NAOC Open IR
The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars
Arzoumanian, Zaven1,2; Brazier, Adam3; Burke-Spolaor, Sarah4,5; Chamberlin, Sydney6; Chatterjee, Shami3; Christy, Brian7; Cordes, James M.3; Cornish, Neil J.8; Crawford, Fronefield9; Cromartie, H. Thankful10; Crowter, Kathryn11; DeCesar, Megan E.12; Demorest, Paul B.13; Dolch, Timothy14; Ellis, Justin A.4,5; Ferdman, Robert D.15; Ferrara, Elizabeth C.16; Fonseca, Emmanuel17; Garver-Daniels, Nathan4,5; Gentile, Peter A.4,5; Halmrast, Daniel14,18; Huerta, E. A.19,20; Jenet, Fredrick A.21; Jessup, Cody14; Jones, Glenn22; Jones, Megan L.4,5; Kaplan, David L.23; Lam, Michael T.4,5; Lazio, T. Joseph W.24; Levin, Lina4,5; Lommen, Andrea25; Lorimer, Duncan R.4,5; Luo, Jing21; Lynch, Ryan S.26; Madison, Dustin27; Matthews, Allison M.10; McLaughlin, Maura A.4,5; McWilliams, Sean T.4,5; Mingarelli, Chiara28; Ng, Cherry11,29; Nice, David J.12; Pennucci, Timothy T.4,5,30,31; Ransom, Scott M.27; Ray, Paul S.32; Siemens, Xavier23; Simon, Joseph24; Spiewak, Renee23,33; Stairs, Ingrid H.11; Stinebring, Daniel R.34; Stovall, Kevin13; Swiggum, Joseph K.23; Taylor, Stephen R.24; Vallisneri, Michele24; van Haasteren, Rutger24,37; Vigeland, Sarah J.23; Zhu, Weiwei35,36
2018-04-01
Source PublicationASTROPHYSICAL JOURNAL SUPPLEMENT SERIES
ISSN0067-0049
Volume235Issue:2Pages:41
AbstractWe present high-precision timing data over time spans of up to 11 years for 45 millisecond pulsars observed as part of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav) project, aimed at detecting and characterizing low-frequency gravitational waves. The pulsars were observed with the Arecibo Observatory and/or the Green Bank Telescope at frequencies ranging from 327 MHz to 2.3 GHz. Most pulsars were observed with approximately monthly cadence, and six high-timing-precision pulsars were observed weekly. All were observed at widely separated frequencies at each observing epoch in order to fit for time-variable dispersion delays. We describe our methods for data processing, time-of-arrival (TOA) calculation, and the implementation of a new, automated method for removing outlier TOAs. We fit a timing model for each pulsar that includes spin, astrometric, and (for binary pulsars) orbital parameters; time-variable dispersion delays; and parameters that quantify pulse-profile evolution with frequency. The timing solutions provide three new parallax measurements, two new Shapiro delay measurements, and two new measurements of significant orbital-period variations. We fit models that characterize sources of noise for each pulsar. We find that 11 pulsars show significant red noise, with generally smaller spectral indices than typically measured for non-recycled pulsars, possibly suggesting a different origin. A companion paper uses these data to constrain the strength of the gravitational-wave background.
Keywordbinaries: general gravitational waves parallaxes proper motions pulsars: general stars: neutron
Funding OrganizationNational Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences
DOI10.3847/1538-4365/aab5b0
WOS KeywordBLACK-HOLE BINARIES ; RELATIVISTIC CELESTIAL MECHANICS ; CONTINUOUS GRAVITATIONAL-WAVES ; GENERAL-RELATIVITY ; PROPER MOTIONS ; ARRAY LIMITS ; SPIN NOISE ; PARALLAXES ; RADIATION ; GRAVITY
Language英语
Funding ProjectNational Science Foundation (NSF) Physics Frontiers Center[1430284] ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Simons Foundation ; University of Toronto ; NASA Einstein Fellowship[PF4-150120] ; NASA Einstein Fellowship[PF3-140116] ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB23000000]
Funding OrganizationNational Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Science Foundation (NSF) Physics Frontiers Center ; National Science Foundation (NSF) Physics Frontiers Center ; NSERC Discovery Grant ; NSERC Discovery Grant ; Canadian Institute for Advanced Research ; Canadian Institute for Advanced Research ; Simons Foundation ; Simons Foundation ; University of Toronto ; University of Toronto ; NASA Einstein Fellowship ; NASA Einstein Fellowship ; CAS Pioneer Hundred Talents Program ; CAS Pioneer Hundred Talents Program ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000429560000002
PublisherIOP PUBLISHING LTD
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/37188
Collection中国科学院国家天文台
Corresponding AuthorNice, David J.
