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FERMIL2PSR - Fermi LAT Second Catalog of Gamma-Ray Pulsars (2PC)

 HEASARC
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Overview

This catalog summarizes 0.1 GeV gamma-ray pulsar detections using data acquired by the Large Area Telescope (LAT) on the Fermi satellite. These pulsars are neutron stars identified using LAT data through periodicity searches in gamma-ray and radio data around LAT unassociated source positions. The catalogued pulsars are divided into three groups: millisecond pulsars, young radio-loud pulsars, and young radio-quiet pulsars. This catalog summarizes results of the analysis of pulse profiles and energy spectra, and analysis of the off-peak phase intervals, and compares the gamma-ray properties with those in the radio, optical, and X-ray bands. Flux limits for pulsars with no observed gamma-ray emission are provided.

Catalog Bibcode

2013ApJS..208...17A

References

The second Fermi Large Area Telescope catalog of gamma-ray pulsars.
    Abdo 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.
   <Astrophys. J. Suppl. Ser., 208, 17 (2013)>
   =2013ApJS..208...17A
A full description of the LAT Second Catalog of Gamma-Ray Pulsars is given in the Second Fermi Large Area Telescope Catalog of Gamma-Ray Pulsars (Abdo et al., 2013). The catalog and associated data products are available from the Fermi Science Support Center.

Provenance

This database was constructed by the HEASARC by combining the tabulated data in the psrcat.dat, spec.dat, offpk.dat and refs.dat obtained from http://adsabs.harvard.edu/abs/2013yCat..22080017A.

Parameters

Name
The designation of the pulsar, PSR JHHMM+DDMMA.

RA
The Right Ascension of the gamma-ray source in the selected equinox. This was given in J2000 decimal degrees to a precision of 0.0001 degrees (0.36 arcseconds) in the original table.

Dec
The Declination of the gamma-ray source in the selected equinox. This was given in J2000 decimal degree coordinates in the original table.

LII
The Galactic Longitude of the gamma-ray source, as derived from the J2000 position in the original table.

BII
The Galactic Latitude of the gamma-ray source, as derived from the J2000 position in the original table.

Period
The pulsar rotation period, in milliseconds.

Pdot
The pulsar rotation period first time derivative, in seconds per second.

Edot
The pulsar spin-down luminosity, uncorrected for the Shklovskii Effect due to the proper motion of the pulsar, Shklovskii 1970) or galactic acceleration, in erg/s.

Photon_Flux
The best-fit photon flux integrated from 100MeV to 100GeV, in photons/s/cm2.

Photon_Flux_Error
the statistical error for the best-fit photon flux integrated from 100 MeV to 100 GeV, in photons/s/cm2.

Flux
The best-fit energy flux from 100MeV to 100GeV, in erg/s/cm2.

Flux_Error
The statistical error for the best-fit energy flux from 100MeV to 100GeV, in erg/s/cm2.

TS_Dc
The test statistic for PLSuperExpCutoff model, with the parameter representing the sharpness of the cutoff (b) fixed to 1. This is abbreviated as the PLEC1 model by the table authors, and defined in equation B1 of Abdo et al. (2013).

TS_Cutoff
The significance of the spectral cutoff, obtained from the improvement in log(likelihood) from the PLSuperExpCutoff spectral model fit over a PowerLaw spectral fit.

TS_Improvement
The improvement in the test statistic when the exponential index is left free in the PLSuperExpCutoff spectral fit. A value of 0 indicates no improvement in the fit using the PLSuperExpCutoff model.

Photon_Index
The best-fit photon index (alpha) for the PLSuperExpCutoff (PLEC) spectral model.

Photon_Index_Error
The statistical error for the best-fit photon index (alpha).

Cutoff
The best-fit cutoff energy for the PLSuperExpCutoff spectral model, in MeV.

Cutoff_Error
The statistical error in the best-fit cutoff energy, in MeV.

Distance
The distance to the pulsar, in parsecs. Null values indicate that only an upper limit has been determined.

Distance_Neg_Err
The negative uncertainty for the pulsar distance, in parsecs.

Distance_Pos_Err
The positive uncertainty for the pulsar distance, in parsecs

Distance_Upper
The upper limit on pulsar distance, in parsecs.

Distance_Method
A code to describe the method used to determine the distance. Methods are: K for the kinematic model, DM for the dispersion measure using the NE2001 model of Cordes & Lazio (2002), O for optical measurements, and X for X-ray measurements. DMM means that the distance to the Galaxy's edge, as determined by the maximum DM value provided by the NE2001 model for that line of sight, is taken as an upper limit.

