A broad-band flux scale for low-frequency radio telescopes
A broad-band flux scale for low-frequency radio telescopes
We present parametrized broad-band spectral models valid at frequencies between 30 and 300 MHz for six bright radio sources selected from the 3C survey, spread in right ascension from 0 to 24 h. For each source, data from the literature are compiled and tied to a common flux density scale. These data are then used to parametrize an analytic polynomial spectral calibration model. The optimal polynomial order in each case is determined using the ratio of the Bayesian evidence for the candidate models. Maximum likelihood parameter values for each model are presented, with associated errors, and the percentage error in each model as a function of frequency is derived. These spectral models are intended as an initial reference for science from the new generation of low-frequency telescopes now coming online, with particular emphasis on the Low Frequency Array (LOFAR).
observational methods, statistical methods
L30-L34
Scaife, Anna M.M.
327b962f-9003-45ca-a6ea-284346c5cc85
Heald, George H.
55b7dbc9-b0a1-4f78-9d25-f1d0c761bcc0
June 2012
Scaife, Anna M.M.
327b962f-9003-45ca-a6ea-284346c5cc85
Heald, George H.
55b7dbc9-b0a1-4f78-9d25-f1d0c761bcc0
Scaife, Anna M.M. and Heald, George H.
(2012)
A broad-band flux scale for low-frequency radio telescopes.
Monthly Notices of the Royal Astronomical Society: Letters, 423 (1), .
(doi:10.1111/j.1745-3933.2012.01251.x).
Abstract
We present parametrized broad-band spectral models valid at frequencies between 30 and 300 MHz for six bright radio sources selected from the 3C survey, spread in right ascension from 0 to 24 h. For each source, data from the literature are compiled and tied to a common flux density scale. These data are then used to parametrize an analytic polynomial spectral calibration model. The optimal polynomial order in each case is determined using the ratio of the Bayesian evidence for the candidate models. Maximum likelihood parameter values for each model are presented, with associated errors, and the percentage error in each model as a function of frequency is derived. These spectral models are intended as an initial reference for science from the new generation of low-frequency telescopes now coming online, with particular emphasis on the Low Frequency Array (LOFAR).
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MNRAS-2012-Scaife-L30-4-1.pdf
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e-pub ahead of print date: 29 March 2012
Published date: June 2012
Keywords:
observational methods, statistical methods
Organisations:
Astronomy Group
Identifiers
Local EPrints ID: 350616
URI: http://eprints.soton.ac.uk/id/eprint/350616
ISSN: 1745-3925
PURE UUID: 5f9b80a6-74f1-443a-91e5-1d8bee13013b
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Date deposited: 27 Mar 2013 12:00
Last modified: 14 Mar 2024 13:30
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Author:
Anna M.M. Scaife
Author:
George H. Heald
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