J/ApJS/208/17ivo://CDS.VizieR/J/ApJS/208/17doi:10.26093/cds/vizier.22080017CDSAbdo A.A.Ajello M.Allafort A.Baldini L.Ballet J.Barbiellini G.,Baring M.G.Bastieri D.Belfiore A.Bellazzini R.Bhattacharyya B.,Bissaldi E.Bloom E.D.Bonamente E.Bottacini E.Brandt T.J.,Bregeon J.Brigida M.Bruel P.Buehler R.Burgay M.Burnett T.H.,Busetto G.Buson S.Caliandro G.A.Cameron R.A.Camilo F.,Caraveo P.A.Casandjian J.M.Cecchi C.Celik O.Charles E.Chaty S.,Chaves R.C.G.Chekhtman A.Chen A.W.Chiang J.Chiaro G.Ciprini S.,Claus R.Cognard I.Cohen-Tanugi J.Cominsky L.R.Conrad J.Cutini S.,D'Ammando F.de Angelis A.DeCesar M.E.De Luca A.den Hartog P.R.,de Palma F.Dermer C.D.Desvignes G.Digel S.W.Di Venere L.,Drell P.S.Drlica-Wagner A.Dubois R.Dumora D.Espinoza C.M.,Falletti L.Favuzzi C.Ferrara E.C.Focke W.B.Franckowiak A.,Freire P.C.C.Funk S.Fusco P.Gargano F.Gasparrini D.Germani S.,Giglietto N.Giommi P.Giordano F.Giroletti M.Glanzman T.,Godfrey G.Gotthelf E.V.Grenier I.A.Grondin M.-H.Grove J.E.,Guillemot L.Guiriec S.Hadasch D.Hanabata Y.Harding A.K.,Hayashida M.Hays E.Hessels J.Hewitt J.Hill A.B.Horan D.Hou X.,Hughes R.E.Jackson M.S.Janssen G.H.Jogler T.Johannesson G.,Johnson R.P.Johnson A.S.Johnson T.J.Johnson W.N.Johnston S.,Kamae T.Kataoka J.Keith M.Kerr M.Knodlseder J.Kramer M.Kuss M.,Lande J.Larsson S.Latronico L.Lemoine-Goumard M.Longo F.,Loparco F.Lovellette M.N.Lubrano P.Lyne A.G.Manchester R.N.,Marelli M.Massaro F.Mayer M.Mazziotta M.N.McEnery J.E.,McLaughlin M.A.Mehault J.Michelson P.F.Mignani R.P.Mitthumsiri W.,Mizuno T.Moiseev A.A.Monzani M.E.Morselli A.Moskalenko I.V.,Murgia S.Nakamori T.Nemmen R.Nuss E.Ohno M.Ohsugi T.Orienti M.,Orlando E.Ormes J.F.Paneque D.Panetta J.H.Parent D.Perkins J.S.,Pesce-Rollins M.Pierbattista M.Piron F.Pivato G.Pletsch H.J.,Porter T.A.Possenti A.Raino S.Rando R.Ransom S.M.Ray P.S.,Razzano M.Rea N.Reimer A.Reimer O.Renault N.Reposeur T.Ritz S.,Romani R.W.Roth M.Rousseau R.Roy J.Ruan J.Sartori A.,Saz Parkinson P.M.Scargle J.D.Schulz A.Sgro C.Shannon R.,Siskind E.J.Smith D.A.Spandre G.Spinelli P.Stappers B.W.,Strong A.W.Suson D.J.Takahashi H.Thayer J.G.Thayer J.B.,Theureau G.Thompson D.J.Thorsett S.E.Tibaldo L.Tibolla O.,Tinivella M.Torres D.F.Tosti G.Troja E.Uchiyama Y.Usher T.L.,Vandenbroucke J.Vasileiou V.Venter C.Vianello G.Vitale V.Wang N.,Weltevrede P.Winer B.L.Wolff M.T.Wood D.L.Wood K.S.Wood M.,Yang Z.2017-06-22T14:28:55Z2014-01-14T13:07:34ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frpulsarsgamma-ray-astronomyThis catalog summarizes 117 high-confidence >= 0.1 GeV gamma-ray pulsar detections using three years of data acquired by the Large Area Telescope (LAT) on the Fermi satellite. Half are neutron stars discovered using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The 117 pulsars are evenly divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. We characterize the pulse profiles and energy spectra and derive luminosities when distance information exists. Spectral analysis of the off-peak phase intervals indicates probable pulsar wind nebula emission for four pulsars, and off-peak magnetospheric emission for several young and millisecond pulsars. We compare the gamma-ray properties with those in the radio, optical, and X-ray bands. We provide flux limits for pulsars with no observed gamma-ray emission, highlighting a small number of gamma-faint, radio-loud pulsars. The large, varied