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Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources

Identifieur interne : 001B87 ( PascalFrancis/Checkpoint ); précédent : 001B86; suivant : 001B88

Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources

Auteurs : M. J. Keith [Australie] ; S. Johnston [Australie] ; P. S. Ray [États-Unis] ; E. C. Ferrara [États-Unis] ; P. M. Saz Parkinson [États-Unis] ; Ö. Celik [États-Unis] ; A. Belfiore [États-Unis, Italie] ; D. Donato [États-Unis] ; C. C. Cheung [États-Unis] ; A. A. Abdo [États-Unis] ; F. Camilo [États-Unis] ; P. C. C. Freire [Allemagne] ; L. Guillemot [Allemagne] ; A. K. Harding [États-Unis] ; M. Kramer [Allemagne, Royaume-Uni] ; P. F. Michelson [États-Unis] ; S. M. Ransom [États-Unis] ; R. W. Romani [États-Unis] ; D. A. Smith [France] ; D. J. Thompson [États-Unis] ; P. Weltevrede [Royaume-Uni] ; K. S. Wood [États-Unis]

Source :

RBID : Pascal:11-0287659

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English descriptors

Abstract

Using the Parkes Radio Telescope, we have carried out deep observations of 11 unassociated gamma-ray sources. Periodicity searches of these data have discovered two millisecond pulsars, PSRJ1103-5403 (1FGLJ1103.9-5355) and PSRJ2241-5236 (1FGLJ2241.9-5236), and a long-period pulsar, PSRJ1604-44 (1FGLJ1604.7-4443). In addition, we searched for but did not detect any radio pulsations from six gamma-ray pulsars discovered by the Fermi satellite to a level of ˜0.04 mJy (for pulsars with a 10 per cent duty cycle). The timing of the millisecond pulsar PSRJ1103-5403 has shown that its position is 9 arcmin from the centroid of the gamma-ray source. Since these observations were carried out, independent evidence has shown that 1FGL J1103.9-5355 is associated with the flat spectrum radio source PKS 1101-536. It appears certain that the pulsar is not associated with the gamma-ray source, despite the seemingly low probability of a chance detection of a radio millisecond pulsar. We consider that PSRJ1604-44 is a chance discovery of a weak, long-period pulsar and is unlikely to be associated with 1FGL J1604.7-4443. PSR J2241-5236 has a spin period of 2.2 ms and orbits a very low mass companion with a 3.5-h orbital period. The relatively high flux density and low dispersion measure of PSR J2241-5236 make it an excellent candidate for high precision timing experiments. The gamma rays of 1FGL J2241.9-5236 have a spectrum that is well modelled by a power law with an exponential cut-off, and phase binning with the radio ephemeris results in a multipeaked gamma-ray pulse profile. Observations with Chandra have identified a coincident X-ray source within 0.1 arcsec of the position of the pulsar obtained by radio timing.


