AustralieFrV1, PascalFrancis, Corpus, bibRecord, 001C26

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

Identifieur interne : 001C26 ( PascalFrancis/Corpus ); précédent : 001C25; suivant : 001C27

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

Auteurs : M. J. Keith ; S. Johnston ; P. S. Ray ; E. C. Ferrara ; P. M. Saz Parkinson ; Ö. Celik ; A. Belfiore ; D. Donato ; C. C. Cheung ; A. A. Abdo ; F. Camilo ; P. C. C. Freire ; L. Guillemot ; A. K. Harding ; M. Kramer ; P. F. Michelson ; S. M. Ransom ; R. W. Romani ; D. A. Smith ; D. J. Thompson ; P. Weltevrede ; K. S. Wood

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2011.

RBID : Pascal:11-0287659

Descripteurs français

Pascal (Inist)
- Pulsar milliseconde, Pulsar radio, Source Rγ, Périodicité, Pulsation radio, Rayonnement gamma, Timing, Position, Spectre radio, Probabilité, Orbite, Densité élevée, Densité flux, Mesure dispersion, Loi puissance, Forme impulsion.

English descriptors

KwdEn :
- Dispersion measure, Flux density, Gamma radiation, Gamma ray source, High density, Millisecond pulsar, Orbits, Periodicity, Positions, Power law, Probability, Pulse shape, Radio pulsation, Radio spectrum, Radiopulsar, Timing.

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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

