http://arxiv.org/abs/2208.10337
Many astronomical systems display complex, rapid variability across the electromagnetic spectrum. Studying this variability is the key to understanding the underlying processes at play. However, a combination of limited or patchy telescope availability, viewing constraints, and the unpredictable and faint nature of many sources mean that obtaining data well-suited to this task can be tricky, especially when it comes to simultaneous multiwavelength observations. As a result, researchers can often find themselves tuning observational parameters in real-time by trial-and-error, or may realise later that their observation was not long enough to achieve their goals. Here, we present a code to mitigate some of these issues and aid planning of multiwavelength coordinated observations. The code takes a temporal and Fourier model of a system (i.e. Power Spectra, Coherence, and Lags) as input, and returns a simulated multiwavelength observation, including effects of noise, telescope parameters, and finite sampling. The goals of this are: (i) To simulate a potential observation (to inform decisions about an observation’s feasibility); (ii) To investigate how different Fourier models affect the variability of the system (e.g. how altering the frequency-dependent coherence or Fourier lags between bands can affect data products like cross-correlation functions); and (iii) To simulate existing data and investigate its trustworthiness. We outline the methodology behind the code, show how a variety of parameters (e.g. noise sources, observation length, and telescope choice) can affect data, and present examples of the software in action.
J. Paice, P. Gandhi and R. Misra
Tue, 23 Aug 22
33/79
Comments: 20 pages + Supplementary Material
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