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Dr a S Arya, PI MCC & Mars Science Team Space Applications Centre

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Dr a S Arya, PI MCC & Mars Science Team Space Applications Centre Dr A S Arya, PI MCC & Mars Science Team Space Applications Centre Ahmedabad VEDAS, Feb 28, 2017 MCC : 80k km Ideal for comprehensive geological interpretation (Varying Scales) 372 km PLANNED OBJECTIVES - 1. To map various morphological features on Mars with varying resolution and scales using the unique elliptical orbit. 2. To observe dynamic events like dust storms, dust devils, clouds etc. 3. To attempt opportunistic imaging of natural satellites of Mars and other celestial bodies, if any. 4. To provide context information for other science payloads. 5. To map the geological setting around sites of Methane emission source. 6.To map Martian polar ice caps and its seasonal variations . MCC coverage 24-09-2014 to 27-02-2017 Number of images having spatial resolution i) up to 20 m:6 ii) 20 to 50m :84 iii) 50-100m:30 iv) 100-200:95 v) >200m: 501 Total number of data sets:716 MCC Horizontal Pixel Start Date Spacecraft AltitudeScale Version OD 2015-02-19 13:37:59.0 367 19.08 V1 0 2015-02-19 13:37:39.0 363 18.90 V1 0 Last date of acquisition: 2015-02-16 20:10:04.0 360 18.74 V1 0 2015-02-14 02:43:14.0 361 18.76 V1 0 03-01-2017 2015-02-11 09:16:07.0 367 19.08 V1 0 2015-02-08 15:49:11.0 364 18.92 V1 0 Marci, MRO (NASA) MCC Visual Monitoring Uniform Radiomety Camera, VMC (ESA) Good Geometric Control Movie • Morphological • Structural • Polar Ice • Change detection studies • Surface Age Determination • Dust Storms / Dust Devils - Monitoring • AOD • Clouds s2 s1 Offset ridge Fault 0.8 km Offset ridge 36 kms Date : 2015-02-16 20:10:04.0 UTC Altitude: 360.3772 km int.time 0.4 ms Orbit.no: 75 Sp. Resolution: 18.74 m MCC Data (2014) Formation of new Impact crater or exposure of buried crater :Amazonis Planitia, Mars MOC Data (1997) Viking Data (1976) Fine Dust Mantling Gale Lasswitz Crater 139m Spatial resolution Altitude 2664 km Start Time 2015-02-25, 231 m Spatial resolution T01:00:02.795 MGS-MOC Mosaic (1996) ØLength of streaks: ̴8km to ̴45 km ØArea of bright region in south- east side of Kinkora crater (yellow) could be new deposits of sand or dust is 2095 sq. km. (MCC), 1710 sq. km. (MOC) ØTotal number of streaks in the present study regions: 68 ØNew streaks found in MCC: 2 230 m Spatial resolution (they also have been seen in MGS- Viking Mosaic (1975 to 1980) MOC) Crater Size Frequency Distribution (CSFD) technique Gale crater Apollo 17 landing Site dating by Chandryaan 1-TMC Study area- Terra Cimmeria, Results : The estimated age is 3.82, 3.92 Ga (Noachian unit) which matches with published maps (Middle Noachian highland ) ü(Noachian epoch 4.5 billion years ago to 3.5 billion years ) ``All the adequate no. of craters have been picked up by MCC Required for age-determination of surface’’ (Arya et al 2012, Current Science ) MCC mosaic of the North Pole of Mars Martian North Polar Possible Region, material outliers and 6 glacial retreat VASTITAS BOREALIS 1. Layered deposits and features Korolev permanent ice (ld-pi) Scandia Tholi 2. Smooth plains (sp1) 3. 3. Rippled plains (rp) Olympia Undae 4. Etch-pitted plains (epp) 5. A light Olympia Olympia Planum 3 deposit that thinly reentrants mantles the Possible underlying cratered Material plains (sp2) 6. Small reentrants Outlier 5 Mottled cratered Chasma Boreale plains (mcp). Two lesser units shown Gemini Lingula Lobate deposit are 7. Craters (c) and 2 8. Volcanic deposits Hyperboreae Undae (vd). 8 7 MCC observation Date: 16 Dec 2015 - 26 Jan 2016 Comparison of MCC and MOC image of the same season (near Summer Solstice) Mars Color Camera (onboard Mars Orbiter Mission) image mosaic from 24-26 Dec 2015 Area=792375 km2 (upto 8 degrees from north pole) 10 to 12 days before 3 Jan 2016 (summer solstice). Mars Orbiter Camera (onboard Mars Global Surveyor) image taken on 5 Dec 2000, Area=862625 km2 (upto 8 degrees from north pole ) is 11 days before 16 Dec 2000 (summer solstice). 