Visible and near-infrared spectrophotometry of the Deep Impact ejecta of Comet 9P/Tempel 1
We have obtained optical spectrophotometry of the evolution of Comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field Spectrograph (SNIFS) at the UH 2.2-m telescope, as well as simultaneous optical and infrared spectra using the Lick Visible-to-Near-Infrared...
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Published in | Icarus (New York, N.Y. 1962) Vol. 187; no. 1; pp. 185 - 198 |
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01.03.2007
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Abstract | We have obtained optical spectrophotometry of the evolution of Comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field Spectrograph (SNIFS) at the UH 2.2-m telescope, as well as simultaneous optical and infrared spectra using the Lick Visible-to-Near-Infrared Imaging Spectrograph (VNIRIS). The spatial distribution and temporal evolution of the “violet band” CN (0–0) emission and of the 630 nm [OI] emission was studied. We found that CN emission centered on the nucleus increased in the 2 h after impact, but that this CN emission was delayed compared to the light curve of dust-scattered sunlight. The CN emission also expanded faster than the cloud of scattering dust. The emission of [OI] at 630 nm rose similarly to the scattered light, but then remained nearly constant for several hours after impact. On the day following the impact, both CN and [OI] emission concentrated on the comet nucleus had returned nearly to pre-impact levels. We have also searched for differences in the scattering properties of the dust ejected by the impact compared to the dust released under normal conditions. Compared to the pre-impact state of the comet, we find evidence that the color of the comet was slightly bluer during the post-impact rise in brightness. Long after the impact, in the following nights, the comet colors returned to their pre-impact values. This can be explained by postulating a change to a smaller particle size distribution in the ejecta cloud, in agreement with the findings from mid-infrared observations, or by postulating a large fraction of clean ice particles, or by a combination of these two. |
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AbstractList | We have obtained optical spectrophotometry of the evolution of comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field Spectrograph (SNIFS) at the UH 2.2m telescope, as well as simultaneous optical and infrared spectra using the Lick Visible-to-Near-Infrared Imaging Spectrograph (VNIRIS) spectrograph. The spatial distribution and temporal evolution of the "violet band" CN (0-0) emission and of the 630 nm [OI] emission was studied. We found that CN emission centered on the nucleus increased in the two hours after impact, but that this CN emission was delayed compared to the light curve of dust-scattered sunlight. The CN emission also expanded faster than the cloud of scattering dust. The emission of [OI] at 630 nm rose similarly to the scattered light, but then remained nearly constant for several hours after impact. On the day following the impact, both CN and [OI] emission concentrated on the comet nucleus had returned nearly to pre-impact levels. We have also searched for differences in the scattering properties of the dust ejected by the impact compared to the dust released under normal conditions. Compared to the pre-impact state of the comet, we find evidence that the color of the comet was slightly bluer during the post-impact rise in brightness. Long after the impact, in the following nights, the comet colors returned to their pre-impact values. This can be explained by postulating a change to a smaller particle size distribution in the ejecta cloud, in agreement with the findings from mid-infrared observatons, or by postulating a large fraction of clean ice particles, or by a combination of these two. We have obtained optical spectrophotometry of the evolution of Comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field Spectrograph (SNIFS) at the UH 2.2-m telescope, as well as simultaneous optical and infrared spectra using the Lick Visible-to-Near-Infrared Imaging Spectrograph (VNIRIS). The spatial distribution and temporal evolution of the “violet band” CN (0–0) emission and of the 630 nm [OI] emission was studied. We found that CN emission centered on the nucleus increased in the 2 h after impact, but that this CN emission was delayed compared to the light curve of dust-scattered sunlight. The CN emission also expanded faster than the cloud of scattering dust. The emission of [OI] at 630 nm rose similarly to the scattered light, but then remained nearly constant for several hours