The Physics of the Accelerating Universe Camera

Cristóbal Padilla, Francisco J. Castander, Alex Alarcón, Jelena Aleksic, Otger Ballester, Laura Cabayol, Laia Cardiel-Sas, Jorge Carretero, Ricard Casas, Javier Castilla, Martin Crocce, Manuel Delfino, Carlos Díaz, Martin Eriksen, Enrique Fernández, Pablo Fosalba, Juan García-Bellido, Enrique Gaztañaga, Javier Gaweda, Ferran GrañenaJosé María Ílla, Jorge Jiménez, Luis López, Pol Martí, Ramon Miquel, Christian Neissner, Cristóbal Pío, Eusebio Sánchez, Santiago Serrano, Ignacio Sevilla-Noarbe, Pau Tallada, Nadia Tonello, Juan De Vicente

Research output: Contribution to journalArticleResearch

4 Citations (Scopus)

Abstract

© 2019. The American Astronomical Society. All rights reserved.. The Physics of the Accelerating Universe (PAU) Survey goal is to obtain photometric redshifts (photo-z) and spectral energy distributions (SEDs) of astronomical objects with a resolution roughly one order of magnitude better than current broadband (BB) photometric surveys. To accomplish this, a new large field-of-view (FoV) camera (PAUCam) has been designed, built, and commissioned and is now operated at the William Herschel Telescope (WHT). With the current WHT prime focus corrector, the camera covers an ∼1° diameter FoV, of which only the inner ∼40′ diameter is unvignetted. The focal plane consists of a mosaic of 18 2k × 4k Hamamatsu fully depleted CCDs, with high quantum efficiency up to 1 μm in wavelength. To maximize the detector coverage within the FoV, filters are placed in front of the CCDs inside the camera cryostat (made out of carbon fiber) using a challenging movable tray system. The camera uses a set of 40 narrowband filters ranging from ∼4500 to ∼8500 Å complemented with six standard BB filters, ugrizY. The PAU Survey aims to cover roughly 100 deg2 over fields with existing deep photometry and galaxy shapes to obtain accurate photometric redshifts for galaxies down to i AB ∼ 22.5, also detecting galaxies down to i AB ∼ 24 with less precision in redshift. With this data set, we will be able to measure intrinsic alignments and galaxy clustering and perform galaxy evolution studies in a new range of densities and redshifts. Here we describe the PAU camera, its first commissioning results, and its performance.
Original languageEnglish
Article number246
JournalAstronomical Journal
Volume157
DOIs
Publication statusPublished - 1 Jan 2019

Keywords

  • dark energy
  • instrumentation: photometers
  • large-scale structure of universe
  • surveys
  • techniques: photometric

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