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Ice Cloud and Dust Climatologies Over 4 Martian Years From TGO/NOMAD‐UVIS Nadir Retrieval.

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Title: Ice Cloud and Dust Climatologies Over 4 Martian Years From TGO/NOMAD‐UVIS Nadir Retrieval.
Authors: Willame, Y.1 (AUTHOR) yannick.willame@aeronomie.be, Neary, L.1 (AUTHOR), Daerden, F.1 (AUTHOR), Wolff, M. J.2 (AUTHOR), Erwin, J. T.1 (AUTHOR), Thomas, I. R.1 (AUTHOR), Robert, S.1 (AUTHOR), Mason, J. P.3 (AUTHOR), Trompet, L.1 (AUTHOR), Vandaele, A. C.1 (AUTHOR), Piccialli, A.1 (AUTHOR), Pereira, N.1,4 (AUTHOR), Flimon, Z.1,5 (AUTHOR), Depiesse, C.1 (AUTHOR), Ristic, B.1 (AUTHOR), Patel, M. R.3,6 (AUTHOR), Bellucci, G.7 (AUTHOR), López‐Valverde, M. A.8 (AUTHOR)
Source: Journal of Geophysical Research. Planets. Jun2026, Vol. 131 Issue 6, p1-19. 19p.
Subject Terms: *Dust storms, *Climatology, *Atmospheric aerosols, *Particulate matter, Ice clouds, Scientific apparatus & instruments, Martian atmosphere
Abstract: We generate climatologies of ice cloud and dust optical depth derived from the NOMAD/UVIS nadir measurements onboard ExoMars Trace Gas Orbiter (TGO) for almost four Martian Years (MY), from mid MY34 to mid MY38. Our retrieval algorithm has been updated with new results for aerosol models and surface reflectance. It now uses 3 dust particle sizes: the nominal Reff = 1.5 μm, along with two larger sizes of 2.0 and 2.5 μm. The inclusion of the two larger sizes improves the retrieval during large dust loading events. We present the retrieved zonal‐mean distribution of water ice cloud optical depth (OD), as well as spatial distributions for portions of the MY that highlight distinct cloud features, such as the Aphelion Cloud Belt (ACB), orographic clouds and the edges of polar clouds. The diurnal trend of ice cloud optical depth during the aphelion season is shown and agrees with recent results. We also present the retrieved seasonal zonal averaged distribution of the dust OD. We have compared our aerosol OD results (i.e., dust + ice clouds) with the measurements of MastCam and MastCam‐Z onboard Curiosity and Perseverance rovers serving as ground truth validation: UVIS shows a good qualitative agreement, reproducing usually well the seasonal variations. Quantitatively, we observe UVIS values to be usually lower or similar, than MastCams' ones. We also provide and consider retrieval sensitivities of our results (altitude sensitivity, altitude profile, particle size, scattering properties) to potentially explain the differences between our nadir retrievals with the direct extinction measurements from the rovers. Plain Language Summary: We have analyzed 4 Martian years of satellite measurements to deduce the ice cloud and dust content in the Martian atmosphere. We have considered three different dust particle sizes, the two larger ones being suitable for large dust loading events, namely dust storms. For ice clouds, we observe and present the main known cloud features through seasonal and spatial distributions: the cloud belt present around aphelion, the polar hoods and the orographic clouds present above the tallest volcanoes. We have also derived the cloudiness variation through the day during the first (cooler) part of the Martian year showing agreement with previous results. For dust, we present the seasonal distribution which variations qualitatively match with previous results and observations. Quantitatively, the comparison with the direct measurements from rovers on the surface of Mars shows our values to be usually lower or similar. The differences can potentially be explained by the altitude sensitivity of our measurements and/or the aerosol models used. Key Points: NOMAD/UVIS provides a 4‐Martian‐year climatology of ice cloud opacity, including seasonal, spatial and diurnal variabilityDust opacity was retrieved over 4 Martian years using three particle sizes, improving retrievals under high dust‐loading conditionsUVIS aerosol opacity reproduces rover seasonal trends and dust storms, with mean biases of −14% vs Perseverance and −29% vs Curiosity [ABSTRACT FROM AUTHOR]
Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Ice Cloud and Dust Climatologies Over 4 Martian Years From TGO/NOMAD‐UVIS Nadir Retrieval.
