This data set consists of the set of visual and thermal infrared band photometry of Mars obtained by the KRFM experiment on the Phobos 2 spacecraft. The data are presented as a table of samples for 14 wavelength channels, with successive lines (rows) in the table obtained at 1-second intervals. The 5 infrared channels occur first, followed by 9 visual band channels. These data are preserved for historical reasons, but are not considered to be of archival quality.

This data set consists of the set of images obtained by the VSK-Fregat experiment on the Phobos 2 spacecraft. This data set is saved for historical reasons, but is not considered to be of archival quality.

This data set consists of the set of images obtained by the VSK-Fregat experiment on the Phobos 2 spacecraft. This data set is saved for historical reasons, but is not considered to be of archival quality.

In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30 deg.S to 6 deg.N latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. These data are saved for historical reasons; they are not considered to be of archival quality.

In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30 deg.S to 6 deg.N latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. These data are saved for historical reasons; they are not considered to be of archival quality.

In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30S to 6N latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. These data are saved for historical reasons; they are not considered to be of archival quality.

In February and March, 1989, the Termoskan instrument on board the Phobos '88 spacecraft of the USSR acquired a limited set of very high resolution simultaneous observations of the reflected solar flux (hereafter referred to as the visible channel) and emitted thermal flux (thermal infrared (IR)) from Mars's equatorial region. These are, so far, the highest spatial resolution thermal data ever obtained for Mars. Four slightly overlapping thermal panoramas (also called scans or swaths) cover a large portion of the equatorial region from 30S to 6N latitude. Simultaneous visible panoramas were taken during each of the four observing sessions; due to spacecraft memory limitations, visible channel processing was stopped early relative to the thermal channel for 2 of the sessions (2 and 4). Thus, the visible channel panoramas are shorter than the thermal panoramas for these sessions. These data are saved for historical reasons; they are not considered to be of archival quality.

The Mars Express PFS data set contains raw (CODMAC Level 2) measurements from the Planetary Fourier Spectrometer collected during the first extension Mars orbit phases.

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The Mars Express PFS data set contains raw (CODMAC Level 2) measurements from the Planetary Fourier Spectrometer collected during the first extension Mars orbit phases.