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Cataclysmic Variables in the First Year of the Zwicky Transient Facility

Szkody, Paula and Dicenzo, Brooke and Ho, Anna Y. Q. and Hillenbrand, Lynne A. and van Roestel, Jan and Ridder, Margaret and Lima, Isabel DeJesus and Graham, Melissa L. and Bellm, Eric C. and Burdge, Kevin and Kupfer, Thomas and Prince, Thomas A. and Masci, Frank J. and Mróz, Przemyslaw J. and Golkhou, V. Zach and Coughlin, Michael and Cunningham, Virginia A. and Dekany, Richard and Graham, Matthew J. and Hale, David and Kaplan, David and Kasliwal, Mansi M. and Miller, Adam A. and Neill, James D. and Patterson, Maria T. and Riddle, Reed and Smith, Roger and Soumagnac, Maayanne T. (2020) Cataclysmic Variables in the First Year of the Zwicky Transient Facility. . (Unpublished)

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Using selection criteria based on amplitude, time and color, we have identified 329 objects as known or candidate cataclysmic variable (CVs) during the first year of testing and operation of the Zwicky Transient Facility (ZTF). Of these, 90 are previously confirmed CVs, 218 are strong candidates based on the shape and color of their light curves obtained during 3-562 days of observations, and the remaining 21 are possible CVs but with too few data points to be listed as good candidates. Almost half the strong candidates are within 10 deg of the galactic plane, in contrast to most other large surveys which have avoided crowded fields. The available Gaia parallaxes are consistent with sampling the low mass transfer CVs, as predicted by population models. Our followup spectra have confirmed Balmer/helium emission lines in 27 objects, with four showing high excitation HeII emission, including candidates for an AM CVn, a polar and an intermediate polar. Our results demonstrate that a complete survey of the galactic plane is needed to accomplish an accurate determination of the number of CVs existing in the Milky Way.

Item Type:Report or Paper (Discussion Paper)
Related URLs:
URLURL TypeDescription Paper
Szkody, Paula0000-0003-4373-7777
Ho, Anna Y. Q.0000-0002-9017-3567
van Roestel, Jan0000-0002-2626-2872
Graham, Melissa L.0000-0002-9154-3136
Bellm, Eric C.0000-0001-8018-5348
Burdge, Kevin0000-0002-7226-836X
Kupfer, Thomas0000-0002-6540-1484
Prince, Thomas A.0000-0002-8850-3627
Masci, Frank J.0000-0002-8532-9395
Golkhou, V. Zach0000-0001-8205-2506
Coughlin, Michael0000-0002-8262-2924
Graham, Matthew J.0000-0002-3168-0139
Kaplan, David0000-0001-6295-2881
Kasliwal, Mansi M.0000-0002-5619-4938
Miller, Adam A.0000-0001-9515-478X
Neill, James D.0000-0002-0466-1119
Patterson, Maria T.0000-0002-4753-3387
Riddle, Reed0000-0002-0387-370X
Additional Information:Received December 10, 2019; Accepted February 16, 2010. PS and BD acknowledge funding from NSF grant AST-1514737. A.Y.Q.H. is supported by a National Science Foundation Graduate Research Fellowship under Grant No.DGE-1144469. MC is supported by the David and Ellen Lee Prize Postdoctoral Fellowship at the California Institute of Technology. MLG acknowledges support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation. We would like to thank occasional observers on the UW APO ZTF follow-up team, including: Brigitta Sipőcz, James Davenport, Daniela Huppenkothen, Dino Bektešević, Gwendolyn Eadie, and Bryce T. Bolin. The authors thank the Observatoire de la Côte d’Azur for support. This work was supported by the GROWTH project funded by the National Science Foundation under PIRE Grant No. 1545949. Based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the NSF under grant AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley national Laboratories. Operations are conducted by COO, IPAC and The SED Machine is based upon work supported by NSF under grant 1106171. Some observations were made with the Apache Point 3.5m telescope, which is owned and operated by the Astrophysical Research Corporation. The Liverpool Telescope is operated on the is land of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Facilities: APO:3.5m; Hale; ING:Herschel; Keck:I; Liverpool:2m; PO:1.2m; PO:1.5m
Group:Astronomy Department, LIGO, TAPIR, Zwicky Transient Facility
Funding AgencyGrant Number
NSF Graduate Research FellowshipDGE-1144469
David and Ellen Lee Postdoctoral ScholarshipUNSPECIFIED
University of WashingtonUNSPECIFIED
Charles and Lisa Simonyi Fund for Arts and SciencesUNSPECIFIED
Washington Research FoundationUNSPECIFIED
Infrared Processing and Analysis Center (IPAC)UNSPECIFIED
Weizmann Institute of ScienceUNSPECIFIED
Stockholm UniversityUNSPECIFIED
University of MarylandUNSPECIFIED
Deutsches Elektronen-SynchrotronUNSPECIFIED
Humboldt UniversityUNSPECIFIED
Los Alamos National Laboratory (LANL)UNSPECIFIED
University of Wisconsin-MilwaukeeUNSPECIFIED
Lawrence Berkeley National LaboratoryUNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Subject Keywords:editorials, notices — miscellaneous — catalogs — surveys
Record Number:CaltechAUTHORS:20200311-102354791
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:101850
Deposited By: Tony Diaz
Deposited On:11 Mar 2020 17:51
Last Modified:11 Mar 2020 17:51

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