J/ApJS/208/17 2nd Fermi LAT cat. of gamma-ray pulsars (2PC) (Abdo+, 2013)
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 2013ApJS..208...17A
ADC_Keywords: Pulsars ; Gamma rays
Keywords: catalogs, pulsars: general, stars: neutron
Abstract:
This 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.
Description:
Fermi was launched on 2008 June 11, carrying two gamma-ray
instruments; among them the Large Area Telescope (LAT). The LAT is
sensitive to gamma rays with energies from 20MeV to over 300GeV,
with an on-axis effective area of ∼8000 cm2 above 1 GeV.
The data used here to search for gamma-ray pulsars span 2008 August 4
to 2011 August 4. Events were selected with reconstructed energies
from 0.1 to 100GeV and directions within 2° of each pulsar
position for pulsation searches (Section 3) and 15° for spectral
analyses (Section 6).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
psrcat.dat 757 117 LAT 2nd pulsar catalog: PULSAR_CATALOG
spec.dat 344 117 LAT second pulsar catalog: SPECTRAL table
offpk.dat 1316 117 LAT second pulsar catalog: OFF_PEAK table
refs.dat 177 100 LAT second pulsar catalog: REFERENCES
fits/* . 117 Individual FITS files for each pulsar
par/* . 123 Individual text files for rotation ephemeris in
a TEMPO2 (Hobbs et al. 2006ChJAS...6b.189H 2006ChJAS...6b.189H)
parameter for each pulsar
sed/* . 117 Individual SED images (in png format)
lc/* . 117 Individual light curve images (in png format)
--------------------------------------------------------------------------------
See also:
VII/189 : Catalog of Pulsars (Taylor+ 1995)
J/MNRAS/424/2832 : Pulsars in γ-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 page
Byte-by-byte Description of file: psrcat.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Pulsar name (JHHMM+DDMMA)
13- 20 F8.4 deg RAdeg Pulsar right ascension (J2000)
22- 29 F8.4 deg DEdeg Pulsar declination (J2000)
31- 36 F6.2 deg GLON Pulsar Galacitc longitude
38- 43 F6.2 deg GLAT Pulsar Galactic latitude
45- 50 F6.2 ms Per [1.5/445] Pulsar rotation period
52- 61 E10.3 s/s Pdot [3.8e-21/4.1e-12] Period first derivative (1)
63- 73 E11.3 10-7W Edot [4.6e+32/4.4e+38] Pulsar spin-down
luminosity in erg/s (1)
75- 84 E10.4 ph/cm2/s Fph [9.6e-10/1.1e-05]? Best-fit photon flux
integrated from 100MeV to 100GeV (2)
86- 94 E9.3 ph/cm2/s e_Fph [2.9e-10/5.3e-08]? Fph statistical error
96-105 E10.4 mW/m2 Ferg [1.9e-12/9.1e-09]? Best-fit energy flux
from 100MeV to 100GeV in erg/s/cm2 (2)
107-113 E7.3 mW/m2 e_Ferg [8.1e-13/2.7e-11]? Ferg statistical error
115-121 I7 --- TS-DC [0/1659005] Test statistic for PLEC1 model (3)
123-127 I5 --- TS-c [-5/43084] Spectral cutoff significance (4)
129-131 I3 --- TS-f [0/916] Test statistic improvement (5)
133-141 F9.3 --- pInd [0/2.04]? Best-fit photon index α for the
"PLSuperExpCutoff" spectral model (G1)
143-151 F9.3 --- e_pInd [0/1.4]? pInd statistical error
153-164 E12.4 MeV cOff [226/5889]? Best-fit cutoff energy Ec for the
"PLSuperExpCutoff" spectral model (G1)
166-177 E12.3 MeV e_cOff [19/3891]? cOff statistical error
