{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2025,11,3]],"date-time":"2025-11-03T22:51:07Z","timestamp":1762210267476},"reference-count":24,"publisher":"American Association for the Advancement of Science (AAAS)","issue":"5469","content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Science"],"published-print":{"date-parts":[[2000,5,19]]},"abstract":"<jats:p>Infrared spectral images of Jupiter's volcanic moon Io, acquired during the October and November 1999 and February 2000 flybys of the Galileo spacecraft, were used to study the thermal structure and sulfur dioxide distribution of active volcanoes. Loki Patera, the solar system's most powerful known volcano, exhibits large expanses of dark, cooling lava on its caldera floor. Prometheus, the site of long-lived plume activity, has two major areas of thermal emission, which support ideas of plume migration. Sulfur dioxide deposits were mapped at local scales and show a more complex relationship to surface colors than previously thought, indicating the presence of other sulfur compounds.<\/jats:p>","DOI":"10.1126\/science.288.5469.1201","type":"journal-article","created":{"date-parts":[[2002,7,27]],"date-time":"2002-07-27T09:40:21Z","timestamp":1027762821000},"page":"1201-1204","source":"Crossref","is-referenced-by-count":67,"title":["A Close-Up Look at Io from Galileo's Near-Infrared Mapping Spectrometer"],"prefix":"10.1126","volume":"288","author":[{"given":"Rosaly","family":"Lopes-Gautier","sequence":"first","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"S.","family":"Doute\u0301","sequence":"additional","affiliation":[{"name":"IGPP, University of California, Los Angeles, CA 90095, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"W. D.","family":"Smythe","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"L. W.","family":"Kamp","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"R. W.","family":"Carlson","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"A. G.","family":"Davies","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"F. E.","family":"Leader","sequence":"additional","affiliation":[{"name":"IGPP, University of California, Los Angeles, CA 90095, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"A. S.","family":"McEwen","sequence":"additional","affiliation":[{"name":"Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"P. E.","family":"Geissler","sequence":"additional","affiliation":[{"name":"Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"S. W.","family":"Kieffer","sequence":"additional","affiliation":[{"name":"S. W. Kieffer Science Consulting Inc., 6 Queen Street, Suite 206, Post Office Box 520, Bolton, ON L7E 5T4 Canada."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"L.","family":"Keszthelyi","sequence":"additional","affiliation":[{"name":"Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"E.","family":"Barbinis","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"R.","family":"Mehlman","sequence":"additional","affiliation":[{"name":"IGPP, University of California, Los Angeles, CA 90095, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"M.","family":"Segura","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"J.","family":"Shirley","sequence":"additional","affiliation":[{"name":"Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]},{"given":"L. A.","family":"Soderblom","sequence":"additional","affiliation":[{"name":"U.S. Geological Survey, Flagstaff, AZ 86001, USA."}],"role":[{"role":"author","vocabulary":"crossref"}]}],"member":"221","reference":[{"key":"e_1_3_1_2_2","doi-asserted-by":"publisher","DOI":"10.1006\/icar.1999.6129"},{"key":"e_1_3_1_3_2","doi-asserted-by":"publisher","DOI":"10.1029\/97GL02609"},{"key":"e_1_3_1_4_2","unstructured":"S. Dout\u00e9 et al. in preparation."},{"key":"e_1_3_1_5_2","doi-asserted-by":"publisher","DOI":"10.1006\/icar.1999.6128"},{"key":"e_1_3_1_6_2","unstructured":"R. G. Strom and N. M. Schneider in Satellites of Jupiter D. Morrison Ed. (Univ. of Arizona Press Tucson AZ 1982) pp. 598\u2013633 and references therein."},{"key":"e_1_3_1_7_2","unstructured":"Web fig. 1 is available at www.sciencemag.org\/feature\/data\/1049493.shl"},{"key":"e_1_3_1_8_2","unstructured":"A. G. Davies et al. Lunar Planet. Sci. XXX (1999) [CD-ROM]."