J/A+A/492/923 Pulsar Timing for Fermi Gamma-ray Space Telescope (Smith+, 2008)
Pulsar Timing for the Fermi Gamma-ray Space Telescope.
Smith D.A., Guillemot L., Camilo F., Cognard I., Dumora D., Espinoza C.,
Freire P.C.C., Gotthelf E.V., Harding A.K., Hobbs G.B., Johnston S.,
Kaspi V.M., Kramer M., Livingstone M.A., Lyne A.G., Manchester R.N.,
Marshall F.E., McLaughlin M.A., Noutsos A., Ransom S.M., Roberts M.S.E.,
Romani R.W., Stappers B.W., Theureau G., Thompson D.J., Thorsett S.E.,
Wang N., Weltevrede P.
<Astron. Astrophys. 492, 923 (2008)>
=2008A&A...492..923S 2008A&A...492..923S
ADC_Keywords: Pulsars ; Radio sources ; Gamma rays
Keywords: space vehicles: instruments - stars: pulsars: general -
gamma-rays: observations - ephemerides
Abstract:
We describe a comprehensive pulsar monitoring campaign for the Large
Area Telescope (LAT) on the Fermi Gamma-ray Space Telescope (formerly
GLAST). The detection and study of pulsars in gamma rays give insights
into the populations of neutron stars and supernova rates in the
Galaxy, into particle acceleration mechanisms in neutron star
magnetospheres, and into the "engines" driving pulsar wind nebulae.
LAT's unprecedented sensitivity between 20MeV and 300GeV together with
its 2.4sr field-of-view makes detection of many gamma-ray pulsars
likely, justifying the monitoring of over two hundred pulsars with
large spin-down powers. To search for gamma-ray pulsations from most
of these pulsars requires a set of phase-connected timing solutions
spanning a year or more to properly align the sparse photon arrival
times. We describe the choice of pulsars and the instruments involved
in the campaign.
Description:
Pulsars being timed for the Fermi Large Area Telescope (all known
pulsars with dE/dt>1034ergs/s), ordered by sqrt(dE/dt)/d2, where
dE/dt is the spin-down energy loss rate and d is the distance.
sqrt(dE/dt)/d2 as an indicator of expected gamma flux suffers many
large uncertainties (see text).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 139 230 FERMI pulsar candidates
table1.fit 19 2880 FITS version of table1
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See also:
J/ApJS/123/79 : Third EGRET catalog (3EG) (Hartman+, 1999)
http://www.atnf.csiro.au/research/pulsar/psrcat/ : ATNF Pulsar Catalogue
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- PSR PSR name
13- 23 A11 --- PSRJ PSRJ name
25- 34 F10.6 % gamma sqrt(Edot)/d2, indicator of γ-ray flux
expected, in percent of Vela pulsar
36- 42 E7.2 10-7W Edot Spin-down energy loss rate (erg/s)
44- 47 F4.1 kpc Dist Heliocentric distance
49- 55 F7.2 mJy S1.4 ?=- Radio flux intensity at 1400MHz
56 A1 --- r_S1.4 [bde] Reference for S1.4 (1)
58- 64 F7.2 mJy S0.4 ?=- Radio flux intensity at 400MHz
65 A1 --- r_S0.4 [ac] Reference for S0.4 (1)
67- 73 A7 --- Host Name of the globular cluster or the host
galaxy, if the pulsar is in one
75- 76 A2 --- O/X Optical/X-ray observation code (2)
78- 80 A3 --- --- [3EG]
82- 91 A10 --- 3EG Egret name (3)
93 A1 --- n_3EG [*] * when 3EG source has more than one
possible counterpart in the table
95- 98 F4.2 deg Edist ? EGRET angular distance
100-113 A14 --- TeV HESS or MILAGRO TeV association (4)
115-139 A25 --- Notes Notes (5)
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Note (1): The data in the first 8 columns were obtained from the ATNF
database except for the radio flux densities with the note as follows:
a = F. Camilo, private communication
b = Jacoby et al. 2003ApJ...599L..99J 2003ApJ...599L..99J
c = Kaspi et al. 1998ApJ...503L.161K 1998ApJ...503L.161K
d = Ray et al. 1996ApJ...470.1103R 1996ApJ...470.1103R
e = D'Amico et al. 2001ApJ...548L.171D 2001ApJ...548L.171D
f = Camilo et al. 2000ApJ...535..975C 2000ApJ...535..975C
Note (2): Optical/X-ray observation code as follows:
OX = source observed in optical and X-ray
X = source observed in X-rays
np = source observed in X-rays, but not pulsed
Note (3): If the pulsar is located less than 2° away from a 3rd EGRET
catalog source (Hartman et al., 1999, Cat. J/ApJS/123/79), the EGRET
name and the angular distance are listed.
Note (4): The TeV associations are taken from Wagner (2008), available at
http://www.mpi-hd.mpg.de/hfm/HESS/public/HESS_catalog.htm, and from
MILAGRO: (Abdo et al. 2007ApJ...664L..91A 2007ApJ...664L..91A).
Note (5): Nearby pulsar wind nebulae (PWN) are noted in the last column
(Kaspi et al., 2006csxs.book..279K 2006csxs.book..279K; Roberts, 2004,
http://www.physics.mcgill.ca/~pulsar/pwncat.html).
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Acknowledgements:
David A. Smith, smith(at)cenbg.in2p3.fr
Lucas Guillemot, guillemo(at)cenbg.in2p3.fr
(End) D.A. Smith, L. Guillemot [CENBG, France], P. Vannier [CDS] 06-Nov-2008