179-186 F8.3 kpc Dist [0.1/16]? Pulsar distance
188-196 F9.3 kpc e_Dist [0.001/4.2]? Negative uncertainty on Dist
198-205 F8.3 kpc E_Dist [0.001/13.2]? Positive uncertainty on Dist
207-214 F8.3 kpc B_Dist [8.2/25.3]? Upper limit on pulsar distance (6)
216-218 A3 --- n_Dist Method used to determine the distance (7)
220-221 I2 --- r_Dist [0/97]?=0 Dist reference (see refs.dat file)
223-230 F8.2 mas/yr pm [0.8/169]? Proper motion for the pulsar
232-239 F8.2 mas/yr e_pm [0.01/170]? pm uncertainty
241-243 I3 --- r_pm [0/100]?=0 pm reference (see refs.dat file)
245-253 E9.4 s/s iPdot [4.4e-22/1.92e-13]? Intrinsic P-dot (8)
255-263 E9.3 s/s e_iPdot [2.2e-23/2.5e-17]? iPdot negative uncertainty
265-273 E9.3 s/s E_iPdot [2.6e-23/2.5e-17]? iPdot positive uncertainty
275-283 E9.3 10-7W iEdot [4.6e+32/4.4e+38]? Intrinsic spin down power
in erg/s
285-293 E9.3 10-7W e_iEdot [3.9e+28/1.8e+34]? iEdot negative uncertainty
295-304 E10.3 10-7W E_iEdot [3.9e+28/1.2e+34]? iEdot positive uncertainty
306-315 E10.4 10-7W Lum [4.8e+31/6.0e+36]? Pulsar luminosity (erg/s)
317-323 E7.3 10-7W s_Lum [3.2e+30/3.0e+35]? Lum statistical error
325-334 E10.3 10-7W e_Lum [6.2e+29/3.8e+36]? Negative systematic error on
Lum (9)
336-345 E10.3 10-7W E_Lum [6.2e+29/2.7e+36]? Lum positive sys. error (9)
347-356 E10.4 10-7W B_Lum [1.1e+35/2.8e+37]? Upper limit on Lum (10)
358-366 F9.4 % Eff [0.0009/11.8]? Pulsar efficiency
368-377 F10.4 % s_Eff [0/1.93]? Eff statistical error
379-388 F10.4 % e_Eff [0/5.73]? Negative systematic error on Eff
390-398 F9.4 % E_Eff [0/64.5]? Positive systematic error on Eff
400-409 F10.4 % B_Eff [0.6/303.6]? Upper limit on Eff (10)
411-418 F8.3 mJy S1400 [0.003/1100]? 1400MHz radio flux density (11)
420-428 F9.3 mJy B_S1400 [0.003/0.51]? Upper limit on S1400
430-432 I3 --- r_S1400 [0/100]?=0 S1400 reference (see refs.dat file)
434 I1 --- Npk [1/3] Number of peaks in the gamma-ray profile
436-437 A2 --- n_Rlag [phso -] Method used to choose the radio
fiducial phase (12)
439-447 F9.3 --- Rlag [0/0.997]? Phase separation (δ) between
the first gamma-ray peak and the radio peak
449-458 F10.4 --- e_Rlag [0/0.077]? Rlag uncertainty
460-468 F9.3 --- Pksep [0/0.808]? Phase separation (Δ) between
the first and last gamma-ray peaks (13)
470-478 F9.3 --- e_Pksep [0/0.192]? Pksep uncertainty
480-485 F6.4 --- HWP1L [0.0008/0.34] Half-width half-maximum of the
leading (left) first peak edge, as fitted (14)
487-492 F6.4 --- e_HWP1L [0.0001/0.08] HWP1L uncertainty
494-499 F6.4 --- HWP1R [0.0008/0.39] Half-width half-maximum of the
trailing (right) first peak edge (14)
501-506 F6.4 --- e_HWP1R [0/0.18]? HWP1R uncertainty
508-517 F10.4 --- HWP2L [0/0.28]? Half-width half-maximum of the
leading (left) 2nd peak edge, as fitted (14)
519-528 F10.4 --- e_HWP2L [0/0.19]? HWP2L uncertainty
530-539 F10.4 --- HWP2R [0/0.22]? Half-width half-maximum of the
trailing (right) 2nd peak edge, as fitted (14)
541-550 F10.4 --- e_HWP2R [0/0.15]? HWP2R uncertainty
552-559 E8.3 cm-2 NH [0/3.8e+22]? Hydrogen column density
