TY - JOUR
T1 - The Variable Pulsar Wind Nebula of PSR J1809-1917
AU - Klingler, Noel
AU - Kargaltsev, Oleg
AU - Pavlov, George G.
AU - Posselt, Bettina
N1 - Funding Information:
We would like to thank Genavie Spence for her work on data analysis, and Samar Safi-Harb for insightful discussions. We would also like to thank the referee for helpful comments. Support for this work was provided by the National Aeronautics and Space Administration through Chandra Award Number GO3-14072, issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060. Facilities: CXO, HESS.
PY - 2018/12/1
Y1 - 2018/12/1
N2 - PSR J1809-1917 is a young (τ = 51 kyr) energetic ( erg s-1) radio pulsar powering a pulsar wind nebula (PWN). We report on the results of three Chandra X-ray Observatory observations that show that the PWN consists of a small (∼20″) bright compact nebula (CN) and faint extended emission seen up to 2′ from the pulsar. The CN is elongated in the northeast-southwest direction and exhibits morphological and flux variability on a timescale of a few months. We also find evidence of small arcsecond-scale jets extending from the pulsar along the same direction, and exhibiting a hard power-law (PL) spectrum with photon index Γjet = 1.2 ± 0.1. The more extended emission and CN share the same symmetry axis, which is also aligned with the direction toward the TeV γ-ray source HESS J1809-193, supporting their association. The spectrum of the extended nebula (EN) fits an absorbed PL with about the same slope as that of the CN, ΓCN ≈ ΓEN = 1.55 ± 0.09; no spectral changes across the EN's 2 pc extent are seen. The total PWN 0.5-8 keV luminosity is L PWN ≈ 9 1032 erg s-1, about half of which is due to the EN.
AB - PSR J1809-1917 is a young (τ = 51 kyr) energetic ( erg s-1) radio pulsar powering a pulsar wind nebula (PWN). We report on the results of three Chandra X-ray Observatory observations that show that the PWN consists of a small (∼20″) bright compact nebula (CN) and faint extended emission seen up to 2′ from the pulsar. The CN is elongated in the northeast-southwest direction and exhibits morphological and flux variability on a timescale of a few months. We also find evidence of small arcsecond-scale jets extending from the pulsar along the same direction, and exhibiting a hard power-law (PL) spectrum with photon index Γjet = 1.2 ± 0.1. The more extended emission and CN share the same symmetry axis, which is also aligned with the direction toward the TeV γ-ray source HESS J1809-193, supporting their association. The spectrum of the extended nebula (EN) fits an absorbed PL with about the same slope as that of the CN, ΓCN ≈ ΓEN = 1.55 ± 0.09; no spectral changes across the EN's 2 pc extent are seen. The total PWN 0.5-8 keV luminosity is L PWN ≈ 9 1032 erg s-1, about half of which is due to the EN.
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U2 - 10.3847/1538-4357/aae0f1
DO - 10.3847/1538-4357/aae0f1
M3 - Article
AN - SCOPUS:85057891065
VL - 868
JO - Astrophysical Journal
JF - Astrophysical Journal
SN - 0004-637X
IS - 2
M1 - 119
ER -