# 15 years of VLT/UVES OH intensities and temperatures in comparison with TIMED/SABER data

## TL;DR

This study analyzes 15 years of UVES spectroscopic data to investigate long-term variations in OH airglow emissions and temperatures, comparing findings with TIMED/SABER satellite data to understand solar cycle effects and atmospheric processes.

## Contribution

It provides a comprehensive long-term analysis of OH emission intensities and temperatures using archival UVES data, validated against SABER satellite measurements, highlighting solar cycle influences and atmospheric dynamics.

## Key findings

- OH intensity varies by 12-17% with the solar cycle.
- OH rotational temperatures change by 4-5 K per 100 sfu solar flux.
- Secular trends in OH emissions are negligible over 15 years.

## Abstract

The high-resolution echelle spectrograph UVES of the Very Large Telescope at Cerro Paranal in Chile has been regularly operated since April 2000. Thus, UVES archival data originally taken for astronomical projects but also including sky emission can be used to study airglow variations on a time scale longer than a solar cycle. Focusing on OH emission and observations until March 2015, we considered about 3,000 high-quality spectra from two instrumental set-ups centred on 760 and 860 nm, which cover about 380 nm each. These data allowed us to measure line intensities for several OH bands in order to derive band intensities and rotational temperatures for different upper vibrational levels as a function of solar activity and observing date. The results were compared with those derived from emission and temperature profile data of the radiometer SABER on the TIMED satellite taken in the Cerro Paranal area between 2002 and 2015. In agreement with the SABER data, the long-term variations in OH intensity and temperature derived from the UVES data are dominated by the solar cycle, whereas secular trends appear to be negligible. Combining the UVES and SABER results, the solar cycle effects for the OH intensity and temperature are about 12 to 17% and 4 to 5 K per 100 sfu and do not significantly depend on the selected OH band. The data also reveal that variations of the effective OH emission layer height and air density can cause significant changes in the OH rotational temperatures due to a varying ratio of OH thermalising collisions by air molecules and OH radiation, deactivation, and destruction processes which impede the rotational relaxation. However, this effect appears to be of minor importance for the explanation of the rotational temperature variations related to the solar activity cycle, which causes only small changes in the OH emission profile.