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Astronomical Image Time Series Segmentation for Faint, Fast Object Detection

  • Authors: Dan Caselden, J. Davy Kirkpatrick, Lindsey Lack, Andrew White, Federico Marocco, Aaron M. Meisner, Guillaume Colin, Bruce Baller, Kareem Ammar, Thomas P. Bickle, Hunter Brooks, S. L. Casewell, Peter R. M. Eisenhardt, Charles A. Elachi, Jacqueline K. Faherty, John W. Fowler, Daniella C. Bardalez Gagliuffi, Jonathan Gagné, Christopher R. Gelino, Jake Grigorian, Les Hamlet, Hiro Higashimura, 村滉 東, Justin Hong, Issam Ibnouhsein, Tarun Kota, Marc J. Kuchner, Ken A. Marsh, Matteo Paz, Yadukrishna Raghu, Adam C. Schneider, Sajesh Singh, Asa Trek, Kieran Wall, Andrew Washburn, Edward L. Wright, David Zurek

Dan Caselden et al 2026 The Astronomical Journal 171 .

  • Provider: AAS Journals

Caption: Figure 7.

Comparisons between SMDET (x-axes) and J. D. Kirkpatrick et al. (2021a, y-axes) photometry (top) and astrometry (bottom). Solid lines show the best-fit linear corrections for SMDET photometry: y = x − 0.452 for W1 and y = x − 0.669 for W2. Dashed lines show y = x for reference. The reference data from J. D. Kirkpatrick et al. (2021a) are more precise, derived from Spitzer IRAC images that are deeper and have better angular resolution than unWISE images. We converted Spitzer IRAC to WISE magnitudes with the relations W1 ≃ (ch1 − 0.78505) × 0.89844−1 and W2 ≃ ch2.

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