2020A&A...640A..76P


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.24CEST09:34:17

2020A&A...640A..76P - Astronomy and Astrophysics, volume 640A, 76-76 (2020/8-1)

Energy dependent morphology of the pulsar wind nebula HESS J1825-137 with Fermi-LAT.

PRINCIPE G., MITCHELL A.M.W., CAROFF S., HINTON J.A., PARSONS R.D. and FUNK S.

Abstract (from CDS):


Aims. Taking advantage of more than 11 years of Fermi-LAT data, we perform a new and deep analysis of the pulsar wind nebula (PWN) HESS J1825-137. Combining this analysis with recent H.E.S.S. results we investigate and constrain the particle transport mechanisms at work inside the source as well as the system evolution.
Methods. The PWN is studied using 11.6 years of Fermi-LAT data between 1GeV and 1TeV. In particular, we present the results of the spectral analysis and the first energy-resolved morphological study of the PWN HESS J1825-137 at GeV energies, which provide new insights into the γ-ray characteristics of the nebula.
Results. An optimised analysis of the source returns an extended emission region larger than 2°, corresponding to an intrinsic size of about 150 pc, making HESS J1825-137 the most extended γ-ray PWN currently known. The nebula presents a strong energy dependent morphology within the GeV range, moving from a radius of ∼1.4° below 10GeV to a radius of ∼0.8° above 100GeV, with a shift in the centroid location.
Conclusions. Thanks to the large extension and peculiar energy-dependent morphology, it is possible to constrain the particle transport mechanisms inside the PWN HESS J1825-137. Using the variation of the source extension and position, as well as the constraints on the particle transport mechanisms, we present a scheme for the possible evolution of the system. Finally, we provide an estimate of the electron energy density and we discuss its nature in the PWN and TeV halo-like scenario.

Abstract Copyright: © ESO 2020

Journal keyword(s): astroparticle physics - pulsars: individual: HESS J1825-137 - pulsars: individual: PSR B1823-13 - gamma rays: stars - acceleration of particles

Simbad objects: 21

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Number of rows : 21

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 GRB 180720B gB 00 02 06.86 -02 55 08.1           ~ 47 0
2 SNR G119.5+10.2 SNR 00 06.6 +72 47           ~ 237 1
3 NGC 253 SyG 00 47 33.134 -25 17 19.68   8.03   6.94 8.1 ~ 2956 2
4 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3582 3
5 GRB 190114C gB 03 38 01.18 -26 56 47.8           ~ 98 0
6 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5652 4
7 NAME Geminga Psr 06 33 54.153 +17 46 12.91           ~ 1096 0
8 NAME Vela Pulsar Psr 08 35 20.65525 -45 10 35.1545           ~ 2074 1
9 Mrk 421 BLL 11 04 27.3139210166 +38 12 31.798324828   13.50 12.90 8.31   ~ 2405 1
10 3C 264.0 QSO 11 45 05.0090520 +19 36 22.741257   14.98 13.97     ~ 540 2
11 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6283 3
12 CPD-63 2495 HXB 13 02 47.6541729595 -63 50 08.625922862 10.34 10.72 9.98 10.03   O9.5Ve 681 1
13 NAME Centaurus A Sy2 13 25 27.61509104 -43 01 08.8056025   8.18 6.84 6.66   ~ 4030 3
14 QSO J1512-0906 QSO 15 12 50.53292491 -09 05 59.8295878   16.74 16.54     ~ 1164 1
15 4C 39.49 BLL 16 53 52.21668494 +39 45 36.6089458 14.09 14.15 13.29 8.26   ~ 1934 2
16 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11760 0
17 PSR J1826-1256 Psr 18 26 08.570 -12 56 33.53           ~ 100 1
18 PSR B1823-13 Psr 18 26 13.06 -13 34 48.1           ~ 355 1
19 V* V479 Sct HXB 18 26 15.0561532140 -14 50 54.249464136 12.02 12.23 11.27 11.04   ON6V((f))z 497 2
20 QSO B2155-304 BLL 21 58 52.0651817803 -30 13 32.120657891   13.36 13.09 12.62   ~ 1576 1
21 NAME Cas A SNR 23 23 24.000 +58 48 54.00           ~ 2440 1

    Equat.    Gal    SGal    Ecl

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2020.10.24-09:34:18

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