Publications by Fred Taylor

First observations of H2O and CO2 vapor in comet 67P/Churyumov-Gerasimenko made by VIRTIS onboard Rosetta


D Bockelee-Morvan, V Debout, S Erard, C Leyrat, F Capaccioni, G Filacchione, N Fougere, P Drossart, G Arnold, M Combi, B Schmitt, J Crovisier, M-C de Sanctis, T Encrenaz, E Kuehrt, E Palomba, FW Taylor, F Tosi, G Piccioni, U Fink, G Tozzi, A Barucci, N Biver, M-T Capria, M Combes, W Ip, M Blecka, F Henry, S Jacquinod, J-M Reess, A Semery, D Tiphene

Models of the global cloud structure on Venus derived from Venus Express observations

Icarus (2011)

JK Barstow, CCC Tsang, CF Wilson, PGJ Irwin, FW Taylor, K McGouldrick, P Drossart, G Piccioni, S Tellmann

Models of the global cloud structure on Venus derived from Venus Express observations

Icarus 217 (2012) 542-560

JK Barstow, CCC Tsang, CF Wilson, PGJ Irwin, FW Taylor, K McGouldrick, P Drossart, G Piccioni, S Tellmann

Spatially-resolved near-infrared spectra from the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on Venus Express have been used to derive improved models of the vertical structure and global distribution of cloud properties in the southern hemisphere of Venus. VIRTIS achieved the first systematic, global mapping of Venus at wavelengths within transparency windows in the 1.6-2.6. μm range, which are sensitive on the nightside to absorption by the lower and middle cloud layers of thermally-emitted radiation from the hot lower atmosphere (Taylor, F.W., Crisp, D., Bézard, B. [1997]. Venus II: Geology, Geophysics, Atmosphere, and Solar Wind Environment, pp. 325-351). The cloud model used to interpret the spectra is based on previous work by Pollack et al. (Pollack, J., Dalton, J., Grinspoon, D., Wattson, R., Freedman, R., Crisp, D., Allen, D., Bézard, B., de Bergh, C., Giver, L. [1993]. Icarus 103, 1-42), Grinspoon et al. (Grinspoon, D.H., Pollack, J.B., Sitton, B.R., Carlson, R.W., Kamp, L.W., Baines, K.H., Encrenaz, T., Taylor, F.W. [1993]. Planet. Space Sci. 41, 515-542) and Crisp (Crisp, D. [1986]. Icarus 67, 484-514), and assumes a composition for the cloud particles of sulfuric acid and water, with acid concentration as a free parameter to be determined. Other retrieved parameters are the average size of the particles and the altitude of the cloud base in the model. Latitudinal variation in the atmospheric temperature structure was incorporated using data from the Venus Radio Science experiment (VeRa). Values are estimated initially using wavelength pairs selected for their unique sensitivity to each parameter, and then validated by comparing measured to calculated spectra over the entire wavelength range, the latter generated using the NEMESIS radiative transfer and retrieval code (Irwin, P.G.J., Teanby, N.A., de Kok, R., Fletcher, L.N., Howett, C.J.A., Tsang, C.C.C., Wilson, C.F., Calcutt, S.B., Nixon, C.A., Parrish, P.D. [2008]. J. Quant. Spectrosc. Radiat. Trans. 109, 1136-1150). The sulfuric acid concentration in the cloud particles is found to be higher in regions of optically thick cloud. The cloud base altitude shows a dependence on latitude, reaching a maximum height near -50°. The increased average particle size near the pole found by Wilson et al. (Wilson, C.F., Guerlet, S., Irwin, P.G.J., Tsang, C.C.C., Taylor, F.W., Carlson, R.W., Drossart, P., Piccioni, G. [2008]. J. Geophys. Res. (Planets) 113, E12) and the finding of spatially variable water vapor abundance at35-40. km altitude first reported by Tsang et al. (Tsang, C.C.C., Wilson, C.F., Barstow, J.K., Irwin, P.G.J., Taylor, F.W., McGouldrick, K., Piccioni, G., Drossart, P., Svedhem, H. [2010]. Geophys. Res. Lett. 37, L02202) are both confirmed. The implications of these improved descriptions of cloud structure and variability for the chemistry, meteorology, and radiative energy balance on Venus are briefly discussed. © 2011 Elsevier Inc.