},{"key":"e_1_3_1_9_2","unstructured":"The brightness temperature T B is defined as B(\u03bb T B ) = I (\u03bb) where B is the Planck function \u03bb is the wavelength and I is the corrected radiance. The corrected radiance is defined as I (\u03bb) = I o (\u03bb) \u2013 A * F (\u03bb) where I o (\u03bb) is the observed radiance F (\u03bb) is incident solar flux at that wavelength and A is an albedo estimate derived from the 1- to 2-\u03bcm region. For nightside observations I = I o . The color temperature T C is defined as B(\u03bb 1 T C )\/B(\u03bb 2 T C ) = I (\u03bb 1 )\/ I (\u03bb 2 ). We used two pairs of (\u03bb 1 \u03bb 2 ): (4.1 4.4 \u03bcm) and (4.4 4.7 \u03bcm). The reported T C is the average between the two values. In dayside observations T B and in particular T C are sensitive to the albedo used to correct the observed radiances both in absolute value and its spectral slope (due to the SO 2 absorption at 4.1 \u03bcm). Therefore calculations are made using a range of albedos typically 60 to 80% of the value obtained at short wavelengths. The results are then averaged. Results displaying a high sensitivity to this variation (typically when T B < 200 K) are omitted as are those in which the error between the two estimates of T C exceeds 20% of the mean. T C is only calculated for pixels in which T B exceeds a threshold (usually 210 to 250 K depending on the noise level) to avoid errors due to the SO 2 absorption since this absorption disappears at hot spots. Correct albedo values should yield I (\u03bb) = 0 for the cold areas of Io. Small residual uncertainties in the NIMS calibration can sometimes yield a spurious T B \u223c 180 K for these areas but pixels where T B < 200 K were not used in this analysis."},{"key":"e_1_3_1_10_2","unstructured":"The relative band depth is defined as the ratio [A(3.0)\/A(4.1)] where A(\u03bb) is the measured albedo (reflectance) at wavelength \u03bb. This ratio was not obtained for pixels in which thermal emission could be detected."},{"key":"e_1_3_1_11_2","doi-asserted-by":"publisher","DOI":"10.1006\/icar.1994.1135"},{"key":"e_1_3_1_11_3","doi-asserted-by":"crossref","unstructured":"; B. Schmitt et al. in Solar System Ices B. Schmitt C. De Bergh M. Festou Eds. (Kluwer Academic Dordrecht Netherlands 1998) pp. 199\u2013240.","DOI":"10.1007\/978-94-011-5252-5_9"},{"key":"e_1_3_1_12_2","unstructured":"We have checked and quantitatively calibrated this simple approach (segregated mixing and linear combination of computed radiances) by comparing the relative band depth map of a global observation taken in I24 with the SO 2 distribution maps of S. Dout\u00e9 et al. (3) which modeled 408-wavelength NIMS spectra."},{"key":"e_1_3_1_13_2","doi-asserted-by":"publisher","DOI":"10.1126\/science.288.5469.1208"},{"key":"e_1_3_1_14_2","unstructured":"Times calculated using the model of A. G. Davies [ Icarus 124 45 (1996)]. These temperatures and cooling rates assume that the surface heat loss is buffered by the release of latent heat from a still-molten flow interior."},{"key":"e_1_3_1_15_2","unstructured":"R. Howell et al. Lunar Planet. Sci. XXXI (2000) [CD-ROM]."},{"key":"e_1_3_1_16_2","doi-asserted-by":"publisher","DOI":"10.1126\/science.288.5469.1193"},{"key":"e_1_3_1_17_2","doi-asserted-by":"publisher","DOI":"10.1126\/science.281.5373.87"},{"key":"e_1_3_1_18_2","doi-asserted-by":"publisher","DOI":"10.1006\/icar.1998.5972"},{"key":"e_1_3_1_19_2","doi-asserted-by":"publisher","DOI":"10.1126\/science.288.5469.1204"},{"key":"e_1_3_1_20_2","unstructured":"Previously undetected hot spots detected by NIMS during I24 and I25 are located at (+21 146W near Surya) (+14 150 W) (+20 149W) (+12 158W near Chaac) (\u20135 132W the dark feature Seth) and (+9 133W)"},{"key":"e_1_3_1_21_2","unstructured":"J. C. Pearl and W. M. Sinton in (5) pp. 724\u2013755."},{"key":"e_1_3_1_22_2","doi-asserted-by":"publisher","DOI":"10.1006\/icar.1996.5670"},{"key":"e_1_3_1_23_2","unstructured":"The pixel size in NIMS-processed images is 0.5\u00d7 the instrument's spatial resolution."},{"key":"e_1_3_1_24_2","unstructured":"Portions of this work were performed at the Jet Propulsion Laboratory California Institute of Technology under contract with NASA."}],"container-title":["Science"],"original-title":[],"language":"en","link":[{"URL":"https:\/\/www.science.org\/doi\/pdf\/10.1126\/science.288.5469.1201","content-type":"unspecified","content-version":"vor","intended-application":"similarity-checking"}],"deposited":{"date-parts":[[2024,1,13]],"date-time":"2024-01-13T10:07:50Z","timestamp":1705140470000},"score":1,"resource":{"primary":{"URL":"https:\/\/www.science.org\/doi\/10.1126\/science.288.5469.1201"}},"subtitle":[],"short-title":[],"issued":{"date-parts":[[2000,5,19]]},"references-count":24,"journal-issue":{"issue":"5469","published-print":{"date-parts":[[2000,5,19]]}},"alternative-id":["10.1126\/science.288.5469.1201"],"URL":"https:\/\/doi.org\/10.1126\/science.288.5469.1201","relation":{},"ISSN":["0036-8075","1095-9203"],"issn-type":[{"value":"0036-8075","type":"print"},{"value":"1095-9203","type":"electronic"}],"subject":[],"published":{"date-parts":[[2000,5,19]]}}}