## Mission Overview

### Ultraviolet Imaging of the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey Fields (UVCANDELS)

Primary Investigator: Harry Teplitz

Full Team: See full team list.

HLSP Authors:
Xin Wang, Laura Prichard, Anahita Alavi, Marc Rafelski, Norman Grogin, Anton Keokemoer, Ben Sunnquist, Harry Teplitz

Released: 2022-06-13

Updated: 2022-06-13

Primary Reference(s): Coming soon...

Citations: Coming soon...

Source Data:

## Overview

UVCANDELS offers wide-area extragalactic UV imaging of four of the premier HST deep-wide survey fields defined by CANDELS. The program is motivated by an investigation of galaxy evolution during the epoch of vigorous star formation at 0.5 < z < 3 by:

1. Using the high spatial resolution UV and Blue data (700 pc at z~1) to study the structural evolution of galaxies and create 2D maps of their star-formation history.
2. Combining UVCANDELS with Herschel legacy data to trace the evolution of the dust content of moderate redshift (z < 1) galaxies.
3. Probing the role of environment in the evolution of low-mass star-forming galaxies.
4. Investigating the decay of star-formation in massive early-type galaxies and the role of minor mergers.
5. Constraining the escape fraction of ionizing radiation from galaxies at z ~ 2.5 to better understand how star-forming galaxies reionized the Universe at z > 6.

UVCANDELS consists of WFC3/F275W imaging of four CANDELS fields (~430 sq. arcmin combined), reaching AB=27 for compact galaxies (SFR~0.2 Msun/yr at z=1), together with parallel ACS/F435W (AB>=28.0) imaging. For each field (GOODS-N, GOODS-S, COSMOS and EGS), we deliver image mosaics of the new F275W observations. The mosaics are made on both 60mas and 30mas pixel grids. The astrometry is aligned to the CANDELS optical 30mas mosaics (F814W for COSMOS and F606W for the rest), with a small relative offset (usually <0.15 pixel [<45 mas]).  We also deliver new ACS/F435W images for the COSMOS and EGS Fields over the same area.  The F275W area of the GOODS fields falls within the original GOODS F435W coverage.

## Data Products

The image files have the following naming convention:

hlsp_uvcandels_hst_<ins>_<field>-<scale>_<filter>_v1.0_<type>.fits

where:

• <ins> = Instrument used, one of "acs-wfc" or "wfc3-uvis".
• <field> = Name of the field, one of "cosmos", "egs", "goodsn", or "goodss".
• <scale> = Pixel grid for this image, in milliarcseconds, one of "30mas" or "60mas".
• <filter> = Filter used, one of "f275w" or "f435w".
• <type> = Type of image product, one of "sci", "wht", or "rms".

Data file types:

 _sci.fits Science image. _wht.fits Weight image, the inverse variance map created by AstroDrizzle. _rms.fits Noise map, after correcting for the correlated noise following Casertano et al. (2000).

## Data Access

Field Pixel Grid F275W F435W
COSMOS 30mas RMS SCI WHT  RMS SCI WHT
60mas RMS SCI WHT  RMS SCI WHT
EGS 30mas RMS SCI WHT  RMS SCI WHT
60mas RMS SCI WHT  RMS SCI WHT
GOODS-N 30mas RMS SCI WHT
60mas RMS SCI WHT
GOODS-S 30mas RMS SCI WHT
60mas RMS SCI WHT

## Citations

Please remember to cite the appropriate paper(s) below and the DOI if you use these data in a published work.

Note: These HLSP data products are licensed for use under CC BY 4.0.