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The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions

Krisciunas, Kevin and Madore, Barry F. (2017) The Carnegie Supernova Project. I. Third Photometry Data Release of Low-redshift Type Ia Supernovae and Other White Dwarf Explosions. Astronomical Journal, 154 (5). Art. No. 211. ISSN 1538-3881.

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We present final natural-system optical (ugriBV) and near-infrared (YJH) photometry of 134 supernovae (SNe) with probable white dwarf progenitors that were observed in 2004–2009 as part of the first stage of the Carnegie Supernova Project (CSP-I). The sample consists of 123 Type Ia SNe, 5 Type Iax SNe, 2 super-Chandrasekhar SN candidates, 2 Type Ia SNe interacting with circumstellar matter, and 2 SN 2006bt-like events. The redshifts of the objects range from z = 0.0037 to 0.0835; the median redshift is 0.0241. For 120 (90%) of these SNe, near-infrared photometry was obtained. Average optical extinction coefficients and color terms are derived and demonstrated to be stable during the five CSP-I observing campaigns. Measurements of the CSP-I near-infrared bandpasses are also described, and near-infrared color terms are estimated through synthetic photometry of stellar atmosphere models. Optical and near-infrared magnitudes of local sequences of tertiary standard stars for each supernova are given, and a new calibration of Y-band magnitudes of the Persson et al. standards in the CSP-I natural system is presented.

Item Type:Article
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URLURL TypeDescription Paper - 2017 December - 2020 December
Krisciunas, Kevin0000-0002-6650-694X
Madore, Barry F.0000-0002-1576-1676
Additional Information:© 2017 The American Astronomical Society. Original content from this work may be used under the terms of the Creative Commons Attribution 3.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI. Received 2017 July 20; revised 2017 September 12; accepted 2017 September 12; published 2017 November 6. This paper is dedicated to the memory of our dear colleague, Wojtek Krzeminski (1933–2017), who played an important role in the early history of Las Campanas Observatory and who, during his retirement, obtained many of the observations presented in this paper. The CSP particularly thanks the mountain staff of the Las Campanas Observatory for their assistance throughout the duration of our observational program, and Jim Hughes and Skip Schaller for computer support. Special thanks are due to Allyn Smith and Douglas Tucker for allowing us to publish their u’g’r’i’ magnitudes of P177D and P330E (and to Dan Scolnic for leading us to Allyn and Douglas). This project was supported by NSF under grants AST-0306969, AST-0908886, AST-0607438, and AST-1008343. M.D.S., C.C., and E.H. acknowledge generous support from the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. M.D.S. is supported by a research grant (13261) from VILLUM FONDEN. M.H. acknowledges support by CONICYT through grants FONDECYT Regular 1060808, Centro de Astrofísica FONDAP 15010003, Centro BASAL CATA (PFB–06), and by the Millennium Center for Supernova Science (P06–045-F). A.V.F. is grateful for the financial support of the NSF, the Richard and Rhoda Goldman Fund, the TABASGO Foundation, the Christopher R. Redlich Fund, and the Miller Institute for Basic Research in Science (University of California, Berkeley). This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. N.S. is grateful for the support provided by the Mitchell/Heep/Munnerlyn Chair in Observational Astronomy at Texas A&M University. The CSP thanks the Mitchell Foundation and Sheridan Lorenz for sponsoring our group meetings at Cook's Branch Nature Conservancy. We thank the Lick Observatory staff for their assistance with the operation of KAIT. LOSS, which discovered many of the SNe studied here, has been supported by many grants from the NSF (most recently AST-0908886 and AST-1211916), the TABASGO Foundation, U.S. Department of Energy SciDAC grant DE-FC02-06ER41453, and U.S. Department of Energy grant DE-FG02-08ER41563. KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the Hewlett-Packard Company, AutoScope Corporation, Lick Observatory, the NSF, the University of California, the Sylvia & Jim Katzman Foundation, and the TABASGO Foundation. We give particular thanks to Russ Genet, who made KAIT possible with his initial special gift, and the TABASGO Foundation, without which this work would not have been completed.
Errata:December 2017: Kevin Krisciunas et al 2017 AJ 154 278; December 2020: Kevin Krisciunas et al 2020 AJ 160 289.
Group:Infrared Processing and Analysis Center (IPAC)
Funding AgencyGrant Number
Agency for Science and Technology and Innovation (Denmark)UNSPECIFIED
Fondo Nacional de Desarrollo Científico y Tecnológico (FONDECYT)1060808
Fondo de Financiamiento de Centros de Investigación en Áreas Prioritarias (FONDAP)15010003
Millennium Center for SupernovaP06-045-F
Richard and Rhoda Goldman FundUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
Miller Institute for Basic Research in ScienceUNSPECIFIED
Department of Energy (DOE)DE-FC02-06ER41453
Department of Energy (DOE)DE-FG02-08ER41563
Sun Microsystems, Inc.UNSPECIFIED
Hewlett-Packard CompanyUNSPECIFIED
AutoScope CorporationUNSPECIFIED
Lick ObservatoryUNSPECIFIED
University of CaliforniaUNSPECIFIED
Sylvia and Jim Katzman FoundationUNSPECIFIED
Subject Keywords:instrumentation: photometers – supernovae: general – surveys – techniques: photometric
Issue or Number:5
Record Number:CaltechAUTHORS:20171106-101722601
Persistent URL:
Official Citation:Kevin Krisciunas et al 2017 AJ 154 211
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:82977
Deposited By: Tony Diaz
Deposited On:06 Nov 2017 18:32
Last Modified:03 Dec 2020 23:49

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