A01	`01`	`1`		`@0 0035-8711`
A02	`01`			`@0 MNRAA4`
A03		`1`		`@0 Mon. Not. R. Astron. Soc.`
A05				`@2 414`
A06				`@2 2`
A08	`01`	`1`	`ENG`	`@1 Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources`
A11	`01`	`1`		`@1 KEITH (M. J.)`
A11	`02`	`1`		`@1 JOHNSTON (S.)`
A11	`03`	`1`		`@1 RAY (P. S.)`
A11	`04`	`1`		`@1 FERRARA (E. C.)`
A11	`05`	`1`		`@1 SAZ PARKINSON (P. M.)`
A11	`06`	`1`		`@1 CELIK (Ö.)`
A11	`07`	`1`		`@1 BELFIORE (A.)`
A11	`08`	`1`		`@1 DONATO (D.)`
A11	`09`	`1`		`@1 CHEUNG (C. C.)`
A11	`10`	`1`		`@1 ABDO (A. A.)`
A11	`11`	`1`		`@1 CAMILO (F.)`
A11	`12`	`1`		`@1 FREIRE (P. C. C.)`
A11	`13`	`1`		`@1 GUILLEMOT (L.)`
A11	`14`	`1`		`@1 HARDING (A. K.)`
A11	`15`	`1`		`@1 KRAMER (M.)`
A11	`16`	`1`		`@1 MICHELSON (P. F.)`
A11	`17`	`1`		`@1 RANSOM (S. M.)`
A11	`18`	`1`		`@1 ROMANI (R. W.)`
A11	`19`	`1`		`@1 SMITH (D. A.)`
A11	`20`	`1`		`@1 THOMPSON (D. J.)`
A11	`21`	`1`		`@1 WELTEVREDE (P.)`
A11	`22`	`1`		`@1 WOOD (K. S.)`
A14	`01`			`@1 Australia Telescope National Facility, CSIRO @2 Epping, NSW 1710 @3 AUS @Z 1 aut. @Z 2 aut.`
A14	`02`			`@1 Space Science Division, Naval Research Laboratory @2 Washington, DC 20375 @3 USA @Z 3 aut. @Z 22 aut.`
A14	`03`			`@1 NASA Goddard Space Flight Center @2 Greenbelt, MD 20771 @3 USA @Z 4 aut. @Z 6 aut. @Z 14 aut. @Z 20 aut.`
A14	`04`			`@1 Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz @2 Santa Cruz, CA 95064 @3 USA @Z 5 aut. @Z 7 aut.`
A14	`05`			`@1 Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center @2 Greenbelt, MD 20771 @3 USA @Z 6 aut. @Z 8 aut.`
A14	`06`			`@1 Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County @2 Baltimore, MD 21250 @3 USA @Z 6 aut.`
A14	`07`			`@1 INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica @2 20133 Milano @3 ITA @Z 7 aut.`
A14	`08`			`@1 Dipartimento di Fisica Teorica e Nucleare (DFNT), Università di Pavia @2 27100 Pavia @3 ITA @Z 7 aut.`
A14	`09`			`@1 Departments of Physics and Gastronomy, University of Maryland @2 College Park, MD 20742 @3 USA @Z 8 aut.`
A14	`10`			`@1 National Research Council Research Associate, National Academy of Sciences @2 Washington, DC 20001 @3 USA @Z 9 aut. @Z 10 aut.`
A14	`11`			`@1 Columbia Astrophysics Laboratory Columbia University @2 New York, NY 10027 @3 USA @Z 11 aut.`
A14	`12`			`@1 Max-Planck-Institut für Radioastronomie, Auf dem Hiigel 69 @2 53121 Bonn @3 DEU @Z 12 aut. @Z 13 aut. @Z 15 aut.`
A14	`13`			`@1 Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester @2 Manchester M13 9PL @3 GBR @Z 15 aut. @Z 21 aut.`
A14	`14`			`@1 W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University @2 Stanford, CA 94305 @3 USA @Z 16 aut. @Z 18 aut.`
