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Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set

Bogdanov, Slavko and Guillot, Sebastien and Ray, Paul S. and Wolff, Michael T. and Chakrabarty, Deepto and Ho, Wynn C. G. and Kerr, Matthew and Lamb, Frederick K. and Lommen, Andrea and Ludlam, Renee M. and Milburn, Reilly and Montano, Sergio and Miller, M. Coleman and Bauböck, Michi and Özel, Feryal and Psaltis, Dimitrios and Remillard, Ronald A. and Riley, Thomas E. and Steiner, James F. and Strohmayer, Tod E. and Watts, Anna L. and Wood, Kent S. and Zeldes, Jesse and Enoto, Teruaki and Okajima, Takashi and Kellogg, James W. and Baker, Charles and Markwardt, Craig B. and Arzoumanian, Zaven and Gendreau, Keith C. (2019) Constraining the Neutron Star Mass–Radius Relation and Dense Matter Equation of State with NICER. I. The Millisecond Pulsar X-Ray Data Set. Astrophysical Journal Letters, 887 (1). Art. No. L25. ISSN 2041-8213. https://resolver.caltech.edu/CaltechAUTHORS:20191213-105051551

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Abstract

We present the set of deep Neutron Star Interior Composition Explorer (NICER) X-ray timing observations of the nearby rotation-powered millisecond pulsars PSRs J0437−4715, J0030+0451, J1231−1411, and J2124−3358, selected as targets for constraining the mass–radius relation of neutron stars and the dense matter equation of state (EoS) via modeling of their pulsed thermal X-ray emission. We describe the instrument, observations, and data processing/reduction procedures, as well as the series of investigations conducted to ensure that the properties of the data sets are suitable for parameter estimation analyses to produce reliable constraints on the neutron star mass–radius relation and the dense matter EoS. We find that the long-term timing and flux behavior and the Fourier-domain properties of the event data do not exhibit any anomalies that could adversely affect the intended measurements. From phase-selected spectroscopy, we find that emission from the individual pulse peaks is well described by a single-temperature hydrogen atmosphere spectrum, with the exception of PSR J0437−4715, for which multiple temperatures are required.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/2041-8213/ab53ebDOIArticle
http://arxiv.org/abs/1912.05706arXivDiscussion Paper
ORCID:
AuthorORCID
Bogdanov, Slavko0000-0002-9870-2742
Guillot, Sebastien0000-0002-6449-106X
Ray, Paul S.0000-0002-5297-5278
Wolff, Michael T.0000-0002-4013-5650
Chakrabarty, Deepto0000-0001-8804-8946
Ho, Wynn C. G.0000-0002-6089-6836
Kerr, Matthew0000-0002-0893-4073
Lamb, Frederick K.0000-0002-3862-7402
Ludlam, Renee M.0000-0002-8961-939X
Miller, M. Coleman0000-0002-2666-728X
Remillard, Ronald A.0000-0003-4815-0481
Riley, Thomas E.0000-0001-9313-0493
Steiner, James F.0000-0002-5872-6061
Strohmayer, Tod E.0000-0001-7681-5845
Watts, Anna L.0000-0002-1009-2354
Wood, Kent S.0000-0002-7376-3151
Enoto, Teruaki0000-0003-1244-3100
Markwardt, Craig B.0000-0001-9803-3879
Additional Information:© 2019. The American Astronomical Society. Received 2019 September 5; revised 2019 October 16; accepted 2019 October 18; published 2019 December 12. Focus on NICER Constraints on the Dense Matter Equation of State. This work was supported by NASA through the NICER mission and the Astrophysics Explorers Program. A portion of the analysis presented was based on archival observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA. S.G. acknowledges the support of the Centre National d'Études Spatiales (CNES). A.L.W. and T.E.R. acknowledge support from ERC Starting grant No. 639217 CSINEUTRONSTAR (PI: Watts). M.C.M. is grateful for the hospitality of Perimeter Institute where part of this work was carried out. Research at Perimeter Institute is supported in part by the Government of Canada through the Department of Innovation, Science and Economic Development Canada and by the Province of Ontario through the Ministry of Economic Development, Job Creation and Trade. This research has made use of data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We acknowledge extensive use of NASA's Astrophysics Data System (ADS) Bibliographic Services and the ArXiv. Facilities: NICER - , XMM-Newton - . Software: HEAsoft (Nasa High Energy Astrophysics Science Archive Research Center (Heasarc), 2014), Tempo2 (Hobbs et al. 2006), PINT (https://github.com/nanograv/pint), XSPEC (Arnaud 1996), NICERSoft (https://github.com/paulray/NICERsoft).
Funders:
Funding AgencyGrant Number
NASA Einstein FellowshipUNSPECIFIED
ESA Member StatesUNSPECIFIED
Centre National d'Études Spatiales (CNES)UNSPECIFIED
European Research Council (ERC)639217
Perimeter Institute for Theoretical PhysicsUNSPECIFIED
Department of Innovation, Science and Economic Development (Canada)UNSPECIFIED
Ontario Ministry of Economic Development, Job Creation and TradeUNSPECIFIED
Subject Keywords:Neutron stars ; Pulsars ; Compact objects ; Nuclear astrophysics ; Millisecond pulsars ; X-ray astronomy ; X-ray observatories ; Pulsar timing method ; Spectroscopy ; Astronomical techniques
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Neutron stars (1108); Pulsars (1306); Compact objects (288); Nuclear astrophysics (1129); Millisecond pulsars (1062); X-ray astronomy (1810); X-ray observatories (1819); Pulsar timing method (1305); Spectroscopy (1558
Record Number:10.3847/2041-8213/ab53eb
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20191213-105051551
Official Citation:Slavko Bogdanov et al 2019 ApJL 887 L25
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:100291
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:16 Dec 2019 15:38
Last Modified:09 Mar 2020 13:19

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