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Dive into the research topics where Jack B. Bishop is active.

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Featured researches published by Jack B. Bishop.


Nature | 2008

Hydrated silicate minerals on Mars observed by the Mars Reconnaissance Orbiter CRISM instrument

John F. Mustard; Scott L. Murchie; Shannon Pelkey; B. L. Ehlmann; Ralph E. Milliken; John A. Grant; Jean-Pierre Bibring; F. Poulet; Jack B. Bishop; E. Z. Noe Dobrea; L. H. Roach; F. P. Seelos; Raymond E. Arvidson; Sandra Margot Wiseman; Robert O. Green; C. D. Hash; David Carl Humm; Erick R. Malaret; J. A. McGovern; Kimberly D. Seelos; Thomas E. Clancy; Roger N. Clark; D. J. Des Marais; Noam R. Izenberg; Amy T. Knudson; Yves Langevin; Terry Z. Martin; Patrick C. McGuire; Richard V. Morris; Mark S. Robinson

Phyllosilicates, a class of hydrous mineral first definitively identified on Mars by the OMEGA (Observatoire pour la Mineralogie, L’Eau, les Glaces et l’Activitié) instrument, preserve a record of the interaction of water with rocks on Mars. Global mapping showed that phyllosilicates are widespread but are apparently restricted to ancient terrains and a relatively narrow range of mineralogy (Fe/Mg and Al smectite clays). This was interpreted to indicate that phyllosilicate formation occurred during the Noachian (the earliest geological era of Mars), and that the conditions necessary for phyllosilicate formation (moderate to high pH and high water activity) were specific to surface environments during the earliest era of Mars’s history. Here we report results from the Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) of phyllosilicate-rich regions. We expand the diversity of phyllosilicate mineralogy with the identification of kaolinite, chlorite and illite or muscovite, and a new class of hydrated silicate (hydrated silica). We observe diverse Fe/Mg-OH phyllosilicates and find that smectites such as nontronite and saponite are the most common, but chlorites are also present in some locations. Stratigraphic relationships in the Nili Fossae region show olivine-rich materials overlying phyllosilicate-bearing units, indicating the cessation of aqueous alteration before emplacement of the olivine-bearing unit. Hundreds of detections of Fe/Mg phyllosilicate in rims, ejecta and central peaks of craters in the southern highland Noachian cratered terrain indicate excavation of altered crust from depth. We also find phyllosilicate in sedimentary deposits clearly laid by water. These results point to a rich diversity of Noachian environments conducive to habitability.


Fourth International Asia-Pacific Environmental Remote Sensing Symposium 2004: Remote Sensing of the Atmosphere, Ocean, Environment, and Space | 2004

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) on MRO (Mars Reconnaissance Orbiter)

Scott L. Murchie; Raymond E. Arvidson; P. Bedini; K. Beisser; Jean-Pierre Bibring; Jack B. Bishop; John D. Boldt; Tech H. Choo; R. Todd Clancy; Edward Hugo Darlington; D. J. Des Marais; R. Espiritu; Melissa J. Fasold; Dennis E. Fort; Richard N. Green; Edward A. Guinness; John Hayes; C. D. Hash; Kevin J. Heffernan; J. Hemmler; Gene A. Heyler; David Carl Humm; J. Hutchison; Noam R. Izenberg; Robert Lee; Jeffrey Lees; David A. Lohr; Erick R. Malaret; Terry Z. Martin; Richard V. Morris

CRISM (Compact Reconnaissance Imaging Spectrometer for Mars) is a hyperspectral imager that will be launched on the MRO (Mars Reconnaissance Orbiter) spacecraft in August 2005. MRO’s objectives are to recover climate science originally to have been conducted on the Mars Climate Orbiter (MCO), to identify and characterize sites of possible aqueous activity to which future landed missions may be sent, and to characterize the composition, geology, and stratigraphy of Martian surface deposits. MRO will operate from a sun-synchronous, near-circular (255x320 km altitude), near-polar orbit with a mean local solar time of 3 PM. CRISM’s spectral range spans the ultraviolet (UV) to the mid-wave infrared (MWIR), 383 nm to 3960 nm. The instrument utilizes a Ritchey-Chretien telescope with a 2.12° field-of-view (FOV) to focus light on the entrance slit of a dual spectrometer. Within the spectrometer, light is split by a dichroic into VNIR (visible-near-infrared, 383-1071 nm) and IR (infrared, 988-3960 nm) beams. Each beam is directed into a separate modified Offner spectrometer that focuses a spectrally dispersed image of the slit onto a two dimensional focal plane (FP). The IR FP is a 640 x 480 HgCdTe area array; the VNIR FP is a 640 x 480 silicon photodiode area array. The spectral image is contiguously sampled with a 6.6 nm spectral spacing and an instantaneous field of view of 61.5 μradians. The Optical Sensor Unit (OSU) can be gimbaled to take out along-track smear, allowing long integration times that afford high signal-to-noise ratio (SNR) at high spectral and spatial resolution. The scan motor and encoder are controlled by a separately housed Gimbal Motor Electronics (GME) unit. A Data Processing Unit (DPU) provides power, command and control, and data editing and compression. CRISM acquires three major types of observations of the Martian surface and atmosphere. In Multispectral Mapping Mode, with the gimbal pointed at planet nadir, data are collected at frame rates of 15 or 30 Hz. A commandable subset of wavelengths is saved by the DPU and binned 5:1 or 10:1 cross-track. The combination of frame rates and binning yields pixel footprints of 100 or 200 m. In this mode, nearly the entire planet can be mapped at wavelengths of key mineralogic absorption bands to select regions of interest. In Targeted Mode, the gimbal is scanned over ±60° from nadir to remove most along-track motion, and a region of interest is mapped at full spatial and spectral resolution. Ten additional abbreviated, pixel-binned observations are taken before and after the main hyperspectral image at longer atmospheric path lengths, providing an emission phase function (EPF) of the site for atmospheric study and correction of surface spectra for atmospheric effects. In Atmospheric Mode, the central observation is eliminated and only the EPF is acquired. Global grids of the resulting lower data volume observation are taken repeatedly throughout the Martian year to measure seasonal variations in atmospheric properties.