561-568 E8.2 cm-2 e_NH [0/1.1e+22]? NH negative systematic error
570-577 E8.2 cm-2 E_NH [0/1.7e+22]? NH positive systematic error
579-587 E9.2 cm-2 B_NH [-9e+20,2e+22]? Upper limit on NH
589-596 E8.3 mW/m2 XFlux [0/4.43e-09]? Non-thermal unabsorbed X-ray
energy flux in the 0.3-10 keV energy band (15)
598-605 E8.2 mW/m2 e_XFlux [0/1.e-10]? XFlux negative uncertainty (90% CL)
607-614 E8.2 mW/m2 E_XFlux [0/1.e-10]? XFlux positive uncertainty (90% CL)
616-623 E8.2 mW/m2 B_XFlux [0/1.5e-10]? XFlux upper limit
625-632 E8.3 mW/m2 FXb [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 band
634-641 E8.2 mW/m2 e_FXb [0/1.e-10]? FXb negative uncertainty (90% CL)
643-650 E8.2 mW/m2 E_FXb [0/1.e-10]? FXb positive uncertainty (90% CL)
652-653 A2 --- qX [012* ] Quality of X-ray detection, 2=best (16)
655-656 A2 --- Obj Object to which the measured optical flux
pertains (17)
658 A1 --- n_mag The filter used for the optical observation
(B, I, J, K, R, U, V or g)
660-666 F7.2 --- mag [15.8/26.7]? Optical magnitude of the optical
counterpart for the pulsar or pulsar system
668-674 F7.2 --- b_mag [19.1/28.5]? Lower limit of mag
676-682 F7.2 --- Ext [0/15]? Optical extinction (18)
684-691 F8.2 --- e_Ext [0/2.5]? Negative uncertainty on Ext
693-700 F8.2 --- E_Ext [0/2.9]? Positive uncertainty on Ext
702-709 F8.2 --- B_Ext [0.01/4.5]? Upper limit of Ext
711-718 E8.3 --- FVc [0/4.6e-12]? Corrected (unabsorbed) optical
energy flux in the V-band (19)
720-727 E8.2 --- e_FVc [0/4.7e-14]? Negative uncertainty on FVc
729-736 E8.2 --- E_FVc [0/4.7e-14]? Positive uncertainty on FVc
738-745 E8.2 --- B_FVc [0/1.1e-11]? Upper limit of FVc
747-749 A3 --- Type [YRL YRQ MSP] Pulsar class (20)
751 A1 --- Bin [NY] Y: the pulsar is in a binary system
753-757 A5 --- Hist Pulsar discovery in "Radio", "X-rays", or
"Gamma"
--------------------------------------------------------------------------------
Note (1): dE/dt uncorrected for Shklovskii effect or Galactic acceleration;
see Section 4.3.
Note (2): Blank values indicate unreliable spectral fits.
Note (3): The test statistic obtained at the position of the pulsar,
assuming a PLEC1 model ("PLSuperExpCutoff" spectral model with the
exponential index fixed to 1, see the note (G1) below). The fit uses
data from 100MeV to 100GeV, and includes all pulse phases except as
noted in Tables 9 and 10.
Note (4): The significance of the spectral cutoff, obtained from the
improvement in log(Likelihood) from the "PLSuperExpCutoff" spectral
model fit over the "PowerLaw" spectral fit (see note (G1) below).
Note (5): The improvement in the test statistic when the exponential index
is left free in the "PLSuperExpCutoff" spectral fit (PLEC compared to
PLEC1, see note (G1) below). If there is no improvement, or the fit is
worse, this value is zero.
Note (6): Upper limit on pulsar distance when no measured value has been
determined; blank values indicate that a distance measurement has been
determined.
Note (7): The method used to determine the pulsar's distance.