14July2015 Ls 12 SWIR Albedo Mapping of Mars using Mars Orbiter Mission Methane Sensor of Mars data (October 2014- February 2015) The 1 pixel per degree binned global MSM SWIR (1.65μm) apparent albedo map over MOLA map. Five months of MSM radiance data for reference channel are converted to the top of atmosphere reflectance normalised to sun- sensor viewing geometry and incoming solar flux. MSM Reference Channel SWIR Albedo Mapping of Mars using Mars Orbiter Mission 90 N 90 N 75 N 75 N 60 N 60 N 45 N 45 N 30 N 30 N 15 N 15 N 180 E 210 E 240 E 270 E 300 E 330 E 360 E 0 E 30 E 60 E 90 E 120 E 150 E 180 E 15 S 15 S 30 S 30 S 45 S 45 S 60 S 60 S 75 S 75 S 90 S 90 S The 1 pixel per degree binned global short wave infrared (SWIR) 1.6 µm albedo map. The bright regions (SWIR albedo greater than 0.4) are localized in Northern hemisphere with the highest albedo found over the Tharsis region. The low SWIR albedo regions (less than 0.2) are mainly localized in Syrtis Major and Southern highlands, although low SWIR albedo regions such as Acidalia are also identified in the Northern hemisphere. Clouds - Lat: 50.536, lon:29.2181 2 The height of the cloud is estimated using shadow method and is found to be 38 kms, which qualifies it to be CO2 ice cloud MCC Unusual Mars Limb View Mars 2 Dec 2014 Mars 13 Dec 21 Nov 2014 Mars disc disc 2014 disc High Altitude Layer (~250 Km High From Mars Altitude Plume Surface) High (~100 Km Altitude From Mars Layer Surface) (~200 Km From Mars Surface) Contrast analysis 4 Oct. 2014 20 Oct. 2014 28 Oct. 2014 Con(20 Oct. 2014) Con(20 Oct. 2014) Con(28 Oct. 2014) Con(28 Oct. 2014) (%) 0 5 10 15 0 1.5 3 4.5 AOD using Stereo method 1.8 1.7 R² = 0.94 1.6 1.5 1.4 AOD 1.3 1.2 1.1 Elevation (km) 1 -10 -5 0 5 Exponential fit : AOD = 1.17 exp(-0.07*Z) Scaled height of optical depth (H): H=(1/0.07) = 14.28 km Manoj K. Mishra, et. al 2016. Estimation of dust variability and scale height of atmospheric optical depth (AOD) in the Valles Marineris on Mars by Indian Mars Orbiter Mission (MOM) data, Icarus, 265, 84–94 3. To attempt opportunistic imaging of natural 71k km satellites of Mars and other celestial bodies, if any. Oct 14, 2014 372 km A.S. Arya, S. Manthira Moorthi, R.P. Rajasekhar, S.S. Sarkar, Koyel Sur, B. Aravind, Rajdeep K. Gambhir, Indranil Misra, V.D. Patel, A.R. Srinivas, Kamlesh K. Patel, Prakash Chauhan, A.S. Kiran Kumar, 2015. Indian Mars-Colour-Camera captures far-side of the Deimos: A rarity among contemporary Mars orbiters. Planetary and Space Science, Vol. 117, November 2015, Pp. 470-474. COMET C/2013A1 SIDING SPRING OBSERVED BY MCC ON 19TH OCT,2014 Counts : along and across the image Brightened Coma of the comet (partial view) Second frame (490 ms) Time of Acq: 18:08:47 Post-Encounter ØFOV Post- ØSize 18-20k Encounter kms MCC = -4.3 (Universe Today : 8 Deg , 19k) The pre-encouter estimates for the size and magnitudeZ AXIS of coma : COUNT of &the Comet are commensurate with the post-encounter resultsX,Y : SAMPLE derived AND from LINE MCC DIRECTION images 4. To provide context information for other science payloads. REASON PLANNED OBJECTIVES - ACHIEVED (Y/N) /COMMENTS 1. To map various morphological Y •Change detecion, features on Mars with varying resolution • Age-determination • Fault Slip and scales using the unique elliptical orbit. Estimation 2. To observe dynamic events like dust Y • Cloud Type storms, dust devils, clouds etc. • AOD estimation • Change Detection 3. To attempt opportunistic imaging of Y • Deimos Far-side natural satellites of Mars and other • Siding Spring celestial bodies, if any. 4. To provide context information for Y MSM / TIS other science payloads. 5. To map the geological setting around N Methane sites of Methane emission source. detection awaited 6.To map Martian polar ice caps and its Y Polar Ice Caps seasonal variations . not imaged so far • Most of the planned objectives of MCC have been met so far • Established the far-side view of Deimos , which is a rarity among contemporary orbiters • Single-shot , illuminated full disc view of Mars captured, which is not possible from contemporary satellites • Atmospheric optical depth estimation using multi-view angle of MCC images has been demonstrated • 1st Martian Albedo map using 1.6 µm (MSM) [1] A. S. Arya, S. S. Sarkar, A. R. Srinivas, S. Manthira Moorthi, Vishnukumar D. Patel, Rimjhim B. Singh, R. P. Rajasekhar, Sampa Roy, Indranil Misra, Sukamal Kr. Paul, Dhrupesh Shah, Kamlesh Patel, Rajdeep K. Gambhir, U. S. H. Rao, Amul Patel, Jalshri Desai, Rahul Dev, Ajay K. Prashar, Hiren Rambhia, Ranjan Parnami, Harish Seth, K. R. Murali, Rishi Kaushik, Deepak Patidar, Nilesh Soni, Prakash Chauhan, D. R. M. Samudraiah and A. S. Kiran Kumar (2015) Mars Colour Camera: the payload characterization/calibration and data analysis from Earth imaging phase. CURRENT SCIENCE, VOL. 109, NO. 6, 25 SEPTEMBER 2015 [2] A.S. Arya1* , S. Manthira Moorthi1, R. P. Rajasekhar1, S.S. Sarkar1, Koyel Sur1, Arvind B2, , Rajdeep K Gambhir1, Indranil Misra1, V.
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