Testing of atmospheric opacity during sun observations with MSRT

Хайкин, В. Б.; Karavaev, D. M.; Rybakov, Yu. V.

doi:10.1109/crmico.2003.159017

Cited by 3 publications

(1 citation statement)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A smooth-walled spline-profile horn (Granet et al, 2004) is an alternative to both corrugated and trimode horns and it allows us to achieve an identical radiation pattern in E/H plane in the band, low sidelobe level(less than -25 dB), more tight array packaging and lower manufacture cost. We are in final stage now to build and test such a horn for array applications al lower frequencies (30)(31)(32)(33)(34)(35)(36)(37)(38) in cooperation with C.Granet(CSIRO) (Khaikin et al,2007).…”

Section: Array Feedsmentioning

confidence: 99%

Spectral spatial fluctuations of CMBR: Strategy and concept of the experiment

2008

Self Cite

View full text Add to dashboard Cite

Spectral Spatial Fluctuations (SSF) of the Cosmic Microwave Background Radiation (CMBR) temperature are considered as a result of an interaction of primordial atoms and molecules with CMBR in proto-objects moving with peculiar velocities relative to the CMBR. Expected optimistic values of ∆T /T are 2×10 −5 −2×10 −6 for SSF caused by HeH + at z =20-30 which are possible redshifts of early reionization scenario. The bandwidth of the lines is 0.1-2% depending on the scale of protoobjects and redshifts. For the SSF search CMBR maps in different spectral channels are to be observed and then processed by the Difference method. Simulation of the experiment is made for MSRT (Tuorla Observatory, Finland) equipped with a 7 × 4 beam cryo-microbolometer array with a chopping flat and frequency multiplexer providing up to 7 spectral channels in each beam (88-100 GHz). Expected ∆T/T limit in the experiment is 2×10 −5 with 6 ′ -7 ′ angular and 2% frequency resolution. Simulation shows that SSF may be recognized in the angular power spectrum when S/N in single frequency CMBR maps is as small as 1.17 or even something less for white noise. Such an experiment gives us a possibility to set upper limit of SSF in MM band and prepare future SSF observations.

show abstract