Coping with Selection Effects: A Primer on Regression with Truncated Data
arXiv:1901.10522 · doi:10.1093/mnras/stz320
Abstract
The finite sensitivity of instruments or detection methods means that data sets in many areas of astronomy, for example cosmological or exoplanet surveys, are necessarily systematically incomplete. Such data sets, where the population being investigated is of unknown size and only partially represented in the data, are called "truncated" in the statistical literature. Truncation can be accounted for through a relatively straightforward modification to the model being fitted in many circumstances, provided that the model can be extended to describe the population of undetected sources. Here I examine the problem of regression using truncated data in general terms, and use a simple example to show the impact of selecting a subset of potential data on the dependent variable, on the independent variable, and on a second dependent variable that is correlated with the variable of interest. Special circumstances in which selection effects are ignorable are noted. I also comment on computational strategies for performing regression with truncated data, as an extension of methods that have become popular for the non-truncated case, and provide some general recommendations.
11 pages, to appear in MNRAS
References in corpus (6)
- Some Aspects of Measurement Error in Linear Regression of Astronomical Data
- Extracting distribution parameters from multiple uncertain observations with selection biases
- Cosmological Evolution of Long Gamma-ray Bursts and Star Formation Rate
- A Model for Multi-property Galaxy Cluster Statistics
- CoMaLit - II. The scaling relation between mass and Sunyaev-Zel'dovich signal for Planck selected galaxy clusters
- A Bayesian approach to truncated data sets: An application to Malmquist bias in Supernova Cosmology
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