Galaxy Sample (MaNDala): stellar profiles and gradients characterization |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.02755 |