Abstract
Abstract It is commonplace in pulsar and fast radio burst literature to estimate sky temperature by frequency-scaling of the Haslam et al. 408 MHz map. I suggest that this practice should stop, in favor of using readily available global sky models of diffuse foregrounds. This practical change will improve accuracy of pulse flux estimates.
Highlights
In searches for fast radio bursts (FRBs) and single pulses from pulsars, it is common for the peak flux to be estimated based on the signal-to-noise (S/N) of the pulse and instrumental characteristics
In the pulsar and FRB literature, it remains common for the sky contribution to be estimated based on the Haslam et al (1982) all-sky map, with a power-law frequency scaling applied to account for the sky-averaged synchrotron spectrum: ν β
A skymap generated from PyGDSM using the de Oliveira-Costa et al (2008) Global Sky Model (GSM) model is shown in Fig 1; as can be seen, β varies across the sky, and is flatter within the Galactic plane
Summary
In searches for fast radio bursts (FRBs) and single pulses from pulsars, it is common for the peak flux to be estimated based on the signal-to-noise (S/N) of the pulse and instrumental characteristics. Where Treceiver is the receiver temperature, and Tsky is the contribution from the sky Note that this approximation ignores several contributors to the noise budget, such as the telescope spillover and the atmosphere/ionosphere; (see for example, Campbell 2002). The Haslam map is a radio continuum all-sky map taken at 408 MHz, which combines data from Northern and Southern hemisphere surveys. This map remains in widespread usage; a improved version with striping artefacts and point sources removed was provided by (Remazeilles et al 2015). Note that the Haslam 408 MHz is included in each sky model
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