Subvisible CO2 ice clouds detected in the mesosphere of Mars

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Observations of the south seasonal cap of Mars during recession in 2004–2006 by the OMEGA visible/near‐infrared imaging spectrometer on board Mars Express (2007, methodology): “The optical depth of mesospheric CO2 ice clouds is very low compared to the path lengths of millimeters to decimeters observed by OMEGA [Clancy and Sandor, 1998; Montmessin et al., 2006].”
The Imaging Ultraviolet Spectrograph (IUVS) for the MAVEN Mission (2015, methodology): “Thousands of occultation events have been observed by SPICAM on Mars Express (Montmessin et al. 2006; Quémerais et al. 2006) and vertical profiles have been used to understand and constrain models of the middle atmosphere.”
Density and temperatures of the upper Martian atmosphere measured by stellar occultations with Mars Express SPICAM (2009, unknown): “Besides, the observations of CO2 ice mesospheric clouds by SPICAM and OMEGA [Montmessin et al., 2006, 2007] confirm the existence of subfreezing temperature as observed by SPICAM.”
QUANTITATIVELY ASSESSING THE ROLE OF CLOUDS IN THE TRANSMISSION SPECTRUM OF GJ 1214b (2013, methodology): “These include sulfuric acid clouds on Venus (Prinn 1973), water and carbon dioxide clouds on Mars (Montmessin et al. 2006; Whiteway et al. 2009), ammonia clouds on Jupiter (Baines et al. 2002), ammonia and water clouds on Saturn (Sromovsky et al. 1983; Baines et al. 2009; Sánchez-Lavega et al.…”