Methods are as follows:
K = kinematic model,
DM = dispersion measure using the NE2001 model of Cordes & Lazio
(2002astro.ph..7156C 2002astro.ph..7156C),
O = optical measurements,
X = X-ray measurements.
DMM = 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.
P = Parallax.
Note (8): The intrinsic P-dot and associated errors, after contributions
from the Shklovskii effect and Galactic acceleration have been
removed, see Section 4.3.
Note (9): Systematic errors are derived from the distance uncertainty.
Note (10): Upper limit on the luminosity/pulsar efficiency when no value
has been determined. Entries are blank when a value has been
determined. Blank values in all Luminosity/Efficiency columns indicate
unreliable spectral fits.
Note (11): Radio flux density at 1400MHz. In some cases, documented in
Section 4.1, this value is extrapolated from measurements at other
frequencies. Entries are blank when only an upper limit has been reported.
Note (12): Method are as follows:
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,
o = for some other method as described in the text (used only
for PSR J0534+2200).
Note (13): This value is blank for pulsars with only a single gamma-ray peak.
Note (14): The best-fit light curve is in the BESTFITLC extension in the
individual FITS file for each pulsar.
Note (15): Non-thermal unabsorbed X-ray energy flux in erg/s/cm2 and 90%
CL statistical errors, in the 0.3-10 keV energy band. Spectrum is an
absorbed power law, plus black body model when needed. Exceptions are
PSRs J0633+1746 and J0659+1414 where a double black body plus power
law model was used. Entries are blank when only an upper limit has
been reported.
Note (16): Quality of X-ray detections as follows:
0 = no confirmed counterpart (or a purely thermal emission without a
non-thermal spectral component).
1 = a counterpart has been identified but with too few counts for further
characterization.
1* = Object found by Suzaku which indicates that there is a non-negligible
possibility of a chance coincidence.
2 = a counterpart has been identified with sufficient counts for spectral
characterization.
2* = An ad hoc analysis was performed for some pulsars for which the standard
analysis could not be applied (e.g., owing to the very intense thermal
component of the spectrum of Vela or to an active galaxy near
PSR J1418-6058).
Note (17): The codes are as follows:
B = binary system;
U = upper limit;
P = neutron star detected;
P* = pulsed optical detection;
P+ = pulsar candidate (possible unpulsed pulsar detection);
C = companion detected;
N = nebula (PWN) detected.
Note (18): Optical extinction and associated errors derived from the
hydrogen column density and using the relation of Fitzpatrick
(1999PASP..111...63F 1999PASP..111...63F). Entries are blank when only an upper limit is
reported.
Note (19): Corrected (unabsorbed) optical energy flux in the V-band in
erg/s/cm2, and associated errors. The optical flux has been
corrected for interstellar reddening, and scaled to the V-band (peak
wavelength λ=5500Å, bandwidth Δλ=890Å) where
necessary. Entries are blank when only an upper limit has been reported.