Ref_Distance
The reference bibcode for the distance.

Proper_Motion
The proper motion of the pulsar, in milli-arcseconds per year.

Proper_Motion_Error
The uncertainty in proper motion of the pulsar, in milli-arcseconds per year.

Ref_Proper_Motion
The reference bibcode for the proper motion.

Ipdot
The intrinsic period derivative (after correction for Shklovskii Effect and galactic acceleration, in seconds per second.

Ipdot_Neg_Err
The negative uncertainty for the intrinsic period derivative, in seconds per second.

Ipdot_Pos_Err
The positive uncertainty for the intrinsic period derivative, in seconds per second.

Iedot
The intrinsic spin-down power (after correction for Shklovskii Effect and galactic acceleration) in erg/s.

Iedot_Neg_Err
The negative uncertainty for the intrinsic spin-down power, in erg/s.

Iedot_Pos_Err
The positive uncertainty for the intrinsic spin-down power, in erg/s.

Luminosity
The pulsar gamma-ray luminosity in the 0.1 - 100 GeV band, in erg/s.

Luminosity_Stat_Err
The statistical error for the pulsar gamma-ray luminosity in the 0.1 - 100 GeV band, in erg/s.

Luminosity_Neg_Err
The negative systematic uncertainty for the pulsar gamma-ray luminosity in the 0.1 - 100 GeV band, in erg/s.

Luminosity_Pos_Err
The positive systematic uncertainty for the pulsar gamma-ray luminosity in the 0.1 - 100 GeV band, in erg/s.

Luminosity_Upper
The upper limit on the pulsar gamma-ray luminosity in the 0.1 - 100 GeV band, in erg/s.

Eff
The pulsar efficiency, defined as the ratio of the gamma-ray luminosity to the spin-down luminosity.

Eff_Stat_Err
The statistical error for the pulsar efficiency.

Eff_Neg_Err
The negative systematic uncertainty for the pulsar efficiency. Systematic uncertainties are derived from the distance uncertainty. Values are null when only an upper limit exists.

Eff_Pos_Err
The positive systematic uncertainty for the pulsar efficiency. Systematic uncertainties are derived from the distance uncertainty. Values are null when only an upper limit exists.

Eff_Upper
The upper limit for the pulsar efficiency. Entries are null when a value has been determined. Null values in any efficiency parameter indicate unreliable spectral fits.

Flux_1400_MHz
The 1400-MHz radio flux density, in milliJansky.

Flux_1400_MHz_Upper
The upper limit for the 1400-MHz radio flux density, in milliJansky.

Ref_Flux_1400_MHz
The reference bibcode for the 1400-MHz radio flux density.

N_Peaks
The number of peaks in the rotationally-phase-folded gamma-ray lightcurve, in the 0.1 - 100 GeV band.

Radio_Phase_Method
A code describing the method used to choose the radio fiducial phase. The codes are: p for the peak radio intensity, h for an opposite hemisphere shift (0.5 phase shift from the peak intensity), s for the point of symmetry in the radio profile, and o for some other method (used only for PSR J0534+2200).

Rg_Phase_Sep
The phase separation between the first gamma-ray peak and the radio peak.

Rg_Phase_Sep_Error
The uncertainty in phase separation between the gamma-ray and radio peaks.

G_Peak_Sep
The phase separation between the first and last gamma-ray peaks. This value is null for pulsars with only a single gamma-ray peak.

G_Peak_Sep_Error
The uncertainty in phase separation between the first and last gamma-ray peaks. This value is null for pulsars with only a single gamma-ray peak.

Peak1l_Hwhm
The half-width half-maximum of the leading (left) first peak edge, as fitted.

Peak1l_Hwhm_Error
The uncertainty in half-width half-maximum of the leading (left) first peak edge.

Peak1r_Hwhm
The half-width half-maximum of the trailing (right) first peak edge.

Peak1r_Hwhm_Error
The uncertainty of the half-width half-maximum of the trailing (right) first peak.

Peak2l_Hwhm
The half-width half-maximum of the leading (left) second peak edge, as fitted.

Peak2l_Hwhm_Error
The uncertainty of the half-width half-maximum of the leading (left) second peak edge.

Peak2r_Hwhm
The half-width half-maximum of the trailing (right) second peak edge, as fitted.

Peak2r_Hwhm_Error
The uncertainty of the half-width half-maximum of the trailing (right) second peak edge.

NH
The hydrogen column density to the source, in hydrogen atoms/cm2. The values are null when only an upper limit for the hydrogen column density exists.

NH_Neg_Err
The negative systematic uncertainty in hydrogen column density, in hydrogen atoms/cm2.