A14	`15`			`@1 National Radio Astronomy Observatory (NRAO) @2 Charlottesville, VA 22903 @3 USA @Z 17 aut.`
A14	`16`			`@1 Centre, d'Études Nucléaires de Bordeaux Gradignan, Université Bordeaux 1, CNRS/IN2p3 @2 33175 Gradignan @3 FRA @Z 19 aut.`
A20				`@1 1292-1300`
A21				`@1 2011`
A23	`01`			`@0 ENG`
A43	`01`			`@1 INIST @2 2067 @5 354000190355760360`
A44				`@0 0000 @1 © 2011 INIST-CNRS. All rights reserved.`
A45				`@0 1/4 p.`
A47	`01`	`1`		`@0 11-0287659`
A60				`@1 P`
A61				`@0 A`
A64	`01`	`1`		`@0 Monthly Notices of the Royal Astronomical Society`
A66	`01`			`@0 USA`
C01	`01`		`ENG`	@0 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.
C02	`01`	`3`		`@0 001E03`
C03	`01`	`X`	`FRE`	`@0 Pulsar milliseconde @5 26`
C03	`01`	`X`	`ENG`	`@0 Millisecond pulsar @5 26`
C03	`01`	`X`	`SPA`	`@0 Pulsar milisegundo @5 26`
C03	`02`	`X`	`FRE`	`@0 Pulsar radio @5 27`
C03	`02`	`X`	`ENG`	`@0 Radiopulsar @5 27`
C03	`02`	`X`	`SPA`	`@0 Pulsar radio @5 27`
C03	`03`	`X`	`FRE`	`@0 Source Rγ @5 28`
C03	`03`	`X`	`ENG`	`@0 Gamma ray source @5 28`
C03	`03`	`X`	`SPA`	`@0 Fuente Rγ @5 28`
C03	`04`	`X`	`FRE`	`@0 Périodicité @5 29`
C03	`04`	`X`	`ENG`	`@0 Periodicity @5 29`
C03	`04`	`X`	`SPA`	`@0 Periodicidad @5 29`
C03	`05`	`X`	`FRE`	`@0 Pulsation radio @5 30`
C03	`05`	`X`	`ENG`	`@0 Radio pulsation @5 30`
C03	`05`	`X`	`SPA`	`@0 Pulsación radio @5 30`
C03	`06`	`3`	`FRE`	`@0 Rayonnement gamma @5 31`
C03	`06`	`3`	`ENG`	`@0 Gamma radiation @5 31`
C03	`07`	`3`	`FRE`	`@0 Timing @5 32`
C03	`07`	`3`	`ENG`	`@0 Timing @5 32`
C03	`08`	`3`	`FRE`	`@0 Position @5 33`
C03	`08`	`3`	`ENG`	`@0 Positions @5 33`
C03	`09`	`X`	`FRE`	`@0 Spectre radio @5 34`
C03	`09`	`X`	`ENG`	`@0 Radio spectrum @5 34`
C03	`09`	`X`	`SPA`	`@0 Espectro radio @5 34`
C03	`10`	`3`	`FRE`	`@0 Probabilité @5 35`
C03	`10`	`3`	`ENG`	`@0 Probability @5 35`
C03	`11`	`3`	`FRE`	`@0 Orbite @5 36`
C03	`11`	`3`	`ENG`	`@0 Orbits @5 36`
C03	`12`	`X`	`FRE`	`@0 Densité élevée @5 37`
C03	`12`	`X`	`ENG`	`@0 High density @5 37`
C03	`12`	`X`	`SPA`	`@0 Densidad elevada @5 37`
C03	`13`	`3`	`FRE`	`@0 Densité flux @5 38`
C03	`13`	`3`	`ENG`	`@0 Flux density @5 38`
C03	`14`	`X`	`FRE`	`@0 Mesure dispersion @5 39`
C03	`14`	`X`	`ENG`	`@0 Dispersion measure @5 39`
C03	`14`	`X`	`SPA`	`@0 Medida dispersión @5 39`
C03	`15`	`X`	`FRE`	`@0 Loi puissance @5 40`
C03	`15`	`X`	`ENG`	`@0 Power law @5 40`
C03	`15`	`X`	`SPA`	`@0 Ley poder @5 40`
C03	`16`	`X`	`FRE`	`@0 Forme impulsion @5 41`
C03	`16`	`X`	`ENG`	`@0 Pulse shape @5 41`
C03	`16`	`X`	`SPA`	`@0 Forma impulsión @5 41`
N21				`@1 192`
N44	`01`			`@1 OTO`
N82				`@1 OTO`

