The Baryonic Tully-Fisher Relation II: Stellar Mass Models
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| Main Authors: | , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866916572020342784 |
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| author | Duey, Francis Schombert, James McGaugh, Stacy Lelli, Federico |
| author_facet | Duey, Francis Schombert, James McGaugh, Stacy Lelli, Federico |
| contents | We present new color-$Υ_*$ (mass-to-light) models to convert WISE W1 fluxes into stellar masses. We outline a range of possible star formation histories and chemical evolution scenarios to explore the confidence limits of stellar population models on the value of $Υ_*$. We conclude that the greatest uncertainties (around 0.1 dex in $Υ_*$) occur for the bluest galaxies with the strongest variation in recent star formation. For high mass galaxies, the greatest uncertainty arises from the proper treatment of bulge/disk separation in which to apply different $Υ_*$ relations appropriate for those differing underlying stellar populations. We compare our deduced stellar masses with those deduced from {\it Spitzer} 3.6$μ$m fluxes and stellar mass estimates in the literature using optical photometry and different $Υ_*$ modeling. We find the correspondence to be excellent, arguing that rest-frame near-IR photometry is still more advantageous than other wavelengths. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2501_10919 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | The Baryonic Tully-Fisher Relation II: Stellar Mass Models Duey, Francis Schombert, James McGaugh, Stacy Lelli, Federico Astrophysics of Galaxies We present new color-$Υ_*$ (mass-to-light) models to convert WISE W1 fluxes into stellar masses. We outline a range of possible star formation histories and chemical evolution scenarios to explore the confidence limits of stellar population models on the value of $Υ_*$. We conclude that the greatest uncertainties (around 0.1 dex in $Υ_*$) occur for the bluest galaxies with the strongest variation in recent star formation. For high mass galaxies, the greatest uncertainty arises from the proper treatment of bulge/disk separation in which to apply different $Υ_*$ relations appropriate for those differing underlying stellar populations. We compare our deduced stellar masses with those deduced from {\it Spitzer} 3.6$μ$m fluxes and stellar mass estimates in the literature using optical photometry and different $Υ_*$ modeling. We find the correspondence to be excellent, arguing that rest-frame near-IR photometry is still more advantageous than other wavelengths. |
| title | The Baryonic Tully-Fisher Relation II: Stellar Mass Models |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2501.10919 |