Retrospective evaluation of whole exome and genome mutation calls in 746 cancer samples

Funder: NCI U24CA211006Abstract: The Cancer Genome Atlas (TCGA) and International Cancer Genome Consortium (ICGC) curated consensus somatic mutation calls using whole exome sequencing (WES) and whole genome sequencing (WGS), respectively. Here, as part of the ICGC/TCGA Pan-Cancer Analysis of Whole Genomes (PCAWG) Consortium, which aggregated whole genome sequencing data from 2,658 cancers across 38 tumour types, we compare WES and WGS side-by-side from 746 TCGA samples, finding that ~80% of mutations overlap in covered exonic regions. We estimate that low variant allele fraction (VAF < 15%) and clonal heterogeneity contribute up to 68% of private WGS mutations and 71% of private WES mutations. We observe that ~30% of private WGS mutations trace to mutations identified by a single variant caller in WES consensus efforts. WGS captures both ~50% more variation in exonic regions and un-observed mutations in loci with variable GC-content. Together, our analysis highlights technological divergences between two reproducible somatic variant detection efforts

Optical calibration of the SuperCam instrument body unit spectrometers

International audienceThe SuperCam remote sensing instrument on NASA's Perseverance rover is capable of four spectroscopic techniques, remote micro-imaging, and audio recording. These analytical techniques provide details of the chemistry and mineralogy of the rocks and soils probed in the Jezero Crater on Mars. Here we present the methods used for optical calibration of the three spectrometers covering the 243-853 nm range used by three of the four spectroscopic techniques. We derive the instrument optical response, which characterizes the instrument sensitivity to incident radiation as a function of a wavelength. The instrument optical response function derived here is an essential step in the interpretation of the spectra returned by SuperCam as it converts the observed spectra, reported by the instrument as "digital counts" from an analog to digital converter, into physical values of spectral radiance

MULTIVARIATE AND ENSEMBLE MANGANESE CALIBRATION MODELS FOR SUPERCAM

International audienceOperator (LASSO) multivariate techniques with blended submodels; similar to the calibration model used from ChemCam [6], and then compared this model to ensemble methods [5,7]. Blended submodels split the data into smaller portions, trains linear models on these portions, and then optimizes the blend ranges of the submodels to cover the full data range [8]. The process of creating optimized submodels is time consuming, and may not yield the best model possible. Ensemble methods are non-linear, and would negate the need to train and optimize submodels. The response of the instrument to atomic emission is likely non-linear, and thus ensemble methods are likely to have better success in calibration than our previous attempts using LASSO, PLS, etc. Ensemble methods tested include Gradient Boosting, Random Forests, and Extra Trees [9]. Methods: Data Collection and Pre-processing. A standard set, for which MnO content is known, consisting of 252 training and 70 test standards, was analyzed using the SuperCam flight model from 1.6 m distance (3 average spectra were collected on each standard consisting of 50 shots averaged in each point) under a Mars-like atmosphere [5]. The standard set covers a range of Mn compositions from 0.0009-76 wt% MnO and contains a variety of rock matrices (e.g., rock, mineral, Mn ores). No outliers were removed. We use the Python Hyperspectral Analysis Tool [10] and the associated graphical interface for point spectra analysis [10] to preprocess the data and evaluate multivariate regression models. Ensemble methods were trained using Python scikit-learn [7,9]. Each spectrum is normalized by the sum of the total emission for each detector [5]. A "peak area" (PA) preprocessing technique is used [6], where local minima and maxima of the average spectra of the dataset is determined. The process then bins the emission between each pair of minima and assigns the result to the wavelength of the corresponding maximum. We compared full spectra with peak area spectra for this work. Based on preliminary work, we masked wavelengths ≥750 nm, where there are no Mn emission lines, to remove lines from alkali, minor elements, and oxygen, all of which had some influence on the LASSO model

MULTIVARIATE AND ENSEMBLE MANGANESE CALIBRATION MODELS FOR SUPERCAM

International audienceOperator (LASSO) multivariate techniques with blended submodels; similar to the calibration model used from ChemCam [6], and then compared this model to ensemble methods [5,7]. Blended submodels split the data into smaller portions, trains linear models on these portions, and then optimizes the blend ranges of the submodels to cover the full data range [8]. The process of creating optimized submodels is time consuming, and may not yield the best model possible. Ensemble methods are non-linear, and would negate the need to train and optimize submodels. The response of the instrument to atomic emission is likely non-linear, and thus ensemble methods are likely to have better success in calibration than our previous attempts using LASSO, PLS, etc. Ensemble methods tested include Gradient Boosting, Random Forests, and Extra Trees [9]. Methods: Data Collection and Pre-processing. A standard set, for which MnO content is known, consisting of 252 training and 70 test standards, was analyzed using the SuperCam flight model from 1.6 m distance (3 average spectra were collected on each standard consisting of 50 shots averaged in each point) under a Mars-like atmosphere [5]. The standard set covers a range of Mn compositions from 0.0009-76 wt% MnO and contains a variety of rock matrices (e.g., rock, mineral, Mn ores). No outliers were removed. We use the Python Hyperspectral Analysis Tool [10] and the associated graphical interface for point spectra analysis [10] to preprocess the data and evaluate multivariate regression models. Ensemble methods were trained using Python scikit-learn [7,9]. Each spectrum is normalized by the sum of the total emission for each detector [5]. A "peak area" (PA) preprocessing technique is used [6], where local minima and maxima of the average spectra of the dataset is determined. The process then bins the emission between each pair of minima and assigns the result to the wavelength of the corresponding maximum. We compared full spectra with peak area spectra for this work. Based on preliminary work, we masked wavelengths ≥750 nm, where there are no Mn emission lines, to remove lines from alkali, minor elements, and oxygen, all of which had some influence on the LASSO model