gamma-ray pulsar sample constrains emission models. Fermi's selection biases complement those of radio surveys, enhancing comparisons with predicted population distributions.2013ApJS..208...17Ahttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/ApJS/208/17CatalogResearchIsServedByTAP VizieR generic serviceIsServedByConesearch servicerelated-toVII/189 : Catalog of Pulsars (Taylor+ 1995)J/MNRAS/424/2832 : Pulsars in {gamma}-ray sources (Lee+, 2012)J/ApJS/199/31 : Fermi LAT second source catalog (2FGL) (Nolan+, 2012)J/ApJS/188/405 : Fermi-LAT first source catalog (1FGL) (Abdo+, 2010)J/ApJS/183/46 : Fermi/LAT bright gamma-ray source list (0FGL) (Abdo+, 2009)J/ApJ/706/L7 : The Fermi LAT sky as seen by INTEGRAL/IBIS (Ubertini+, 2009)J/A+A/492/923 : Fermi Gamma-ray Space Tel. pulsar timings (Smith+, 2008)J/MNRAS/372/777 : Parkes Multibeam Pulsar Survey. VI. (Lorimer+, 2006)J/MNRAS/362/1189 : Proper motions of 74 pulsars (Zou+, 2005)J/MNRAS/360/974 : Proper motions of pulsars (Hobbs+, 2005)J/MNRAS/353/1311 : Long-term timing observations of 374 pulsars (Hobbs+, 2004)J/MNRAS/328/17 : Parkes Multi-Beam Pulsar Survey (Manchester+, 2001)J/A+AS/124/123 : Atlas of the Crab pulsar pulse profiles (Massaro+ 1997)J/MNRAS/273/411 : Multifrequency fluxes of 280 pulsars (Lorimer+ 1995)http://fermi.gsfc.nasa.gov/ssc/ : Fermi Science Support Center home pagehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/ApJS/208/17https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/ApJS/208/17http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/ApJS/208/17https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/ApJS/208/17https://vizier.iucaa.in/viz-bin/votable?-source=J/ApJS/208/17http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/ApJS/208/17GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapCone search capability for table J/ApJS/208/17/psrcat (LAT 2nd pulsar catalog: PULSAR_CATALOG)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/208/17/psrcat?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/208/17/psrcat?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/208/17/psrcat?GETtext/xml+votable180.050000true1.756573.05230.005555555555555556Cone search capability for table J/ApJS/208/17/offpk (LAT second pulsar catalog: OFF_PEAK table)https://vizier.cds.unistra.fr/viz-bin/conesearch/J/ApJS/208/17/offpk?https://vizier.iucaa.in/viz-bin/conesearch/J/ApJS/208/17/offpk?http://vizieridia.saao.ac.za/viz-bin/conesearch/J/ApJS/208/17/offpk?GETtext/xml+votable180.050000true1.934372.89450.0055555555555555566/1199 1684 2411 2855 2860 3302 3681 3819 4750 6787 12446 12871 12958 12975 13106 13191 13465 13750 14051 14219 14268 14270 14413 14424 14454 14608 14619 14621 14690 14692 14712 14840 15310 15376 15644 17955 18153 19535 20552 20896 21511 21519 22154 22255 23646 23830 23952 24185 25065 26824 28751 28805 28808 28814 28825 28879 28894 28918 29002 29261 29471 29505 29521 29523 29575 30193 30244 30593 30634 31228 31976 32160 33457 34034 37341 37343 37361 37365 37721 37848 37912 37923 37924 37937 37940 38020 38022 38081 38354 39235 39241 39789 41583 41598 41681 41685 41743 41758 41804 41857 41937 41964 42173 42176 42206 42332 42384 42396 42438 42916 44356 46237 47306 48193 490539.276497240453405e-25 9.276497240453405e-25https://cdsarc.cds.unistra.fr/viz-bin/moc/J/ApJS/208/17?format=asciiGamma-rayRadiodefaultJ/ApJS/208/17/psrcatLAT 2nd