Intensity and polarization of the atmospheric emission at millimetric wavelengths at Dome Concordia

TL;DR

This study measures atmospheric emission intensity and polarization at Dome C, Antarctica, demonstrating extremely low optical depth and polarization levels, which make it an excellent site for millimeter-wave astronomy and CMB observations.

Contribution

It provides the first detailed measurements of atmospheric emission polarization at Dome C, including upper limits on polarized signals and atmospheric transparency, enhancing site characterization for millimeter astronomy.

Findings

Optical depth at 150 GHz is very low (<tau>=0.050 ± 0.003 ± 0.011).

Atmospheric polarization is below 0.2% circular and 0.1% linear (95% CL).

The atmosphere shows high stability and low PWV (~0.77 mm).

Abstract

Atmospheric emission is a dominant source of disturbance in ground-based astronomy at mm wavelengths. The Antarctic plateau is recognized to be an ideal site for mm and sub-mm observations, and the French/Italian base of Dome C is among the best sites on Earth for these observations. In this paper we present measurements, performed using the BRAIN-pathfinder experiment, at Dome C of the atmospheric emission in intensity and polarization at 150GHz, one of the best observational frequencies for CMB observations when considering cosmic signal intensity, atmospheric transmission, detectors sensitivity, and foreground removal. Careful characterization of the air-mass synchronous emission has been performed, acquiring more that 380 elevation scans (i.e. "skydip") during the third BRAIN-pathfinder summer campaign in December 2009/January 2010. The extremely high transparency of the Antarctic atmosphere over Dome Concordia is proven by the very low measured optical depth: <tau_I>=0.050 \pm 0.003 \pm 0.011 where the first error is statistical and the second is systematic error. Mid term stability, over the summer campaign, of the atmosphere emission has also been studied. Adapting the radiative transfer atmosphere emission model "am" to the particular conditions found at Dome C, we also infer the level of the PWV content of the atmosphere, notoriously the main source of disturbance in millimetric astronomy (<PWV>=0.77 +/- 0.06 + 0.15 - 0.12 mm). Upper limits on the air-mass correlated polarized signal are also placed for the first time. The degree of circular polarization of atmospheric emission is found to be lower than 0.2% (95%CL), while the degree of linear polarization is found to be lower than 0.1% (95%CL). These limits include signal-correlated instrumental spurious polarization.