Material ( SOM ) for : Spectral Evidence for Hydrated Salts in Recurring Slope Lineae on Mars
Material ( SOM ) for : Spectral Evidence for Hydrated Salts in Recurring Slope Lineae on Mars
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发表时间：
2015
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通讯作者：
L. Ojha;M. Wilhelm;S. Murchie;A. McEwen;J. James;Wray;J. Hanley;M. Masse;M. Chojnacki
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作者：
L. Ojha;M. Wilhelm;S. Murchie;A. McEwen;J. James;Wray;J. Hanley;M. Masse;M. Chojnacki
火星上周期性斜坡线中水合盐的光谱证据作者：Lujendra Ojha 1 *，玛丽贝丝威廉1，2，斯科特L。作者：Murchie 3，Alfred S. McEwen 4，James J. Wray 1，Jennifer Hanley 5，Marion Massé 6，Matt Chojnacki 4，附属机构：1美国格鲁吉亚州亚特兰大市格鲁吉亚理工学院地球与大气科学学院。2美国加州莫菲特场美国航天局艾姆斯研究中心空间科学和天体生物学部。3美国马里兰州，月桂，应用物理实验室。4美国亚利桑那州图森市亚利桑那大学月球和行星实验室。5美国科罗拉多博尔德西南研究所空间研究系。6 Planétologie et Géodynamique，南特，法国。该SOM包含（1）我们的数据集和方法的一般描述，（2）我们的大气校正，验证方法和光谱混合模型的细节，（3）补充图，以说明CRISM图像中分析的RSL活动和区域，以及（4）表S1和S2列出了这项工作中使用的数据。(1)数据集和方法：CRISM 1全分辨率目标（FRT ~18 m/pix）、全分辨率短（FRS ~18 m/pix）和沿着航迹过采样（ATO 18 m/pix，具有增强的重叠以支持处理~6 m/pixel）观测，与HiRISE观测协调，用于检查RSL的光谱特征。我们选择不检查VNIR检测器范围（0.4-1.0 μm）内的图像，因为我们的重点是明确的证据，支持或反对水合的迹象，这主要是使用IR检测器波长范围内的反射检测。在表S1中列出了分析CRISM图像以研究此处描述的RSL的光谱特征，沿着最初识别线的协调HiRISE图像。表S1还列出了图像的中心纬度和经度沿着及其太阳经度（Ls），以及此处提供的光谱位置的精确坐标。表S2列出了用于创建此处所示RSL比值谱的分母面积的精确坐标。从PDS下载CRISM I/F图像，并使用ENVI（Exelis Visual Spectral evidence for hydrated salts in recurring slope lineae on Mars）进行预处理。
Spectral Evidence for Hydrated Salts in Recurring Slope Lineae on Mars Authors: Lujendra Ojha1*, Mary Beth Wilhelm1, 2, Scott L. Murchie3, Alfred S. McEwen4, James J. Wray1, Jennifer Hanley5, Marion Massé6, Matt Chojnacki4, Affiliations: 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA. 2Space Science and Astrobiology Division, NASA Ames Research Center, Moffett Field, California, USA. 3Applied Physics Laboratory, Laurel, Maryland, USA. 4Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA. 5Department of Space Studies, Southwest Research Institute, Boulder, Colorado, USA. 6Laboratoire de Planétologie et Géodynamique, Nantes, France. This SOM contains (1) a general description of our dataset and methodology, (2) details of our atmospheric correction, validation approach and spectral mixture model, (3) supplementary figures to illustrate RSL activity and areas analyzed in CRISM images, and (4) Tables S1 and S2 that list the data used in this work. (1) Dataset and Methodology: CRISM1 full-resolution targeted (FRT ~18 m/pix), full-resolution short (FRS ~18 m/pix), and Along Track Oversampled (ATO 18 m/pix, with enhanced overlap to support processing to ~6 m/pixel) observations at Infrared (IR: 1.0-3.9 μm) wavelengths coordinated with HiRISE observations were used to examine the spectral characteristics of RSL. We chose not to inspect images in the VNIR detector range (0.4-1.0 μm), because our focus was clear evidence for or against signs of hydration, which is primarily detected using absorptions in the IR detector wavelength range. The CRISM images which were analyzed to study spectral characteristics of RSL described here are listed in Table S1, along with the coordinated HiRISE images in which the lineae were initially identified. Table S1 also lists the central latitude and longitude of the images along with their solar longitude (Ls), and exact coordinates for the location of spectra presented here. Table S2 lists exact coordinates of the denominator areas used to create the ratio spectra of RSL shown here. CRISM I/F images were downloaded from PDS and were preprocessed using ENVI’s (Exelis Visual Spectral evidence for hydrated salts in recurring slope lineae on Mars SUPPLEMENTARY INFORMATION DOI: 10.1038/NGEO2546