pulsar catalog: PULSAR_CATALOGrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNamePulsar name (JHHMM+DDMMA)meta.id;meta.maincharprimaryRAJ2000Pulsar right ascension (J2000)degpos.eq.ra;meta.mainDEJ2000Pulsar declination (J2000)degpos.eq.dec;meta.mainPer[1.5/445] Pulsar rotation periodmstime.periodfloatPdot[3.8e-21/4.1e-12] Period first derivative (1)s/stime.perioddoubleEdot[4.6e+32/4.4e+38] Pulsar spin-down luminosity in erg/s (1)1e-07Wphys.energydoublecOff[226/5889]? Best-fit cutoff energy Ec for the "PLSuperExpCutoff" spectral model (G1)MeVphys.energy;meta.modelleddoublenullablee_cOff[19/3891]? cOff statistical errorMeVstat.errordoublenullableDist[0.1/16]? Pulsar distancekpcpos.distance;pos.heliocentricdoublenullablee_Dist[0.001/4.2]? Negative uncertainty on Distkpcstat.errordoublenullableE_Dist[0.001/13.2]? Positive uncertainty on Distkpcstat.error;stat.maxdoublenullableB_Dist[8.2/25.3]? Upper limit on pulsar distance (6)kpcpos.distance;stat.maxdoublenullablen_DistMethod used to determine the distance (7)meta.notecharr_Dist[0/97]? Dist reference (see refs.dat file)meta.ref;pos.frameintnullablepm[0.8/169]? Proper motion for the pulsarmas/yrpos.pmdoublenullablee_pm[0.01/170]? pm uncertaintymas/yrstat.errordoublenullabler_pm[0/100]? pm reference (see refs.dat file)meta.ref;pos.frameintnullableiPdot[4.4e-22/1.92e-13]? Intrinsic P-dot (8)s/stime.perioddoublenullablee_iPdot[2.2e-23/2.5e-17]? iPdot negative uncertaintys/sstat.errordoublenullableE_iPdot[2.6e-23/2.5e-17]? iPdot positive uncertaintys/sstat.error;stat.maxdoublenullableiEdot[4.6e+32/4.4e+38]? Intrinsic spin down power in erg/s1e-07Wphys.energydoublenullablee_iEdot[3.9e+28/1.8e+34]? iEdot negative uncertainty1e-07Wstat.errordoublenullableE_iEdot[3.9e+28/1.2e+34]? iEdot positive uncertainty1e-07Wstat.error;stat.maxdoublenullableLum[4.8e+31/6.0e+36]? Pulsar luminosity (erg/s)1e-07Wphys.luminositydoublenullables_Lum[3.2e+30/3.0e+35]? Lum statistical error1e-07Wstat.error;stat.valuedoublenullablee_Lum[6.2e+29/3.8e+36]? Negative systematic error on Lum (9)1e-07Wstat.errordoublenullableE_Lum[6.2e+29/2.7e+36]? Lum positive sys. error (9)1e-07Wstat.error;stat.maxdoublenullableB_Lum[1.1e+35/2.8e+37]? Upper limit on Lum (10)1e-07Wphys.luminosity;stat.maxdoublenullableEff[0.0009/11.8]? Pulsar efficiency%stat.fit.paramdoublenullables_Eff[0/1.93]? Eff statistical error%stat.error;stat.value;arith.ratiodoublenullablee_Eff[0/5.73]? Negative systematic error on Eff%stat.errordoublenullableE_Eff[0/64.5]? Positive systematic error on Eff%stat.error;stat.maxdoublenullableB_Eff[0.6/303.6]? Upper limit on Eff (10)%stat.fit.param;stat.maxdoublenullableS1400[0.003/1100]? 1400MHz radio flux density (11)mJyphot.flux.density;em.radio.750-1500MHzdoublenullableB_S1400[0.003/0.51]? Upper limit on S1400mJyphot.flux.density;em.radio.750-1500MHz;stat.maxdoublenullabler_S1400[0/100]? S1400 reference (see refs.dat file)meta.ref;pos.frameintnullableNpk[1/3] Number of peaks in the gamma-ray profilemeta.numberintn_Rlag[phso -] Method used to choose the radio fiducial phase (12)meta.notecharRlag[0/0.997]? Phase separation ({delta}) between the first gamma-ray peak and the radio peaktime.intervaldoublenullablee_Rlag[0/0.077]? Rlag uncertaintystat.errordoublenullablePksep[0/0.808]? Phase separation ({Delta}) between the first and last gamma-ray peaks (13)time.intervaldoublenullablee_Pksep[0/0.192]? Pksep