Unveiling the trends between dust attenuation and galaxy properties at z ~ 2 - 12 with the James Webb Space Telescope
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| Autores principales: | , , , , , , , , , |
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2025
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| author | Markov, V. Gallerani, S. Pallottini, A. Bradac, M. Carniani, S. Tripodi, R. Noirot, G. Di Mascia, F. Parlanti, E. Martis, N. |
| author_facet | Markov, V. Gallerani, S. Pallottini, A. Bradac, M. Carniani, S. Tripodi, R. Noirot, G. Di Mascia, F. Parlanti, E. Martis, N. |
| contents | A variety of dust attenuation/extinction curves have been observed in high-redshift galaxies, with mixed results regarding their correlations with global galaxy properties. These variations are likely driven by factors such as intrinsic dust properties, total dust content, and the dust-star geometry. In this work, we explore how the shape of dust attenuation curves-quantified by the UV-optical slope (S) and UV bump strength (B)-correlates with galaxy properties. Our goal is to identify the key physical mechanisms shaping attenuation curves through cosmic time. We build on arXiv:2402.05996, analyzing 173 dusty galaxies at z ~ 2-11.5, with attenuation curves inferred via SED fitting of JWST data using a modified version of BAGPIPES (arXiv:2304.11178). We investigate trends between S, B, and properties inferred from SED fitting: AV, SFR, stellar mass (M*), specific SFR (sSFR), mass-weighted stellar age (a*), ionization parameter (U), and metallicity (Z). For a subset, we also consider oxygen abundance (12 + log(O/H)), derived via Te-based methods. We find that lower AV galaxies tend to have steeper slopes and stronger UV bumps, consistent with radiative transfer predictions involving dust geometry and content. S also correlates with a* and sSFR, suggesting that strong radiation fields in young, bursty galaxies may destroy small grains, flattening the slope. B correlates with 12 + log(O/H), possibly due to metallicity-driven dust composition changes. Overall, attenuation curve shapes appear most strongly linked to: (1) redshift (dust evolution), (2) AV (RT effects), (3) a* or sSFR (radiation field), and (4) oxygen abundance (dust composition). Disentangling these effects requires spatially resolved data and theoretical models including dust evolution. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2504_12378 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Unveiling the trends between dust attenuation and galaxy properties at z ~ 2 - 12 with the James Webb Space Telescope Markov, V. Gallerani, S. Pallottini, A. Bradac, M. Carniani, S. Tripodi, R. Noirot, G. Di Mascia, F. Parlanti, E. Martis, N. Astrophysics of Galaxies A variety of dust attenuation/extinction curves have been observed in high-redshift galaxies, with mixed results regarding their correlations with global galaxy properties. These variations are likely driven by factors such as intrinsic dust properties, total dust content, and the dust-star geometry. In this work, we explore how the shape of dust attenuation curves-quantified by the UV-optical slope (S) and UV bump strength (B)-correlates with galaxy properties. Our goal is to identify the key physical mechanisms shaping attenuation curves through cosmic time. We build on arXiv:2402.05996, analyzing 173 dusty galaxies at z ~ 2-11.5, with attenuation curves inferred via SED fitting of JWST data using a modified version of BAGPIPES (arXiv:2304.11178). We investigate trends between S, B, and properties inferred from SED fitting: AV, SFR, stellar mass (M*), specific SFR (sSFR), mass-weighted stellar age (a*), ionization parameter (U), and metallicity (Z). For a subset, we also consider oxygen abundance (12 + log(O/H)), derived via Te-based methods. We find that lower AV galaxies tend to have steeper slopes and stronger UV bumps, consistent with radiative transfer predictions involving dust geometry and content. S also correlates with a* and sSFR, suggesting that strong radiation fields in young, bursty galaxies may destroy small grains, flattening the slope. B correlates with 12 + log(O/H), possibly due to metallicity-driven dust composition changes. Overall, attenuation curve shapes appear most strongly linked to: (1) redshift (dust evolution), (2) AV (RT effects), (3) a* or sSFR (radiation field), and (4) oxygen abundance (dust composition). Disentangling these effects requires spatially resolved data and theoretical models including dust evolution. |
| title | Unveiling the trends between dust attenuation and galaxy properties at z ~ 2 - 12 with the James Webb Space Telescope |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2504.12378 |