Erratum: “The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions” (2017, AJ, 154, 211)

Kevin Krisciunas , Carlos Contreras, Christopher R. Burns , M. M. Phillips , Mario Hamuy, Maximilian D. Stritzinger , Jorge Anais, Luis Boldt, Luis Busta , Abdo Campillay, Sergio Castellón, Gastón Folatelli, Wendy L. Freedman , Consuelo González, Eric Y. Hsiao, Wojtek Krzeminski, Nidia Morrell, Sven Eric Persson, Miguel Roth, Francisco Salgado , Jacqueline Serón, Nicholas B. Suntzeff , Simón Torres, Alexei V. Filippenko , Weidong Li, Barry F. Madore , D. L. Depoy, Jennifer L. Marshall , Jean-Philippe Rheault, and Steven Villanueva 1 George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA; krisciunas@physics.tamu.edu 2 Carnegie Observatories, Las Campanas Observatory, Casilla 601, La Serena, Chile 3 Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, DK-8000 Aarhus C, Denmark 4 Observatories of the Carnegie Institution for Science, 813 Santa Barbara St., Pasadena, CA 91101, USA 5 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile 6 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Instituto de Astrofísica de La Plata (IALP), CONICET, Paseo del Bosque S/N, B1900FWA La Plata, Argentina 7 Department of Astronomy and Astrophysics, University of Chicago, 5640 South Ellis Ave., Chicago, IL 60637, USA 8 Department of Physics, Florida State University, Tallahassee, FL 32306, USA 9 GMTO Corporation, Avenida Presidente Riesco 5335, Suite 501, Las Condes, Santiago, Chile 10 Leiden Observatory, Leiden University, PO Box 9513, NL-2300 RA Leiden, The Netherlands 11 Cerro Tololo Inter-American Observatory, Casilla 603, La Serena, Chile 12 SOAR Telescope, Casilla 603, La Serena, Chile 13 Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA 14 Infrared Processing and Analysis Center, Caltech/Jet Propulsion Laboratory, Pasadena, CA 91125, USA 15 Department of Astronomy, Ohio State University, Columbus, OH 43210, USA Received 2020 October 20; published 2020 November 26


Minor Corrections
In Table 1 the declination of SN2005ku should read −00:00:49.3. The arithmetical sign was wrong. In Table 4 the i-band color term should be identically zero. Revised versions of Tables 1 and 4 are given here in their entirety. In Table 4 note the two different values of the J-band color term for the duPont telescope. Only one was given in the original published version of this paper (Krisciunas et al. 2017a). This omission has already been noted in a published erratum (Krisciunas et al. 2017b).

Field Star Photometry of Our Supernovae
David Rubin, presently at the University of Hawaii, kindly pointed out a problem with Table 5 of our paper. Rubin compared PanSTARRS photometry of field stars with our photometry. He found no problems with the g′r′i′ data. Then he used nonlinear color transformations to compute (i.e., predict) V-band values and used nonlinear transformations and incorporated u′−g′ as an extra color to compute B-band values. There were no problems revealed in the preliminary BV photometry of field stars presented in CSP-I Data Release 2 (Stritzinger et al. 2011), but Rubin found systematic errors in our Band V-band photometry presented in the third (and final) data release paper of CSP-I (Krisciunas et al. 2017a).
We have identified the cause of the problem. Recall that the procedure for our natural system photometry is: (1) Observe fields of standard stars at a range of air masses, and derive color terms and extinction coefficients.
(2) Invert the color equations and transform the standard Sloan u′g′r′i′ photometry (Smith et al. 2002) and BV magnitudes (Landolt 1992) into CSP natural magnitudes.
(3) Calibrate our local sequence stars relative to these natural magnitudes. Note that there are no color terms to deal with here, only extinction coefficients and nightly zero-points. (4) Calibrate supernova photometry relative to local sequences. Supernova photometry is therefore in the natural system of the telescope and camera. (5) Reapply the color terms to convert local sequence star photometry into the standard system for publication.    The mistake happened in step number 5. Thus, if one wishes to use our BV photometry of field stars in the standard system, one should use the revised values in the accompanying table. It is important to note that our SN photometry (which is in the natural system) is not affected by the error described here.
An abbreviated version of Table 5 is given here. The full machine readable table will be available online.  (029) Note. This table replaces Table5 of Krisciunas et al. (2017a) and is published in its entirety in the electronic edition of the journal. A portion is shown here for guidance regarding its form and content. The previously published u′g′r′i′ photometry was correct. Here we present revised Band V-band photometry. a All photometry is measured in magnitudes. Values in parentheses are 1σ uncertainties, measured in thousandths of a magnitude. This photometry of field stars is in the two standard systems, not the natural system.
(This table is available in its entirety in machine-readable form.)