uncertaintystat.errordoublenullableHWP1L[0.0008/0.34] Half-width half-maximum of the leading (left) first peak edge, as fitted (14)spect.line.widthfloate_HWP1L[0.0001/0.08] HWP1L uncertaintystat.errorfloatHWP1R[0.0008/0.39] Half-width half-maximum of the trailing (right) first peak edge (14)spect.line.widthfloate_HWP1R[0/0.18]? HWP1R uncertaintystat.errorfloatnullableHWP2L[0/0.28]? Half-width half-maximum of the leading (left) 2nd peak edge, as fitted (14)spect.line.widthdoublenullablee_HWP2L[0/0.19]? HWP2L uncertaintystat.errordoublenullableHWP2R[0/0.22]? Half-width half-maximum of the trailing (right) 2nd peak edge, as fitted (14)spect.line.widthdoublenullablee_HWP2R[0/0.15]? HWP2R uncertaintystat.errordoublenullableNH[0/3.8e+22]? Hydrogen column densitycm**-2phys.columnDensitydoublenullablee_NH[0/1.1e+22]? NH negative systematic errorcm**-2stat.errordoublenullableE_NH[0/1.7e+22]? NH positive systematic errorcm**-2stat.error;stat.maxdoublenullableB_NH[-9e+20,2e+22]? Upper limit on NHcm**-2phys.columnDensity;stat.maxdoublenullableXFlux[0/4.43e-09]? Non-thermal unabsorbed X-ray energy flux in the 0.3-10 keV energy band (15)mW.m**-2phot.flux;em.X-raydoublenullablee_XFlux[0/1.e-10]? XFlux negative uncertainty (90% CL)mW.m**-2stat.errordoublenullableE_XFlux[0/1.e-10]? XFlux positive uncertainty (90% CL)mW.m**-2stat.error;stat.maxdoublenullableB_XFlux[0/1.5e-10]? XFlux upper limitmW.m**-2phot.flux;em.X-ray;stat.maxdoublenullableFXb[0/4.0e-08]? Estimated non-thermal X-ray flux from the brightest part of the associated plerion, in the 0.3-10 keV energy bandmW.m**-2phot.flux;em.X-raydoublenullablee_FXb[0/1.e-10]? FXb negative uncertainty (90% CL)mW.m**-2stat.errordoublenullableE_FXb[0/1.e-10]? FXb positive uncertainty (90% CL)mW.m**-2stat.error;stat.maxdoublenullableqX[012* ] Quality of X-ray detection, 2=best (16)meta.code.qual;pos.cartesian.xcharObjObject to which the measured optical flux pertains (17)phot.flux;em.optcharn_magThe filter used for the optical observation (B, I, J, K, R, U, V or g)meta.code;instr.filtercharmag[15.8/26.7]? Optical magnitude of the optical counterpart for the pulsar or pulsar systemphot.mag;em.optfloatnullableb_mag[19.1/28.5]? Lower limit of magmeta.notefloatnullableExt[0/15]? Optical extinction (18)phys.absorption;em.optfloatnullablee_Ext[0/2.5]? Negative uncertainty on Extstat.errordoublenullableE_Ext[0/2.9]? Positive uncertainty on Extstat.error;stat.maxdoublenullableB_Ext[0.01/4.5]? Upper limit of Extmeta.notedoublenullableFVc[0/4.6e-12]? Corrected (unabsorbed) optical energy flux in the V-band (19)phot.flux.density;em.opt.Vdoublenullablee_FVc[0/4.7e-14]? Negative uncertainty on FVcstat.errordoublenullableE_FVc[0/4.7e-14]? Positive uncertainty on FVcstat.error;stat.maxdoublenullableB_FVc[0/1.1e-11]? Upper limit of FVcmeta.notedoublenullableType[YRL YRQ MSP] Pulsar class (20)src.classcharBin[NY] Y: the pulsar is in a binary systemmeta.codecharHistPulsar discovery in "Radio", "X-rays", or "Gamma"meta.notecharLCLight curve image for this pulsar (png format)meta.ref.urlcharSEDSED image for this pulsar (png format) if availablemeta.ref.urlcharparRotation ephemeris in a TEMPO2 parameter for this pulsarmeta.ref.urlcharfitsDownload the FITS (binary table) version of the detailed analysis for this pulsarmeta.ref.urlcharSimbadSimbad column added by the CDSmeta.refcharNEDSimbad column added by the