Mars Colour Camera: the payload characterization/calibration and data analysis from Earth imaging phase

Arya, A. S.; Sarkar, Subham; Srinivas, A. R.; Moorthi, S. Manthira; Patel, Vishnukumar D.; Singh, Rimjhim Bhatnagar; Rajasekhar, R. P.; Roy, Sampa; Misra, Indranil; Paul, Sukamal Kr.; Shah, Dhrupesh; Patel, Kamlesh; Gambhir, R. K.; Rao, U. S. H.; Patel, Amul; Desai, Jalshri; Dev, Rahul; Prashar, A.; Rambhia, Hiren; Parnami, Ranjan; Seth, Harish; Murali, K. R.; Kaushik, Rishi; Patidar, Deepak; Soni, N.; Chauhan, Prakash; Samudraiah, D. R. M.; Kumar, A. S. Kiran

doi:10.18520/cs/v109/i6/1076-1086

Cited by 24 publications

(10 citation statements)

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“…IUVS acquires data during nearly every MAVEN orbit with a cadence of ∼4.5 h, enabling it to image recurring phenomena 5. MCC (Mars color camera) (Arya et al, 2015) onboard ISRO (Indian Space Research Organization) MOM, is an RGB color camera that acquires images at different altitudes from a highly elliptical orbit, usually with high resolution 6. VIS (visual imaging system) (Wellman et al, 1976) onboard Viking 2 orbiter was a single-channel visible camera of high resolution.…”

Section: Observations and Methodsmentioning

confidence: 99%

“…Images are usually taken in a series covering several minutes, enabling the measurement of atmospheric motions from the tracking of clouds and dust features (Hernández‐Bernal et al., 2019) HRSC (high‐resolution stereo camera) (Jaumann et al., 2007) onboard MEX is a high‐resolution pushbroom camera that takes images in nine different channels at different altitudes along the highly elliptical orbit OMEGA (Observatoire pour la Minéralogie, l'Eau, les Glaces et l'Activité) (Bibring et al., 2004) onboard MEX, is an imaging spectrometer that takes images simultaneously in several spectral bands IUVS (imaging ultraviolet spectrograph) (Connour et al., 2020; McClintock et al., 2015) onboard MAVEN is a scanning‐slit spectrograph that takes composite false color UV images of Mars. IUVS acquires data during nearly every MAVEN orbit with a cadence of ∼4.5 h, enabling it to image recurring phenomena MCC (Mars color camera) (Arya et al., 2015) onboard ISRO (Indian Space Research Organization) MOM, is an RGB color camera that acquires images at different altitudes from a highly elliptical orbit, usually with high resolution VIS (visual imaging system) (Wellman et al., 1976) onboard Viking 2 orbiter was a single‐channel visible camera of high resolution. Viking orbiters were in highly elliptical non‐sun‐synchronous orbits MARCI (Mars color imager) (Bell et al., 2009) onboard MRO is a pushbroom camera that observes Mars during the afternoon from an afternoon sun‐synchronous orbit, achieving high‐resolution coverage of the whole planet every Martian sol.…”

Section: Observations and Methodsmentioning

confidence: 99%

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An Extremely Elongated Cloud Over Arsia Mons Volcano on Mars: I. Life Cycle

et al. 2021

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We report a previously unnoticed annually repeating phenomenon consisting of the daily formation of an extremely elongated cloud extending as far as 1,800 km westward from Arsia Mons. It takes place in the solar longitude (Ls) range of ∼220°-320°, around the Southern solstice. We study this Arsia Mons Elongated Cloud (AMEC) using images from different orbiters, including ESA Mars Express, NASA MAVEN, Viking 2, MRO, and ISRO Mars Orbiter Mission (MOM). We study the AMEC in detail in Martian year (MY) 34 in terms of local time and Ls and find that it exhibits a very rapid daily cycle: the cloud growth starts before sunrise on the western slope of the volcano, followed by a westward expansion that lasts 2.5 h with a velocity of around 170 m/s in the mesosphere (∼45 km over the areoid). The cloud formation then ceases, detaches from its formation point, and continues moving westward until it evaporates before the afternoon, when most sun-synchronous orbiters make observations. Moreover, we comparatively study observations from different years (i.e., MYs 29-34) in search of interannual variations and find that in MY33 the cloud exhibits lower activity, while in MY34 the beginning of its formation was delayed compared with other years, most likely due to the Global Dust Storm. This phenomenon takes place in a season known for the general lack of clouds on Mars. In this paper we focus on observations, and a theoretical interpretation will be the subject of a separate paper. HERNÁNDEZ-BERNAL ET AL.

