| Full text | |
| Author(s): Show less - |
Jew, Luke
[1]
;
Taylor, Angela C.
[1]
;
Jones, Michael E.
[1]
;
Barr, A.
[2]
;
Chiang, H. C.
[3]
;
Dickinson, C.
[4, 2]
;
Grumitt, R. D. P.
[1]
;
Harper, S. E.
[2]
;
Heilgendorff, H. M.
[5]
;
Hill-Valler, J.
[1]
;
Jonas, J. L.
[6, 7]
;
Leahy, J. P.
[2]
;
Leech, J.
[1]
;
Pearson, T. J.
[4]
;
Peel, M. W.
[8, 9]
;
Readhead, A. C. S.
[4]
;
Sievers, J.
[3]
Total Authors: 17
|
| Affiliation: | [1] Univ Oxford, Sub Dept Astrophys, Denys Wilkinson Bldg, Keble Rd, Oxford OX1 3RH - England
[2] Univ Manchester, Sch Phys & Astron, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Oxford Rd, Manchester M13 9PL, Lancs - England
[3] McGill Univ, Dept Phys, 3600 Rue Univ, Montreal, PQ H3A 2T8 - Canada
[4] CALTECH, Cahill Ctr Astron & Astrophys, Pasadena, CA 91125 - USA
[5] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, Westville Campus, Private Bag X54001, ZA-4000 Durban - South Africa
[6] Rhodes Univ, Dept Phys & Elect, ZA-6139 Grahamstown - South Africa
[7] South African Radio Astron Observ, 2 Fir Rd, ZA-7925 Cape Town - South Africa
[8] Inst Astrofis Canarias, E-38205 Tenerife - Spain
[9] ULL, Dept Astrofis, E-38206 Tenerife - Spain
Total Affiliations: 9
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 490, n. 2, p. 2958-2975, DEC 2019. |
| Web of Science Citations: | 0 |
| Abstract | |
The cosmic microwave background (CMB) B-mode signal is potentially weaker than the diffuse Galactic foregrounds over most of the sky at any frequency. A common method of separating the CMB from these foregrounds is via pixel-based parametric-model fitting. There are not currently enough all-sky maps to fit anything more than the most simple models of the sky. By simulating the emission in seven representative pixels, we demonstrate that the inclusion of a 5 GHz data point allows for more complex models of low-frequency foregrounds to be fitted than at present. It is shown that the inclusion of the C-BASS data will significantly reduce the uncertainties in a number of key parameters in the modelling of both the galactic foregrounds and the CMB. The extra data allow estimates of the synchrotron spectral index to be constrained much more strongly than is presently possible, with corresponding improvements in the accuracy of the recovery of the CMB amplitude. However, we show that to place good limits on models of the synchrotron spectral curvature will require additional low-frequency data. (AU) | |
| FAPESP's process: | 15/19936-1 - BINGO: an ultra-sensitive survey of hydrogen and radio continuum emission to measure the dark universe |
| Grantee: | Michael William Peel |
| Support Opportunities: | Research Grants - Young Investigators Grants |