NH_Pos_Err
The positive systematic uncertainty in hydrogen column density, in hydrogen atoms/cm2.

NH_Upper
The upper limit on hydrogen column density, in hydrogen atoms cm-2. Entries are null when a value has been reported.

Xray_Flux
The non-thermal unabsorbed x-ray energy flux in the 0.3-10 keV energy band, in erg/s/cm2.

Xray_Flux_Neg_Err
The negative uncertainty of the X-ray flux (90% confidence level), in the 0.3-10 keV band, in in erg/s/cm2.

Xray_Flux_Pos_Err
The positive uncertainty of the X-ray flux (90% confidence level), in the 0.3-10 keV band, in in erg/s/cm2.

Xray_Flux_Upper
The upper limit on X-ray flux in the 0.3-10 keV band, in erg/s/cm2. Entries are null when a value has been reported.

Flux_Xbkg
The estimated non-thermal x-ray background flux from the brightest part of the associated plerion in the 0.3-10 keV energy band, in erg/s/cm2.

Flux_Xbkg_Neg_Err
The negative uncertainty (90% cl) in x-ray background flux, in the 0.3-10 keV energy band, in erg/s/cm2.

Flux_Xbkg_Pos_Err
The positive uncertainty (90% cl) in x-ray background flux, in the 0.3-10 keV energy band, in erg/s/cm2.

Xdetect_Flag
A flag which gives an assessment of the quality of X-ray detections: '0' indicates no confirmed counterpart, '1' indicates that a counterpart has been identified but with too few counts for further characterization, and '2' indicates that a counterpart has been identified with sufficient counts for spectral characterization.

Optical_Flux_Obj
A code to indicate the object to which the measured optical flux pertains. The codes are B for binary system; U for upper limit; P = neutron star detected; P* = pulsed optical detection; P+ = pulsar candidate (possible unpulsed pulsar detection); C = companion detected ; N = nebula (PWN) detected.

Mag_Filter
The filter used for the optical observation: B, I, J, K, R, U, V, or g.

App_Mag
The magnitude of the optical counterpart for the pulsar or pulsar system, where a counterpart is detected. This is null if no observation is available.

App_Mag_Lower
The lower limit of magnitude of the optical counterpart.

Extinction
The value of the optical extinction, in magnitudes, derived from the hydrogen column density using the relation of Fitzpatrick (1999). Entries are null when only an upper limit is known.

Extinction_Neg_Err
The negative uncertainty in optical extinction, in magnitudes.

Extinction_Pos_Err
The positive uncertainty in optical extinction, in magnitudes.

Extinction_Upper
The optical extinction upper limit in magnitudes, when no value has been reported. Entries are null when a value has been reported.

Optical_Flux
The corrected (unabsorbed) optical energy flux in the V-band, in erg/s/cm2. The optical flux has been corrected for interstellar reddening, and scaled to the V-band (peak wavelength 5500 Angstrom, bandwidth = 890 Angstrom) where necessary. Entries are null when only an upper limit has been reported.

Optical_Flux_Neg_Err
The negative uncertainty in the corrected (unabsorbed) optical energy flux in the V-band, in erg/s/cm2.

Optical_Flux_Pos_Err
The positive uncertainty in the corrected (unabsorbed) optical energy flux in the V-band, in erg/s/cm2.

Optical_Flux_Upper
The upper limit on the corrected (unabsorbed) optical energy flux in the V-band when no measurement has been reported, in erg/s/cm2. Entries are null when a value has been reported.

Pulsar_Class
A code which indicates the type of pulsar: YRL indicates that the pulsar is a young radio loud (YRL) pulsar; YRQ indicates that the pulsar is a young radio quiet (S1400 > 30 µJy) pulsar; MSP indicates that the pulsar is a millisecond pulsar.

Binary_Flag
A flag [Y/N] which indicates that the pulsar is in a binary system. A value of Y indicates that the pulsar is in a binary system.

Discovery_Band
A code which indicates in which band the pulsar was discovered: Radio Indicates that the pulsar was discovered in the radio band, X-ray indicates that the pulsar was discovered in the X-ray band, and Gamma indicates that the pulsar was discovered in gamma rays.

On_Peak_Flag
A flag [Y/N] that indicates that the spectral fit used only on-peak events. A value of Y indicates that the spectral fit used only on-peak events.

PLEC1_Pref
This give the best-fit prefactor p in the PLEC1 fit, in photons/cm2/s/MeV. PLEC1 is shorthand for the PLSuperExpCutoff model, with the parameter representing the sharpness of the cutoff (b) fixed to 1.