Format Inist (serveur)

NO :	PASCAL 11-0287659 INIST
ET :	Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources
AU :	KEITH (M. J.); JOHNSTON (S.); RAY (P. S.); FERRARA (E. C.); SAZ PARKINSON (P. M.); CELIK (Ö.); BELFIORE (A.); DONATO (D.); CHEUNG (C. C.); ABDO (A. A.); CAMILO (F.); FREIRE (P. C. C.); GUILLEMOT (L.); HARDING (A. K.); KRAMER (M.); MICHELSON (P. F.); RANSOM (S. M.); ROMANI (R. W.); SMITH (D. A.); THOMPSON (D. J.); WELTEVREDE (P.); WOOD (K. S.)
AF :	Australia Telescope National Facility, CSIRO/Epping, NSW 1710/Australie (1 aut., 2 aut.); Space Science Division, Naval Research Laboratory/Washington, DC 20375/Etats-Unis (3 aut., 22 aut.); NASA Goddard Space Flight Center/Greenbelt, MD 20771/Etats-Unis (4 aut., 6 aut., 14 aut., 20 aut.); Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz/Santa Cruz, CA 95064/Etats-Unis (5 aut., 7 aut.); Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center/Greenbelt, MD 20771/Etats-Unis (6 aut., 8 aut.); Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County/Baltimore, MD 21250/Etats-Unis (6 aut.); INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica/20133 Milano/Italie (7 aut.); Dipartimento di Fisica Teorica e Nucleare (DFNT), Università di Pavia/27100 Pavia/Italie (7 aut.); Departments of Physics and Gastronomy, University of Maryland/College Park, MD 20742/Etats-Unis (8 aut.); National Research Council Research Associate, National Academy of Sciences/Washington, DC 20001/Etats-Unis (9 aut., 10 aut.); Columbia Astrophysics Laboratory Columbia University/New York, NY 10027/Etats-Unis (11 aut.); Max-Planck-Institut für Radioastronomie, Auf dem Hiigel 69/53121 Bonn/Allemagne (12 aut., 13 aut., 15 aut.); Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester/Manchester M13 9PL/Royaume-Uni (15 aut., 21 aut.); W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University/Stanford, CA 94305/Etats-Unis (16 aut., 18 aut.); National Radio Astronomy Observatory (NRAO)/Charlottesville, VA 22903/Etats-Unis (17 aut.); Centre, d'Études Nucléaires de Bordeaux Gradignan, Université Bordeaux 1, CNRS/IN2p3/33175 Gradignan/France (19 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 2; Pp. 1292-1300; Bibl. 1/4 p.
LA :	Anglais
EA :	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.
CC :	001E03
FD :	Pulsar milliseconde; Pulsar radio; Source Rγ; Périodicité; Pulsation radio; Rayonnement gamma; Timing; Position; Spectre radio; Probabilité; Orbite; Densité élevée; Densité flux; Mesure dispersion; Loi puissance; Forme impulsion
ED :	Millisecond pulsar; Radiopulsar; Gamma ray source; Periodicity; Radio pulsation; Gamma radiation; Timing; Positions; Radio spectrum; Probability; Orbits; High density; Flux density; Dispersion measure; Power law; Pulse shape
SD :	Pulsar milisegundo; Pulsar radio; Fuente Rγ; Periodicidad; Pulsación radio; Espectro radio; Densidad elevada; Medida dispersión; Ley poder; Forma impulsión
LO :	INIST-2067.354000190355760360
ID :	11-0287659

