Surface Brightness Bias in the Shape Statistics of High-Redshift Galaxies
Fuente:
arXiv
Saved in:
| Main Author: | |
|---|---|
| Format: | Preprint |
| Published: |
2024
|
| Subjects: | |
| Online Access: | |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866916099971350528 |
|---|---|
| author | Loeb, Abraham |
| author_facet | Loeb, Abraham |
| contents | Recently, Pandya et al. (2023) argued that the shapes of dwarf galaxies in JWST-CEERS observations show a prolate fraction that rises from ~25% at redshifts z=0.5-1 to ~50-80% at z=3-8. Here we suggest that this apparent change could result from a surface-brightness bias, favoring the detection of edge-on disks at low-luminosities and high-redshifts. Changing edge-on projections with an axis ratio of 10 to a face-on orientation reduces their apparent surface brightness by 2.5 magnitude per arcsec$^2$ and could shift a substantial fraction of the observed galaxies below the detection limit. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_03592 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Surface Brightness Bias in the Shape Statistics of High-Redshift Galaxies Loeb, Abraham Cosmology and Nongalactic Astrophysics Recently, Pandya et al. (2023) argued that the shapes of dwarf galaxies in JWST-CEERS observations show a prolate fraction that rises from ~25% at redshifts z=0.5-1 to ~50-80% at z=3-8. Here we suggest that this apparent change could result from a surface-brightness bias, favoring the detection of edge-on disks at low-luminosities and high-redshifts. Changing edge-on projections with an axis ratio of 10 to a face-on orientation reduces their apparent surface brightness by 2.5 magnitude per arcsec$^2$ and could shift a substantial fraction of the observed galaxies below the detection limit. |
| title | Surface Brightness Bias in the Shape Statistics of High-Redshift Galaxies |
| topic | Cosmology and Nongalactic Astrophysics |
| url | https://arxiv.org/abs/2401.03592 |