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The NANOGrav Collaboration receives support from National Science Foundation (NSF) Physics Frontiers Center award Nos. 1430284 and 2020265, the Gordon and Betty Moore Foundation, NSF AccelNet award No. 2114721, an NSERC Discovery Grant, and CIFAR. The Arecibo Observatory is a facility of the NSF operated under cooperative agreement (AST-1744119) by the University of Central Florida (UCF) in alliance with Universidad Ana G. Mendez (UAGM) and Yang Enterprises (YEI), Inc. The Green Bank Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. The National Radio Astronomy Observatory is a facility of the NSF operated under cooperative agreement by Associated Universities, Inc. This work was conducted using the Thorny Flat HPC Cluster at West Virginia University (WVU), which is funded in part by National Science Foundation (NSF) Major Research Instrumentation Program (MRI) award No. 1726534 and West Virginia University. This work was also conducted in part using the resources of the Advanced Computing Center for Research and Education (ACCRE) at Vanderbilt University, Nashville, TN. NANOGrav is part of the International Pulsar Timing Array (IPTA); we would like to thank our IPTA colleagues for their help with this paper.L.B. acknowledges support from the National Science Foundation under award AST-1909933 and from the Research Corporation for Science Advancement under Cottrell Scholar award No. 27553. P.R.B. is supported by the Science and Technology Facilities Council, grant No. ST/W000946/1. S.B. gratefully acknowledges the support of a Sloan Fellowship and the support of NSF under award No. 1815664. M.C. and S.R.T. acknowledge support from NSF AST-2007993. M.C. and N.S.P. were supported by the Vanderbilt Initiative in Data Intensive Astrophysics (VIDA) Fellowship. Support for this work was provided by the NSF through the Grote Reber Fellowship Program administered by Associated Universities, Inc./National Radio Astronomy Observatory. Support for H.T.C. is provided by NASA through the NASA Hubble Fellowship Program grant No. HST-HF2-51453.001 awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. K.C. is supported by a UBC Four Year Fellowship (6456). M.E.D. acknowledges support from the Naval Research Laboratory by NASA under contract S-15633Y. T.D. and M.T.L. are supported by an NSF Astronomy and Astrophysics Grant (AAG) award No. 2009468. E.C.F. is supported by NASA under award No. 80GSFC21M0002. G.E.F., S.C.S., and S.J.V. are supported by NSF award PHY-2011772. The Flatiron Institute is supported by the Simons Foundation. A.D.J. and M.V. acknowledge support from the Caltech and Jet Propulsion Laboratory President's and Director's Research and Development Fund. A.D.J. acknowledges support from the Sloan Foundation. The work of N.La. and X.S. is partly supported by the George and Hannah Bolinger Memorial Fund in the College of Science at Oregon State University. N.La. acknowledges the support from Larry W. Martin and Joyce B. O'Neill Endowed Fellowship in the College of Science at Oregon State University. Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). D.R.L. and M.A.M. are supported by NSF No. 1458952. M.A.M. is supported by NSF No. 2009425. C.M.F.M. was supported in part by the National Science Foundation under grant Nos. NSF PHY-1748958 and AST-2106552. A.Mi. is supported by the Deutsche Forschungsgemeinschaft under Germany's Excellence Strategy-EXC 2121 Quantum Universe-390833306. The Dunlap Institute is funded by an endowment established by the David Dunlap family and the University of Toronto. K.D.O. was supported in part by NSF grant No. 2207267. T.T.P. acknowledges support from the Extragalactic Astrophysics Research Group at Eotvos Lorand University, funded by the Eotvos Lorand Research Network (ELKH), which was used during the development of this research. S.M.R. and I.H.S. are CIFAR Fellows. Portions of this work performed at NRL were supported by ONR 6.1 basic research funding. J.D.R. also acknowledges support from start-up funds from Texas Tech University. J.S. is supported by an NSF Astronomy and Astrophysics Postdoctoral Fellowship under award AST-2202388 and acknowledges previous support by the NSF under award 1847938. S.R.T. acknowledges support from NSF CAREER award No. 2146016. C.U. acknowledges support from BGU (Kreitman fellowship) and the Council for Higher Education and Israel Academy of Sciences and Humanities (Excellence fellowship). C.A.W. acknowledges support from CIERA, the Adler Planetarium, and the Brinson Foundation through a CIERA-Adler postdoctoral fellowship. O.Y. is supported by the National Science Foundation Graduate Research Fellowship under grant No. DGE-2139292.