PLEC1_Pref_Error
The uncertainty in best-fit prefactor p in the PLEC1 fit, in photons/cm2/s/MeV.

PLEC1_Scaling_Energy
The scaling energy for the spectral fit using a PLEC1 model (where the exponential index is fixed at a value of 1), in MeV.

PLEC1_Cutoff
The best-fit cutoff energy for the PLEC1 fit, in MeV.

PLEC1_Cutoff_Error
Uncertainty in the best-fit cutoff energy for the PLEC1 fit, in MeV.

PLEC_Pref
The best-fit prefactor and associated error for the spectral fit using a PLSuperExpCutoff model (where the exponential index is left free), in photons/cm2/s/MeV.

PLEC_Pref_Error
Uncertainty in the best-fit prefactor and associated error for the spectral fit using a PLSuperExpCutoff model (PLEC, where the exponential index is left free), in photons/cm2/s/MeV.

PLEC_Photon_Index
The best-fit photon index for the PLEC model.

PLEC_Photon_Index_Error
The uncertainty in the best-fit photon index for the PLEC model.

PLEC_Energy_Scaling
The scaling energy for the spectral fit for the PLEC model, in MeV.

PLEC_Beta
The best-fit value for the spectral fit using the PLEC model.

PLEC_Beta_Error
Uncertainty in the best-fit value for the spectral fit using the PLEC model.

PLEC_Photon_Flux
The photon flux integrated from 100 MeV to 100 GeV for the PLEC model, in photons/s/cm2.

PLEC_Photon_Flux_Error
Uncertainty in the photon flux integrated from 100 MeV to 100 GeV for the PLEC model, in photons/s/cm2.

PLEC_Flux
The energy flux integrated from 100 MeV to 100 GeV for the spectral fit using the PLEC model, in erg/s/cm2.

PLEC_Flux_Error
Uncertainty in the energy flux integrated from 100 MeV to 100 GeV for the spectral fit using the PLEC model, in erg/s/cm2.

PLaw_Pref
Best-fit prefactor P using the PowerLaw model, in photons/cm2/s/MeV.

PLaw_Pref_Error
Uncertainty in the best-fit prefactor P using the PowerLaw model, in photons/cm2/s/MeV.

PLaw_Photon_Index
The best-fit photon index for the spectral fit using a PowerLaw model.

PLaw_Photon_Index_Error
Uncertainty in the best-fit photon index for the spectral fit using a PowerLaw model.

PLaw_Scaling_Energy
The scaling energy for the spectral fit using a PowerLaw model, in MeV.

PLaw_Photon_Flux
The photon flux integrated from 100 MeV to 100 GeV for the spectral fit using a PowerLaw model, in photons/cm2/s/MeV.

PLaw_Photon_Flux_Error
Uncertainty in the photon flux integrated from 100 MeV to 100 GeV for the spectral fit using a PowerLaw model, in photons/cm2/s/MeV.

PLaw_Flux
The energy flux integrated from 100 MeV to 100 GeV and associated error for the spectral fit using a PowerLaw model, in erg/s/cm2.

PLaw_Flux_Error
The uncertainty the energy flux integrated from 100 MeV to 100 GeV and associated error for the spectral fit using a PowerLaw model, in erg/s/cm2.

OP_Class
A flag that indicates off-peak emission class. Possible values: M for magnetospheric (pulsar-like), W for possible PWN emission, and U for Unidentified, and L is assigned to a source with no significant off-peak emission.

OP_Min_Phase
The minimum phase that defines the off-peak interval.

OP_Max_Phase
The maximum phase that defines the off-peak interval.

Op2_Min_Phase
For pulsars with two off-peak phase ranges, the minimum phase for the second off-peak interval.

Op2_Max_Phase
or pulsars with two off-peak phase ranges, the maximum phase for the second off-peak interval.

OP_TS_Point
The test statistic obtained at the best-fit position of the assumed point-like source. TS is computed at the best-fit position assuming a power-law spectral model (except for PSR J0534+2200).

OP_TS_Extend
The significance of any possible extension for the source.

OP_TS_Cutoff
The significance of any spectral cutoff for a source detected in the off-peak region, computed at the pulsar's position.

OP_TS_Var
The significance of variability in the off-pulse emission.

OP_Model
For regions with a significant detection, this is the best spectral model selected by the analysis procedure described in Section 7.2 of Abdo et al. 2013. The possible spectral models are PowerLaw, PLSuperExpCutoff, and FileFunction and are consistent with naming convention in the FERMI science analysis tool "gtlike".

OP_Photon_Flux
The best-fit photon flux integrated from 100 MeV to 316 GeV, in photons/cm2/s/MeV.