Journal of Geophysical Research | 2007

Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) on Mars Reconnaissance Orbiter (MRO)

Scott L. Murchie; Raymond E. Arvidson; P. Bedini; K. Beisser; J.-P. Bibring; Jack B. Bishop; John D. Boldt; Peter J. Cavender; T. H. Choo; R. T. Clancy; Edward Hugo Darlington; D. J. Des Marais; R. Espiritu; Dennis E. Fort; Robert O. Green; Edward A. Guinness; J. M. Hayes; C. D. Hash; Kevin J. Heffernan; J. Hemmler; Gene A. Heyler; David Carl Humm; J. Hutcheson; Noam R. Izenberg; Robert Lee; Jeffrey Lees; David A. Lohr; Erick R. Malaret; Terry Z. Martin; J. A. McGovern


Archive | 2007

CRISM Spectral Signatures of the North Polar Gypsum Dunes

Leah Hutchison Roach; John F. Mustard; Scott L. Murchie; Y. Langevin; J.-P. Bibring; Jack B. Bishop; Nathan T. Bridges; Alexander Brown; Alex Byrne; B. L. Ehlmann; Kenneth E. Herkenhoff; Patrick C. McGuire; Ralph E. Milliken; Shannon M. Pelkey; F. Poulet; F. P. Seelos; K. D. Seelos


Archive | 2007

CRISM Mapping of Layered Deposits in Western Candor Chasma

Scott L. Murchie; Ralph E. Milliken; Leah Hutchison Roach; J.-P. Bibring; John F. Mustard; Shannon M. Pelkey; F. P. Seelos; Jack B. Bishop; John P. Grotzinger; Alfred S. McEwen


Archive | 2008

Mg- and Fe-Sulfate Layers in Aram Chaos, Mars

Kimberly Ann Lichtenberg; Raymond E. Arvidson; Jack B. Bishop; Timothy D. Glotch; Eldar Zeev Noe Dobrea; Scott L. Murchie; John F. Mustard; Leah Hutchison Roach


Archive | 2007

Spectral Evidence for Aqueous Alteration of the Plains Surrounding Valles Marineris, Mars

Ralph E. Milliken; Gregg A. Swayze; Scott L. Murchie; Jack B. Bishop; R. N. Clark; B. L. Ehlmann; J. Grtozinger; John F. Mustard; Catherine M. Weitz


Archive | 2008

New Evidence for the Origin of Layered Deposits in Valles Marineris

Scott L. Murchie; F. P. Seelos; Leah Hutchison Roach; John F. Mustard; Ralph E. Milliken; Raymond E. Arvidson; Sandra Margot Wiseman; Kimberly Ann Lichtenberg; Jeffrey C. Andrews-Hanna; J.-P. Bibring; Jack B. Bishop; M. P. L. Parente; Richard V. Morris


Archive | 2009

CONTENTS — M through Z

Scott L. Murchie; Raymond E. Arvidson; P. Bedini; P. Bibring; Jack B. Bishop; Peter J. Cavender; T. H. Choo; R. T. Clancy; D. Des Marais; R. Espiritu; Robert O. Green; E. A. Guinness; J. M. Hayes; C. D. Hash; Kevin J. Heffernan; David Carl Humm; J. Hutcheson; Noam R. Izenberg; Erick R. Malaret; Terry Z. Martin; J. A. McGovern; Patrick C. McGuire; Richard V. Morris; John F. Mustard; Shannon M. Pelkey; Mark S. Robinson; Ted L. Roush; F. P. Seelos; Susan Slavney; M. D. Smith


Archive | 2008

An Overview of Classes of Martian Phyllosilicate Deposits from Orbital Remote Sensing

Scott L. Murchie; John F. Mustard; B. L. Ehlmann; Ralph E. Milliken; Jack B. Bishop; F. P. Seelos

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Scott L. Murchie

Johns Hopkins University Applied Physics Laboratory

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Raymond E. Arvidson

Washington University in St. Louis

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F. P. Seelos

Johns Hopkins University Applied Physics Laboratory

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Noam R. Izenberg

Johns Hopkins University Applied Physics Laboratory

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Robert O. Green

California Institute of Technology

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