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QLP Data Release Notes 004: TESS-Gaia Light Curve Photometry Implementation

Glen Petitpas, Jack Haviland, Te Han, Willie Fong, Katharine Hesse, Avi Shporer, Jeroen Audenaert, Daniel Muthukrishna, Roland Vanderspek, George R. Ricker

Abstract

The Quick-Look Pipeline (QLP; Huang et al. 2020, Kunimoto et al. 2021 and references therein) generates light curves for up to 2 million stars every 27.4 days observed by TESS as part of its planet search. As machine learning methods enable deeper searches and scientific priorities shift toward fainter stars, there is a motivation for QLP to perform better at fainter magnitudes. We have adopted the photometry methods employed by the TESS-Gaia Light Curve package (Han & Brandt 2023), which has been shown to have better noise characteristics than the original QLP photometry from 10.5 $<$ $T$ $<$ 13.5. We still perform aperture photometry and deliver 3 apertures, and 3 levels of detrending for all stars brighter than $T$ = 13.5, so the changes should be seamless for external users. This method is implemented as of Sector 94 in QLP light curves and is providing users with higher precision light curves and allows detection of fainter signals in our planet searches.

QLP Data Release Notes 004: TESS-Gaia Light Curve Photometry Implementation

Abstract

The Quick-Look Pipeline (QLP; Huang et al. 2020, Kunimoto et al. 2021 and references therein) generates light curves for up to 2 million stars every 27.4 days observed by TESS as part of its planet search. As machine learning methods enable deeper searches and scientific priorities shift toward fainter stars, there is a motivation for QLP to perform better at fainter magnitudes. We have adopted the photometry methods employed by the TESS-Gaia Light Curve package (Han & Brandt 2023), which has been shown to have better noise characteristics than the original QLP photometry from 10.5 13.5. We still perform aperture photometry and deliver 3 apertures, and 3 levels of detrending for all stars brighter than = 13.5, so the changes should be seamless for external users. This method is implemented as of Sector 94 in QLP light curves and is providing users with higher precision light curves and allows detection of fainter signals in our planet searches.
Paper Structure (4 sections, 1 figure)

This paper contains 4 sections, 1 figure.

Table of Contents

  1. Introduction
  2. Updates
  3. Performance
  4. Acknowledgements

Figures (1)

  • Figure 1: Photometric precision [$1.48/\sqrt{2}$$\times$ (median difference between adjacent flux points), Han2023] over the QLP magnitude range for 950,000 light curves from Orbit-185, binned to 30 minute time resolution. The FIPHOT data used in QLP initially is shown in blue, and the updated TGLC values are shown in orange. The lower plot shows the ratio of lightcurve scatter between the two methods. The discontinuity in QLP-original at $T$=11.5 is the result of the transition to the smallest fixed QLP aperture.