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  Data: <searchLink fieldCode="AR" term="%22Willame%2C+Y%2E%22">Willame, Y.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<i> yannick.willame@aeronomie.be</i><br /><searchLink fieldCode="AR" term="%22Neary%2C+L%2E%22">Neary, L.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Daerden%2C+F%2E%22">Daerden, F.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Wolff%2C+M%2E+J%2E%22">Wolff, M. J.</searchLink><relatesTo>2</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Erwin%2C+J%2E+T%2E%22">Erwin, J. T.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Thomas%2C+I%2E+R%2E%22">Thomas, I. R.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Robert%2C+S%2E%22">Robert, S.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Mason%2C+J%2E+P%2E%22">Mason, J. P.</searchLink><relatesTo>3</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Trompet%2C+L%2E%22">Trompet, L.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Vandaele%2C+A%2E+C%2E%22">Vandaele, A. C.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Piccialli%2C+A%2E%22">Piccialli, A.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Pereira%2C+N%2E%22">Pereira, N.</searchLink><relatesTo>1,4</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Flimon%2C+Z%2E%22">Flimon, Z.</searchLink><relatesTo>1,5</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Depiesse%2C+C%2E%22">Depiesse, C.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Ristic%2C+B%2E%22">Ristic, B.</searchLink><relatesTo>1</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Patel%2C+M%2E+R%2E%22">Patel, M. R.</searchLink><relatesTo>3,6</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22Bellucci%2C+G%2E%22">Bellucci, G.</searchLink><relatesTo>7</relatesTo> (AUTHOR)<br /><searchLink fieldCode="AR" term="%22López‐Valverde%2C+M%2E+A%2E%22">López‐Valverde, M. A.</searchLink><relatesTo>8</relatesTo> (AUTHOR)
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  Data: <searchLink fieldCode="JN" term="%22Journal+of+Geophysical+Research%2E+Planets%22">Journal of Geophysical Research. Planets</searchLink>. Jun2026, Vol. 131 Issue 6, p1-19. 19p.
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  Data: *<searchLink fieldCode="DE" term="%22Dust+storms%22">Dust storms</searchLink><br />*<searchLink fieldCode="DE" term="%22Climatology%22">Climatology</searchLink><br />*<searchLink fieldCode="DE" term="%22Atmospheric+aerosols%22">Atmospheric aerosols</searchLink><br />*<searchLink fieldCode="DE" term="%22Particulate+matter%22">Particulate matter</searchLink><br /><searchLink fieldCode="DE" term="%22Ice+clouds%22">Ice clouds</searchLink><br /><searchLink fieldCode="DE" term="%22Scientific+apparatus+%26+instruments%22">Scientific apparatus & instruments</searchLink><br /><searchLink fieldCode="DE" term="%22Martian+atmosphere%22">Martian atmosphere</searchLink>
– Name: Abstract
  Label: Abstract
  Group: Ab
  Data: We generate climatologies of ice cloud and dust optical depth derived from the NOMAD/UVIS nadir measurements onboard ExoMars Trace Gas Orbiter (TGO) for almost four Martian Years (MY), from mid MY34 to mid MY38. Our retrieval algorithm has been updated with new results for aerosol models and surface reflectance. It now uses 3 dust particle sizes: the nominal Reff = 1.5 μm, along with two larger sizes of 2.0 and 2.5 μm. The inclusion of the two larger sizes improves the retrieval during large dust loading events. We present the retrieved zonal‐mean distribution of water ice cloud optical depth (OD), as well as spatial distributions for portions of the MY that highlight distinct cloud features, such as the Aphelion Cloud Belt (ACB), orographic clouds and the edges of polar clouds. The diurnal trend of ice cloud optical depth during the aphelion season is shown and agrees with recent results. We also present the retrieved seasonal zonal averaged distribution of the dust OD. We have compared our aerosol OD results (i.e., dust + ice clouds) with the measurements of MastCam and MastCam‐Z onboard Curiosity and Perseverance rovers serving as ground truth validation: UVIS shows a good qualitative agreement, reproducing usually well the seasonal variations. Quantitatively, we observe UVIS values to be usually lower or similar, than MastCams' ones. We also provide and consider retrieval sensitivities of our results (altitude sensitivity, altitude profile, particle size, scattering properties) to potentially explain the differences between our nadir retrievals with the direct extinction measurements from the rovers. Plain Language Summary: We have analyzed 4 Martian years of satellite measurements to deduce the ice cloud and dust content in the Martian atmosphere. We have considered three different dust particle sizes, the two larger ones being suitable for large dust loading events, namely dust storms. For ice clouds, we observe and present the main known cloud features through seasonal and spatial distributions: the cloud belt present around aphelion, the polar hoods and the orographic clouds present above the tallest volcanoes. We have also derived the cloudiness variation through the day during the first (cooler) part of the Martian year showing agreement with previous results. For dust, we present the seasonal distribution which variations qualitatively match with previous results and observations. Quantitatively, the comparison with the direct measurements from rovers on the surface of Mars shows our values to be usually lower or similar. The differences can potentially be explained by the altitude sensitivity of our measurements and/or the aerosol models used. Key Points: NOMAD/UVIS provides a 4‐Martian‐year climatology of ice cloud opacity, including seasonal, spatial and diurnal variabilityDust opacity was retrieved over 4 Martian years using three particle sizes, improving retrievals under high dust‐loading conditionsUVIS aerosol opacity reproduces rover seasonal trends and dust storms, with mean biases of −14% vs Perseverance and −29% vs Curiosity [ABSTRACT FROM AUTHOR]
– Name: AbstractSuppliedCopyright
  Label:
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  Data: <i>Copyright of Journal of Geophysical Research. Planets is the property of Wiley-Blackwell and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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