Light curve
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About
A light curve is a graphical record of how the brightness of an astronomical object changes over time, typically plotting measured flux or magnitude against time across one or more wavelength bands. In robotics and AI-driven astronomy, light curves are fundamental observational products generated by automated and robotic telescope systems that continuously monitor the sky. They are used to study an enormous range of phenomena: the explosive brightening and fading of supernovae and gamma-ray bursts, the periodic dimming caused by transiting exoplanets or stellar pulsations, the variability of active galactic nuclei and blazars, and the rotational modulation of starspots. Machine learning algorithms are increasingly applied to classify, detect anomalies in, and extract physical parameters from large light curve datasets produced by wide-field robotic surveys. Light curves matter because they encode the physical processes driving astrophysical events — energy release rates, distances, masses, and environmental conditions — making them an indispensable diagnostic tool for both fundamental science and the development of intelligent, automated observing systems capable of responding in real time to transient events.
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THE FIRST SYSTEMATIC STUDY OF TYPE Ibc SUPERNOVA MULTI-BAND LIGHT CURVES
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Multi-colour optical monitoring of eight red blazars
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Rates of superluminous supernovae at z ∼ 0.2
R. Quimby, F. Yuan, Carl W. Akerlof, J. C. Wheeler
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DISCOVERY OF THE ULTRA-BRIGHT TYPE II-L SUPERNOVA 2008es
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Starspot photometry with robotic telescopes
K. G. Strassmeier, J. Bartus, G. Cutispoto, M. Rodonò
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The Katzman Automatic Imaging Telescope Gamma‐Ray Burst Alert System, and Observations of GRB 020813
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Decay of the GRB 990123 Optical Afterglow: Implications for the Fireball Model
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Citations: 112 • 1999
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HAT<scp>net</scp>Variability Survey in the High Stellar Density "Kepler Field" with Millimagnitude Image Subtraction Photometry
J. D. Hartman, G. Á. Bakos, K. Z. Stanek, R. W. Noyes
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Photometric AGN reverberation mapping – an efficient tool for BLR sizes, black hole masses, and host-subtracted AGN luminosities
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C. G. Mundell, A. Melandri, C. Guidorzi, S. Kobayashi, I. A. Steele, D. Malesani, L. Amati, P. D’Avanzo, D. Bersier, A. Gomboc, E. Rol, M. F. Bode, D. Carter, C. J. Mottram, A. Monfardini, R. J. Smith, Sangeeta Malhotra, J. Wang, N. Bannister, P. T. O’Brien, N. R. Tanvir
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Citations: 93 • 2003
GRB 091024A AND THE NATURE OF ULTRA-LONG GAMMA-RAY BURSTS
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Citations: 91 • 2013
Discovery Of The Ultra-Bright Type II-L Supernova 2008es
Citations: 88 • 2016
Realisation of a fully‐deterministic microlensing observing strategy for inferring planet populations
M. Dominik, U. G. Jørgensen, Nicholas J. Rattenbury, M. Mathiasen, T. C. Hinse, S. Calchi Novati, K. Harpsøe, V. Bozza, T. Anguita, M. Burgdorf, K. Horne, M. Hundertmark, E. Kerins, P. Kjærgaard, C. Liebig, L. Mancini, G. Masi, S. Rahvar, D. Ricci, G. Scarpetta, C. Snodgrass, J. Southworth, R. A. Street, J. Surdej, C. C. Thöne, Y. Tsapras, J. Wambsganß, M. Zub
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An anomaly detector with immediate feedback to hunt for planets of Earth mass and below by microlensing
M. Dominik, Nicholas J. Rattenbury, A. Allan, Shude Mao, D. M. Bramich, M. Burgdorf, E. Kerins, Y. Tsapras, Ł. Wyrzykowski
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CLUES TO THE NATURE OF SN 2009ip FROM PHOTOMETRIC AND SPECTROSCOPIC EVOLUTION TO LATE TIMES
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Standard Galactic Field RR Lyrae. I. Optical to Mid-infrared Phased Photometry
Andrew Monson, Rachael L. Beaton, Victoria Scowcroft, Wendy L. Freedman, Barry F. Madore, J. Rich, Mark Seibert, Juna A. Kollmeier, G. Clementini
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Optical variability of the BL Lacertae object GC 0109+224
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Long‐Term<i>VRI</i>Photometry of Small‐Amplitude Red Variables. I. Light Curves and Periods
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