Note (20): The pulsar iqs characterized as:
YRL = young radio loud,
YRQ = young radio quiet (S1400>30uJy),
MSP = millisecond pulsar.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: spec.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Pulsar name (JHHMM+DDMMA)
13 A1 --- On [NY] Y: spectral fit used only on-peak events
15- 21 I7 --- TS-DC ? Test statistic in PLEC1 model (G1)
23- 27 I5 --- TS-c ? Spectral cutoff significance (G1)
30- 32 I3 --- TS-f ? Test statistic of improvement of PLEC
over PLEC1 (free β) (G1)
34- 42 E9.4 cm-2/s/MeV Pref1 [2.8e-13/8.4e-09]? Best-fit prefactor p in
the PLEC1 fit in ph/cm2/s/MeV (G1)
44- 52 E9.3 cm-2/s/MeV e_Pref1 [3.1e-13/6.5e-11]? Pref1 uncertainty
54- 62 F9.3 --- pInd1 [0/2.038]? Best-fit photon index α
in the PLEC1 fit (G1)
64- 72 F9.3 --- e_pInd1 [0/1.353]? pInd1 uncertainty
74- 79 F6.1 MeV Sc1 [401/6601]? Scaling energy Eo
in PLEC1 fit (G1)
81- 86 F6.1 MeV Ec1 [226/5889]? Best-fit cutoff energy Ec
in PLEC1 fit (G1)
88- 93 F6.1 MeV e_Ec1 [19/3891]? Ec1 uncertainty
95-103 E9.4 ph/cm2/s Fph [9.6e-10/1.1e-05]? The photon flux integrated
from 100MeV to 100GeV in PLEC1 fit (G1)
105-113 E9.3 ph/cm2/s e_Fph [2.9e-10/5.3e-08]? Fph uncertainty
115-123 E9.4 mW/m2 Ferg [1.9e-12/9.1e-09]? The energy flux integrated
from 100MeV to 100GeV in PLEC1 fit (G1)
125-133 E9.3 mW/m2 e_Ferg [8.1e-13/2.7e-11]? Ferg uncertainty
135-143 E9.4 cm-2/s Preff [1.6e-10/1.9e-08]? The best-fit prefactor p
in the PLEC fit in ph/cm2/s (G1)
145-153 E9.3 cm-2/s e_Preff [1.4e-11/1.3e-10]? Preff uncertainty
155-163 F9.3 --- pIndf [0.362/1.554]? Photon index α
in the PLEC fit (G1)
165-173 F9.3 --- e_pIndf [0.002/0.215]? pIndf uncertainty
175-180 F6.1 MeV Scf [400/2200]? Best-fit caling energy Eo
in the PLEC fit (G1)
182-189 F8.3 MeV Ecf [100/1006]? Cutoff energy Ec in PLEC fit (G1)
191-199 F9.3 MeV e_Ecf [0/204]? Ecf uncertainty
201-209 F9.3 --- eIndf [0.384/0.747]? best-fit exponential β
in the PLEC fit (G1)
211-219 F9.3 --- e_eIndf [0.001/0.048]? eIndf uncertainty
221-229 E9.4 ph/cm2/s Fphf [6.e-08/1.1e-05]? The photon flux integrated
from 100MeV to 100GeV in PLEC fit (G1)
231-239 E9.3 ph/cm2/s e_Fphf [2.7e-09/2.7e-08]? Fphf uncertainty
241-249 E9.4 mW/m2 Fergf [5.5e-11/9.2e-09]? The energy flux integrated
from 100MeV to 100GeV in PLEC fit (G1)
251-259 E9.3 mW/m2 e_Fergf [2.8e-12/3.2e-11]? Fergf uncertainty
261-269 E9.4 cm-2/s/MeV Pref0 [4e-15/2.1e-09]? The best-fit prefactor p in
a "PowerLaw" model in ph/cm2/s/MeV (G1)
271-279 E9.3 cm-2/s/MeV e_Pref0 [5.7e-14/1.3e-11]? Pref0 uncertainty
281-289 F9.3 --- pInd0 [1/3]? Best-fit photon index α
in a "PowerLaw" model (G1)
291-299 F9.3 --- e_pInd0 [0.001/6.9]? pInd0 uncertainty
301-304 I4 MeV Sc0 [586/3805]? Scaling energy Eo using for the
spectral fit using a "PowerLaw" model (G1)
306-314 E9.4 ph/cm2/s Fph0 [1e-11/1.2e-05]? The photon flux integrated
from 100MeV to 100GeV in PL fit (G1)
316-324 E9.3 ph/cm2/s e_Fph0 [1.5e-10/7.6e-08]? Fph0 uncertainty
326-334 E9.4 mW/m2 Ferg0 [1.9e-13/1.7e-08] The energy flux integrated
from 100MeV to 100GeV in PL fit (G1)
336-344 E9.3 mW/m2 e_Ferg0 [5.6e-13/4.4e-11] Ferg0 uncertainty
--------------------------------------------------------------------------------
Byte-by-byte Description of file: offpk.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Pulsar name (JHHMM+DDMMA)