Links to Exploration step

Pascal:11-0287659

Le document en format XML

<record><TEI><teiHeader><fileDesc><titleStmt><title xml:lang="en" level="a">Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources</title>
<author><name sortKey="Keith, M J" sort="Keith, M J" uniqKey="Keith M" first="M. J." last="Keith">M. J. Keith</name>
<affiliation><inist:fA14 i1="01"><s1>Australia Telescope National Facility, CSIRO</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name>
<affiliation><inist:fA14 i1="01"><s1>Australia Telescope National Facility, CSIRO</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ray, P S" sort="Ray, P S" uniqKey="Ray P" first="P. S." last="Ray">P. S. Ray</name>
<affiliation><inist:fA14 i1="02"><s1>Space Science Division, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ferrara, E C" sort="Ferrara, E C" uniqKey="Ferrara E" first="E. C." last="Ferrara">E. C. Ferrara</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><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>
<affiliation><inist:fA14 i1="04"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Celik, O" sort="Celik, O" uniqKey="Celik O" first="Ö." last="Celik">Ö. Celik</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="06"><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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Belfiore, A" sort="Belfiore, A" uniqKey="Belfiore A" first="A." last="Belfiore">A. Belfiore</name>
<affiliation><inist:fA14 i1="04"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica</s1>
<s2>20133 Milano</s2>
<s3>ITA</s3>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Donato, D" sort="Donato, D" uniqKey="Donato D" first="D." last="Donato">D. Donato</name>
<affiliation><inist:fA14 i1="05"><s1>Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Cheung, C C" sort="Cheung, C C" uniqKey="Cheung C" first="C. C." last="Cheung">C. C. Cheung</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Abdo, A A" sort="Abdo, A A" uniqKey="Abdo A" first="A. A." last="Abdo">A. A. Abdo</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Camilo, F" sort="Camilo, F" uniqKey="Camilo F" first="F." last="Camilo">F. Camilo</name>
<affiliation><inist:fA14 i1="11"><s1>Columbia Astrophysics Laboratory Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
<sZ>11 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><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>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Guillemot, L" sort="Guillemot, L" uniqKey="Guillemot L" first="L." last="Guillemot">L. Guillemot</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Harding, A K" sort="Harding, A K" uniqKey="Harding A" first="A. K." last="Harding">A. K. Harding</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Michelson, P F" sort="Michelson, P F" uniqKey="Michelson P" first="P. F." last="Michelson">P. F. Michelson</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ransom, S M" sort="Ransom, S M" uniqKey="Ransom S" first="S. M." last="Ransom">S. M. Ransom</name>
<affiliation><inist:fA14 i1="15"><s1>National Radio Astronomy Observatory (NRAO)</s1>
<s2>Charlottesville, VA 22903</s2>
<s3>USA</s3>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Romani, R W" sort="Romani, R W" uniqKey="Romani R" first="R. W." last="Romani">R. W. Romani</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smith, D A" sort="Smith, D A" uniqKey="Smith D" first="D. A." last="Smith">D. A. Smith</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Thompson, D J" sort="Thompson, D J" uniqKey="Thompson D" first="D. J." last="Thompson">D. J. Thompson</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Weltevrede, P" sort="Weltevrede, P" uniqKey="Weltevrede P" first="P." last="Weltevrede">P. Weltevrede</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Wood, K S" sort="Wood, K S" uniqKey="Wood K" first="K. S." last="Wood">K. S. Wood</name>
<affiliation><inist:fA14 i1="02"><s1>Space Science Division, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</titleStmt>
<publicationStmt><idno type="wicri:source">INIST</idno>
<idno type="inist">11-0287659</idno>
<date when="2011">2011</date>
<idno type="stanalyst">PASCAL 11-0287659 INIST</idno>
<idno type="RBID">Pascal:11-0287659</idno>
<idno type="wicri:Area/PascalFrancis/Corpus">001C26</idno>
</publicationStmt>
<sourceDesc><biblStruct><analytic><title xml:lang="en" level="a">Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources</title>
<author><name sortKey="Keith, M J" sort="Keith, M J" uniqKey="Keith M" first="M. J." last="Keith">M. J. Keith</name>
<affiliation><inist:fA14 i1="01"><s1>Australia Telescope National Facility, CSIRO</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Johnston, S" sort="Johnston, S" uniqKey="Johnston S" first="S." last="Johnston">S. Johnston</name>
<affiliation><inist:fA14 i1="01"><s1>Australia Telescope National Facility, CSIRO</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ray, P S" sort="Ray, P S" uniqKey="Ray P" first="P. S." last="Ray">P. S. Ray</name>
