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Article: Discovery of nine gamma-ray pulsars in Fermi Large Area Telescope data using a new blind search method

TitleDiscovery of nine gamma-ray pulsars in Fermi Large Area Telescope data using a new blind search method
Authors
KeywordsGamma Rays: Stars
Psr J0622+3749
Psr J1620-4927
Psr J1746-3239
Psr J1803-2149
Psr J2028+3332
Psr J2030+4415
Psr J2111+4606
Psr J2139+4716)
Pulsars: General
Pulsars: Individual (Psr J0106+4855
Issue Date2012
PublisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/
Citation
Astrophysical Journal, 2012, v. 744 n. 2 How to Cite?
AbstractWe report the discovery of nine previously unknown gamma-ray pulsars in a blind search of data from the Fermi Large Area Telescope (LAT). The pulsars were found with a novel hierarchical search method originally developed for detecting continuous gravitational waves from rapidly rotating neutron stars. Designed to find isolated pulsars spinning at up to kHz frequencies, the new method is computationally efficient and incorporates several advances, including a metric-based gridding of the search parameter space (frequency, frequency derivative, and sky location) and the use of photon probability weights. The nine pulsars have spin frequencies between 3 and 12Hz, and characteristic ages ranging from 17kyr to 3Myr. Two of them, PSRs J1803-2149 and J2111+ 4606, are young and energetic Galactic-plane pulsars (spin-down power above 6 × 1035ergs-1 and ages below 100kyr). The seven remaining pulsars, PSRs J0106+4855, J0622+3749, J1620-4927, J1746-3239, J2028+3332, J2030+4415, and J2139+4716, are older and less energetic; two of them are located at higher Galactic latitudes (|b| > 10°). PSR J0106+4855 has the largest characteristic age (3Myr) and the smallest surface magnetic field (2 × 1011G) of all LAT blind-search pulsars. PSR J2139+4716 has the lowest spin-down power (3 × 1033ergs-1) among all non-recycled gamma-ray pulsars ever found. Despite extensive multi-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars. © 2012 The American Astronomical Society. All rights reserved.
Persistent Identifierhttp://hdl.handle.net/10722/188415
ISSN
2015 Impact Factor: 5.909
2015 SCImago Journal Rankings: 3.266
ISI Accession Number ID
References

 