CDSmeta.refcharOn[NY] Y: spectral fit used only on-peak eventsmeta.codecharTS-DC? Test statistic in PLEC1 model (G1)stat.fit.goodnessintnullableTS-c? Spectral cutoff significance (G1)stat.fit.goodnessintnullableTS-f? Test statistic of improvement of PLEC over PLEC1 (free {beta}) (G1)stat.fit.goodnessintnullablePref1[2.8e-13/8.4e-09]? Best-fit prefactor p in the PLEC1 fit in ph/cm^2^/s/MeV (G1)cm**-2.s**-1.MeV**-1stat.fit.paramdoublenullablee_Pref1[3.1e-13/6.5e-11]? Pref1 uncertaintycm**-2.s**-1.MeV**-1stat.errordoublenullablepInd1[0/2.038]? Best-fit photon index {alpha} in the PLEC1 fit (G1)spect.indexdoublenullablee_pInd1[0/1.353]? pInd1 uncertaintystat.errordoublenullableSc1[401/6601]? Scaling energy Eo in PLEC1 fit (G1)MeVstat.fit.paramfloatnullableEc1[226/5889]? Best-fit cutoff energy Ec in PLEC1 fit (G1)MeVstat.fit.paramfloatnullablee_Ec1[19/3891]? Ec1 uncertaintyMeVstat.errorfloatnullableFph[9.6e-10/1.1e-05]? The photon flux integrated from 100MeV to 100GeV in PLEC1 fit (G1)ph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullablee_Fph[2.9e-10/5.3e-08]? Fph uncertaintyph.cm**-2.s**-1stat.errordoublenullableFerg[1.9e-12/9.1e-09]? The energy flux integrated from 100MeV to 100GeV in PLEC1 fit (G1)mW.m**-2phot.flux.density;em.gamma.harddoublenullablee_Ferg[8.1e-13/2.7e-11]? Ferg uncertaintymW.m**-2stat.errordoublenullablePreff[1.6e-10/1.9e-08]? The best-fit prefactor p in the PLEC fit in ph/cm^2^/s (G1)cm**-2.s**-1stat.fit.paramdoublenullablee_Preff[1.4e-11/1.3e-10]? Preff uncertaintycm**-2.s**-1stat.errordoublenullablepIndf[0.362/1.554]? Photon index {alpha} in the PLEC fit (G1)spect.indexdoublenullablee_pIndf[0.002/0.215]? pIndf uncertaintystat.errordoublenullableScf[400/2200]? Best-fit caling energy Eo in the PLEC fit (G1)MeVstat.fit.paramfloatnullableEcf[100/1006]? Cutoff energy Ec in PLEC fit (G1)MeVstat.fit.paramdoublenullablee_Ecf[0/204]? Ecf uncertaintyMeVstat.errordoublenullableeIndf[0.384/0.747]? best-fit exponential {beta} in the PLEC fit (G1)spect.indexdoublenullablee_eIndf[0.001/0.048]? eIndf uncertaintystat.errordoublenullableFphf[6.e-08/1.1e-05]? The photon flux integrated from 100MeV to 100GeV in PLEC fit (G1)ph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullablee_Fphf[2.7e-09/2.7e-08]? Fphf uncertaintyph.cm**-2.s**-1stat.errordoublenullableFergf[5.5e-11/9.2e-09]? The energy flux integrated from 100MeV to 100GeV in PLEC fit (G1)mW.m**-2phot.flux.density;em.gamma.harddoublenullablee_Fergf[2.8e-12/3.2e-11]? Fergf uncertaintymW.m**-2stat.errordoublenullablePref0[4e-15/2.1e-09]? The best-fit prefactor p in a "PowerLaw" model in ph/cm^2^/s/MeV (G1)cm**-2.s**-1.MeV**-1stat.fit.paramdoublenullablee_Pref0[5.7e-14/1.3e-11]? Pref0 uncertaintycm**-2.s**-1.MeV**-1stat.errordoublenullablepInd0[1/3]? Best-fit photon index {alpha} in a "PowerLaw" model (G1)spect.indexdoublenullablee_pInd0[0.001/6.9]? pInd0 uncertaintystat.errordoublenullableSc0[586/3805]? Scaling energy Eo using for the spectral fit using a "PowerLaw" model (G1)MeVstat.fit.paramintnullableFph0[1e-11/1.2e-05]? The photon flux integrated from 100MeV to 100GeV in PL fit (G1)ph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullablee_Fph0[1.5e-10/7.6e-08]? Fph0 uncertaintyph.cm**-2.s**-1stat.errordoublenullableFerg0[1.9e-13/1.7e-08] The energy flux integrated from 100MeV to 100GeV in PL fit (G1)mW.m**-2phot.flux.density;em.gamma.harddoublee_Ferg0[5.6e-13/4.4e-11] Ferg0 