13 A1 --- oCl [LMUW ] Off-peak emission class (21)
15- 20 F6.4 --- mPhi ? Minimum phase of the off-peak interval
22- 27 F6.4 --- MPhi ? Maximum phase of the off-peak interval
29- 34 F6.4 --- mPhi2 ? Minimum phase of the 2nd off-peak interval
36- 41 F6.4 --- MPhi2 ? Maximum phase of the 2nd off-peak interval
43- 49 F7.1 --- TS-PS ? Test statistic obtained at the best-fit
position of assumed point-like source (22)
51- 55 F5.1 --- TS-ex [0/283]? Significance of any possible
extension for the source
57- 61 F5.1 --- TS-co [0/365]? Significance of any spectral
cutoff (23)
63- 67 F5.1 --- TS-v [0/373]? Significance of variability in the
off-pulse emission
69- 84 A16 --- Modo Best off-peak spectral model (24)
86- 93 E8.3 ph/cm2/s Fpho [0/1.1e-06]? Best-fit integrated photon flux
(100MeV-316GeV) in spectral model
95- 102 E8.3 ph/cm2/s e_Fpho [0/4.4e-08]? Fph1 statistical error
104- 111 E8.3 mW/m2 Fergo [0/6.8e-10]? Best-fit integrated energy flu
(100MeV-316GeV) in spectral model
113- 120 E8.3 mW/m2 e_Fergo [0/2.9e-11]? Fergo statistical error
122- 129 E8.3 --- Prefo [0/6.7e-10]? Best-fit prefactor p (G1)
131- 138 E8.3 --- e_Prefo [0/4.2e-10]? Prefo statistical error
140- 145 F6.4 --- Norm [0/1.1]? Best-fit "file" normalization (25)
147- 152 F6.4 --- e_Norm [0/0.05]? Norm statistical error
154- 159 F6.1 MeV Sco [0/5624]? Scaling energy Eo in model (G1)
161- 164 F4.2 --- pIndo [0/2.72]? Best-fit photon index α (G1)
166- 169 F4.2 --- e_pIndo [0/0.94]? pIndo statistical error
171- 176 F6.1 MeV Eco [0/2553]? Best-fit cutoff energy (G1)
178- 183 F6.1 MeV e_Eco [0/2484]? Eco statistical uncertainty
185- 193 A9 --- Mod2 Spatial model (26)
195- 202 F8.4 deg RAdeg ? Right ascension of the source (J2000) (27)
204- 211 F8.4 deg DEdeg ? Declination of the source (J2000) (27)
213- 218 F6.2 deg GLON ? Galactic longitude of the source
220- 225 F6.2 deg GLAT ? Galactic latitude of the source
227- 232 F6.4 deg ePos [0/0.09]? Estimated statistical error on
the localization of the source (28)
234- 237 F4.2 deg Ext [0/0.87]? Best-fit extension (in case of
"Extended" model)
239- 244 F6.4 deg e_Ext [0/0.06]? Ext statistical error
246- 253 E8.3 ph/cm2/s pFup0 [0/8.3e-08]? 95% confidence-level photon
flux upper limit in power-law model (29)
255- 262 E8.3 mW/m2 eFup0 [0/5.8e-11]? 95% confidence level energy
flux upper limit in power-law model (29)
264- 271 E8.3 ph/cm2/s pFup1 [0/100]? 95% confidence photon flux upper
limit with PLEC1 model (30)
273- 280 E8.3 mW/m2 eFup1 [0/178]? 95% confidence energy flux upper
limit with PLEC1 model (30)
281- 406 14F9.1 MeV sedle ?=- SEDLowerEnergy vector (31)
407- 532 14F9.1 MeV sedue ?=- SEDUpperEnergy vector (31)
533- 658 14F9.1 MeV sedme ?=- SEDMiddleEnergy vector (31)
659- 756 14F7.1 --- sedTS ?=- The test statistic for each SED point
757- 896 14E10.3 --- sedp ?=- Best-fit SED prefactor (32)
897-1036 14E10.3 --- sedpn ?=- sedpre negative uncertainty (32)
1037-1176 14E10.3 --- sedpp ?=- sedpre positive uncertainty (32)
1177-1316 14E10.3 --- sedpu ?=- 95% confidence-level upper limit (32)
--------------------------------------------------------------------------------
Note (21): Off-peak emission class as follows:
M = magnetospheric ("pulsar-like"),
W = possible PWN emission,
U = Unidentified.