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Pascal:11-0287659

Le document en format XML

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<title xml:lang="en" level="a">Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources</title>
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<settlement type="city">Manchester</settlement>
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<name sortKey="Weltevrede, P" sort="Weltevrede, P" uniqKey="Weltevrede P" first="P." last="Weltevrede">P. Weltevrede</name>
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<settlement type="city">Manchester</settlement>
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<name sortKey="Wood, K S" sort="Wood, K S" uniqKey="Wood K" first="K. S." last="Wood">K. S. Wood</name>
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<title level="j" type="main">Monthly Notices of the Royal Astronomical Society</title>
<title level="j" type="abbreviated">Mon. Not. R. Astron. Soc.</title>
<idno type="ISSN">0035-8711</idno>
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<date when="2011">2011</date>
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<term>Dispersion measure</term>
<term>Flux density</term>
<term>Gamma radiation</term>
<term>Gamma ray source</term>
<term>High density</term>
<term>Millisecond pulsar</term>
<term>Orbits</term>
<term>Periodicity</term>
<term>Positions</term>
<term>Power law</term>
<term>Probability</term>
<term>Pulse shape</term>
<term>Radio pulsation</term>
<term>Radio spectrum</term>
<term>Radiopulsar</term>
<term>Timing</term>
</keywords>
<keywords scheme="Pascal" xml:lang="fr">
<term>Pulsar milliseconde</term>
<term>Pulsar radio</term>
<term>Source Rγ</term>
<term>Périodicité</term>
<term>Pulsation radio</term>
<term>Rayonnement gamma</term>
<term>Timing</term>
<term>Position</term>
<term>Spectre radio</term>
<term>Probabilité</term>
<term>Orbite</term>
<term>Densité élevée</term>
<term>Densité flux</term>
<term>Mesure dispersion</term>
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<front>
<div type="abstract" xml:lang="en">Using the Parkes Radio Telescope, we have carried out deep observations of 11 unassociated gamma-ray sources. Periodicity searches of these data have discovered two millisecond pulsars, PSRJ1103-5403 (1FGLJ1103.9-5355) and PSRJ2241-5236 (1FGLJ2241.9-5236), and a long-period pulsar, PSRJ1604-44 (1FGLJ1604.7-4443). In addition, we searched for but did not detect any radio pulsations from six gamma-ray pulsars discovered by the Fermi satellite to a level of ˜0.04 mJy (for pulsars with a 10 per cent duty cycle). The timing of the millisecond pulsar PSRJ1103-5403 has shown that its position is 9 arcmin from the centroid of the gamma-ray source. Since these observations were carried out, independent evidence has shown that 1FGL J1103.9-5355 is associated with the flat spectrum radio source PKS 1101-536. It appears certain that the pulsar is not associated with the gamma-ray source, despite the seemingly low probability of a chance detection of a radio millisecond pulsar. We consider that PSRJ1604-44 is a chance discovery of a weak, long-period pulsar and is unlikely to be associated with 1FGL J1604.7-4443. PSR J2241-5236 has a spin period of 2.2 ms and orbits a very low mass companion with a 3.5-h orbital period. The relatively high flux density and low dispersion measure of PSR J2241-5236 make it an excellent candidate for high precision timing experiments. The gamma rays of 1FGL J2241.9-5236 have a spectrum that is well modelled by a power law with an exponential cut-off, and phase binning with the radio ephemeris results in a multipeaked gamma-ray pulse profile. Observations with Chandra have identified a coincident X-ray source within 0.1 arcsec of the position of the pulsar obtained by radio timing.</div>
