Converging on the Cepheid Metallicity Dependence: Implications of Non-Standard Gaia Parallax Recalibration on Distance Measures
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| Autores principales: | , , , , , , , , , , , , , , , , , , , , , , |
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| Formato: | Preprint |
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2025
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| author | Breuval, Louise Anand, Gagandeep S. Anderson, Richard I. Beaton, Rachael Bhardwaj, Anupam Casertano, Stefano Clementini, Gisella Reyes, Mauricio Cruz De Somma, Giulia Groenewegen, Martin A. T. Huang, Caroline D. Kervella, Pierre Khan, Saniya Macri, Lucas M. Marconi, Marcella Minniti, Javier H. Riess, Adam G. Ripepi, Vincenzo Romaniello, Martino Scolnic, Daniel Trentin, Erasmo Wielgorski, Piotr Yuan, Wenlong |
| author_facet | Breuval, Louise Anand, Gagandeep S. Anderson, Richard I. Beaton, Rachael Bhardwaj, Anupam Casertano, Stefano Clementini, Gisella Reyes, Mauricio Cruz De Somma, Giulia Groenewegen, Martin A. T. Huang, Caroline D. Kervella, Pierre Khan, Saniya Macri, Lucas M. Marconi, Marcella Minniti, Javier H. Riess, Adam G. Ripepi, Vincenzo Romaniello, Martino Scolnic, Daniel Trentin, Erasmo Wielgorski, Piotr Yuan, Wenlong |
| contents | By comparing Cepheid brightnesses with geometric distance measures including Gaia EDR3 parallaxes, most recent analyses conclude metal-rich Cepheids are brighter, quantified as $γ\sim -0.2$ mag/dex. While the value of $γ$ has little impact on the determination of the Hubble constant in contemporary distance ladders (due to the similarity of metallicity across these ladders), $γ$ plays a role in gauging the distances to metal-poor dwarf galaxies like the Magellanic Clouds and is of considerable interest in testing stellar models. Recently, Madore & Freedman (2025, hereafter MF25) recalibrated Gaia EDR3 parallaxes by adding to them a magnitude offset to match certain historic Cepheid parallaxes which otherwise differ by $\sim1.6σ$. A calibration which adjusts Gaia parallaxes by applying a magnitude offset (i.e., a multiplicative correction in parallax) differs significantly from the Gaia Team's calibration (Lindegren et al. 2021), which is additive in parallax space - especially at distances much closer than 1 kpc or beyond 10 kpc, outside the $\sim$2-3 kpc range on which the MF25 calibration was based. The MF25 approach reduces $γ$ to zero. If extrapolated, it places nearby cluster distances like the Pleiades too close compared to independent measurements, while leaving distant quasars with negative parallaxes. We conclude that the MF25 proposal for Gaia calibration and $γ\sim 0$ produces farther-reaching consequences, many of which are strongly disfavored by the data. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_15936 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Converging on the Cepheid Metallicity Dependence: Implications of Non-Standard Gaia Parallax Recalibration on Distance Measures Breuval, Louise Anand, Gagandeep S. Anderson, Richard I. Beaton, Rachael Bhardwaj, Anupam Casertano, Stefano Clementini, Gisella Reyes, Mauricio Cruz De Somma, Giulia Groenewegen, Martin A. T. Huang, Caroline D. Kervella, Pierre Khan, Saniya Macri, Lucas M. Marconi, Marcella Minniti, Javier H. Riess, Adam G. Ripepi, Vincenzo Romaniello, Martino Scolnic, Daniel Trentin, Erasmo Wielgorski, Piotr Yuan, Wenlong Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics Solar and Stellar Astrophysics By comparing Cepheid brightnesses with geometric distance measures including Gaia EDR3 parallaxes, most recent analyses conclude metal-rich Cepheids are brighter, quantified as $γ\sim -0.2$ mag/dex. While the value of $γ$ has little impact on the determination of the Hubble constant in contemporary distance ladders (due to the similarity of metallicity across these ladders), $γ$ plays a role in gauging the distances to metal-poor dwarf galaxies like the Magellanic Clouds and is of considerable interest in testing stellar models. Recently, Madore & Freedman (2025, hereafter MF25) recalibrated Gaia EDR3 parallaxes by adding to them a magnitude offset to match certain historic Cepheid parallaxes which otherwise differ by $\sim1.6σ$. A calibration which adjusts Gaia parallaxes by applying a magnitude offset (i.e., a multiplicative correction in parallax) differs significantly from the Gaia Team's calibration (Lindegren et al. 2021), which is additive in parallax space - especially at distances much closer than 1 kpc or beyond 10 kpc, outside the $\sim$2-3 kpc range on which the MF25 calibration was based. The MF25 approach reduces $γ$ to zero. If extrapolated, it places nearby cluster distances like the Pleiades too close compared to independent measurements, while leaving distant quasars with negative parallaxes. We conclude that the MF25 proposal for Gaia calibration and $γ\sim 0$ produces farther-reaching consequences, many of which are strongly disfavored by the data. |
| title | Converging on the Cepheid Metallicity Dependence: Implications of Non-Standard Gaia Parallax Recalibration on Distance Measures |
| topic | Astrophysics of Galaxies Cosmology and Nongalactic Astrophysics Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2507.15936 |