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Section: Observations and Methodsmentioning

confidence: 99%

Section: Observations and Methodsmentioning

confidence: 99%

An Extremely Elongated Cloud Over Arsia Mons Volcano on Mars: I. Life Cycle

et al. 2021

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“…Data acquired by Mars-orbiting instruments provided vital context for Curiosity's field site and the other locations examined here. The data we studied came from the Mars Reconnaissance Orbiter (MRO) High Resolution Imaging Science Experiment (HiRISE;McEwen et al, 2007) and Context Camera (CTX; Malin et al, 2007); Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC; Malin et al, 2010) and Mars Orbiter Laser Altimeter (MOLA;Smith et al, 2001); Mars Odyssey Thermal Emission Imaging System infrared subsystem (THEMIS-IR; Christensen et al, 2004a); the Viking orbiter cameras (Carr et al, 1972); and India's MOM Mars Color Camera (MCC; Arya et al, 2015). Elevations for sites inside Gale crater were determined using a topographic map produced by Parker and Calef (2016) that combines digital terrain models derived from stereopair HiRISE images with lower-spatial-resolution MOLA observations.…”

Section: Orbiter Datamentioning

confidence: 99%

Extraformational sediment recycling on Mars

et al. 2020

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Extraformational sediment recycling (old sedimentary rock to new sedimentary rock) is a fundamental aspect of Earth’s geological record; tectonism exposes sedimentary rock, whereupon it is weathered and eroded to form new sediment that later becomes lithified. On Mars, tectonism has been minor, but two decades of orbiter instrument–based studies show that some sedimentary rocks previously buried to depths of kilometers have been exposed, by erosion, at the surface. Four locations in Gale crater, explored using the National Aeronautics and Space Administration’s Curiosity rover, exhibit sedimentary lithoclasts in sedimentary rock: At Marias Pass, they are mudstone fragments in sandstone derived from strata below an erosional unconformity; at Bimbe, they are pebble-sized sandstone and, possibly, laminated, intraclast-bearing, chemical (calcium sulfate) sediment fragments in conglomerates; at Cooperstown, they are pebble-sized fragments of sandstone within coarse sandstone; at Dingo Gap, they are cobble-sized, stratified sandstone fragments in conglomerate derived from an immediately underlying sandstone. Mars orbiter images show lithified sediment fans at the termini of canyons that incise sedimentary rock in Gale crater; these, too, consist of recycled, extraformational sediment. The recycled sediments in Gale crater are compositionally immature, indicating the dominance of physical weathering processes during the second known cycle. The observations at Marias Pass indicate that sediment eroded and removed from craters such as Gale crater during the Martian Hesperian Period could have been recycled to form new rock elsewhere. Our results permit prediction that lithified deltaic sediments at the Perseverance (landing in 2021) and Rosalind Franklin (landing in 2023) rover field sites could contain extraformational recycled sediment.

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“…Planet Mars has an opulence of different satellite datasets, which have been acquired since the beginning of the Mariner Program by NASA's Jet Propulsion Laboratory to explore the Red planet to the present day. Images have been acquired by different imaging cameras and spectrometers such as the Viking Orbiter Visual Imaging Subsystems (VIS) [1], the Mars Orbiter Camera (MOC) of Mars Global Surveyor [2], the Thermal Emission Imaging Systems (THEMIS) [3] [4] using multispectral thermal-infrared and visible/near-infrared images, the High-Resolution Stereo Camera (HRSC) [5] onboard ESA's Mars Express Mission bridging the gap between medium to low resolution coverage and the very high-resolution images of the MOC, the Mars Reconnaissance Orbiters High Resolution Imaging Science Experiment (HiRISE) [6], Context Imager (CTX) [7] on the Mars Reconnaissance Orbiter (MRO), the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) [8] having hyperspectral imager on the Mars Reconnaissance Orbiter (MRO), and Mars Color Camera (MCC) onboard Mars Orbiter Mission [9]. A number of rover/lander missions set out on Mars since the 1970s have revolutionized the way we understand the Planet.…”

Section: Introductionmentioning

confidence: 99%

A New Method of Mosaicking Context Camera (CTX) Images for the Geomorphological Study of Martian Landscape

Chavan¹,

Sarkar²,

Thakkar³

et al. 2021

OJG

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Various spacecraft and satellites from the world's best space agencies are exploring Mars since 1970, constantly with great ability to capture the maximum amount of dataset for a better understanding of the red planet. In this paper, we propose a new method for making a mosaic of Mars Reconnaissance Orbiter (MRO) spacecraft payload Context Camera (CTX) images. In this procedure, we used ERDAS Imagine for image rectification and mosaicking as a tool for image processing, which is a new and unique method of generating a mosaic of thousands of CTX images to visualize the large-scale areas. The output product will be applicable for mapping of Martian geomorphological features, 2D mapping of the linear feature with high resolution, crater counting, and morphometric analysis to a certain extent.

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Mars Colour Camera: the payload characterization/calibration and data analysis from Earth imaging phase

Cited by 24 publications

References 0 publications

An Extremely Elongated Cloud Over Arsia Mons Volcano on Mars: I. Life Cycle

An Extremely Elongated Cloud Over Arsia Mons Volcano on Mars: I. Life Cycle

Extraformational sediment recycling on Mars

A New Method of Mosaicking Context Camera (CTX) Images for the Geomorphological Study of Martian Landscape

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