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<s1>Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County</s1>
<s2>Baltimore, MD 21250</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
</fA14>
<fA14 i1="07">
<s1>INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica</s1>
<s2>20133 Milano</s2>
<s3>ITA</s3>
<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="08">
<s1>Dipartimento di Fisica Teorica e Nucleare (DFNT), Università di Pavia</s1>
<s2>27100 Pavia</s2>
<s3>ITA</s3>
<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="09">
<s1>Departments of Physics and Gastronomy, University of Maryland</s1>
<s2>College Park, MD 20742</s2>
<s3>USA</s3>
<sZ>8 aut.</sZ>
</fA14>
<fA14 i1="10">
<s1>National Research Council Research Associate, National Academy of Sciences</s1>
<s2>Washington, DC 20001</s2>
<s3>USA</s3>
<sZ>9 aut.</sZ>
<sZ>10 aut.</sZ>
</fA14>
<fA14 i1="11">
<s1>Columbia Astrophysics Laboratory Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
<sZ>11 aut.</sZ>
</fA14>
<fA14 i1="12">
<s1>Max-Planck-Institut für Radioastronomie, Auf dem Hiigel 69</s1>
<s2>53121 Bonn</s2>
<s3>DEU</s3>
<sZ>12 aut.</sZ>
<sZ>13 aut.</sZ>
<sZ>15 aut.</sZ>
</fA14>
<fA14 i1="13">
<s1>Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester</s1>
<s2>Manchester M13 9PL</s2>
<s3>GBR</s3>
<sZ>15 aut.</sZ>
<sZ>21 aut.</sZ>
</fA14>
<fA14 i1="14">
<s1>W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University</s1>
<s2>Stanford, CA 94305</s2>
<s3>USA</s3>
<sZ>16 aut.</sZ>
<sZ>18 aut.</sZ>
</fA14>
<fA14 i1="15">
<s1>National Radio Astronomy Observatory (NRAO)</s1>
<s2>Charlottesville, VA 22903</s2>
<s3>USA</s3>
<sZ>17 aut.</sZ>
</fA14>
<fA14 i1="16">
<s1>Centre, d'Études Nucléaires de Bordeaux Gradignan, Université Bordeaux 1, CNRS/IN2p3</s1>
<s2>33175 Gradignan</s2>
<s3>FRA</s3>
<sZ>19 aut.</sZ>
</fA14>
<fA20>
<s1>1292-1300</s1>
</fA20>
<fA21>
<s1>2011</s1>
</fA21>
<fA23 i1="01">
<s0>ENG</s0>
</fA23>
<fA43 i1="01">
<s1>INIST</s1>
<s2>2067</s2>
<s5>354000190355760360</s5>
</fA43>
<fA44>
<s0>0000</s0>
<s1>© 2011 INIST-CNRS. All rights reserved.</s1>
</fA44>
<fA45>
<s0>1/4 p.</s0>
</fA45>
<fA47 i1="01" i2="1">
<s0>11-0287659</s0>
</fA47>
<fA60>
<s1>P</s1>
</fA60>
<fA61>
<s0>A</s0>
</fA61>
<fA64 i1="01" i2="1">
<s0>Monthly Notices of the Royal Astronomical Society</s0>
</fA64>
<fA66 i1="01">
<s0>USA</s0>
</fA66>
<fC01 i1="01" l="ENG">
<s0>Using the Parkes Radio Telescope, we have carried out deep observations of 11 unassociated gamma-ray sources. Periodicity searches of these data have discovered two millisecond pulsars, PSRJ1103-5403 (1FGLJ1103.9-5355) and PSRJ2241-5236 (1FGLJ2241.9-5236), and a long-period pulsar, PSRJ1604-44 (1FGLJ1604.7-4443). In addition, we searched for but did not detect any radio pulsations from six gamma-ray pulsars discovered by the Fermi satellite to a level of ˜0.04 mJy (for pulsars with a 10 per cent duty cycle). The timing of the millisecond pulsar PSRJ1103-5403 has shown that its position is 9 arcmin from the centroid of the gamma-ray source. Since these observations were carried out, independent evidence has shown that 1FGL J1103.9-5355 is associated with the flat spectrum radio source PKS 1101-536. It appears certain that the pulsar is not associated with the gamma-ray source, despite the seemingly low probability of a chance detection of a radio millisecond pulsar. We consider that PSRJ1604-44 is a chance discovery of a weak, long-period pulsar and is unlikely to be associated with 1FGL J1604.7-4443. PSR J2241-5236 has a spin period of 2.2 ms and orbits a very low mass companion with a 3.5-h orbital period. The relatively high flux density and low dispersion measure of PSR J2241-5236 make it an excellent candidate for high precision timing experiments. The gamma rays of 1FGL J2241.9-5236 have a spectrum that is well modelled by a power law with an exponential cut-off, and phase binning with the radio ephemeris results in a multipeaked gamma-ray pulse profile. Observations with Chandra have identified a coincident X-ray source within 0.1 arcsec of the position of the pulsar obtained by radio timing.</s0>
