Browsing by Author "Zwart, J."
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Item The Q/U imaging experiment instrument(The American Astronomical Society, 2013) Biscoff, C.; Brizius, A.; Zwart, J.; Buder, I.; Chinone, Y.; Cleary, K.; Dumoulin, R.N.; Kusaka, A.; Monsalve, R.; Naess, S.K.; Newburgh, L.B.; Nixon, G.; Reeves, R.; Smith, K.M.; Vanderlinde, K.; Wehus, I.K.; Bogdan, M.; Bustos, R.; Church, S.E.; Davis, Robert; Dickenson, C.; Eriksen, H.K.; Gaier, T.; Gundersen, J.O.; Hasegawa, M.; Hazumi, M.; Holler, C.; Huffenberger, K.M.; Imbriale, W.A.; Ishidoshiro, K.; Jones, M.E.; Kangaslahti, P.; Kapner, D.J.; Lawrence, C.R.; Leitch, E.M.; Limon, M.; McMahon, J.J.; Miller, A.D.; Nagai, M.; Nguyen, H.; Pearson, T.J.; Piccirillo, L.; Radford, S.J.E.; Readhead, A.C.S.; Richards, J.L.; Samtleben, D.; Seiffert, M.; Shepherd, M.C.; Staggs, S.T.; Tajima, O.; Thompson, K.L.; Williamson, R.; Winstein, B.; Wollack, E.J.The Q/U Imaging ExperimenT (QUIET) is designed to measure polarization in the cosmic microwave background, targeting the imprint of inflationary gravitational waves at large angular scales(∼1◦). Between 2008 October and 2010 December, two independent receiver arrays were deployed sequentially on a 1.4m side-fed Dragonian telescope. The polarimeters that form the focal planes use a compact design based on high electron mobility transistors (HEMTs) that provides simultaneous measurements of the Stokes parameters Q, U, and I in a single module. The 17-element Q-band polarimeter array, with a central frequency of 43.1 GHz, has the best sensitivity (69 μKs1/2) and the lowest instrumental systematic errors ever achieved in this band, contributing to the tensor-to-scalar ratio at r < 0.1. The 84-element W-band polarimeter array has a sensitivity of 87 μKs1/2 at a central frequency of 94.5 GHz. It has the lowest systematic errors to date, contributing at r < 0.01. The two arrays together cover multipoles in the range ∼ 25–975. These are the largest HEMT-based arrays deployed to date. This article describes the design, calibration, performance, and sources of systematic error of the instrument.Item The VISTA Deep Extragalactic Observations (VIDEO) survey(Oxford University Press, 2013) Jarvis, Matt; Bonfield, David G.; Bruce, V.A.; Zwart, J.; Geach, J.E.; McAlpine, K.; McLure, R.J.; Gonzalez-Solares, Eduardo A.; Irwin, M.; Lewis, J.; Kupcu Yoldas, A.; Andreon, S.; Cross, N.J.G.; Emerson, J.P.; Dalton, G.; Dunlop, J.S.; Hodgkin, S. T.; Le Fevre, O.; Karouzos, M.; Meisenheimer, K.; Oliver, S.; Rawlings, S.; Simpson, Chris; Smail, I.; Smith, Daniel J.B.; Sullivan, M.; Sutherland, W.; White, S.V.In this paper we describe the first data release of the the Visible and Infrared Survey Telescope for Astronomy (VISTA) Deep Extragalactic Observations (VIDEO) survey. VIDEO is a 12 degree2 survey in the near-infrared Z,Y ,J,H andKs bands, specifically designed to enable the evolution of galaxies and large structures to be traced as a function of both epoch and environment from the present day out to z=4, and active galactic nuclei (AGN) and the most massive galaxies up to and into the epoch of reionization. With its depth and area, VIDEO will be able to fully explore the period in the Universe where AGN and starburst activity were at their peak and the first galaxy clusters were beginning to virialize. VIDEO therefore offers a unique data set with which to investigate the interplay between AGN, starbursts and environment, and the role of feedback at a time when it was potentially most crucial. We provide data over the VIDEO-XMM3 tile, which also covers the Canada-France- Hawaii-Telescope Legacy Survey Deep-1 field (CFHTLS-D1). The released VIDEO data reach a 5 AB-magnitude depth of Z = 25:7, Y = 24:5, J = 24:4, H = 24:1 and Ks = 23:8 in 2 arcsec diameter apertures (the full depth of Y = 24:6 will be reached within the full integration time in future releases). The data are compared to previous surveys over this field and we find good astrometric agreement with the Two-Micron All Sky Survey, and source counts in agreement with the recently released UltraVISTA survey data. The addition of the VIDEO data to the CFHTLS-D1 optical data increases the accuracy of photometric redshifts and significantly reduces the fraction of catastrophic outliers over the redshift range 0 < z < 1 from 5.8 to 3.1 per cent in the absence of an iband luminosity prior. However, we expect the main improvement in photometric redshifts will come in the redshift range 1 < z < 4 due to the sensitivity to the Balmer and 4000°A breaks provided by the near-infrared VISTA filters. All images and catalogues presented in this paper are publicly available through ESO’s phase 3 archive and the VISTA Science Archive.