L = source with no significant off-peak emission
Note (22): TS is computed at the best-fit position assuming a power-law
spectral model (except for PSR J0534+2200 as described in Section 7.2).
Note (23): The significance of any spectral cutoff for a source detected in
the off-peak region (computed at the pulsar's position).
Note (24): For regions with a significant detection, this is the best spectral
model selected by our analysis procedure described in Section 7.2. The
possible spectral models are "PowerLaw" (PL), "PLSuperExpCutoff" (PLEC1),
and "FileFunction" and are consistent with naming convention in "gtlike"
analysis in the "pyLikelihood" python module of the Fermi Science Tools.
See Note (G1) below for the definition of the models.
Note (25): The best-fit normalization and estimated statistical error for
"FileFunction" spectral models (relative of Crab or Vela), defined in
Equation (B5): dN/dE=f(dN/dE)file. This spectral model was only
used for the Crab Nebula and Vela-X.
Note (26): For off-peak regions with a significant detection, the spatial
model selected by our analysis procedure described in Section 7.2. The
choices are "At_Pulsar", "Point", and "Extended".
Note (27): The position of the source in celestial coordinates. 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.
Note (28): For sources with a "Point" spatial model, the estimated
statistical error on the localization of the source. For sources with
an "Extended" spatial model, the estimated statistical error on the
center of the extended source.
Note (29): For regions with no significant detection, this is the 95%
confidence-level photon flux/energy flux upper limit computed assuming
a "PowerLaw" spectral model with Index=2 and integrated from 100MeV to
316GeV.
Note (30): For regions with no significant detection, the 95% confidence
level photon flux/energy flux upper limit assuming a
"PLSuperExpCutoff" (PLEC1) spectral model with a canonical pulsar
spectrum of index α=1.7 and energy cutoff Ec=3. This is the flux
upper limit integrated from 100MeV to 316GeV.
Note (31): For each region, we computed a spectral energy distribution
(SED) for the source in 14 energy bins spaced uniformly from 100MeV to
316GeV (4 bins per energy decade). Therefore, each sed* column
corresponds to a vector of 14 values, one for each energy bin.
SEDLowerEnergy, SEDUpperEnergy, and SEDMiddleEnergy are the
lower energy, upper energy, and energy in the geometric mean of the
energy bin for each SED point.
Note (32): The best-fit prefactor, asymmetric lower and upper error, and
95% confidence-level upper limit computed for the source in each
energy bin. When TS≥25, a detection is quoted when sedTS>4 and an
upper limit is quoted otherwise. When TS<25, all SED points are quoted
as upper limits.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: refs.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 3 I3 --- Ref [1/100] Reference code number
5- 24 A20 --- Aut Author's name(s)
26- 44 A19 --- BibCode Bibcode
46-177 A132 --- Title Title of the reference
--------------------------------------------------------------------------------
Global Notes:
Note (G1): the models described in Appendix B are named "PowerLaw" (PL),
"PLSuperExpCutoff" (PLEC), can be written as:
* PL model: dN/dE = p(E/Eo)-α
* PLEC model: dN/dE = p(E/Eo)-α exp[-(E/Ec)β]
* PLEC1 model: is PLEC model with β=1
The parameters are:
p = "Prefactor" (in ph/cm2/s/MeV)
Eo = "Scale", scale energy (in MeV)
Ec = "Cutoff", cut-off energy (in MeV)
α = "Photon_Index", photon index
β = "Exponential_Index", exponential index (=1 in the PLEC1 model)
History:
From http://fermi.gsfc.nasa.gov/ssc/data/access/lat/2nd_PSR_catalog/:
2PCauxiliaryfiles_v04.tgz (29 July 2013)
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 24-Oct-2013