TutorialsClick on the title to download the Tutorial material- In this tutorial session, I will walk you through the data reduction steps on low-resolution spectroscopic data. I will use IRAF which will help you to learn basic data reduction steps such as tracing and extraction, accurate wavelength solution and flux calibration. Most telescopes now have automated pipelines to perform most of the steps of data reduction.However, it is best to understand how each individual step is obtained so that you can debug the data further easily. Several calibration spectra (like bias, flat fields and arc lamps) needs to be obtained during observation and advantages of observing 2 flux standards in a given night of observation will be discussed. In the second part of the session, I will quickly introduce GALFIT, which is a 2D image decomposition of a galaxy structure obtained by modelling their light distribution using analytical functions. When run successfully, it derives various physical parameters such as size, luminosity, central concentration, etc. Parameters thus obtained can help to analyse the morphology of a given galaxy and facilitate new science. Integral-field imaging capabilities provide both imaging and spectroscopic data and GALFIT forms a sophisticated tool to analyse them across wavelength ranges. 10-Jan- Introduction to MUSE Integral field spectroscopy and data analysis- Jyoti Yadav- The Multi Unit Spectroscopic Explorer (MUSE) is a second- generation instrument installed on the Nasmyth focus of UT4 at the Very Large Telescope (VLT) of the European Southern Observatory (ESO). It is a panoramic integral-field spectrograph operating in the visible wavelength range. It combines a wide field of view with fine spatial sampling and a large simultaneous spectral range. It is the most powerful optical 3D spectrograph for astrophysics to date. With only one sky image, MUSE can simultaneously register more than 90,000 spectra of astronomical objects. It is designed to take advantage of the improved spatial resolution provided by the adaptive optics facility (AOF). Various science objectives, from the formation of galaxies to the solar system, can be studied with the help of MUSE. In the tutorial, we will see how to extract images and spectra from the 3D data and use them for the primary analyses. We will also see how MUSE can help in discovering new galaxies. This tutorial describes the procedure of HI-21cm interferometric spectral line data analysis using AIPS (Astronomical Image Processing System) and CASA (Common Astronomy Software Applications). The data reduction process involves different steps for calibration, flagging and imaging. We will briefly explain the data reduction process and demonstrate the step-by-step analysis using both AIPS and CASA. 13th-Jan- Adaptive Optics at the Indian Institute of Astrophysics- Sridharan Rengaswamy
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