Forty years of satellite meteorology at Oxford


FW Taylor

Comparative planetology, climatology and biology of Venus, Earth and Mars


FW Taylor

Infrared limb sounding of Titan with the cassini composite infrared spectrometer: Effects of the mid-IR detector spatial responses: Errata

Applied Optics 49 (2010) 5575-5576

CA Nixon, NA Teanby, SB Calcutt, S Aslam, DE Jennings, VG Kunde, FM Flasar, PGJ Irwin, FW Taylor, DA Glenar, MD Smith

We provide a revised Table 5 for the paper by Nixon et al. [Appl. Opt. 48, 1912 (2009)], in which the abundances of 13CO2 and C 18O were incorrect . © 2010 Optical Society of America.

Correlations between cloud thickness and sub-cloud water abundance on Venus


CCC Tsang, CF Wilson, JK Barstow, PGJ Irwin, FW Taylor, K McGouldrick, G Piccioni, P Drossart, H Svedhem

Martian atmosphere as observed by VIRTIS-M on Rosetta spacecraft


A Coradini, D Grassi, F Capaccioni, G Filacchione, F Tosi, E Ammannito, MC De Sanctis, V Formisano, P Wolkenberg, G Rinaldi, G Arnold, MA Barucci, G Bellucci, J Benkhoff, JP Bibring, A Blanco, D Bockelee-Morvan, MT Capria, R Carlson, U Carsenty, P Cerroni, L Colangeli, M Combes, M Combi, J Crovisier, P Drossart, T Encrenaz, S Erard, C Federico, U Fink, S Fonti, W-H Ip, PGJ Irwin, R Jaumann, E Kuehrt, Y Langevin, G Magni, T McCord, V Mennella, S Mottola, G Neukum, V Orofino, P Palumbo, G Piccioni, H Rauer, B Schmitt, D Tiphene, FW Taylor, GP Tozzi

Mars' south polar hood as observed by the Mars Climate Sounder


JL Benson, DM Kass, A Kleinboehl, DJ McCleese, JT Schofield, FW Taylor

Diviner lunar radiometer observations of cold traps in the moon's south polar region

Science 330 (2010) 479-482

DA Paige, MA Siegler, JA Zhang, PO Hayne, EJ Foote, KA Bennett, AR Vasavada, BT Greenhagen, JT Schofield, DJ McCleese, MC Foote, E DeJong, BG Bills, W Hartford, BC Murray, CC Allen, K Snook, LA Soderblom, S Calcutt, FW Taylor, NE Bowles, JL Bandfield, R Elphic, R Ghent, TD Glotch, MB Wyatt, PG Lucey

Diviner Lunar Radiometer Experiment surface-temperature maps reveal the existence of widespread surface and near-surface cryogenic regions that extend beyond the boundaries of persistent shadow. The Lunar Crater Observation and Sensing Satellite (LCROSS) struck one of the coldest of these regions, where subsurface temperatures are estimated to be 38 kelvin. Large areas of the lunar polar regions are currently cold enough to cold-trap water ice as well as a range of both more volatile and less volatile species. The diverse mixture of water and high-volatility compounds detected in the LCROSS ejecta plume is strong evidence for the impact delivery and cold-trapping of volatiles derived from primitive outer solar system bodies.