Affiliation1.NASA, Goddard Space Flight Ctr, Ctr Res & Explorat Space Sci & Technol, Code 662, Greenbelt, MD 20771 USA
2.NASA, Goddard Space Flight Ctr, XRay Astrophys Lab, Code 662, Greenbelt, MD 20771 USA
3.Cornell Univ, Dept Astron, Ithaca, NY 14853 USA
4.West Virginia Univ, Dept Phys & Astron, POB 6315, Morgantown, WV 26506 USA
5.West Virginia Univ, Ctr Gravitat Waves & Cosmol, Chestnut Ridge Res Bldg, Morgantown, WV 26505 USA
6.Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA
7.Notre Dame Maryland Univ, Dept Math Comp Sci & Phys, 4701 N Charles St, Baltimore, MD 21210 USA
8.Montana State Univ, Dept Phys, Bozeman, MT 59717 USA
9.Franklin & Marshall Coll, Dept Phys & Astron, POB 3003, Lancaster, PA 17604 USA
10.Univ Virginia, Dept Astron, POB 400325, Charlottesville, VA 22904 USA
11.Univ British Columbia, Dept Phys & Astron, 6224 Agr Rd, Vancouver, BC V6T 1Z1, Canada
12.Lafayette Coll, Dept Phys, Easton, PA 18042 USA
13.Natl Radio Astron Observ, 1003 Lopezville Rd, Socorro, NM 87801 USA
14.Hillsdale Coll, Dept Phys, 33 E Coll St, Hillsdale, MI 49242 USA
15.Univ East Anglia, Sch Chem, Norwich NR4 7TJ, Norfolk, England
16.NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
17.McGill Univ, Dept Phys, 3600 Univ St, Montreal H3A 2T8, PQ H3A 2T8, Canada
18.Univ Calif Santa Barbara, Dept Math, Santa Barbara, CA 93106 USA
19.Univ Illinois, NCSA, Urbana, IL 61801 USA
20.Univ Illinois, Dept Astron, Urbana, IL 61801 USA
21.Univ Texas Rio Grande Valley, Ctr Gravitat Wave Astron, Brownsville, TX 78520 USA
22.Columbia Univ, Dept Phys, New York, NY 10027 USA
23.Univ Wisconsin, Dept Phys, Ctr Gravitat Cosmol & Astrophys, POB 413, Milwaukee, WI 53201 USA
24.CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
25.Haverford Coll, Dept Phys & Astron, Haverford, PA 19041 USA
26.Green Bank Observ, POB 2, Green Bank, WV 24944 USA
27.Natl Radio Astron Observ, 520 Edgemont Rd, Charlottesville, VA 22903 USA
28.Flatiron Inst, Ctr Computat Astrophys, 10010,162 5th Ave, New York, NY 10010 USA
29.Univ Toronto, Dunlap Inst Astron & Astrophys, 50 St George St, Toronto, ON M5S 3H4, Canada
30.Eotvos Lorand Univ, Inst Phys, Pazmany Ps 1-A, H-1117 Budapest, Hungary
31.Hungarian Acad Sci, MTA ELTE Extragalat Astrophys Res Grp, H-1117 Budapest, Hungary
32.Naval Res Lab, Space Sci Div, Washington, DC 20375 USA
33.Swinburne Univ Technol, Ctr Astrophys & Supercomp, POB 218, Hawthorn, Vic 3122, Australia
34.Oberlin Coll, Dept Phys & Astron, Oberlin, OH 44074 USA
35.Chinese Acad Sci, Natl Astron Observ, 20A Datun Rd, Beijing 100012, Peoples R China
36.Max Planck Inst Radio Astron, Hugel 69, D-53121 Bonn, Germany
37.Microsoft Corp, Redmond, WA 98052 USA
Recommended Citation
GB/T 7714
Arzoumanian, Zaven,Brazier, Adam,Burke-Spolaor, Sarah,et al. The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars[J]. ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,2018,235(2):41.
APA Arzoumanian, Zaven.,Brazier, Adam.,Burke-Spolaor, Sarah.,Chamberlin, Sydney.,Chatterjee, Shami.,...&Zhu, Weiwei.(2018).The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars.ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES,235(2),41.
MLA Arzoumanian, Zaven,et al."The NANOGrav 11-year Data Set: High-precision Timing of 45 Millisecond Pulsars".ASTROPHYSICAL JOURNAL SUPPLEMENT SERIES 235.2(2018):41.
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