OP_Photon_Flux_Error
The statistical error in the best-fit photon flux integrated from 100 MeV to 316 GeV, in photons/cm2/s/MeV.

OP_Flux
The best-fit energy flux integrated from 100 MeV to 316 GeV, in erg/s/cm2.

OP_Flux_Error
The statistical error in the best-fit energy flux integrated from 100 MeV to 316 GeV, in erg/s/cm2.

OP_Pref
The best-fit prefactor for the PowerLaw and PLSuperExpCutoff spectral models, in photons/cm2/s/MeV. The prefactor is defined in Eq. 3 and Eq. 4 of Abdo et al. (2013) for the two spectral models.

OP_Pref_Error
The statistical error in the best-fit prefactor for the PowerLaw and PLSuperExpCutoff spectral models, in photons/cm2/s/MeV. The prefactor is defined in Eq. 3 and Eq. 4 of Abdo et al. (2013) for the two spectral models.

OP_Norm
The best-fit normalization for FileFunction spectral models. The normalization is defined in Eq. 5 of Abdo et al. (2013).

OP_Norm_Error
The statistical error in the best-fit normalization for FileFunction spectral models. The normalization is defined in Eq. 5 of Abdo et al. (2013).

OP_Scaling_Energy
The scaling energy for the PowerLaw and PLSuperExpCutoff spectral models, in MeV. The scale is defined in Eq. 3 and Eq. 4 of Abdo et al. (2013).

OP_Photon_Index
The best-fit photon index for the PowerLaw and PLSuperExpCutoff spectral models. The photon index is defined in Eq. 3 and Eq. 4 of Abdo et al. (2013) for the two spectral models.

OP_Photon_Index_Error
The statistical error in the best-fit photon index for the PowerLaw and PLSuperExpCutoff spectral models. The photon index is defined in Eq. 3 and Eq. 4 of Abdo et al. (2013) for the two spectral models.

OP_Cutoff
The best-fit cutoff energy for the PLSuperExpCutoff spectral model, in MeV, as defined in Eq. 4 of Abdo et al. (2013).

OP_Cutoff_Error
The statistical uncertainty in the best-fit cutoff energy for the PLSuperExpCutoff spectral model, in MeV, as defined in Eq. 4 of Abdo et al. (2013)

OP_Spatial_Model
For off-peak regions with a significant detection, the spatial model selected by the analysis procedure described in Section 7.2 of Abdo et al. (2013). The choices are "At Pulsar", "Point", and "Extended".

OP_RA
The Right Ascension, in degrees, of the off-peak source. For upper limits and sources with a best-fit spatial model at the pulsar position, this is the pulsar's position. For sources where the localized position is the selected spatial model, this is the best-fit position. For spatially-extended sources, this is the center of the best-fit extended source spatial model.

OP_Dec
The Declination, in degrees, of the off-peak source. For upper limits and sources with a best-fit spatial model at the pulsar position, this is the pulsar's position. For sources where the localized position is the selected spatial model, this is the best-fit position. For spatially-extended sources, this is the center of the best-fit extended source spatial model.

OP_Error_Radius
For sources with a "Point" spatial model, the statistical error on the source localization. For sources with an "Extended" spatial model, the statistical error on the center of the extended source. Values are given in degrees.

OP_Ext
For sources with an "Extended" spatial model, the best fit extension, in degrees.

OP_Ext_Error
For sources with an "Extended" spatial model, the statistical uncertainty in the best fit extension, in degrees.

OP_Plf_Upper
For regions with no significant detection, this is the 95% confidence-level photon flux upper limit computed assuming a PowerLaw spectral model with Index = 2 and integrated from 100 MeV to 316 GeV, in photons/s/cm2.

OP_Plef_Upper
For regions with no significant detection, this is the 95% confidence-level energy flux upper limit computed assuming a PowerLaw spectral model with Index = 2 and integrated from 100 MeV to 316 GeV, in erg/s/cm2.

OP_Pflp1_Upper
For regions with no significant detection, this is the 95% confidence-level photon flux upper limit computed assuming a PLEC1 spectral model integrated from 100 MeV to 316 GeV, in photons/s/cm2.

OP_Eflp1_Upper
For regions with no significant detection, this is the 95% confidence-level energy flux upper limit computed assuming a PLEC1 spectral model integrated from 100 MeV to 316 GeV, in erg/s/cm2.

Contact Person

Questions regarding the FERMIL2PSR database table can be addressed to the HEASARC Help Desk.
Page Author: Browse Software Development Team
Last Modified: Monday, 16-Sep-2024 17:27:27 EDT