Quantification of manganese for ChemCam Mars and laboratory spectra using a multivariate model

International audienc

Dataset for the manuscript Manganese-rich sandstones as an indicator of ancient oxic lake water conditions in Gale crater, Mars

&lt;p&gt;This file is a csv file containing the average composition of rocks in the Murray formation in Gale crater, as determined by ChemCam, and metadata, for the manuscript &lt;em&gt;Manganese-rich sandstones as an indicator of ancient oxic lake water conditions in Gale crater, Mars&lt;/em&gt; submitted to the Journal of Geophysical Research: Planets. The file contains the major oxide composition data for each observation point (comprised of at least 30 shots where the first 5 are removed due to Mars dust), the root mean squared error (RMSE) for each ChemCam observation point, and the standard deviation of the shot-to-shot data of that observation point (shot_stdev), and the sum of oxides of the observation point. The metadata includes the &lsquo;Plot Label&rsquo; to indicate the category of the target (Dark Sandstones, Light Sandstones, Concretion, Other Diagenetic, Murray) as indicated in Figure 1 of the manuscript. The data was also used to produce Table 1. The filename, sol, spacecraft clock, target name, target distance from ChemCam, laser power, spectral totals, elevation, longitude, latitude, easting, northing, and notes metadata columns are provided for each observation point. The observations points are in order of &lsquo;Plot Label&rsquo; and then by Spacecraft Clock.&lt;/p&gt

Dark microbiome and extremely low organics in Atacama fossil delta unveil Mars life detection limits

International audienceIdentifying unequivocal signs of life on Mars is one of the most important objectives for sending missions to the red planet. Here we report Red Stone, a 163-100 My alluvial fan–fan delta that formed under arid conditions in the Atacama Desert, rich in hematite and mudstones containing clays such as vermiculite and smectites, and therefore geologically analogous to Mars. We show that Red Stone samples display an important number of microorganisms with an unusual high rate of phylogenetic indeterminacy, what we refer to as “dark microbiome”, and a mix of biosignatures from extant and ancient microorganisms that can be barely detected with state-of-the-art laboratory equipment. Our analyses by testbed instruments that are on or will be sent to Mars unveil that although the mineralogy of Red Stone matches that detected by ground-based instruments on the red planet, similarly low levels of organics will be hard, if not impossible to detect in Martian rocks depending on the instrument and technique used. Our results stress the importance in returning samples to Earth for conclusively addressing whether life ever existed on Mars

Oriented Bedrock Samples Drilled by the Perseverance Rover on Mars

Abstract A key objective of the Perseverance rover mission is to acquire samples of Martian rocks for future return to Earth. Eventual laboratory analyses of these samples would address key questions about the evolution of the Martian climate, interior, and habitability. Many such investigations would benefit greatly from samples of Martian bedrock that are oriented in absolute Martian geographic coordinates. However, the Mars 2020 mission was designed without a requirement for orienting the samples. Here we describe a methodology that we developed for orienting rover drill cores in the Martian geographic frame and its application to Perseverance's first 20 rock samples. To orient the cores, three angles were measured: the azimuth and hade of the core pointing vector (i.e., vector oriented along the core axis) and the core roll (i.e., the solid body angle of rotation around the pointing vector). We estimated the core pointing vector from the attitude of the rover's Coring Drill during drilling. To orient the core roll, we used oriented images of asymmetric markings on the bedrock surface acquired with the rover's Wide Angle Topographic Sensor for Operations and eNgineering (WATSON) camera. For most samples, these markings were in the form of natural features on the outcrop, while for four samples they were artificial ablation pits produced by the rover's SuperCam laser. These cores are the first geographically‐oriented (<2.7° 3σ total uncertainty) bedrock samples from another planetary body. This will enable a diversity of paleomagnetic, sedimentological, igneous, tectonic, and astrobiological studies on the returned samples

Dark microbiome and extremely low organics in Atacama fossil delta unveil Mars life detection limits

International audienceIdentifying unequivocal signs of life on Mars is one of the most important objectives for sending missions to the red planet. Here we report Red Stone, a 163-100 My alluvial fan–fan delta that formed under arid conditions in the Atacama Desert, rich in hematite and mudstones containing clays such as vermiculite and smectites, and therefore geologically analogous to Mars. We show that Red Stone samples display an important number of microorganisms with an unusual high rate of phylogenetic indeterminacy, what we refer to as “dark microbiome”, and a mix of biosignatures from extant and ancient microorganisms that can be barely detected with state-of-the-art laboratory equipment. Our analyses by testbed instruments that are on or will be sent to Mars unveil that although the mineralogy of Red Stone matches that detected by ground-based instruments on the red planet, similarly low levels of organics will be hard, if not impossible to detect in Martian rocks depending on the instrument and technique used. Our results stress the importance in returning samples to Earth for conclusively addressing whether life ever existed on Mars