uncertaintymW.m**-2stat.errordoubleJ/ApJS/208/17/refsLAT second pulsar catalog: REFERENCESrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintRef[1/100] Reference code numbermeta.id;meta.mainintAutAuthor's name(s)meta.bib.authorcharBibCodeBibcodemeta.bib.bibcodecharTitleTitle of the referencemeta.refcharJ/ApJS/208/17/offpkLAT second pulsar catalog: OFF_PEAK tableMod2Spatial model (26)meta.id;stat.fitcharModoBest off-peak spectral model (24)meta.id;stat.fitcharrecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintNamePulsar name (JHHMM+DDMMA)meta.id;meta.maincharoCl[LMUW ] Off-peak emission class (21)src.classcharmPhi? Minimum phase of the off-peak intervaltime.phasefloatnullableMPhi? Maximum phase of the off-peak intervaltime.phasefloatnullablemPhi2? Minimum phase of the 2nd off-peak intervaltime.phasefloatnullableMPhi2? Maximum phase of the 2nd off-peak intervaltime.phasefloatnullableTS-PS? Test statistic obtained at the best-fit position of assumed point-like source (22)stat.fit.goodnessfloatnullableTS-ex[0/283]? Significance of any possible extension for the sourcestat.fit.goodnessfloatnullableTS-co[0/365]? Significance of any spectral cutoff (23)stat.fit.goodnessfloatnullableTS-v[0/373]? Significance of variability in the off-pulse emissionstat.fit.goodnessfloatnullableFpho[0/1.1e-06]? Best-fit integrated photon flux (100MeV-316GeV) in spectral modelph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullablee_Fpho[0/4.4e-08]? Fph1 statistical errorph.cm**-2.s**-1stat.errordoublenullableFergo[0/6.8e-10]? Best-fit integrated energy flu (100MeV-316GeV) in spectral modelmW.m**-2phot.flux.density;em.gamma.harddoublenullablee_Fergo[0/2.9e-11]? Fergo statistical errormW.m**-2stat.errordoublenullablePrefo[0/6.7e-10]? Best-fit prefactor p (G1)stat.fit.paramdoublenullablee_Prefo[0/4.2e-10]? Prefo statistical errorstat.errordoublenullableNorm[0/1.1]? Best-fit "file" normalization (25)stat.fit.paramfloatnullablee_Norm[0/0.05]? Norm statistical errorstat.errorfloatnullableSco[0/5624]? Scaling energy Eo in model (G1)MeVstat.fit.paramfloatnullablepIndo[0/2.72]? Best-fit photon index {alpha} (G1)spect.indexfloatnullablee_pIndo[0/0.94]? pIndo statistical errorstat.errorfloatnullableEco[0/2553]? Best-fit cutoff energy (G1)MeVphys.energy;meta.modelledfloatnullablee_Eco[0/2484]? Eco statistical uncertaintyMeVstat.errorfloatnullableRAJ2000? Right ascension of the source (J2000) (27)degpos.eq.ra;meta.mainnullableDEJ2000? Declination of the source (J2000) (27)degpos.eq.dec;meta.mainnullableePos[0/0.09]? Estimated statistical error on the localization of the source (28)degstat.error;stat.valuefloatnullableExt[0/0.87]? Best-fit extension (in case of "Extended" model)degphys.angSize;meta.modelledfloatnullablee_Ext[0/0.06]? Ext statistical errordegstat.errorfloatnullablepFup0[0/8.3e-08]? 95% confidence-level photon flux upper limit in power-law model (29)ph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullableeFup0[0/5.8e-11]? 95% confidence level energy flux upper limit in power-law model (29)mW.m**-2phot.flux.density;em.gamma.harddoublenullablepFup1[0/100]? 95% confidence photon flux upper limit with PLEC1 model (30)ph.cm**-2.s**-1phot.flux.density;em.gamma.harddoublenullableeFup1[0/178]? 95% confidence energy flux upper limit with PLEC1 model (30)mW.m**-2phot.flux.density;em.gamma.harddoublenullable