D. T. Hoai

Morphology and kinematics of the gas envelope of protostar L1527 as obtained from ALMA observations of the C18O(2–1) line emission

Using ALMA observations of the C

Space reconstruction of the morphology and kinematics of axisymmetric radio sources

^{18}

Morphology and kinematics of the gas envelope of Mira Ceti

O(2-1) line emission of the gas envelope of protostar L1527, we have reconstructed its morphology and kinematics under the assumption of axisymmetry about the west-east axis. The main original contribution to our understanding of the formation process of L1527 is the presentation of a simple 3D parameterisation based solely on regions that are not dominated by absorption. In the explored range (

De-projection of radio observations of axisymmetric expanding circumstellar envelopes

sim

High-resolution ALMA observation of the 12CO(3–2) and 350 GHz continuum emissions of the debris disc of 49 Ceti

0.7 to 5 arcsec from the star) the model reproduces observations better than earlier attempts. The main results include: a measurement of the rotation velocity that confirms its evolution to Keplerian toward short distances; a measurement of the mean in-fall velocity, 0.43

On the dust and gas components of the

pm

z

0.10 kms

= 2.8 gravitationally lensed quasar host RX J0911.4+0551

^{-1}

Profile of the \(^{12}\)CO(3-2) Emission Line Detected From the Debris Disc of 49 Ceti

, lower than free fall velocity, with no evidence for the significant

Modelling the millimetre/submillimeter emission of the gas envelope of evolved axially symmetric stars

r