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A Systematic Search of Zwicky Transient Facility Data for Ultracompact Binary LISA-detectable Gravitational-wave Sources

Burdge, Kevin B. and Prince, Thomas A. and Fuller, Jim and Kaplan, David L. and Marsh, Thomas R. and Tremblay, Pier-Emmanuel and Zhuang, Zhuyun and Bellm, Eric C. and Caiazzo, Ilaria and Coughlin, Michael W. and Dhillon, Vik S. and Gaensicke, Boris and Rodríguez-Gil, Pablo and Graham, Matthew J. and Hermes, J. J. and Kupfer, Thomas and Littlefair, S. P. and Mróz, Przemek and Phinney, E. S. and van Roestel, Jan and Yao, Yuhan and Dekany, Richard G. and Drake, Andrew J. and Duev, Dmitry A. and Hale, David and Feeney, Michael and Helou, George and Kaye, Stephen and Mahabal, Ashish A. and Masci, Frank J. and Riddle, Reed and Smith, Roger and Soumagnac, Maayane T. and Kulkarni, S. R. (2020) A Systematic Search of Zwicky Transient Facility Data for Ultracompact Binary LISA-detectable Gravitational-wave Sources. Astrophysical Journal, 905 (1). Art. No. 32. ISSN 1538-4357. doi:10.3847/1538-4357/abc261.

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Using photometry collected with the Zwicky Transient Facility, we are conducting an ongoing survey for binary systems with short orbital periods (P_b < 1 hr) with the goal of identifying new gravitational-wave sources detectable by the upcoming Laser Interferometer Space Antenna (LISA). We present a sample of 15 binary systems discovered thus far, with orbital periods ranging from 6.91 to 56.35 minutes. Of the 15 systems, seven are eclipsing systems that do not show signs of significant mass transfer. Additionally, we have discovered two AM Canum Venaticorum systems and six systems exhibiting primarily ellipsoidal variations in their lightcurves. We present follow-up spectroscopy and high-speed photometry confirming the nature of these systems, estimates of their LISA signal-to-noise ratios, and a discussion of their physical characteristics.

Item Type:Article
Related URLs:
URLURL TypeDescription Paper
Burdge, Kevin B.0000-0002-7226-836X
Prince, Thomas A.0000-0002-8850-3627
Fuller, Jim0000-0002-4544-0750
Kaplan, David L.0000-0001-6295-2881
Marsh, Thomas R.0000-0002-2498-7589
Tremblay, Pier-Emmanuel0000-0001-9873-0121
Zhuang, Zhuyun0000-0002-1945-2299
Bellm, Eric C.0000-0001-8018-5348
Caiazzo, Ilaria0000-0002-4770-5388
Coughlin, Michael W.0000-0002-8262-2924
Dhillon, Vik S.0000-0003-4236-9642
Gaensicke, Boris0000-0002-2761-3005
Rodríguez-Gil, Pablo0000-0002-4717-5102
Graham, Matthew J.0000-0002-3168-0139
Hermes, J. J.0000-0001-5941-2286
Kupfer, Thomas0000-0002-6540-1484
Littlefair, S. P.0000-0001-7221-855X
Mróz, Przemek0000-0001-7016-1692
Phinney, E. S.0000-0002-9656-4032
van Roestel, Jan0000-0002-2626-2872
Yao, Yuhan0000-0001-6747-8509
Dekany, Richard G.0000-0002-5884-7867
Duev, Dmitry A.0000-0001-5060-8733
Helou, George0000-0003-3367-3415
Mahabal, Ashish A.0000-0003-2242-0244
Masci, Frank J.0000-0002-8532-9395
Riddle, Reed0000-0002-0387-370X
Smith, Roger0000-0001-7062-9726
Soumagnac, Maayane T.0000-0001-6753-1488
Kulkarni, S. R.0000-0001-5390-8563
Additional Information:© 2020. The American Astronomical Society. Received 2020 September 4; revised 2020 October 13; accepted 2020 October 15; published 2020 December 9. K.B.B. thanks the National Aeronautics and Space Administration and the Heising-Simons Foundation for supporting his research. M.W.C. acknowledges support from the National Science Foundation with grant No. PHY-2010970. P.R.-G. acknowledges support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU), and the European Regional Development Fund (FEDER) under grant AYA2017–83383–P. V.S.D., ULTRACAM, and HiPERCAM are supported by STFC. The research leading to these results has received funding from the European Research Council under the European Union's Horizon 2020 research and innovation program numbers 677706 (WD3D) and 340040 (HiPERCAM). This work is 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 National Science Foundation under grant No. 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 UW. This work is based on observations made with the Gran Telescopio Canarias (GTC) installed in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. This work is based on observations made at the European Southern Observatory New Technology Telescope (NTT), La Silla. The KPED team thanks the National Science Foundation and the National Optical Astronomical Observatory for making the Kitt Peak 2.1 m telescope available. The KPED team thanks the National Science Foundation, the National Optical Astronomical Observatory, and the Murty family for support in the building and operation of KPED. In addition, they thank the CHIMERA project for use of the Electron Multiplying CCD (EMCCD). Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. This article is based on observations made in the Observatorios de Canarias del IAC with the William Herschel Telescope operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Observatorio del Roque de los Muchachos. This research benefited from interactions at the ZTF Theory Network Meeting that were funded by the Gordon and Betty Moore Foundation through grant GBMF5076 and support from the National Science Foundation through PHY-1748958. Facilities: PO:1.2 m (ZTF) - , KPNO:2.1 m (KPED) - , NTT (ULTRACAM) - , Hale (CHIMERA - , DBSP) - , GTC (HiPERCAM) - , Keck:I (LRIS). -
Group:Astronomy Department, Infrared Processing and Analysis Center (IPAC), TAPIR, Zwicky Transient Facility
Funding AgencyGrant Number
Heising-Simons FoundationUNSPECIFIED
Ministerio de Ciencia, Innovación y Universidades (MICIU)AYA2017-83383-P
Fondo Europeo de Desarrollo Regional (FEDER)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
European Research Council (ERC)677706
European Research Council (ERC)340040
ZTF partner institutionsUNSPECIFIED
National Optical Astronomy Observatory (NOAO)UNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Gordon and Betty Moore FoundationGBMF5076
Subject Keywords:Compact binary stars ; Close binary stars ; Interacting binary stars ; Eclipsing binary stars ; Ellipsoidal variable stars ; Gravitational wave sources ; White dwarf stars
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Compact binary stars (283); Close binary stars (254); Interacting binary stars (801); Eclipsing binary stars (444); Ellipsoidal variable stars (455); Gravitational wave sources (677); White dwarf stars (1799)
Record Number:CaltechAUTHORS:20200916-113006965
Persistent URL:
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:105433
Deposited By: George Porter
Deposited On:16 Sep 2020 20:39
Last Modified:16 Nov 2021 18:43

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