<affiliation><inist:fA14 i1="02"><s1>Space Science Division, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ferrara, E C" sort="Ferrara, E C" uniqKey="Ferrara E" first="E. C." last="Ferrara">E. C. Ferrara</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><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>
<affiliation><inist:fA14 i1="04"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Celik, O" sort="Celik, O" uniqKey="Celik O" first="Ö." last="Celik">Ö. Celik</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="05"><s1>Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="06"><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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Belfiore, A" sort="Belfiore, A" uniqKey="Belfiore A" first="A." last="Belfiore">A. Belfiore</name>
<affiliation><inist:fA14 i1="04"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist:fA14 i1="07"><s1>INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica</s1>
<s2>20133 Milano</s2>
<s3>ITA</s3>
<sZ>7 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Donato, D" sort="Donato, D" uniqKey="Donato D" first="D." last="Donato">D. Donato</name>
<affiliation><inist:fA14 i1="05"><s1>Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Cheung, C C" sort="Cheung, C C" uniqKey="Cheung C" first="C. C." last="Cheung">C. C. Cheung</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Abdo, A A" sort="Abdo, A A" uniqKey="Abdo A" first="A. A." last="Abdo">A. A. Abdo</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Camilo, F" sort="Camilo, F" uniqKey="Camilo F" first="F." last="Camilo">F. Camilo</name>
<affiliation><inist:fA14 i1="11"><s1>Columbia Astrophysics Laboratory Columbia University</s1>
<s2>New York, NY 10027</s2>
<s3>USA</s3>
<sZ>11 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><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>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Guillemot, L" sort="Guillemot, L" uniqKey="Guillemot L" first="L." last="Guillemot">L. Guillemot</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Harding, A K" sort="Harding, A K" uniqKey="Harding A" first="A. K." last="Harding">A. K. Harding</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Kramer, M" sort="Kramer, M" uniqKey="Kramer M" first="M." last="Kramer">M. Kramer</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Michelson, P F" sort="Michelson, P F" uniqKey="Michelson P" first="P. F." last="Michelson">P. F. Michelson</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Ransom, S M" sort="Ransom, S M" uniqKey="Ransom S" first="S. M." last="Ransom">S. M. Ransom</name>
<affiliation><inist:fA14 i1="15"><s1>National Radio Astronomy Observatory (NRAO)</s1>
<s2>Charlottesville, VA 22903</s2>
<s3>USA</s3>
<sZ>17 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Romani, R W" sort="Romani, R W" uniqKey="Romani R" first="R. W." last="Romani">R. W. Romani</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Smith, D A" sort="Smith, D A" uniqKey="Smith D" first="D. A." last="Smith">D. A. Smith</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Thompson, D J" sort="Thompson, D J" uniqKey="Thompson D" first="D. J." last="Thompson">D. J. Thompson</name>
<affiliation><inist:fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Weltevrede, P" sort="Weltevrede, P" uniqKey="Weltevrede P" first="P." last="Weltevrede">P. Weltevrede</name>
<affiliation><inist: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>
</inist:fA14>
</affiliation>
</author>
<author><name sortKey="Wood, K S" sort="Wood, K S" uniqKey="Wood K" first="K. S." last="Wood">K. S. Wood</name>
<affiliation><inist:fA14 i1="02"><s1>Space Science Division, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>22 aut.</sZ>
</inist:fA14>
</affiliation>
</author>
</analytic>
<series><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>
<imprint><date when="2011">2011</date>
</imprint>
</series>
</biblStruct>
</sourceDesc>
<seriesStmt><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>
</seriesStmt>
</fileDesc>
<profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><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>
<term>Loi puissance</term>
<term>Forme impulsion</term>
</keywords>
</textClass>
</profileDesc>
</teiHeader>
<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>
</front>
</TEI>
<inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0>
</fA01>
<fA02 i1="01"><s0>MNRAA4</s0>
</fA02>
<fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0>
</fA03>
<fA05><s2>414</s2>
</fA05>
<fA06><s2>2</s2>
</fA06>
<fA08 i1="01" i2="1" l="ENG"><s1>Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources</s1>
</fA08>
<fA11 i1="01" i2="1"><s1>KEITH (M. J.)</s1>
</fA11>
<fA11 i1="02" i2="1"><s1>JOHNSTON (S.)</s1>
</fA11>
<fA11 i1="03" i2="1"><s1>RAY (P. S.)</s1>
</fA11>
<fA11 i1="04" i2="1"><s1>FERRARA (E. C.)</s1>
</fA11>
<fA11 i1="05" i2="1"><s1>SAZ PARKINSON (P. M.)</s1>
</fA11>
<fA11 i1="06" i2="1"><s1>CELIK (Ö.)</s1>
</fA11>
