THEMIS Thermal Inertia Mosaic Quantitative 30N240E 100mpp

Primary Authors

Robin Fergason

Originators

USGS Astrogeology Science Center, Arizona State University Mars Space Flight Facility, NASA Mars Data Analysis Program

Publisher

USGS Astrogeology Science Center

Publication Date

2014-05-30

Abstract

This product is a quantitative (32-bit) thermal inertia image mosaic generated using Thermal Emission Imaging System (THEMIS) images from the 2001 Mars Odyssey orbiter mission using techniques as described in Fergason et al. (2006), High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications, J. Geophys. Res., 111(E12004), doi:10.1029/2006JE002735. The mosaic is generated at the full spatial scale of the THEMIS infrared dataset, which is approximately 100 meters/pixel. The objective of this work is to improve our understanding of the variability of surface properties as a function of both location and season. This objective was addressed through the creation of a global thermal inertia map from high-resolution THEMIS infrared images that allows the identification, assessment, and global correlation of surface materials. The higher spatial resolution of THEMIS data (100 m per pixel), relative to Thermal Emission Spectrometer (TES) globally binned data (~3 km per pixel), enables one to quantify the physical properties of morphologic features observed in high-resolution images, and to better understand geologic processes acting on local scales. Thermophysical variations often correspond to features identified in high-resolution images, and the integration of these data sets allows more robust scientific conclusions to be reached.

Purpose

This work was funded by the NASA Mars Data Analysis Program (MDAP) to make high-resolution thermal inertia data available to the public. This product is a global thermal inertia mosaic of Mars generated from high-resolution Thermal Emission Imaging System (THEMIS) nighttime infrared images (Christensen et al., 2004; Fergason et al., 2006a) that allows the identification, assessment, and global correlation of martian surface materials. The higher spatial resolution of THEMIS data (100 m per pixel), relative to Thermal Emission Spectrometer (TES) globally binned data (~3 km per pixel (Mellon et al., 2000; Putzig et al., 2005; Putzig and Mellon, 2007)), enables one to more easily quantify the physical properties of morphologic features observed in high-resolution images, such as those from the High Resolution Imaging Science Experiment (HiRISE), Context Camera (CTX), and Mars Orbiter Camera (MOC), and to better understand geologic processes acting on local scales. Thermophysical variations often correspond to features identified in high-resolution images, and the integration of these data sets allows more robust scientific conclusions to be reached.

Contact and Distribution

Format

Raster Data, Regional Mosaic, Remote-sensing Data

Access Constraints

Public domain

Access Scope

Astrogeology

Use Constraints

Please cite authors

Edition

1

Native Data Set Environment

ISIS v3

Astrogeology Theme

Geophysical, Remote Sensing

Mission Names

Mars Odyssey

Instrument Names

IR, THEMIS

Online Package Link

https://astrogeology.usgs.gov/search/map/themis_thermal_inertia_mosaic_quantitative_30n240e_100mpp

External File Size

2532510192

Online File Link

http://astropedia.astrogeology.usgs.gov/download/Mars/Odyssey/THEMIS-Global-Thermal-Inertia-Mosaic/Quantitative-32-Bit/THEMIS_TI_Mosaic_Quant_30N240E_100mpp.cub

Contact Address

2255 N. Gemini Drive

Contact City

Flagstaff

Contact State

AZ

Contact Postal Code

86001

Contact Email

astroweb@usgs.gov

Progress

Complete

Update Frequency

None planned

Completeness Report

When generating the thermal inertia mosaic, Thermal Emission Imaging System (THEMIS) infrared images were constrained by the latitude and longitude of the bounding coordinates of the region. We also constrained the following parameters: emission angle 0 to 30, number of lines in the image of 300 to 50, 000, and a data quality of high or better. Images were manually deleted from the mosaic if the images were of poor image quality or redundant images caused mis-registration in the averaged mosaic. Areas within the mosaic that have gaps either have no THEMIS infrared coverage at the time the mosaic was created or poor quality images were removed.

Process Description

To generate this mosaic, thermal inertia values are first derived from individual THEMIS nighttime infrared images using the technique described in Fergason et al. (2006), High-resolution thermal inertia derived from the Thermal Emission Imaging System (THEMIS): Thermal model and applications, J. Geophys. Res., 111(E12004), doi:10.1029/2006JE002735. The absolute accuracy of the THEMIS thermal inertia is ~20%. Uncertainties in the THEMIS derived thermal inertia values are primarily due to: 1) instrument calibration limitations; 2) uncertainties in model input parameters at the resolution of the THEMIS instrument; and 3) thermal model limitations. The mosaics themselves are generated using the THEMIS mosaicking procedure developed by Arizona State University (Edwards et al. (2011), Mosaicking of global planetary image datasets: 1. Techniques and data processing for Thermal Emission Imaging System (THEMIS) multi-spectral data, J. Geophys. Res., 116, E10009, doi:10.1029/2010JE003755), which uses DaVinci software scripts to post-process images ("uddw"), reduce image noise ("deplaid, "), and remove seams between images ("blend, " "sstretch, " and a high-pass filter). The resulting mosaics are qualitative (8-bit) products. The mosaics cover an area ±60˚ in latitude, are separated into 24 individual tiles (each are 30˚ in latitude and 60˚ in longitude and match the tiling scheme of the THEMIS daytime and nighttime IR mosaics), and are processed at a resolution of 100 m/pixel. We did not complete a mosaic for latitudes higher than 60˚because the THEMIS data are sparse and the temperatures are too low to enable accurate derivation of thermal inertia in most instances. Mosaic products are available in ISIS3, Geo-Tiff, and PNG data file formats. For the THEMIS infrared images used in the mosaic, see ancillary file list.

Lineage

Process Date

2011-07-20

Source Title

THEMIS IR

Source Online Linkage

http://global-data.mars.asu.edu/bin/themis.pl

Attribute Accuracy Report

Best Effort

Geospatial Information

Target

Mars

System

Mars

Minimum Latitude

30

Maximum Latitude

60

Minimum Longitude

-120

Maximum Longitude

-60

Direct Spatial Reference Method

Raster

Object Type

Grid Cell

Raster Row Count (lines)

17783

Raster Column Count (samples)

35565

Bit Type (8, 16, 32)

32

Quad Name

Radius A

3396190

Radius C

3376200

Bands

1

Pixel Resolution (meters/pixel)

100

Scale (pixels/degree)

592.74697523306

Map Projection Name

Simple Cylindrical

Latitude Type

Planetocentric

Longitude Direction

Positive East

Longitude Domain

-180 to 180