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The NANOGrav 15 yr Data Set: Observations and Timing of 68 Millisecond Pulsars

Publicado en:Astrophysical Journal Letters. 951 (1): L9- - 2023-07-01 951(1), DOI: 10.3847/2041-8213/acda9a

Autores: Agazie, Gabriella; Alam, Md Faisal; Anumarlapudi, Akash; Archibald, Anne M; Arzoumanian, Zaven; Baker, Paul T; Blecha, Laura; Bonidie, Victoria; Brazier, Adam; Brook, Paul R; Burke-Spolaor, Sarah; Becsy, Bence; Chapman, Christopher; Charisi, Maria; Chatterjee, Shami; Cohen, Tyler; Cordes, James M; Cornish, Neil J; Crawford, Fronefield; Cromartie, H Thankful; Crowter, Kathryn; DeCesar, Megan E; Demorest, Paul B; Dolch, Timothy; Drachler, Brendan; Ferrara, Elizabeth C; Fiore, William; Fonseca, Emmanuel; Freedman, Gabriel E; Garver-Daniels, Nate; Gentile, Peter A; Glaser, Joseph; Good, Deborah C; Gueltekin, Kayhan; Hazboun, Jeffrey S; Jennings, Ross J; Jessup, Cody; Johnson, Aaron D; Jones, Megan L; Kaiser, Andrew R; Kaplan, David L; Kelley, Luke Zoltan; Kerr, Matthew; Key, Joey S; Kuske, Anastasia; Laal, Nima; Lam, Michael T; Lamb, William G; W Lazio, T Joseph W; Lewandowska, Natalia; Lin, Ye; Liu, Tingting; Lorimer, Duncan R; Luo, Jing; Lynch, Ryan S; Ma, Chung-Pei; Madison, Dustin R; Maraccini, Kaleb; McEwen, Alexander; McKee, James W; McLaughlin, Maura A; McMann, Natasha; Meyers, Bradley W; Mingarelli, Chiara M F; Mitridate, Andrea; Ng, Cherry; Nice, David J; Ocker, Stella Koch; Olum, Ken D; Panciu, Elisa; Pennucci, Timothy T; Perera, Benetge B P; Pol, Nihan S; Radovan, Henri A; Ransom, Scott M; Ray, Paul S; Romano, Joseph D; Salo, Laura; Sardesai, Shashwat C; Schmiedekamp, Carl; Schmiedekamp, Ann; Schmitz, Kai; Shapiro-Albert, Brent J; Siemens, Xavier; Simon, Joseph; Siwek, Magdalena S; Stairs, Ingrid H; Stinebring, Daniel R; Stovall, Kevin; Susobhanan, Abhimanyu; Swiggum, Joseph K; Taylor, Stephen R; Turner, Jacob E; Unal, Caner; Vallisneri, Michele; Vigeland, Sarah J; Wahl, Haley M; Wang, Qiaohong H; Witt, Caitlin A; Young, Olivia

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Resumen

We present observations and timing analyses of 68 millisecond pulsars (MSPs) comprising the 15 yr data set of the North American Nanohertz Observatory for Gravitational Waves (NANOGrav). NANOGrav is a pulsar timing array (PTA) experiment that is sensitive to low-frequency gravitational waves (GWs). This is NANOGrav's fifth public data release, including both "narrowband" and "wideband" time-of-arrival (TOA) measurements and corresponding pulsar timing models. We have added 21 MSPs and extended our timing baselines by 3 yr, now spanning nearly 16 yr for some of our sources. The data were collected using the Arecibo Observatory, the Green Bank Telescope, and the Very Large Array between frequencies of 327 MHz and 3 GHz, with most sources observed approximately monthly. A number of notable methodological and procedural changes were made compared to our previous data sets. These improve the overall quality of the TOA data set and are part of the transition to new pulsar timing and PTA analysis software packages. For the first time, our data products are accompanied by a full suite of software to reproduce data reduction, analysis, and results. Our timing models include a variety of newly detected astrometric and binary pulsar parameters, including several significant improvements to pulsar mass constraints. We find that the time series of 23 pulsars contain detectable levels of red noise, 10 of which are new measurements. In this data set, we find evidence for a stochastic GW background.

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