Speaker
Description
Water vapor is the main cause of atmospheric attenuation at high frequencies. The
measurement of atmospheric opacity (τ ) is important because it allows us to obtain the
true brightness temperature of an astrophysical object. Melo et al. (2005), presented
the method of brightness of the Sun to determine atmospheric opacity in sub-millimeter
waves. Then, using the same method Cornejo et al. (2017) estimated the opacity at
212 and 405 GHz for the period of 2006 and 2014. The measurements were made with
the Solar Telescope for Sub-Metallic Waves (SST), at the El Leoncito Astronomical
Complex (CASLEO). In this work we will use a new method to calculate the variation
of opacity in time scales from minutes to hours. We will use the opacities determined
by the method of brightness as an input parameter, on days when the Sun does not
have any active regions. The method assumes that any observed intensity variation is
then due to τ variations in the observation direction.
