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1
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1842386154
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note
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We used the Danish Faint Object Spectrograph (DFOSC), a focal reducer-type instrument which allowed us to switch between spectra (3700 to 7000 Å; resolution: April and June: 15 Å, August and October: 18 Å), and imaging. The field-of-view was ≈13 arc min. The slit was aligned with the sun-comet axis.
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2
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1842263745
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note
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2]. Filter no. 510 at 4467 Å (band width 56 Å) has been used for continuum subtraction.
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3
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1842391039
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note
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We used the medium-resolution spectrograph CARELEC in the range 3600 to 6800 Å (resolution: 7 Å). The slit length was 5 arc min. Spectra were taken with different slit orientations and averages obtained from these spectra.
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5
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1842310055
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in preparation
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Z. Sekanina and H. Boehnhardt, IAU Circular 6542 (1997); M. R. Kidger et al., in preparation.
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Kidger, M.R.1
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7
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0000837742
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M. F. A'Hearn et al., Astron. J. 89 579 (1984). Here, A is the albedo, f is the filling factor (ratio between total cross section of grains and area of the field of view), and ρ is the radius of the circular field of view.
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A'Hearn, M.F.1
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8
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0000018874
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h. To correct for the dependence of magnitude on phase angle, a factor of 0.03 mag/degree was used, as measured in comet Bowell at 3.7 to 5.6 AU. [R. L. Newburn and H. Spinrad, Astron. J. 90, 2591, (1985); J. F. Crifo, Astron. Astrophys. 187, 438, (1987); K. Meech and D. Jewitt, ibid., p. 585.
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Newburn, R.L.1
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9
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0000074230
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h. To correct for the dependence of magnitude on phase angle, a factor of 0.03 mag/degree was used, as measured in comet Bowell at 3.7 to 5.6 AU. [R. L. Newburn and H. Spinrad, Astron. J. 90, 2591, (1985); J. F. Crifo, Astron. Astrophys. 187, 438, (1987); K. Meech and D. Jewitt, ibid., p. 585.
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Crifo, J.F.1
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10
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26544442432
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h. To correct for the dependence of magnitude on phase angle, a factor of 0.03 mag/degree was used, as measured in comet Bowell at 3.7 to 5.6 AU. [R. L. Newburn and H. Spinrad, Astron. J. 90, 2591, (1985); J. F. Crifo, Astron. Astrophys. 187, 438, (1987); K. Meech and D. Jewitt, ibid., p. 585.
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Astron. Astrophys.
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Meech, K.1
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11
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R. L. Newburn, M. Neugebauer, J. Rahe, Eds. Kluwer, Dordrecht
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Jewitt, D.1
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14
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1842381337
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National Solar Observatory
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All spectra were bias-subtracted, flatfielded, and extinction-corrected. The contribution from the night sky was determined from separate sky exposures. Variability in intensity of the [OI] emission at 5577 Å led to under-and oversubtraction in some cases. The underlying continuum of solar light reflected by the cometary dust was subtracted using a solar atlas [R. L. Kurucz et al., Sunspot, National Solar Observatory, (1984)] smoothed to the resolution of the cometary spectra, or using spectra of jovian satellites, when possible. Absolute calibration was performed using standard stars observed on the same night.
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Sunspot
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Kurucz, R.L.1
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18
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N. Biver et al., Nature 380, 137 (1996); D. Jewitt, M. Senay, H. Matthews, Science 271, 1110 (1996).
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1842268626
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note
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3 from (8), for CN from: D. Schleicher, thesis, University of Maryland (1983); others from (22).
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Irvine, W.M.1
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1842400771
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This paper is based on observations at the European Southern Observatory (ESO), Chile (prop. 57.F-0396), and the Observatoire de Haute Provence, France. We gratefully acknowledge the collaboration with members of the ESO ROSETTA/ISO target comets imaging team in the context of their observing programs at ESO [57.F-0274, 58.F-0431 (ESO time)], whose members are H. Boehnhardt, L. Colangeli, G. Cremonese, J. Crovisier, M. Fulle, L. Jorda, H. Rauer, H. Rickman, R. Schulz, G. Schwehm, and R. M. West. We thank also V. Buat and D. Burgarella, who gave us some of their observing time. H.R. acknowledges the support of an European Space Agency external research fellowship.
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