The PAU Survey (PAUS, www.pausurvey.org) is an international collaboration between Spain, Holland, Switzerland, Germany, UK to collect a fluxed limited accurate redshift and spectral energy distribution information for millions of galaxies (and stars) to a depth and area never explored before. This is done without the need of target selection which provides a valuable tool to understand sample selection and completeness. To do this, a spanish group had built PAUcam, a large imager (1 degree square FoV, with18 CCD of 4094x2048 pixels each) capable of doing imaging with 40 narrow-band filters (~130A wide in steps of 100A) and 6 wide-band filtres (u,g,r,i,z,Y), which results in high resolution spectra energy distributions for all galaxies in a given field of view. PAUcam was commissioned in the William Herschel 4.2m Telescope (WHT) in the Canary Islands on June 2015. The PAU Survey is using PAUcam to image an area of ?100 deg2 to iAB ~23 to reach a volume of 0.3-0.5 (Gpc/h)3 with a few million redshifts split into 3 to 4 wide fields (of several tens of deg2 each). Deep Broad-Band (BB) photometric measurements have already been obtained by CFHTLenS and KiDS over the same fields and spectroscopic redshifts for calibration are available from the GAMA, VIPERS, DEEP2 and zCOSMOS redshift surveys. This will enable:
- to improve redshift estimates and target selection incompleteness to reach the accuracy required for large-scale clustering and weak lensing analices in KiDS, DES, DESI, LSST and Euclid
- detailed studies of intermediate-scale cosmic structure
- first precise measurement of intrinsic alignments at z ? 0.75
- cross-correlation techniques for redshift measurements, magnification and sampling variance cancelation studies
A number of large surveys (e.g. KiDS, DES, SDSS, LSST, DESI) aim to map the 3D structure of the Universe to understand the nature of dark matter and dark energy. To achieve the required statistical precision, these focus on large scales, sparse samples of selected spectroscopic targets, or restrict the line-of-sight resolution by employing photometric redshifts based on a few broad- bands (BB). In contrast, studies aiming to explore the role of environment are limited to the small scales provided by pencil-beam surveys. We need to bridge this gap and probe the intermediate to small scales (below 10-20 Mpc/h), i.e. the weakly non-linear regime where the statistical signal-to-noise is largest. Our currently limited understanding of these scales, where baryonic and environmental effects become relevant, has to improve dramatically over the coming years to allow for a robust separation of cosmological and galaxy formation effects. This requires surveying large contiguous areas while simultaneously achieving a high number density of galaxies with sub-percent redshift accuracy. This is now possible thanks to PAUCam: a unique combination of a large field-of-view and 40 narrow-band that span the wavelength range from 450nm to 850nm and that was commissioned successfully in June 2015 on the WHT. This exquisite wavelength sampling results in photometric redshifts with a precision that approaches that of spectroscopic measurements, while being able to cover large areas of sky.
During 2017 we transported PAUcam from LaPalma to Barcelona and back o do some repairs and maintenance. We have some observing runs at the WHT Telescope before and after the repairs and we made some progress in the Survey. In total we had 45 observing nights, but about 75% of them where lost to bad weather conditions. So the Survey in progressing, but at very low pace…. We refine and tested the zero point calibrations, scatter light detection and force photometry software. We also improve photometric redshift performance to 90% of our original goals. We are now writing the first papers of the PAU Survey camera, data management, simulations and photometric redshifts.
Cosmological constraints from multiple tracers in spectroscopic surveys Alarcon, A., Eriksen, M., & Gaztanaga, E. 2016, arXiv:1609.08510
Characterization and performance of PAUCam filters Casas, R., Cardiel-Sas, L., Castander, F.J., et al. 2016, PSPIE, 9908, 99084K
The PAU camera carbon fiber cryostat and filter interchange system Lopez, L., Padilla, C., Cardiel-Sas, L., et al. 2016, PSPIE, 9908, 99084G
The PAU camera at the WHT Padilla, C., Ballester, O., Cardiel-Sas, L., et al. 2016, PSPIE, 9908, 99080Z
Calibrating the PAU Survey's 46 Filters Bauer, A., Castander, F., Gaztanaga, E., et al. 2016, The Science of Calibration, 503, 99
Senior Institute members involved
, F. Castander, M. Crocce, P. Fosalba