Software pipeline for the LWA Pulsar Archive

Using machine learning and neural networks to efficiently search for pulsars in processed radio telescope data.

These are Classes to communicate with a SPID RAS antenna rotator. These control the Big RAS Rotator for WVU radio telescope

This is an experimental python script predicts the Time of Arrival (TOA) and gate boundaries for a pulsar for gated imaging applications. Currently, the code is tailored for GMRT observations

Set of scripts to calculate proper motions of for astronomical masers detected with VLBI.

Simple, fast package for simulating radio interferometric visibilities using the radio interferometry measurement equation (RIME)

General programs and scripts developed by myself or others. Affiliated with Society of Amateur Radio Astronomers.

Using ARROW radio telescope to investigate the structure of spiral arms of Perseus and Cygnus. ARROW utilises the 21 cm line from atomic hydrogen .

SETI Synthesis Imaging (SETISIM) : A python based package for Synthesis Imaging using CASA for SETI. Spectral Imaging for uGMRT data

Detecting Radio Signals with Spectral Structure

Radio interferometric calibration with PyTorch. An example of how to solve a general optimization problem.

LK009 filler project to observe pulsars with LWA1

Pipeline with scripts for running pulsar search software (PRESTO and custom Python routines) on HPC nodes.

Merge datasets obtained by the ASTE-XFFTS system into a single file

Hint assisted reinforcement learning

⚠️ Python 2 package for the FMLO method (discontinued)

A customizable scientific software pipeline for detecting, categorizing, and viewing single pulse candidates that may be Fast Radio Burst (FRB) sources in Radio Astronomy data.

A python library to jointly analyse the data products of cosmological simulations and radio sky surveys. It provides the functionalities to go from data-cubes (simulations) and .fits maps (surveys) to object catalogues.

A project in which we study the feasibility of correlation calibration (Sievers 2016) in the Murchison Widefield Array in attempt to bridge the gap between Redudant Calibration and Sky Model Based Calibration