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2013, AJ,Zasowski, G., Cohen, R. E., Chojnowski, S. D., et al. ApJS, 219, 12Ammons, S. M., Robinson, S. E., Strader, J., et al. The TIC is available on the STScI MAST server, and an enhanced CTL is available through the Filtergraph data visualization portal system at the URL https://filtergraph.vanderbilt.edu/tess-ctl. The points represent actual measurements for a set of stars from TICv7.Comparison of T eff from dereddened photometric colors versus spectroscopic. 2018, A&A, 615,Zacharias, N., Finch, C. T., Girard, T. M., et al. overview of the WISE mission, facilities, and operations, a detailed To determine masses for at least 50 planets with radii smaller than 4 that the set of targets for TESS be optimized for detection of small planets.of bright stars that are likely to be dwarfs across the skyconsideration is to assemble a list of dwarf stars all oenough for TESS to observe, and taking extra steps to include the scientifically vdesired ranges in apparent magnitude and spectral type, and to eliminate evolved stars.exclusion from the CTL. 2011, AJ, 142,Brown, T. M., Latham, D. W., Everett, M. E., & Esquerdo,Buder, S., Asplund, M., Duong, L., et al. achieving 5-sigma point source sensitivities per band better than 0.08, DOI: 10.3847/1538-3881/aad050. that describe known limitations of the All-Sky Release products. The Explanatory Supplement is 2006, AJ,Sliski, D. H., & Kipping, D. M. 2014, ApJ, 788, 148Soubiran, C., Le Campion, J.-F., Brouillet, N., & Chemin,Stassun, K. G., Oelkers, R. J., Pepper, J., et al. 2018, AJ,Stassun, K. G., Collins, K. A., & Gaudi, B. S. 2017, AJ,von Essen, C., Ofir, A., Dreizler, S., et al. and formats of the image and tabular data products, and cautionary notes maintained at: We also describe a revised ranking system for prioritizing stars for 2 minute cadence observations, and we assemble a revised Candidate Target List (CTL) using that ranking. It is a pleasure to thank the members of the TESS Target Selection Working Group for their input regarding the development of the procedures described here, including especially the contribution of the specially curated target lists. 2017,Akeson, R. L., Chen, X., Ciardi, D., et al. We describe the catalogs assembled and the algorithms used to populate the revised TESS Input Catalog (TIC), based on the incorporation of the Gaia second data release. The median T eff difference is ≈20 K, and the 95th percentile range is −410 K to +220 K.Flux contamination as a function of sky position in TICv8.All content in this area was uploaded by Philip Muirhead on Dec 01, 2019 the Filtergraph data visualization portal system at the URL The TESS Input Catalog (TIC) is a comprehensive collection of sources on the skyto select target stars to observe, and to provide stellar parameters useful for the evTIC is intended to enable the selection of optimal targets for the planet transit search, to enable calculation of fluxcontamination in the TESS aperture for each target, and to provide reliable stellar radii for calculating planetary radii,which in turn determines the targets that will receive mission-supported photometric and spectroscopic follow-up.The area of the sky projected onto each TESS pixel is large (21is typically 1–2 pixels in radius (depending on stellar brightness and position in the focal plane).the photometric aperture surrounding a given TESS target may include flux from multiple objects.important that the TIC contain every optically luminous, persistent, non-moving object in the skyAn initial version of the TIC for use in the first year of TESS observstars in the TIC had their properties calculated from broadband photometry (and spectroscopy in a tiny minority ofcases), on the basis of a complex set of logic rules, algorithms, and empirical relations,radii accurately for the vast majority of the stars in the TIC.
the Jet Propulsion Laboratory/California Institute of Technology, funded astrometric characteristics and completeness and reliability of the
2016, A&A,Deleuil, M., Meunier, J. C., Moutou, C., et al. which stars to observe at the two-minute cadence is driven by the need to detect small transiting planets, which leads to the selection of primarily bright, cool dwarfs. We describe the catalogs assembled and the algorithms used to populate the TESS Input Catalog (TIC).

Release data products include: (1) an Atlas of
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