DC FieldValueLanguage
dc.contributor.authorPletsch, HJen_US
dc.contributor.authorGuillemot, Len_US
dc.contributor.authorAllen, Ben_US
dc.contributor.authorKramer, Men_US
dc.contributor.authorAulbert, Cen_US
dc.contributor.authorFehrmann, Hen_US
dc.contributor.authorRay, PSen_US
dc.contributor.authorBarr, EDen_US
dc.contributor.authorBelfiore, Aen_US
dc.contributor.authorCamilo, Fen_US
dc.contributor.authorCaraveo, PAen_US
dc.contributor.authorÇelik, Öen_US
dc.contributor.authorChampion, DJen_US
dc.contributor.authorDormody, Men_US
dc.contributor.authorEatough, RPen_US
dc.contributor.authorFerrara, ECen_US
dc.contributor.authorFreire, PCCen_US
dc.contributor.authorHessels, JWTen_US
dc.contributor.authorKeith, Men_US
dc.contributor.authorKerr, Men_US
dc.contributor.authorDe Luca, Aen_US
dc.contributor.authorLyne, AGen_US
dc.contributor.authorMarelli, Men_US
dc.contributor.authorMclaughlin, MAen_US
dc.contributor.authorParent, Den_US
dc.contributor.authorRansom, SMen_US
dc.contributor.authorRazzano, Men_US
dc.contributor.authorReich, Wen_US
dc.contributor.authorSaz Parkinson, PMen_US
dc.contributor.authorStappers, BWen_US
dc.contributor.authorWolff, MTen_US
dc.date.accessioned2013-09-03T04:05:40Z-
dc.date.available2013-09-03T04:05:40Z-
dc.date.issued2012en_US
dc.identifier.citationAstrophysical Journal, 2012, v. 744 n. 2en_US
dc.identifier.issn0004-637Xen_US
dc.identifier.urihttp://hdl.handle.net/10722/188415-
dc.description.abstractWe report the discovery of nine previously unknown gamma-ray pulsars in a blind search of data from the Fermi Large Area Telescope (LAT). The pulsars were found with a novel hierarchical search method originally developed for detecting continuous gravitational waves from rapidly rotating neutron stars. Designed to find isolated pulsars spinning at up to kHz frequencies, the new method is computationally efficient and incorporates several advances, including a metric-based gridding of the search parameter space (frequency, frequency derivative, and sky location) and the use of photon probability weights. The nine pulsars have spin frequencies between 3 and 12Hz, and characteristic ages ranging from 17kyr to 3Myr. Two of them, PSRs J1803-2149 and J2111+ 4606, are young and energetic Galactic-plane pulsars (spin-down power above 6 × 1035ergs-1 and ages below 100kyr). The seven remaining pulsars, PSRs J0106+4855, J0622+3749, J1620-4927, J1746-3239, J2028+3332, J2030+4415, and J2139+4716, are older and less energetic; two of them are located at higher Galactic latitudes (|b| > 10°). PSR J0106+4855 has the largest characteristic age (3Myr) and the smallest surface magnetic field (2 × 1011G) of all LAT blind-search pulsars. PSR J2139+4716 has the lowest spin-down power (3 × 1033ergs-1) among all non-recycled gamma-ray pulsars ever found. Despite extensive multi-frequency observations, only PSR J0106+4855 has detectable pulsations in the radio band. The other eight pulsars belong to the increasing population of radio-quiet gamma-ray pulsars. © 2012 The American Astronomical Society. All rights reserved.en_US
dc.languageengen_US
dc.publisherInstitute of Physics Publishing, Inc. The Journal's web site is located at http://iopscience.iop.org/0004-637X/en_US
dc.relation.ispartofAstrophysical Journalen_US
dc.subjectGamma Rays: Starsen_US
dc.subjectPsr J0622+3749en_US
dc.subjectPsr J1620-4927en_US
dc.subjectPsr J1746-3239en_US
dc.subjectPsr J1803-2149en_US
dc.subjectPsr J2028+3332en_US
dc.subjectPsr J2030+4415en_US
dc.subjectPsr J2111+4606en_US
dc.subjectPsr J2139+4716)en_US
dc.subjectPulsars: Generalen_US
dc.subjectPulsars: Individual (Psr J0106+4855en_US
dc.titleDiscovery of nine gamma-ray pulsars in Fermi Large Area Telescope data using a new blind search methoden_US
dc.typeArticleen_US
dc.description.naturelink_to_subscribed_fulltexten_US
dc.identifier.doi10.1088/0004-637X/744/2/105en_US
dc.identifier.scopuseid_2-s2.0-84555196289en_US
dc.relation.referenceshttp://www.scopus.com/mlt/select.url?eid=2-s2.0-84555196289&selection=ref&src=s&origin=recordpageen_US
dc.identifier.volume744en_US
dc.identifier.issue2en_US
dc.identifier.isiWOS:000298666400025-
dc.publisher.placeUnited Statesen_US
dc.identifier.scopusauthoridPletsch, HJ=22136414100en_US
dc.identifier.scopusauthoridGuillemot, L=36739789600en_US
dc.identifier.scopusauthoridAllen, B=7401697906en_US
dc.identifier.scopusauthoridKramer, M=23968081200en_US
dc.identifier.scopusauthoridAulbert, C=35226967900en_US
dc.identifier.scopusauthoridFehrmann, H=24334445300en_US
dc.identifier.scopusauthoridRay, PS=7401892043en_US
dc.identifier.scopusauthoridBarr, ED=36815610100en_US
dc.identifier.scopusauthoridBelfiore, A=26535417200en_US
dc.identifier.scopusauthoridCamilo, F=7006263946en_US
dc.identifier.scopusauthoridCaraveo, PA=14006843000en_US
dc.identifier.scopusauthoridÇelik, Ö=36969322100en_US
dc.identifier.scopusauthoridChampion, DJ=8920388300en_US
dc.identifier.scopusauthoridDormody, M=13807358800en_US
dc.identifier.scopusauthoridEatough, RP=26029120300en_US
dc.identifier.scopusauthoridFerrara, EC=7005472148en_US
dc.identifier.scopusauthoridFreire, PCC=7005742539en_US
dc.identifier.scopusauthoridHessels, JWT=6701717720en_US
dc.identifier.scopusauthoridKeith, M=7004565374en_US
dc.identifier.scopusauthoridKerr, M=7403308674en_US
dc.identifier.scopusauthoridDe Luca, A=22136414100en_US
dc.identifier.scopusauthoridLyne, AG=36739789600en_US
dc.identifier.scopusauthoridMarelli, M=7401697906en_US
dc.identifier.scopusauthoridMcLaughlin, MA=23968081200en_US
dc.identifier.scopusauthoridParent, D=35226967900en_US
dc.identifier.scopusauthoridRansom, SM=24334445300en_US
dc.identifier.scopusauthoridRazzano, M=7401892043en_US
dc.identifier.scopusauthoridReich, W=36815610100en_US
dc.identifier.scopusauthoridSaz Parkinson, PM=26535417200en_US
dc.identifier.scopusauthoridStappers, BW=7006263946en_US
dc.identifier.scopusauthoridWolff, MT=14006843000en_US

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