<fA11 i1="07" i2="1"><s1>BELFIORE (A.)</s1>
</fA11>
<fA11 i1="08" i2="1"><s1>DONATO (D.)</s1>
</fA11>
<fA11 i1="09" i2="1"><s1>CHEUNG (C. C.)</s1>
</fA11>
<fA11 i1="10" i2="1"><s1>ABDO (A. A.)</s1>
</fA11>
<fA11 i1="11" i2="1"><s1>CAMILO (F.)</s1>
</fA11>
<fA11 i1="12" i2="1"><s1>FREIRE (P. C. C.)</s1>
</fA11>
<fA11 i1="13" i2="1"><s1>GUILLEMOT (L.)</s1>
</fA11>
<fA11 i1="14" i2="1"><s1>HARDING (A. K.)</s1>
</fA11>
<fA11 i1="15" i2="1"><s1>KRAMER (M.)</s1>
</fA11>
<fA11 i1="16" i2="1"><s1>MICHELSON (P. F.)</s1>
</fA11>
<fA11 i1="17" i2="1"><s1>RANSOM (S. M.)</s1>
</fA11>
<fA11 i1="18" i2="1"><s1>ROMANI (R. W.)</s1>
</fA11>
<fA11 i1="19" i2="1"><s1>SMITH (D. A.)</s1>
</fA11>
<fA11 i1="20" i2="1"><s1>THOMPSON (D. J.)</s1>
</fA11>
<fA11 i1="21" i2="1"><s1>WELTEVREDE (P.)</s1>
</fA11>
<fA11 i1="22" i2="1"><s1>WOOD (K. S.)</s1>
</fA11>
<fA14 i1="01"><s1>Australia Telescope National Facility, CSIRO</s1>
<s2>Epping, NSW 1710</s2>
<s3>AUS</s3>
<sZ>1 aut.</sZ>
<sZ>2 aut.</sZ>
</fA14>
<fA14 i1="02"><s1>Space Science Division, Naval Research Laboratory</s1>
<s2>Washington, DC 20375</s2>
<s3>USA</s3>
<sZ>3 aut.</sZ>
<sZ>22 aut.</sZ>
</fA14>
<fA14 i1="03"><s1>NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>4 aut.</sZ>
<sZ>6 aut.</sZ>
<sZ>14 aut.</sZ>
<sZ>20 aut.</sZ>
</fA14>
<fA14 i1="04"><s1>Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz</s1>
<s2>Santa Cruz, CA 95064</s2>
<s3>USA</s3>
<sZ>5 aut.</sZ>
<sZ>7 aut.</sZ>
</fA14>
<fA14 i1="05"><s1>Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center</s1>
<s2>Greenbelt, MD 20771</s2>
<s3>USA</s3>
<sZ>6 aut.</sZ>
<sZ>8 aut.</sZ>
</fA14>
<fA14 i1="06"><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>
<server><NO>PASCAL 11-0287659 INIST</NO>
<ET>Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources</ET>
<AU>KEITH (M. J.); JOHNSTON (S.); RAY (P. S.); FERRARA (E. C.); SAZ PARKINSON (P. M.); CELIK (Ö.); BELFIORE (A.); DONATO (D.); CHEUNG (C. C.); ABDO (A. A.); CAMILO (F.); FREIRE (P. C. C.); GUILLEMOT (L.); HARDING (A. K.); KRAMER (M.); MICHELSON (P. F.); RANSOM (S. M.); ROMANI (R. W.); SMITH (D. A.); THOMPSON (D. J.); WELTEVREDE (P.); WOOD (K. S.)</AU>
<AF>Australia Telescope National Facility, CSIRO/Epping, NSW 1710/Australie (1 aut., 2 aut.); Space Science Division, Naval Research Laboratory/Washington, DC 20375/Etats-Unis (3 aut., 22 aut.); NASA Goddard Space Flight Center/Greenbelt, MD 20771/Etats-Unis (4 aut., 6 aut., 14 aut., 20 aut.); Santa Cruz Institute for Particle Physics, Department of Physics and Department of Astronomy and Astrophysics, University of California at Santa Cruz/Santa Cruz, CA 95064/Etats-Unis (5 aut., 7 aut.); Center for Research and Exploration in Space Science and Technology (CRESST) and NASA Goddard Space Flight Center/Greenbelt, MD 20771/Etats-Unis (6 aut., 8 aut.); Department of Physics and Center for Space Sciences and Technology, University of Maryland Baltimore County/Baltimore, MD 21250/Etats-Unis (6 aut.); INAF-Istituto di Astrofisica Spaziale e Fisica Cosmica/20133 Milano/Italie (7 aut.); Dipartimento di Fisica Teorica e Nucleare (DFNT), Università di Pavia/27100 Pavia/Italie (7 aut.); Departments of Physics and Gastronomy, University of Maryland/College Park, MD 20742/Etats-Unis (8 aut.); National Research Council Research Associate, National Academy of Sciences/Washington, DC 20001/Etats-Unis (9 aut., 10 aut.); Columbia Astrophysics Laboratory Columbia University/New York, NY 10027/Etats-Unis (11 aut.); Max-Planck-Institut für Radioastronomie, Auf dem Hiigel 69/53121 Bonn/Allemagne (12 aut., 13 aut., 15 aut.); Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester/Manchester M13 9PL/Royaume-Uni (15 aut., 21 aut.); W. W. Hansen Experimental Physics Laboratory, Kavli Institute for Particle Astrophysics and Cosmology, Department of Physics and SLAC National Accelerator Laboratory, Stanford University/Stanford, CA 94305/Etats-Unis (16 aut., 18 aut.); National Radio Astronomy Observatory (NRAO)/Charlottesville, VA 22903/Etats-Unis (17 aut.); Centre, d'Études Nucléaires de Bordeaux Gradignan, Université Bordeaux 1, CNRS/IN2p3/33175 Gradignan/France (19 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Etats-Unis; Da. 2011; Vol. 414; No. 2; Pp. 1292-1300; Bibl. 1/4 p.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
<CC>001E03</CC>
<FD>Pulsar milliseconde; Pulsar radio; Source Rγ; Périodicité; Pulsation radio; Rayonnement gamma; Timing; Position; Spectre radio; Probabilité; Orbite; Densité élevée; Densité flux; Mesure dispersion; Loi puissance; Forme impulsion</FD>
<ED>Millisecond pulsar; Radiopulsar; Gamma ray source; Periodicity; Radio pulsation; Gamma radiation; Timing; Positions; Radio spectrum; Probability; Orbits; High density; Flux density; Dispersion measure; Power law; Pulse shape</ED>
<SD>Pulsar milisegundo; Pulsar radio; Fuente Rγ; Periodicidad; Pulsación radio; Espectro radio; Densidad elevada; Medida dispersión; Ley poder; Forma impulsión</SD>
<LO>INIST-2067.354000190355760360</LO>
<ID>11-0287659</ID>
</server>
</inist>
</record>

