The CMBR spectrum:: new upper limits for the distortion parameters y and μ

被引:4
作者
Battistelli, ES [1 ]
Fulcoli, V [1 ]
Macculi, C [1 ]
机构
[1] Univ Roma La Sapienza, Dept Phys, I-00185 Rome, Italy
关键词
instrumentation : detectors; cosmic microwave background; COBE-FIRAS; cosmology : theory; distortion parameters;
D O I
10.1016/S1384-1076(00)00014-2
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The CMBR Spectrum has been measured by the COBE-FIRAS experiment. Upper limits only have been found for distortion parameters y and mu: y(up) = 1.5 x 10(-5) and mu(up) = 9 x 10(-5) at 95% of confidence. FIRAS made differential measurements between sky and blackbody calibrator. The knowledge of its emissivity is important as far as y and mu measurements as concerned. We have re-estimated the XCAL emissivity by using Ray-Tracing techniques. Diffraction problems have been analyzed by a model based on waveguide approximation: it allowed us to define a propagation function tau inside the XCAL V-groove. The emission of the external calibrator distorted with respect to the Black-Body emission may result in lower upper limits to y and mu. New upper limits for distortion parameters y and mu have been calculated considering the new XCAL emissivity. The results are: y(up) = 3.1 x 10(-5) and mu(up) = 4.5 x 10(-4) at 95% of confidence. (C) 2000 Elsevier Science B.V. All rights reserved.
引用
收藏
页码:77 / 90
页数:14
相关论文
共 20 条
[1]  
BAILIN B, 1956, IRE T ANTENNAS PROPA, P5
[2]  
BARROW B, 1939, P IRE, P51
[3]   THE COBE MISSION - ITS DESIGN AND PERFORMANCE 2 YEARS AFTER LAUNCH [J].
BOGGESS, NW ;
MATHER, JC ;
WEISS, R ;
BENNETT, CL ;
CHENG, ES ;
DWEK, E ;
GULKIS, S ;
HAUSER, MG ;
JANSSEN, MA ;
KELSALL, T ;
MEYER, SS ;
MOSELEY, SH ;
MURDOCK, TL ;
SHAFER, RA ;
SILVERBERG, RF ;
SMOOT, GF ;
WILKINSON, DT ;
WRIGHT, EL .
ASTROPHYSICAL JOURNAL, 1992, 397 (02) :420-429
[4]  
CHANDOS J, 1974, APPL OPTICS, V13
[5]  
EISENMAN A, 1963, J OPT SOC AM, V53
[6]   The cosmic microwave background spectrum from the full COBE FIRAS data set [J].
Fixsen, DJ ;
Cheng, ES ;
Gales, JM ;
Mather, JC ;
Shafer, RA ;
Wright, EL .
ASTROPHYSICAL JOURNAL, 1996, 473 (02) :576-587
[7]  
HALPERN H, 1986, APPL OPTICS, V25
[8]  
HAMID H, 1968, IEEE T ANTENNAS PROP, V16
[9]  
HARRINGTON H, 1961, TIME HARMONIC ELECTR
[10]  
HEMMATI H, 1985, APPL OPTICS, V24