Structure and dynamics of the Martian lower and middle atmosphere as observed by the Mars Climate Sounder: Seasonal variations in zonal mean temperature, dust, and water ice aerosols


DJ McCleese, NG Heavens, JT Schofield, WA Abdou, JL Bandfield, SB Calcutt, PGJ Irwin, DM Kass, A Kleinbohl, SR Lewis, DA Paige, PL Read, MI Richardson, JH Shirley, FW Taylor, N Teanby, RW Zurek

The Lunar Reconnaissance Orbiter Diviner Lunar Radiometer Experiment

SPACE SCIENCE REVIEWS 150 (2010) 125-160

DA Paige, MC Foote, BT Greenhagen, JT Schofield, S Calcutt, AR Vasavada, DJ Preston, FW Taylor, CC Allen, KJ Snook, BM Jakosky, BC Murray, LA Soderblom, B Jau, S Loring, J Bulharowski, NE Bowles, IR Thomas, MT Sullivan, C Avis, EM De Jong, W Hartford, DJ McCleese

Venus: Not evil, just a bit unfortunate

ASTRONOMY & GEOPHYSICS 51 (2010) 26-31

FW Taylor

Venus Cloud Properties from Venus Express VIRTIS Observations

AAS/Division for Planetary Sciences Meeting Abstracts #42 42 (2010) 994-994

J Barstow, FW Taylor, CCC Tsang, CF Wilson, PGJ Irwin, P Drossart, G Piccioni

The Scientific Exploration of Mars

Cambridge University Press, 2010

FW Taylor

What do we know about Mars? What remains to be understood? Is there evidence of life there? Will humans ever travel there? The dream of exploring Mars has ...

Planetary atmospheres


FW Taylor

Mars Climate Sounder limb profile retrieval of atmospheric temperature, pressure, and dust and water ice opacity


A Kleinboehl, JT Schofield, DM Kass, WA Abdou, CR Backus, B Sen, JH Shirley, WG Lawson, MI Richardson, FW Taylor, NA Teanby, DJ McCleese

Thermal tides in the Martian middle atmosphere as seen by the Mars Climate Sounder


C Lee, WG Lawson, MI Richardson, NG Heavens, A Kleinboehl, D Banfield, DJ McCleese, R Zurek, D Kass, JT Schofield, CB Leovy, FW Taylor, AD Toigo

Determining vertical cloud structure on Venus using near-infrared spectroscopy

European Planetary Science Congress 2009 (2009) 249-249

JK Barstow, FW Taylor, CCC Tsang, CF Wilson, PGJ Irwin, P Drossart, G Piccioni

Venus express: Highlights of the nominal mission

Solar System Research 43 (2009) 185-209

DV Titov, H Svedhem, FW Taylor, S Barabash, JL Bertaux, P Drossart, V Formisano, B Häusler, O Korablev, WJ Markiewicz, D Nevejans, M Pätzold, G Piccioni, JA Sauvaud, TL Zhang, O Witasse, JC Gerard, A Fedorov, A Sanchez-Lavega, J Helbert, R Hoofs

Venus Express is the first European (ESA) mission to the planet Venus. Its main science goal is to carry out a global survey of the atmosphere, the plasma environment, and the surface of Venus from orbit. The payload consists of seven experiments. It includes a powerful suite of remote sensing imagers and spectrometers, instruments for in-situ investigation of the circumplanetary plasma and magnetic field, and a radio science experiment. The spacecraft, based on the Mars Express bus modified for the conditions at Venus, provides a versatile platform for nadir and limb observations as well as solar, stellar, and radio occultations. In April 2006 Venus Express was inserted in an elliptical polar orbit around Venus, with a pericentre height of km and apocentre distance of km and an orbital period of 24 hours. The nominal mission lasted from June 4, 2006 till October 2, 2007, which corresponds to about two Venus sidereal days. Here we present an overview of the main results of the nominal mission, based on a set of papers recently published in Nature, Icarus, Planetary and Space Science, and Geophysical Research Letters. © 2009 Pleiades Publishing, Ltd.