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Colloquia Series

For more information on colloquia at the Centre for Astrophysics and Supercomputing please contact Dr. Simon Stevenson and Dr. Stefan Osłowski ()

Swinburne Virtual Reality Theatre
AR Building, Room 104
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2020 Colloquia


Thursday Mar 12, 10:30
Camila Correa (UvA)
Colloquium: TBA
TBA
Tuesday Mar 10, 10:30
Bron Reichardt-Chu ()
Student Review: Reichardt-Chu CoC
Thursday Mar 5, 10:30
Rychard Bouwens (Leiden)
Colloquium: TBA
TBA
Tuesday Mar 3, 10:30
Sara Webb ()
Student Review: Sara Webb MCR
Sara's mid-candidature review
Thursday Feb 27, 10:30
Daniel Ceverino (Universidad Autonoma de Madrid )
Colloquium: TBD
TBA
Tuesday Feb 25, 10:30
Gurvarinder (CAS)
Student Review: Gurvarinder CoC
Thursday Feb 20, 10:30
Prof Sukyoung Yi (Yonsei University Korea)
Colloquium: Sukyoung Yi Colloquium
TBA
Tuesday Feb 18, 10:30
Grace Lawrence (Swinburne)
Student Review: Grace Lawrence CoC
Grace Lawrence CoC review talk on detecting dark matter, all welcome
Tuesday Feb 11, 10:30
Juan Espejo (CAS)
Student Review: Juan Espejo Confirmation of Candidature review - The evolution of galaxy Angular Momentum across cosmic time
Title:

The role of angular momentum in the evolution of star forming galaxies

Abstract:

The age of the Universe at which star formation peaks is interesting, angular momentum (j) has been measured to be low and gas fractions (f_gas) are high (compared to local analogues). Both j and f_gas play an important role in the evolution of disk galaxies to the grand design spirals we observe today and so it is important to measure them accurately. Measuring j at high redshift is particularly difficult, one needs deep observations in both infrared photometry (stellar mass distribution) and integral field spectroscopy (emission line kinematics) in order to get an accurate description of the angular momentum content. Currently, most high-z IFS data are natural seeing (NS) limited, which prevents accurate morphological classification, introduces artefacts and hides small scale kinematic structures that affect the real shape of the rotation curves. On the other hand, adaptive optics (AO) assisted observations improve resolution but suffer from SN loss. One way to account for this is to combine data at the different resolutions: i) AO high resolution data for the inner parts where signal is enough to prevail over the SN loss introduced by the AO correction (and where the rotation curve rises rapidly) and ii) NS low resolution data for the outer parts since SN is high (and where the rotation curve has already flattened). We have analysed a sample of 10 galaxies with the combination method at z∼1.5 and z∼2 (the largest sample at high-z with combined j measurements to our knowledge) from Keck/OSIRIS + VLT/KMOS+SINFONI + HST and we have explored the capabilities of applying the combination method such as a decrease in uncertainty and a more realistic determination of shape and morphology for each galaxy.