Vol. 31 No. 2 (2021)
Papers

Morpho-kinematics of the Molecular Gas in a Quasar Host Galaxy at Redshift Z=0.654

Thai Thi Tran
Vietnam National Space Center
Bio
Tuan-Anh Pham
Vietnam National Space Center
Hoai Thi Do
Vietnam National Space Center
Nhung Tuyet Pham
Vietnam National Space Center
Diep Ngoc Pham
Vietnam National Space Center
Ngoc Bich Nguyen
Vietnam National Space Center
Phuong Thi Nguyen
Vietnam National Space Center

Published 10-05-2021

Keywords

  • galaxies,
  • evolution – galaxies,
  • ISM – radio lines,
  • galaxies.

How to Cite

Tran, T. T., Pham, T.-A., Darriulat, P., Do, H. T., Pham, N. T., Pham, D. N., Nguyen, N. B., & Nguyen, P. T. (2021). Morpho-kinematics of the Molecular Gas in a Quasar Host Galaxy at Redshift Z=0.654. Communications in Physics, 31(2), 149. https://doi.org/10.15625/0868-3166/15599

Abstract

e present a new study of archival ALMA observations of the CO(2-1) line emission of
the host galaxy of quasar RX J1131. The quasar, at redshift z S ∼0.654, is lensed by a foreground galaxy at z L ∼0.30. Particular attention is paid to the mechanism of gravitational lensing. A simple lens model, shown to well reproduce the optical images obtained by the Hubble Space Telescope, is applied to the ALMA CO(2-1) images, providing a tool to understand the uncertainties attached to the evaluation of the source brightness and kinematics. Uncertainties attached to the process of data reduction are carefully evaluated. Evidence for the robustness of previously published results is obtained. A system of polar coordinates is introduced to better match the specificity of
the imaging process. It provides particularly clear evidence for rotation of the gas contained in the galaxy. A simple rotating disc model is shown to give an excellent overall description of the morpho-kinematics of the source. It gives evidence for a hot spot of emission located near the quasar, overlapping the caustic and corresponding to an enhancement of emission by a factor ∼2.5. The possible presence of a companion galaxy suggested by some previous authors is not confirmed. The rotation curve is studied with reference to the predictions of the disc model. De-tailed comparison between model and observations gives evidence for a more complex dynamics than implied by the model. Doppler velocity dispersion within the beam size in the image plane is found to contribute 60±10 km s −1 to the line width. It accounts for the observed line width when a
2- σ cut is applied to the data. However, when using a less severe cut, a significant amount of turbulence may be accommodated, preventing a reliable evaluation of the contribution of turbulence to the line width.

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