Brown Dwarf Candidates in the JADES and CEERS Extragalactic Surveys
Fuente:
arXiv
Saved in:
| Main Authors: | , , , , , , , , , , , , , , , |
|---|---|
| Format: | Preprint |
| Published: |
2023
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866929216172326912 |
|---|---|
| author | Hainline, Kevin N. Helton, Jakob M. Johnson, Benjamin D. Sun, Fengwu Topping, Michael W. Leisenring, Jarron M. Baker, William M. Eisenstein, Daniel J. Hausen, Ryan Hviding, Raphael E. Lyu, Jianwei Robertson, Brant Tacchella, Sandro Williams, Christina C. Willmer, Christopher N. A. Roellig, Thomas L. |
| author_facet | Hainline, Kevin N. Helton, Jakob M. Johnson, Benjamin D. Sun, Fengwu Topping, Michael W. Leisenring, Jarron M. Baker, William M. Eisenstein, Daniel J. Hausen, Ryan Hviding, Raphael E. Lyu, Jianwei Robertson, Brant Tacchella, Sandro Williams, Christina C. Willmer, Christopher N. A. Roellig, Thomas L. |
| contents | By combining the JWST/NIRCam JADES and CEERS extragalactic datasets, we have uncovered a sample of twenty-one T and Y brown dwarf candidates at best-fit distances between 0.1 - 4.2 kpc. These sources were selected by targeting the blue 1$μ$m - 2.5$μ$m colors and red 3$μ$m - 4.5$μ$m colors that arise from molecular absorption in the atmospheres of T$_{\mathrm{eff}} < $ 1300K brown dwarfs. We fit these sources using multiple models of low-mass stellar atmospheres and present the resulting fluxes, sizes, effective temperatures and other derived properties for the sample. If confirmed, these fits place the majority of the sources in the Milky Way thick disk and halo. We observe proper motion for seven of the candidate brown dwarfs with directions in agreement with the plane of our galaxy, providing evidence that they are not extragalactic in nature. We demonstrate how the colors of these sources differ from selected high-redshift galaxies, and explore the selection of these sources in planned large-area JWST NIRCam surveys. Deep imaging with JWST/NIRCam presents an an excellent opportunity for finding and understanding these very cold low-mass stars at kpc distances. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2309_03250 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Brown Dwarf Candidates in the JADES and CEERS Extragalactic Surveys Hainline, Kevin N. Helton, Jakob M. Johnson, Benjamin D. Sun, Fengwu Topping, Michael W. Leisenring, Jarron M. Baker, William M. Eisenstein, Daniel J. Hausen, Ryan Hviding, Raphael E. Lyu, Jianwei Robertson, Brant Tacchella, Sandro Williams, Christina C. Willmer, Christopher N. A. Roellig, Thomas L. Solar and Stellar Astrophysics Astrophysics of Galaxies By combining the JWST/NIRCam JADES and CEERS extragalactic datasets, we have uncovered a sample of twenty-one T and Y brown dwarf candidates at best-fit distances between 0.1 - 4.2 kpc. These sources were selected by targeting the blue 1$μ$m - 2.5$μ$m colors and red 3$μ$m - 4.5$μ$m colors that arise from molecular absorption in the atmospheres of T$_{\mathrm{eff}} < $ 1300K brown dwarfs. We fit these sources using multiple models of low-mass stellar atmospheres and present the resulting fluxes, sizes, effective temperatures and other derived properties for the sample. If confirmed, these fits place the majority of the sources in the Milky Way thick disk and halo. We observe proper motion for seven of the candidate brown dwarfs with directions in agreement with the plane of our galaxy, providing evidence that they are not extragalactic in nature. We demonstrate how the colors of these sources differ from selected high-redshift galaxies, and explore the selection of these sources in planned large-area JWST NIRCam surveys. Deep imaging with JWST/NIRCam presents an an excellent opportunity for finding and understanding these very cold low-mass stars at kpc distances. |
| title | Brown Dwarf Candidates in the JADES and CEERS Extragalactic Surveys |
| topic | Solar and Stellar Astrophysics Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2309.03250 |