</fC01>
<fC02 i1="01" i2="3">
<s0>001E03</s0>
</fC02>
<fC03 i1="01" i2="X" l="FRE">
<s0>Pulsar milliseconde</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="X" l="ENG">
<s0>Millisecond pulsar</s0>
<s5>26</s5>
</fC03>
<fC03 i1="01" i2="X" l="SPA">
<s0>Pulsar milisegundo</s0>
<s5>26</s5>
</fC03>
<fC03 i1="02" i2="X" l="FRE">
<s0>Pulsar radio</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="ENG">
<s0>Radiopulsar</s0>
<s5>27</s5>
</fC03>
<fC03 i1="02" i2="X" l="SPA">
<s0>Pulsar radio</s0>
<s5>27</s5>
</fC03>
<fC03 i1="03" i2="X" l="FRE">
<s0>Source Rγ</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="ENG">
<s0>Gamma ray source</s0>
<s5>28</s5>
</fC03>
<fC03 i1="03" i2="X" l="SPA">
<s0>Fuente Rγ</s0>
<s5>28</s5>
</fC03>
<fC03 i1="04" i2="X" l="FRE">
<s0>Périodicité</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="ENG">
<s0>Periodicity</s0>
<s5>29</s5>
</fC03>
<fC03 i1="04" i2="X" l="SPA">
<s0>Periodicidad</s0>
<s5>29</s5>
</fC03>
<fC03 i1="05" i2="X" l="FRE">
<s0>Pulsation radio</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG">
<s0>Radio pulsation</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA">
<s0>Pulsación radio</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="3" l="FRE">
<s0>Rayonnement gamma</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="3" l="ENG">
<s0>Gamma radiation</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="3" l="FRE">
<s0>Timing</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="3" l="ENG">
<s0>Timing</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="3" l="FRE">
<s0>Position</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="3" l="ENG">
<s0>Positions</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="X" l="FRE">
<s0>Spectre radio</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="ENG">
<s0>Radio spectrum</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="X" l="SPA">
<s0>Espectro radio</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="3" l="FRE">
<s0>Probabilité</s0>
<s5>35</s5>
</fC03>
<fC03 i1="10" i2="3" l="ENG">
<s0>Probability</s0>
<s5>35</s5>
</fC03>
<fC03 i1="11" i2="3" l="FRE">
<s0>Orbite</s0>
<s5>36</s5>
</fC03>
<fC03 i1="11" i2="3" l="ENG">
<s0>Orbits</s0>
<s5>36</s5>
</fC03>
<fC03 i1="12" i2="X" l="FRE">
<s0>Densité élevée</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="ENG">
<s0>High density</s0>
<s5>37</s5>
</fC03>
<fC03 i1="12" i2="X" l="SPA">
<s0>Densidad elevada</s0>
<s5>37</s5>
</fC03>
<fC03 i1="13" i2="3" l="FRE">
<s0>Densité flux</s0>
<s5>38</s5>
</fC03>
<fC03 i1="13" i2="3" l="ENG">
<s0>Flux density</s0>
<s5>38</s5>
</fC03>
<fC03 i1="14" i2="X" l="FRE">
<s0>Mesure dispersion</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="ENG">
<s0>Dispersion measure</s0>
<s5>39</s5>
</fC03>
<fC03 i1="14" i2="X" l="SPA">
<s0>Medida dispersión</s0>
<s5>39</s5>
</fC03>
<fC03 i1="15" i2="X" l="FRE">
<s0>Loi puissance</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="ENG">
<s0>Power law</s0>
<s5>40</s5>
</fC03>
<fC03 i1="15" i2="X" l="SPA">
<s0>Ley poder</s0>
<s5>40</s5>
</fC03>
<fC03 i1="16" i2="X" l="FRE">
<s0>Forme impulsion</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="ENG">
<s0>Pulse shape</s0>
<s5>41</s5>
</fC03>
<fC03 i1="16" i2="X" l="SPA">
<s0>Forma impulsión</s0>
<s5>41</s5>
</fC03>
<fN21>
<s1>192</s1>
</fN21>
<fN44 i1="01">
<s1>OTO</s1>
</fN44>
<fN82>
<s1>OTO</s1>
</fN82>
</pA>
</standard>
</inist>
<affiliations>
<list>
<country>
<li>Allemagne</li>
<li>Australie</li>
<li>France</li>
<li>Italie</li>
<li>Royaume-Uni</li>
<li>États-Unis</li>
</country>
<region>
