First results from the Very Small Array - II. Observations of the cosmic microwave background

June 2003 • 2003MNRAS.341.1066T

Authors • Taylor, Angela C. • Carreira, Pedro • Cleary, Kieran • Davies, Rod D. • Davis, Richard J. • Dickinson, Clive • Grainge, Keith • Gutiérrez, Carlos M. • Hobson, Michael P. • Jones, Michael E. • Kneissl, Rüdiger • Lasenby, Anthony • Leahy, J. P. • Maisinger, Klaus • Pooley, Guy G. • Rebolo, Rafael • Rubiño-Martin, José Alberto • Rusholme, Ben • Saunders, Richard D. E. • Savage, Richard • Scott, Paul F. • Slosar, Anže • Sosa Molina, Pedro J. • Titterington, David • Waldram, Elizabeth • Watson, Robert A. • Wilkinson, Althea

Abstract • We have observed the cosmic microwave background (CMB) temperature fluctuations in eight fields covering three separated areas of sky with the Very Small Array at 34 GHz. A total area of 101 square degrees has been imaged, with sensitivity on angular scales of (equivalent to angular multipoles l= 150-900). We describe the field selection and observing strategy for these observations. In the full-resolution images (with synthesized beam of FWHM ~=17 arcmin) the thermal noise is typically 45 μK and the CMB signal typically 55 μK. The noise levels in each field agree well with the expected thermal noise level of the telescope, and there is no evidence of any residual systematic features. The same CMB features are detected in separate, overlapping observations. Discrete radio sources have been detected using a separate 15-GHz survey and their effects removed using pointed follow-up observations at 34 GHz. We estimate that the residual confusion noise arising from unsubtracted radio sources is less than 14 mJy beam^-1 (15 μK in the full-resolution images), which added in quadrature to the thermal noise increases the noise level by 6 per cent. We estimate that the rms contribution to the images from diffuse Galactic emission is less than 6 μK. We also present images that are convolved to maximize the signal-to-noise ratio of the CMB features and are co-added in overlapping areas, in which the signal-to-noise ratio of some individual CMB features exceeds 8.

Links

• PREPRINT http://arxiv.org/abs/astro-ph/0205381
• NED https://ned.ipac.caltech.edu/uri/NED::InRefcode/2003MNRAS.341.1066T
• SPIRES http://inspirehep.net/search?p=find+j+MNRAA,341,1066
• ELECTR http://dx.doi.org/10.1046/j.1365-8711.2003.06493.x
• SIMBAD http://simbad.u-strasbg.fr/simbo.pl?bibcode=2003MNRAS.341.1066T
• PDF https://academic.oup.com/mnras/pdf-lookup/doi/10.1046/j.1365-8711.2003.06493.x
• DATA http://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/341/1066
• DATA https://cdsarc.cds.unistra.fr/viz-bin/cat/J/MNRAS/341/1066
• GIF http://articles.adsabs.harvard.edu/full/2003MNRAS.341.1066T
• ARTICLE http://articles.adsabs.harvard.edu/full/2003MNRAS.341.1066T?defaultprint=YES
• SPIRES http://inspirehep.net/search?p=find+eprint+astro-ph/0205381