after impact. On the day following the impact, both CN and [OI] emission concentrated on the comet nucleus had returned nearly to pre-impact levels. We have also searched for differences in the scattering properties of the dust ejected by the impact compared to the dust released under normal conditions. Compared to the pre-impact state of the comet, we find evidence that the color of the comet was slightly bluer during the post-impact rise in brightness. Long after the impact, in the following nights, the comet colors returned to their pre-impact values. This can be explained by postulating a change to a smaller particle size distribution in the ejecta cloud, in agreement with the findings from mid-infrared observations, or by postulating a large fraction of clean ice particles, or by a combination of these two. |
Author | Blanc, Nathalie Lynch, David K. Cochran, Anita L. Chickering, William Aldering, Greg Antilogus, Pierre Copin, Yannick Rudy, Richard J. Puetter, Richard C. Pécontal, Emmanuel Mazuk, S. Venturini, Catherine C. Perry, Raleigh B. Hodapp, Klaus W. Meech, Karen J. |
Author_xml | – sequence: 1 givenname: Klaus W. surname: Hodapp fullname: Hodapp, Klaus W. email: hodapp@ifa.hawaii.edu organization: Institute for Astronomy, University of Hawaii, 640 N. Aohoku Place, Hilo, HI 96720, USA – sequence: 2 givenname: Greg surname: Aldering fullname: Aldering, Greg organization: Lawrence Berkeley Lab, Physics Div., MS-50/232, One Cyclotron Rd., Berkeley, CA 94720, USA – sequence: 3 givenname: Karen J. surname: Meech fullname: Meech, Karen J. organization: Institute for Astronomy, University of Hawaii, and NASA Astrobiology Institute, 2680 Woodlawn Drive, Honolulu, HI 96822, USA – sequence: 4 givenname: Anita L. surname: Cochran fullname: Cochran, Anita L. organization: McDonald Observatory, University of Texas at Austin, 1 University Station C1402, Austin, TX 78712-0259, USA – sequence: 5 givenname: Pierre surname: Antilogus fullname: Antilogus, Pierre organization: Laboratoire de Physique Nucléaire et des Hautes Energies, IN2P3 - CNRS, Universités Paris VI et Paris VII, 4 Place Jussieu Tour 33 - Rez des chaussée, 75252 Paris Cedex 05, France – sequence: 6 givenname: Emmanuel surname: Pécontal fullname: Pécontal, Emmanuel organization: Centre de Recherche Astronomique de Lyon, 9, av. Charles André, 69561 Saint Genis Laval Cedex, France – sequence: 7 givenname: William surname: Chickering fullname: Chickering, William organization: Lawrence Berkeley Lab, Physics Div., MS-50/232, One Cyclotron Rd., Berkeley, CA 94720, USA – sequence: 8 givenname: Nathalie surname: Blanc fullname: Blanc, Nathalie organization: Institut de Physique Nucleéaire de Lyon, UMR5822, CNRS-IN2P3, Université Claude Bernard Lyon 1, F-69622 Villeurbanne, France – sequence: 9 givenname: Yannick surname: Copin fullname: Copin, Yannick organization: Institut de Physique Nucleéaire de Lyon, UMR5822, CNRS-IN2P3, Université Claude Bernard Lyon 1, F-69622 Villeurbanne, France – sequence: 10 givenname: David K. surname: Lynch fullname: Lynch, David K. organization: The Aerospace Corporation, P.O. Box 92957, MS 266, Los Angeles, CA 90009, USA – sequence: 11 givenname: Richard J. surname: Rudy fullname: Rudy, Richard J. organization: The Aerospace Corporation, P.O. Box 92957, MS 266, Los Angeles, CA 90009, USA – sequence: 12 givenname: S. surname: Mazuk fullname: Mazuk, S. organization: The Aerospace Corporation, P.O. Box 92957, MS 266, Los Angeles, CA 90009, USA – sequence: 13 givenname: Catherine C. surname: Venturini fullname: Venturini, Catherine C. organization: The Aerospace Corporation, P.O. Box 92957, MS 266, Los Angeles, CA 90009, USA – sequence: 14 givenname: Richard C. surname: Puetter fullname: Puetter, Richard C. organization: University of California, San Diego, CASS 0424, 9500 Gilman Dr., La Jolla, San Diego, CA 92093, USA – sequence: 15 givenname: Raleigh B. surname: Perry fullname: Perry, Raleigh B. organization: NASA Langley Research Center, MS 160, Science Support Office, Hampton, VA 23681, USA |
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Snippet | We have obtained optical spectrophotometry of the evolution of Comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field... We have obtained optical spectrophotometry of the evolution of comet 9P/Tempel 1 after the impact of the Deep Impact probe, using the Supernova Integral Field... |
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SubjectTerms | Astrophysics Comet Tempel 1 Comets Cosmology and Extra-Galactic Astrophysics Photometry Physics Sciences of the Universe Spectroscopy |
Title | Visible and near-infrared spectrophotometry of the Deep Impact ejecta of Comet 9P/Tempel 1 |
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