Pour manipuler ce document sous Unix (Dilib)

EXPLOR_STEP=$WICRI_ROOT/Wicri/Asie/explor/AustralieFrV1/Data/PascalFrancis/Corpus

HfdSelect -h $EXPLOR_STEP/biblio.hfd -nk 001C26 | SxmlIndent | more

HfdSelect -h $EXPLOR_AREA/Data/PascalFrancis/Corpus/biblio.hfd -nk 001C26 | SxmlIndent | more

Pour mettre un lien sur cette page dans le réseau Wicri

{{Explor lien
   |wiki=    Wicri/Asie
   |area=    AustralieFrV1
   |flux=    PascalFrancis
   |étape=   Corpus
   |type=    RBID
   |clé=     Pascal:11-0287659
   |texte=   Discovery of millisecond pulsars in radio searches of southern Fermi Large Area Telescope sources
}}

This area was generated with Dilib version V0.6.33.
Data generation: Tue Dec 5 10:43:12 2017. Site generation: Tue Mar 5 14:07:20 2024

	Serveur d'exploration sur les relations entre la France et l'Australie
	Attention, ce site est en cours de développement ! Attention, site généré par des moyens informatiques à partir de corpus bruts. Les informations ne sont donc pas validées.

Serveur d'exploration sur les relations entre la France et l'Australie

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

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

Source :

Descripteurs français

English descriptors

Abstract

Notice en format standard (ISO 2709)

Format Inist (serveur)

Links to Exploration step

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri