|
| | | | |
| | | |
| Stat |
Members: 3645
Articles: 2'501'711
Articles rated: 2609
19 April 2024 |
|
| | | | |
|
Article overview
| |
|
|
Ultra-deep Large Binocular Camera U-band Imaging of the GOODS-North Field: Depth vs. Resolution | | Teresa A. Ashcraft
; Rogier A. Windhorst
; Rolf A. Jansen
; Seth H. Cohen
; Andrea Grazian
; Diego Paris
; Adriano Fontana
; Emanuele Giallongo
; Roberto Speziali
; Vincenzo Testa
; Konstantina Boutsia
; Robert W. O'Connell
; Michael Rutkowski
; Russell Ryan
; Claudia Scarlata
; Benjamin Weiner
; | | Date: |
29 Mar 2017 | | Abstract: | We present a study of the trade-off between depth and resolution using a
large number of U-band imaging observations in the GOODS-North field
(Giavalisco et al. 2004) from the Large Binocular Camera (LBC) on the Large
Binocular Telescope (LBT). Having acquired over 30 hours of data (315 images
with 5-6 mins exposures), we generated multiple image mosaics, starting with
the best atmospheric seeing images (FWHM $lesssim$0.8"), which constitute
$sim$10% of the total data set. For subsequent mosaics, we added in data with
larger seeing values until the final, deepest mosaic included all images with
FWHM $lesssim$1.8" ($sim$94% of the total data set). From the mosaics, we
made object catalogs to compare the optimal-resolution, yet shallower image to
the lower-resolution but deeper image. We show that the number counts for both
images are $sim$90% complete to $U_{AB}$ $lesssim26$. Fainter than
$U_{AB}$$sim$ 27, the object counts from the optimal-resolution image start to
drop-off dramatically (90% between $U_{AB}$ = 27 and 28 mag), while the deepest
image with better surface-brightness sensitivity ($mu^{AB}_{U}$$lesssim$ 32
mag arcsec$^{-2}$) show a more gradual drop (10% between $U_{AB}$ $simeq$ 27
and 28 mag). For the brightest galaxies within the GOODS-N field, structure and
clumpy features within the galaxies are more prominent in the
optimal-resolution image compared to the deeper mosaics. Finally, we find - for
220 brighter galaxies with $U_{AB}$$lesssim$ 24 mag - only marginal
differences in total flux between the optimal-resolution and lower-resolution
light-profiles to $mu^{AB}_{U}$$lesssim$ 32 mag arcsec$^{-2}$. In only 10% of
the cases are the total-flux differences larger than 0.5 mag. This helps
constrain how much flux can be missed from galaxy outskirts, which is important
for studies of the Extragalactic Background Light. | | Source: | arXiv, 1703.9874 | | Services: | Forum | Review | PDF | Favorites | |
|
|
No review found.
Did you like this article?
Note: answers to reviews or questions about the article must be posted in the forum section.
Authors are not allowed to review their own article. They can use the forum section.
browser Mozilla/5.0 AppleWebKit/537.36 (KHTML, like Gecko; compatible; ClaudeBot/1.0; +claudebot@anthropic.com)
|
| |
|
|
|
|
News, job offers and information for researchers and scientists:
| |
REGISTER