Focal lengths of Venus Monitoring Camera from limb locations. (August 2015)

• Record Type: Journal Article
• Authors: Limaye, Sanjay S.; Markiewicz, W.J.; Krauss, R.; Ignatiev, N.; Roatsch, T.; Matz, K.D.
• Is Part Of: Planetary and space science. Volume 113/114(2015)
• Page Start: 169
• Page End: 183
• Publication Date: 2015-08
• Subjects: Venus Monitoring Camera -- Focal length -- Slant optical depth -- Limb radius -- Haze -- Optical distortion; Space sciences -- Periodicals; Atmosphere, Upper -- Periodicals; Sciences spatiales -- Périodiques; Haute atmosphère -- Périodiques; 523
• DOI: 10.1016/j.pss.2015.01.010
• Languages: English
• ISSNs: 0032-0633

Abstract

Abstract: The Venus Monitoring Camera (VMC) carried by European Space Agency's Venus Express orbiter (Svedhem et al., 2007) consists of four optical units, each with a separate filter casting an image on a single CCD (Markiewicz et al., 2007a, 2007b ). The desire to capture as much of the planet in a single frame during the spacecraft's 24 h, 0.84 eccentricity orbit led to optics with 18° field of view. Analysis of Venus images obtained by the VMC indicated that the computed limb radius and altitude of haze layers were somewhat inconsistent with prior knowledge and expectations. Possible causes include errors in the knowledge of image geometry, misalignment of the optic axis from the pointing direction, and optical distortion. These were explored and eliminated, leaving only deviations from the ground and pre-solar damage estimate of the focal length lengths as the most likely reason. We use the location of planet's limb to estimate the focal length of each camera using images of the planet when the orbiter was more than 20, 000 km from planet center. The method relies on the limb radius to be constant at least over a small range of solar zenith angles. We were able to achieve better estimates for the focal lengths for all four cameras and also estimate small offsets to the boresight alignment. An outcome of this analysis is the finding that the slant unit optical depth varies more rapidly with solar zenith angle in the afternoon as compared to morning, with lowest values at local noon. A variation of this level is also observed with latitude. Both are indicative of the presence of overlying haze above the clouds, and the morning afternoon asymmetry suggests different photochemical processes in destruction and production of the haze. Highlights: Analysis of Venus monitoring camera images revealed that computed planet radius was not as expected. Planet's sunlit limb locations were used to estimate focal length and boresight alignment. We discovered that limb radius varies asymmetrically from morning to evening about local noon.