The PAU (BAO) Survey
(Institut de Ciències de l'Espai)
Mardi 24/06/2008, 15:00
Bat 141, salle André Berthelot Masque obligatoire; en cas de nécessité de dépassement, contacter préalablement le chef d’installation., CEA Paris-Saclay
Baryon Acoustic Oscillations (BAO) provide a “standard ruler” of known physical length, making it one of the most promising probes of the nature of dark energy. Contrary to usual assumptions, it is possible to obtain photometric redshifts with enough precision to measure BAO along the line of sight. We show that sigma_z~0.003(1 + z) is sufficient: a much better precision will produce an oversampling of the BAO peak without a significant improvement on its detection, while a much worse precision will result in the effective loss of the radial information. This precision in redshift can be achieved for bright, red galaxies, featuring a prominent 4000 Å break, by using a filter system comprising about 40 filters, each with a width close to 100 Å, covering the wavelength range from 4000 Å to 8000 Å, supplemented by two broad-band filters similar to the SDSS u and z bands. We describe the practical implementation of this idea, a new galaxy survey project, PAU, to be carried out with a telescope/camera combination with an etendue about 20 m2 deg2, equivalent to a 2 m telescope equipped with a 6 deg2-FoV camera, and covering 8000 deg2 in the sky in four years. We expect to measure positions and redshifts for over 14 million red, early-type galaxies with L > L* and IAB <22.5 in the redshift interval 0.1 < z < 1, with a precision sigma_z < 0.003(1 + z). This population has a number density n > 10^3 Mpc^3/h^3 galaxies within the11 (Gpc/h)3 volume to be sampled by our survey, ensuring that the error in the determination of the BAO scale is not limited by shot-noise. By itself, such a survey will deliver precisions of order 5% in the dark-energy equation of state parameter w, if assumed constant, and can determine its time derivative when combined with future CMB measurements. In addition, PAU will yield high-quality redshift and low-resolution spectroscopy for hundreds of millions of other galaxies, including a very significant high-redshift population. The data set produced by this survey will have a unique legacy value, allowing a wide range of astrophysical studies.