<li>Angleterre</li>
<li>District de Cologne</li>
<li>Grand Manchester</li>
<li>Maryland</li>
<li>Rhénanie-du-Nord-Westphalie</li>
</region>
<settlement>
<li>Bonn</li>
<li>College Park (Maryland)</li>
<li>Manchester</li>
</settlement>
<orgName>
<li>Université de Manchester</li>
<li>Université du Maryland</li>
</orgName>
</list>
<tree>
<country name="Australie">
<noRegion>
<name sortKey="Keith, M J" sort="Keith, M J" uniqKey="Keith M" first="M. J." last="Keith">M. J. Keith</name>
</noRegion>
<name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name>
</country>
<country name="États-Unis">
<noRegion>
<name sortKey="Ray, P S" sort="Ray, P S" uniqKey="Ray P" first="P. S." last="Ray">P. S. Ray</name>
</noRegion>
<name sortKey="Abdo, A A" sort="Abdo, A A" uniqKey="Abdo A" first="A. A." last="Abdo">A. A. Abdo</name>
<name sortKey="Belfiore, A" sort="Belfiore, A" uniqKey="Belfiore A" first="A." last="Belfiore">A. Belfiore</name>
<name sortKey="Camilo, F" sort="Camilo, F" uniqKey="Camilo F" first="F." last="Camilo">F. Camilo</name>
<name sortKey="Celik, O" sort="Celik, O" uniqKey="Celik O" first="Ö." last="Celik">Ö. Celik</name>
<name sortKey="Celik, O" sort="Celik, O" uniqKey="Celik O" first="Ö." last="Celik">Ö. Celik</name>
<name sortKey="Celik, O" sort="Celik, O" uniqKey="Celik O" first="Ö." last="Celik">Ö. Celik</name>
<name sortKey="Cheung, C C" sort="Cheung, C C" uniqKey="Cheung C" first="C. C." last="Cheung">C. C. Cheung</name>
<name sortKey="Donato, D" sort="Donato, D" uniqKey="Donato D" first="D." last="Donato">D. Donato</name>
<name sortKey="Donato, D" sort="Donato, D" uniqKey="Donato D" first="D." last="Donato">D. Donato</name>
<name sortKey="Ferrara, E C" sort="Ferrara, E C" uniqKey="Ferrara E" first="E. C." last="Ferrara">E. C. Ferrara</name>
<name sortKey="Harding, A K" sort="Harding, A K" uniqKey="Harding A" first="A. K." last="Harding">A. K. Harding</name>
<name sortKey="Michelson, P F" sort="Michelson, P F" uniqKey="Michelson P" first="P. F." last="Michelson">P. F. Michelson</name>
<name sortKey="Ransom, S M" sort="Ransom, S M" uniqKey="Ransom S" first="S. M." last="Ransom">S. M. Ransom</name>
<name sortKey="Romani, R W" sort="Romani, R W" uniqKey="Romani R" first="R. W." last="Romani">R. W. Romani</name>
<name sortKey="Saz Parkinson, P M" sort="Saz Parkinson, P M" uniqKey="Saz Parkinson P" first="P. M." last="Saz Parkinson">P. M. Saz Parkinson</name>
<name sortKey="Thompson, D J" sort="Thompson, D J" uniqKey="Thompson D" first="D. J." last="Thompson">D. J. Thompson</name>
<name sortKey="Wood, K S" sort="Wood, K S" uniqKey="Wood K" first="K. S." last="Wood">K. S. Wood</name>
</country>
<country name="Italie">
<noRegion>
<name sortKey="Belfiore, A" sort="Belfiore, A" uniqKey="Belfiore A" first="A." last="Belfiore">A. Belfiore</name>
</noRegion>
<name sortKey="Belfiore, A" sort="Belfiore, A" uniqKey="Belfiore A" first="A." last="Belfiore">A. Belfiore</name>
</country>
<country name="Allemagne">
<region name="Rhénanie-du-Nord-Westphalie">
<name sortKey="Freire, P C C" sort="Freire, P C C" uniqKey="Freire P" first="P. C. C." last="Freire">P. C. C. Freire</name>
</region>
<name sortKey="Guillemot, L" sort="Guillemot, L" uniqKey="Guillemot L" first="L." last="Guillemot">L. Guillemot</name>
<name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
</country>
<country name="Royaume-Uni">
<region name="Angleterre">
<name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
</region>
<name sortKey="Weltevrede, P" sort="Weltevrede, P" uniqKey="Weltevrede P" first="P." last="Weltevrede">P. Weltevrede</name>
</country>
<country name="France">
<noRegion>
<name sortKey="Smith, D A" sort="Smith, D A" uniqKey="Smith D" first="D. A." last="Smith">D. A. Smith</name>
</noRegion>
</country>
</tree>
</affiliations>
</record>

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