The LLAMA radio telescope, installed in a high altitude site in the Northwestern area of Argentina, at 4820 meters above sea level, can be used to conduct research in several fields of astronomy and inicially, the telescope will work as a single-dish telescope.
As part of an interferometric system of VLBI associated with ALMA, APEX and/or ASTE telescopes, this network will reach one of the highest angular resolutions that can be achieved today in astronomy, of the order of 1 milliseconds of arc (0".001) at a wavelengths of 1 mm. The antenna could also be incorporated as part of the planetary global VLBI network, and could thus contribute to achieve resolutions of the order of 20 microseconds of arc at the same wavelength. It is worth stressing that is important, in order to be able to obtain high quality images, to increase the number of telescopes forming the global network, and LLAMA may be one of those telescopes. In the world there are few instruments that can operate successfully at these frequencies since they require to be located in sites situated above 4000 meters above sea level. A few of them are the telescopes ASTE (4800 m), APEX and ALMA (5100 m) (all of them installed in northern of Chile), the Great Millimeter Telescope (GMT - 4600 m) in Mexico, and telescopes in Hawaii (USA) located at 4100 m, namely the James Clerk Millimeter Telescope (JCMT), the Caltech Submillimeter Observatory (CSO) and the Submillimeter Array (SMA). In this regard, it is easily understandable, that it is of high scientific importance to make every possible effort to increase the number of telescopes to be involved in this global network. Thereupon, the LLAMA telescope may also play an important role in this regards.
Some fields of research that could benefit from the use of LLAMA working as a single-dish telescope are mentioned in the following listing:
a) The Sun
* Structure of the lower solar atmosphere.
* Active and quiescent filaments.
* Solar flares.
* Dynamics of the chromospheres and its magnetic field.
* Extra-solar planetary systems around stars near the Sun.
* Proto-planetary disks in star located in the Solar neighborhood.
* Near-Earth objects.
c) Stellar objects
* Star forming regions, young stellar objects, and mechanisms of the star formation.
* Non-thermal processes in stellar magnetospheres.
* Interaction of stars and remnants of supernova with the interstellar medium.
d) Astrophysical jets and maser emission
* Astrophysical jets.
* Maser phenomena of the recombination lines of the hydrogen atom.
* Maser emission in star-forming regions.
* Maser emission in late stars stellar envelopes.
e) Galactic and Intergalactic interstellar medium
* Continuum radiation from extragalactic cold dust.
* Molecular material in the direction of different stellar objects.
* Intergalactic Medium using the detection of molecular absorption lines in the direction of quasars.
* Cosmic background radiation.
* Search for CO in galaxies with high redshift.
* Molecular abundance.
* Active Galactic Nuclei (AGN).
* Variation of the fundamental constants by the observation of gravitational lensing.
* High redshifts of regions with very high rate of star formation.
* Proto-clusters of galaxies.
* Space-time distortion produced by massive black holes.
g) High energies
* Search for counterparts of gamma-ray sources detected with the future array of Cherenkov telescopes. (CTA: Cherenkov Telescope Array).