The missing light of the Hubble Ultra Deep Field⋆
Instituto de Astrofísica de Canarias, C/ Vía Láctea, 38200 La Laguna, Tenerife, Spain
2 Facultad de Física, Universidad de La Laguna, Avda. Astrofísico Fco. Sánchez s/n, 38200 La Laguna, Tenerife, Spain
3 Consejo Superior de Investigaciones Científicas, Spain
4 Instituto de Ciencias Matemáticas, Consejo Superior de Investigaciones Científicas, Madrid, Spain
5 Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
6 Departamento de Astrofísica y CC. de la Atmósfera, Universidad Complutense de Madrid, 28040 Madrid, Spain
7 Univ. Lyon, Univ. Lyon1, ENS de Lyon, CNRS, Centre de Recherche Astrophysique de Lyon UMR5574, 69230 Saint-Genis-Laval, France
Accepted: 12 November 2018
Context. The Hubble Ultra Deep field (HUDF) is the deepest region ever observed with the Hubble Space Telescope. With the main objective of unveiling the nature of galaxies up to z ∼ 7 − 8, the observing and reduction strategy have focused on the properties of small and unresolved objects, rather than the outskirts of the largest objects, which are usually over-subtracted.
Aims. We aim to create a new set of WFC3 IR mosaics of the HUDF using novel techniques to preserve the properties of the low surface brightness regions.
Methods. We created ABYSS: a pipeline that optimises the estimate and modelling of low-level systematic effects to obtain a robust background subtraction. We have improved four key points in the reduction: 1) creation of new absolute sky flat fields, 2) extended persistence models, 3) dedicated sky background subtraction and 4) robust co-adding.
Results. The new mosaics successfully recover the low surface brightness structure removed on the previous HUDF published reductions. The amount of light recovered with a mean surface brightness dimmer than μ¯ = 26 mag arcsec−2 is equivalent to a m = 19 mag source when compared to the XDF and a m = 20 mag compared to the HUDF12.
Conclusions. We present a set of techniques to reduce ultra-deep images (μ > 32.5 mag arcsec−2, 3σ in 10 × 10 arcsec boxes), that successfully allow us to detect the low surface brightness structure of extended sources on ultra deep surveys. The developed procedures are applicable to HST, JWST, EUCLID and many other space and ground-based observatories.
Key words: techniques: image processing / techniques: photometric / methods: observational / galaxies: evolution / galaxies: structure / galaxies: high-redshift
The final ABYSS WFC3 IR HUDF mosaics are only available at http://www.iac.es/proyecto/abyss/ and at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (188.8.131.52) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/621/A133
© ESO 2019