Spectroscopy is the basic tool employed in astronomy to derive physical
parameters, like temperature, density, chemical composition, velocity
and magnetic fields that give insights into the physical processes
that are operative in the celestial objects. Much of our
understanding of stellar atmospheres and even low-density
collisionally excited plasma, such as supernova remnants, is based on
the understanding of plasma processes in the solar atmosphere.
Although some of these processes can be studied by high spatial
resolution images of the sun, our knowledge of the temperature,
densities and dynamics of different regions of the solar atmosphere
is based on the high resolution spectroscopy in the X-ray, UV and
optical spectral regions.
The atomic and molecular spectroscopy plays a key role in understanding
astrochemistry. For example, the carbon bearing molecules, such as
polycyclic aromatic hydrocarbons (PAHs), are now thought to be
widespread in the interstellar medium in their neutral and ionized
forms. Identifying the carriers responsible for several observed
interstellar bands will allow us to derive important information on
cosmic elemental abundance as well as on the physical conditions
reigning in specific interstellar environments. The identifications
of these carriers are the key for a correct understanding of the
energetic mechanisms that govern the origin and evolution of the
interstellar medium.
In the last two decades great progress has been made in our
understanding of the physics of molecules, and neutral and ionized
atoms, and the application of physics to develop spectroscopic
diagnostics to analyze the spectra of sun, stars and other celestial
objects.
Comprehensive and accurate transition probability data are needed to
determine the abundances of a neutral atom and all of its ions in different
astrophysical environments. Determination of radiative lifetimes can
provide the absolute scale for converting the branching fractions
into atomic transition probabilities and vice versa. Since the
derivation of the physical parameters of the prevailing astrophysical
conditions is an inverse problem, accurate theories of line formation
under widely varying conditions that one encounters in celestial
objects have to be developed.
Hence
a multi-disciplinary approach, by combining astrophysical observation
with laboratory simulations and theoretical modelings, is essential
to address the complex issues involved in interpreting the data for
the ultimate aim of understanding the physical conditions prevalent
in celestial objects. Also for a proper interpretation of the high
resolution data that we obtain from space missions, it has become
necessary to improve the accuracy of the theory of line formation to
a great extent.
We have scientists who are actively working in various fields, like
observational astronomy, theoretical astrophysics, theoretical and
experimental atomic and molecular spectroscopy. The purpose of this
conference is to bring them together to discuss their research
activities and to plan new collaborations among scientists working in
related fields which would yield better scientific results. For young
researchers and Ph. D. students, the conference would give a great
opportunity to interact with experts and learn different aspects of
spectroscopy.