Revisiting LS I +61◦303 with VLBI astrometry

Wu, Y. W.; Torricelli-Ciamponi, G.; Massi, M.; Reid, M. J.; Zhang, B.; Shao, L.; Zheng, X. W.

doi:10.1093/mnras/stx3003

アイテム詳細

登録内容を編集ファイル形式で保存

一時保存へ追加

タグ情報を表示リリース履歴を表示詳細要約

公開

学術論文

Revisiting LS I +61◦303 with VLBI astrometry

MPS-Authors

/persons/resource/persons192121

Shao, L.
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

External Resource

There are no locators available

Fulltext (restricted access)

There are currently no full texts shared for your IP range.

フルテキスト (公開)

1711.07598.pdf
(プレプリント), 741KB

付随資料 (公開)

There is no public supplementary material available

引用

Wu, Y. W., Torricelli-Ciamponi, G., Massi, M., Reid, M. J., Zhang, B., Shao, L., & Zheng, X. W. (2018). Revisiting LS I +61◦303 with VLBI astrometry. Monthly Notices of the Royal Astronomical Society: Letters, 474, 4245-4253. doi:10.1093/mnras/stx3003.

引用: https://hdl.handle.net/21.11116/0000-0000-ADF1-D

要旨

We conducted multi-epoch VLBA phase reference observations of LS I +61 303 in
order to study its precessing radio jet. Compared to similar observations in
2006, we find that the observed elliptical trajectory of emission at 8.4 GHz
repeats after the 9-year gap. The accurate alignment of the emission patterns
yields a precession period of 26.926 +- 0.005 d, which is consistent with that
determined by Lomb-Scargle analysis of the radio light curve. We analytically
model the projection on the sky plane of the peak position of a precessing,
synchrotron-emitting jet, which traces an elliptical trajectory on the sky.
Comparing the simulation with the VLBA astrometry we improve our knowledge of
the geometry of the system.We measure the LS I +61 303 absolute proper motion
to be -0.150 +- 0.006 mas/yr eastward and -0.264 +- 0.006 mas/yr northward.
Removing Galactic rotation, this reveals a small, < 20 km/s, non-circular
motion, which indicates a very low kick velocity when the black hole was
formed.