Subaru telescope observations of Deep Impact

Science

Volumn 310, Issue 5746, 2005, Pages 274-278

  Sugita, S ^a,b,c   Ootsubo, T ^d   Kadono, T ^a,e   Honda, M ^b   Sako, S ^a   Miyata, T ^a   Sakon, I ^a   Yamashita, T ^f   Kawakita, H ^g   Fujiwara, H ^a   Fujiyoshi, T ^f   Takato, N ^f   Fuse, T ^f   Watanabe, J ^f   Furusho, R ^h   Hasegawa, S ^b   Kasuga, T ^f   Sekiguchi, T ^f   Kinoshita, D ⁱ   Meech, K J ^j   Wooden, D H ^k   Ip, W H ⁱ   A'Hearn, M F ^l   more..

^a UNIVERSITY OF TOKYO   (Japan)

^b JAPAN AEROSPACE EXPLORATION AGENCY   (Japan)

^c BROWN UNIVERSITY   (United States)

^d NAGOYA UNIVERSITY   (Japan)

^e JAPAN AGENCY FOR MARINE EARTH SCIENCE AND TECHNOLOGY   (Japan)

^f NATIONAL ASTRONOMICAL OBSERVATORY OF JAPAN   (Japan)

^g KYOTO SANGYO UNIVERSITY   (Japan)

^h WASEDA UNIVERSITY   (Japan)

ⁱ NATIONAL CENTRAL UNIVERSITY   (Taiwan)

^j UNIVERSITY OF HAWAII   (United States)

^k NASA AMES RESEARCH CENTER   (United States)

^l UNIVERSITY OF MARYLAND   (United States)

more..

Author keywords

[No Author keywords available]

Indexed keywords

DUST; INFRARED DEVICES; PLANETS; SPECTROMETERS; TELESCOPES; TEMPERATURE INDICATING CAMERAS;

COMETS; COOLED MID-INFRARED CAMERA AND SPECTROMETER (COMICS); IMPACT CRATERING PROCESS; SUBARU TELESCOPES;

ASTROPHYSICS;

COMET;

ARTICLE; ASTRONOMY; COLLISION; COMET; COMET 9P/TEMPEL 1; COOLED MID INFRARED CAMERA AND SPECTROMETER; DEEP IMPACT PROGRAM; DEVICE; DUST; EVAPORATION; GRAVITY; IMPACT CRATERING PROCESS; METEOROLOGICAL PHENOMENA; METEOROLOGY; PRIORITY JOURNAL; PROCESS DESIGN; QUANTITATIVE ANALYSIS; REMOTE SENSING; SPACE FLIGHT; SPECTROMETER; TELESCOPE;

COSMIC DUST; JUPITER; METEOROIDS; SPECTROPHOTOMETRY, INFRARED; VOLATILIZATION;

EID: 26844437430     PISSN: 00368075     EISSN: 10959203     Source Type: Journal    
DOI: 10.1126/science.1119091     Document Type: Article

References (31)

1. Observation was conducted for four nights on UT 2 to 5 July 2005. In particular, observation on UT 4 July 2005 was conducted in coordination with the Gemini telescope in order to obtain data complementary to each other (13).
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5. Materials and methods are available as supporting material on Science Online.
6. The scale for the COMICS imaging mode is 0.130″ per pixel. This corresponds to 84.2 km/pixel on the surface of comet 9P/Tempel 1.
7. The cooling of impact-generated heat is not expected to contribute significantly to the decrease in light flux. The radiative cooling time scale for 10-μm size silicate particles from 1000 K to 200 K is on the order of a minute, much shorter than the observation time scale of this study.
8. The observed data do not rule out a minor dust supply from the surface, which has a total dust production much smaller than the total dust amount in the plume.
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12. The porosity of amorphous grains is given by fractal dimension D. The porosity increases as a function of size when D < 3. The porosity of crystalline grains is assumed to be zero (i.e., D = 3).
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17. Because most of the light in the 10-μm emission peak comes from the smallest grains (sub-μm to μm), the smallest grains can account for the magnitude of the observed 10-μm peak light flux. The observed N-band spectral shape of the 10-μm peak, however, cannot be reproduced well with the smallest grains only and requires larger grains. The synthetic spectral shape improves gradually as the maximum grain size is increased to 10 μm. In contrast, when the maximum size is increased to significantly larger than 10 μm, the synthetic spectrum neither improves nor deteriorates. Thus, N-band spectroscopy cannot constrain the size distribution of dust larger than 10 μm. This is because these large grains do not contribute to the silicate feature around the 10-μm wavelength (9, 70).
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31. This report is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan (allocation nos. S05A-042 and S05A-OT11). This research is partially supported by a Grant in Aid from the Japan Society for the Promotion of Science.