2014ApJ...796...14C


C.D.S. - SIMBAD4 rel 1.7 - 2021.05.15CEST22:01:56

2014ApJ...796...14C - Astrophys. J., 796, 14 (2014/November-3)

Diffuse γ-ray emission from galactic pulsars.

CALORE F., DI MAURO M. and DONATO F.

Abstract (from CDS):

Millisecond pulsars (MSPs) are old fast-spinning neutron stars that represent the second most abundant source population discovered by the Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope (Fermi). As guaranteed γ-ray emitters, they might contribute non-negligibly to the diffuse emission measured at high latitudes by Fermi-LAT (i.e., the Isotropic Diffuse γ-Ray Background (IDGRB)), which is believed to arise from the superposition of several components of galactic and extragalactic origin. Additionally, γ-ray sources also contribute to the anisotropy of the IDGRB measured on small scales by Fermi-LAT. In this manuscript we aim to assess the contribution of the unresolved counterpart of the detected MSPs population to the IDGRB and the maximal fraction of the measured anisotropy produced by this source class. To this end, we model the MSPs' spatial distribution in the Galaxy and the γ-ray emission parameters by considering observational constraints coming from the Australia Telescope National Facility pulsar catalog and the Second Fermi-LAT Catalog of γ-ray pulsars. By simulating a large number of MSP populations through a Monte Carlo simulation, we compute the average diffuse emission and the anisotropy 1σ upper limit. We find that the emission from unresolved MSPs at 2 GeV, where the peak of the spectrum is located, is at most 0.9% of the measured IDGRB above 10° in latitude. The 1σ upper limit on the angular power for unresolved MSP sources turns out to be about a factor of 60 smaller than Fermi-LAT measurements above 30°. Our results indicate that this galactic source class represents a negligible contributor to the high-latitude γ-ray sky and confirm that most of the intensity and geometrical properties of the measured diffuse emission are imputable to other extragalactic source classes (e.g., blazars, misaligned active galactic nuclei, or star-forming galaxies). Nevertheless, because MSPs are more concentrated toward the galactic center, we expect them to contribute significantly to the γ-ray diffuse emission at low latitudes. Because, along the galactic disk, the population of young pulsars overcomes in number that of MSPs, we compute the γ-ray emission from the whole population of unresolved pulsars, both young and millisecond, in two low-latitude regions: the inner Galaxy and the galactic center.

Abstract Copyright:

Journal keyword(s): gamma rays: diffuse background

Simbad objects: 60

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Number of rows : 60

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 PSR J0023+0923 Psr 00 23 16.890 +09 23 24.18           ~ 78 0
2 PSR J0030+0451 Psr 00 30 27.4277 +04 51 39.710           ~ 287 1
3 PSR J0034-05 Psr 00 34 21.8281 -05 34 36.620           ~ 163 0
4 PSR J0101-6422 Psr 01 01 11.1163 -64 22 30.171           ~ 41 0
5 PSR J0103+48 Psr 01 03 00.000 +48 00 00.00           ~ 28 0
6 PSR J0218+42 Psr 02 18 06.3604 +42 32 17.365           ~ 306 2
7 PSR J0340+41 Psr 03 40 23.2887 +41 30 45.300           ~ 54 0
8 PSR J0437-47 Psr 04 37 15.99744 -47 15 09.7170           DC 788 0
9 PSR J0514-4002A Psr 05 14 06.6927 -40 02 48.897           ~ 33 1
10 V* CM Tau Psr 05 34 31.93830 +22 00 52.1758           ~ 4889 1
11 PSR J0610-2100 Psr 06 10 13.5921 -21 00 28.016           ~ 65 0
12 PSR B0613-02.0 Psr 06 13 43.9759 -02 00 47.228           ~ 213 1
13 PSR J0614-3329 Psr 06 14 10.3479 -33 29 54.116           ~ 75 1
14 PSR J0751+1807 Psr 07 51 09.1539 +18 07 38.335           ~ 261 1
15 PSR J1017-7156 Psr 10 17 51.3283 -71 56 41.640           ~ 30 1
16 PSR J1023+0038 LXB 10 23 47.6840307966 +00 38 41.006983532     17.31     GV 330 0
17 PSR J1024-0719 Psr 10 24 38.697 -07 19 19.07           ~ 194 0
18 PSR J1124-36 Psr 11 24 00.000 -36 00 00.00           ~ 34 0
19 PSR J1125-58 Psr 11 25 44.3654 -58 25 16.896           ~ 34 1
20 PSR J1231-1411 Psr 12 31 11.3069 -14 11 43.628           ~ 93 0
21 PSR B1257+12 Psr 13 00 03.1075 +12 40 55.155           ~ 483 1
22 PSR J1327-0755 Psr 13 27 57.5880 -07 55 29.800           ~ 11 0
23 PSR J1342+2822B Psr 13 42 11.0871 +28 22 40.141           ~ 9 1
24 PSR J1446-4701 Psr 14 46 35.7143 -47 01 26.762           ~ 44 1
25 PSR J1455-3300 Psr 14 55 47.9624 -33 30 46.360           ~ 114 1
26 PSR J1514-4946 Psr 15 14 19.1142 -49 46 15.528           ~ 35 0
27 PSR J1544+4937 Psr 15 44 04.166 +49 37 57.45           ~ 43 1
28 PSR J1600-3053 Psr 16 00 51.90403 -30 53 49.3190           ~ 126 0
29 PSR J1614-2230 Psr 16 14 36.5070 -22 30 31.207           ~ 312 1
30 PSR B1620-26 Psr 16 23 38.2218 -26 31 53.769     21.30     ~ 275 2
31 PSR J1658-5324 Psr 16 58 43.000 -53 17 45.00           ~ 26 0
32 PSR J1709+2313 Psr 17 09 05.792 +23 13 27.85           ~ 28 1
33 PSR J1713+0447 Psr 17 13 49.53053 +07 47 37.5264           ~ 375 1
34 PSR J1740-5340 Psr 17 40 44.589 -53 40 40.90   17.43   16.25   ~ 134 2
35 PSR J1741+1351 Psr 17 41 28.0 +13 54 33           ~ 68 0
36 PSR J1744-1134 Psr 17 44 29.4172 -11 34 54.710           ~ 217 1
37 NAME Galactic Center gam 17 45 39.60213 -29 00 22.0000           ~ 12183 0
38 PSR J1747-4036 Psr 17 47 29.000 -40 36 00.00           ~ 47 0
39 PSR J1810+17 Psr 18 10 37.2803754941 +17 44 37.471906499           ~ 74 0
40 PSR J1820-30A Psr 18 23 40.4842 -30 21 39.920           ~ 131 1
41 PSR J1858-2216 Psr 18 58 04.42 -22 19 13.7           ~ 23 0
42 PSR J1902-5105 Psr 19 02 02.8476 -51 05 56.969           ~ 34 0
43 PSR J1909-3744 Psr 19 09 47.42820 -37 44 14.7740           ~ 215 2
44 PSR J1933-6210 Psr 19 33 32.4272 -62 11 46.881           ~ 23 0
45 PSR B1937+21 Psr 19 39 39.6 +21 37 22           ~ 983 2
46 PSR J1959+2048 Psr 19 59 36.7480 +20 48 14.599   20.4       ~ 719 2
47 PSR J2010-1323 Psr 20 10 45.9196 -13 23 56.027           ~ 53 0
48 PSR J2017+0603 Psr 20 17 22.7048 +06 03 05.585           ~ 80 1
49 PSR J2043+1711 Psr 20 43 20.8828 +17 11 28.941           ~ 83 1
50 PSR J2047+1053 Psr 20 47 00.000 +10 53 00.00           ~ 27 0
51 V* LY Aqr Psr 20 51 07.5145 -08 27 37.795           ~ 172 2
52 PSR J2124-3358 Psr 21 24 43.8464 -33 58 44.961           ~ 257 1
53 PSR J2129-5718 Psr 21 29 22.7618 -57 21 14.169           ~ 88 1
54 PSR B2127+11E Psr 21 29 58.187 +12 10 08.63           ~ 19 0
55 PSR J2214+3000 Psr 22 14 38.8480 +30 00 38.209           ~ 82 0
56 PSR J2215+51 Psr 22 15 32.6864199137 +51 35 36.406276103           ~ 98 0
57 PSR J2229+26 Psr 22 29 50.8864 +26 43 57.785           ~ 86 1
58 PSR J2236-5527 Psr 22 36 51.8510 -55 27 48.833           ~ 7 0
59 PSR J2241-5236 Psr 22 41 42.03161 -52 36 36.2492           ~ 79 1
60 PSR J2302+4442 Psr 23 02 46.9789 +44 42 22.102           ~ 80 0

    Equat.    Gal    SGal    Ecl

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2021.05.15-22:01:56

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