HELM's deep: Highly Extincted Low-Mass galaxies seen by JWST
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arXiv
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| Autori principali: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
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| Natura: | Preprint |
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2025
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| author | Bisigello, L. Gandolfi, G. Grazian, A. Rodighiero, G. Girardi, G. Renzini, A. Vietri, A. McGrath, E. Holwerda, B. Abdurro'uf Castellano, M. Giulietti, M. Gruppioni, C. Hathi, N. Koekemoer, A. M. Lucas, R. Pacucci, F. Pérez-González, P. G. Yung, L. Y. A. Haro, P. Arrabal Backhaus, B. E. Bagley, M. Dickinson, M. Finkelstein, S. Kartaltepe, J. Kirkpatrick, A. Papovich, C. Pirzkal, N. |
| author_facet | Bisigello, L. Gandolfi, G. Grazian, A. Rodighiero, G. Girardi, G. Renzini, A. Vietri, A. McGrath, E. Holwerda, B. Abdurro'uf Castellano, M. Giulietti, M. Gruppioni, C. Hathi, N. Koekemoer, A. M. Lucas, R. Pacucci, F. Pérez-González, P. G. Yung, L. Y. A. Haro, P. Arrabal Backhaus, B. E. Bagley, M. Dickinson, M. Finkelstein, S. Kartaltepe, J. Kirkpatrick, A. Papovich, C. Pirzkal, N. |
| contents | The dust content of star-forming galaxies is generally positively correlated with their stellar mass. However, some recent JWST studies have shown the existence of a population of dwarf galaxies with an unexpectedly large dust attenuation. Using the Cosmic Evolution Early Release Science Survey (CEERS) data, we identified a sample of 1361 highly extincted low-mass (HELM) galaxies, defined as dwarf galaxies ($M_*<10^{8.5}$) with Av>1mag or more massive galaxies with an exceptionally high dust attenuation given their stellar mass (i.e., $Av>1.6log_{10}(M_*/Mo)-12.6$). The selection is performed using the multiparameter distribution obtained through a comprehensive spectral energy distribution fitting analysis, based on optical to near-infrared data. After excluding possible contaminants, like brown dwarfs, little red dots, high-z (z>8.5) and ultra-high-z (z>15) galaxies, the sample mainly includes sources at z<1, with a tail extending up to z=7.2. The sample has a median stellar mass of $10^7$ Mo and a median dust attenuation of Av=2mag. We analysed the morphology, environment and star-formation rate of these sources to investigate the reason of their large dust attenuation. In particular, HELM sources have sizes (effective radii, Re) similar to non-dusty dwarf galaxies and no correlation is visible between the axis ratios (b/a) and the dust attenuation. This findings indicate that it is unlikely that the large dust attenuation is due to projection effects, but a prolate or a disk-on oblate geometry are still possible, at least for a subsample of the sources. We have found that the distribution of HELM sources is slightly skewed toward more clustered environments than non-dusty dwarfs and tend to be slightly less star forming. This finding, if confirmed by spectroscopic follow-up, indicates that HELM sources could be going through some environmental processes, such as galaxy interactions. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2512_14822 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | HELM's deep: Highly Extincted Low-Mass galaxies seen by JWST Bisigello, L. Gandolfi, G. Grazian, A. Rodighiero, G. Girardi, G. Renzini, A. Vietri, A. McGrath, E. Holwerda, B. Abdurro'uf Castellano, M. Giulietti, M. Gruppioni, C. Hathi, N. Koekemoer, A. M. Lucas, R. Pacucci, F. Pérez-González, P. G. Yung, L. Y. A. Haro, P. Arrabal Backhaus, B. E. Bagley, M. Dickinson, M. Finkelstein, S. Kartaltepe, J. Kirkpatrick, A. Papovich, C. Pirzkal, N. Astrophysics of Galaxies The dust content of star-forming galaxies is generally positively correlated with their stellar mass. However, some recent JWST studies have shown the existence of a population of dwarf galaxies with an unexpectedly large dust attenuation. Using the Cosmic Evolution Early Release Science Survey (CEERS) data, we identified a sample of 1361 highly extincted low-mass (HELM) galaxies, defined as dwarf galaxies ($M_*<10^{8.5}$) with Av>1mag or more massive galaxies with an exceptionally high dust attenuation given their stellar mass (i.e., $Av>1.6log_{10}(M_*/Mo)-12.6$). The selection is performed using the multiparameter distribution obtained through a comprehensive spectral energy distribution fitting analysis, based on optical to near-infrared data. After excluding possible contaminants, like brown dwarfs, little red dots, high-z (z>8.5) and ultra-high-z (z>15) galaxies, the sample mainly includes sources at z<1, with a tail extending up to z=7.2. The sample has a median stellar mass of $10^7$ Mo and a median dust attenuation of Av=2mag. We analysed the morphology, environment and star-formation rate of these sources to investigate the reason of their large dust attenuation. In particular, HELM sources have sizes (effective radii, Re) similar to non-dusty dwarf galaxies and no correlation is visible between the axis ratios (b/a) and the dust attenuation. This findings indicate that it is unlikely that the large dust attenuation is due to projection effects, but a prolate or a disk-on oblate geometry are still possible, at least for a subsample of the sources. We have found that the distribution of HELM sources is slightly skewed toward more clustered environments than non-dusty dwarfs and tend to be slightly less star forming. This finding, if confirmed by spectroscopic follow-up, indicates that HELM sources could be going through some environmental processes, such as galaxy interactions. |
| title | HELM's deep: Highly Extincted Low-Mass galaxies seen by JWST |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2512.14822 |