3- TO 14-ΜM SPECTROSCOPY OF COMET C/1999 T1 (MCNAUGHT-HARTLEY)
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Icarus 159, 234–238 (2002)
doi:10.1006/icar.2002.6882
3- to 14-µm Spectroscopy of Comet C/1999 T1 (McNaught–Hartley)
David K. Lynch1 and Ray W. Russell1
The Aerospace Corporation, M2/266, P.O. Box 92957, Los Angeles, California 90009
E-mail: david.k.lynch@aero.org
and
Michael L. Sitko1
Department of Physics, University of Cincinnati, Cincinnati, Ohio 45221-0011
Received November 2, 2001; revised March 4, 2002
Viewed from a distance, the Sun would have a weak and prob-
We report spectroscopy of Comet C/1991 T1 (McNaught– ably undetectable IR excess with current instruments (Leger
Hartley) at 3–13 µm on January 31.62 and February 1.7 2001 UT et al. 1996, Angel and Woolf 1997.) The Oort and Kuiper belts
(delta = 1.29 AU, r = 1.40 AU) using the broadband array spectro- are nonetheless key components of our Sun’s disk because
graph system on the IRTF. The spectrum showed a silicate emission ejected comet dust is thought to produce a significant part of
feature extending about 20% above the continuum. Two emission the zodiacal dust.
features at 10.3 and 11.2 µm appeared above the silicate band, the Comets themselves were surely formed in the outer reaches
latter seemingly indicative of crystalline olivine. The 10.3-µm fea-
of the Solar System. This is evident from their composition of
ture is only a 1–2 sigma detection but if real could indicate the
lighter elements and volatiles, in parallel with the outer plan-
presence of hydrated silicates. The color temperature at 8–13 µm
was 260 ± 10 K, approximately 6% above the blackbody radiative ets. Though composed mostly of water ice, they have a compo-
equilibrium temperature of 235 K. The magnitude at [N] was 3.13 ± nent of nonvolatile dust. The dust particles range from less than
0.02. On the second night, the comet had brightened slightly ([N] = a micrometer to many tens or hundreds of micrometers. This
2.98 ± 0.02) and the two prominent emission features were absent, is known from the spectral structure seen in the infrared (e.g.,
although the silicate emission feature maintained its trapezoidal Hanner et al. 1994).
shape with shoulders at 9.5 and 11.2 µm. c 2002 Elsevier Science (USA) And yet, we still do not know the precise composition of comet
Key Words: comets, composition; comets, origin; infrared obser- dust. IR spectroscopy has provided strong evidence of silicate
vations; interplanetary dust; spectrophotometry. minerals since the early 1970s and the dust collectors from the
comet fly-bys in the 1980s did indeed find the in situ atomic
building blocks of Fe, Mg, Si, O, etc. (Kissel et al. 1986a,b). By
collecting interplanetary dust particles (Bradley 1984, Sanford
I. INTRODUCTION and Walker 1985, Bradley et al. 1992, Brownlee et al. 1993),
we have a chance to look closely at what may be actual dust
With the growing number of disks (Aumann 1988, Knacke particles from a comet. These have exhibited a wide variety of
et al. 1993, Beckwith and Sargent 1996, Backman et al. 1997), compositions, many of them unexpected, such as FeS (Bradley
planets (Mayor and Queloz 1995, Marcy and Butler 1996, Butler 1995), but most of them were siliceous at heart and frequently
and Marcy 1996), and possibly even comets (Grady et al. 1997, amorphous or “glassy.”
2000) discovered around solar-type stars, the understanding of In the roughly 25 years since it has been possible to obtain
comets in our own Solar System has become key to interpret- 10-µm spectra of comets, it has become clear that while there
ing these observations. Our Oort and Kuiper belts represent are many aspects of comet dust that are similar, all comets are
remnants of a disk left over from the Solar System’s forma- different. Some are quiescent and show no silicates; others are
tion and their relative sparseness presumably represents an ad- active and the silicate feature changes, often within hours, which
vanced, though probably normal, stage in the disk’s evolution. is indicative of an inhomogeneous composition or particle size
distribution or both. Our best hope in identifying the types of
1 Visiting Astronomer, NASA Infrared Telescope Facility, operated by the dust and paving the way toward understanding their role in the
University of Hawaii under contract with the National Aeronautics and Space Solar System is to observe these rare bodies as often as possible.
Administration. In 1999, one such comet was discovered.
234
0019-1035/02 $35.00
c 2002 Elsevier Science (USA)
All rights reserved.INFRARED SPECTROSCOPY OF COMET C/1999 T1 235
Comet C/1999 T1 was discovered by McNaught and Hartley
(1999) on October 7.64, 1999. It is a long-period (P ∼ 300,000
years), high-inclination (80◦ ) comet that reached perihelion on
December 14, 2000, and passed closest to Earth on February
2, 2001. In this paper we report and discuss spectra of Comet
C/1999 T1 (McNaught–Hartley) at 3–13 µm about a month and
a half after perihelion, when it was near its closest approach to
Earth.
II. OBSERVATIONS
The comet was observed on January 31.62 and February 1.7,
2001 UT at the NASA Infrared Telescope Facility (IRTF) on
Mauna Kea. At this time the comet was 1.4 AU from the Sun
and receding after perihelion (December 13.47, 2000). Observa-
tions were made with Aerospace’s broadband array spectrograph FIG. 2. The spectrum changed significantly in 24 h. The peaks at 10.3
system (BASS; Hackwell et al. 1990) with a 3.2-arcsecond- and 11.2 µm have disappeared. The 10-µm excess shows the now-familiar
diameter aperture, through which all wavelengths are measured trapezoidal shape with breaks at around 9.6 and 12.2 µm and the 8- to 10-µm
wing of the excess is depressed compared to the earlier spectrum. The 8- to
simultaneously.
13-µm color temperature has increased to around 280 K.
The calibration source was Sirius (α CMa) on the first night
and Arcturus (α Boo) on the second night, with α Boo being cal-
ibrated against α CMa on both nights. Both stars were observed
mean of the spectra (9 spectra with 200 s of integration each on
at about the same air mass as the comet so no extinction correc-
the first night and 12 on the second night). Also shown is the
tions were necessary. The flux model for α CMa was taken as a
260-K gray body fit to the spectrum through the regions 8 and
Planck function at 11,070 K and normalized to magnitude −1.41
13 µm. The unusually large error bars and nonconforming points
at 10 µm. For zero magnitude at all wavelengths we adopted a
between 9.3 and 9.7 µm are due to poor ozone cancellation
9700-K blackbody normalized to a value of 1.26 × 10−16 W
and little can be learned about the comet from this wavelength
cm−2 µm−1 at 10 µm.
interval.
On the first night the spectrum showed a silicate emission
III. THE SPECTRA feature extending about 20% above the gray body continuum.
Two emission features, one at 10.3 µm and the other at 11.2 µm,
Figure 1 shows the spectrum of the comet on January 31,
appeared above the silicate band. The 11.2-µm feature matched
2001. The error bars represent ±1 standard deviation of the
the wavelength and width of the olivine feature seen in many
comets (Bregman et al. 1987, Campins and Ryan 1989, Lynch
et al. 1992, Hanner et al. 1994, Wooden et al. 1999). This is
also the highest contrast that this feature has ever displayed in a
comet and resembles a true emission feature more closely than it
does a shoulder. The 10.3-µm feature is new and has never been
seen in comets before. While this appears to be a firm detection,
it is possible that it could be a statistical artifact, being only a
2-sigma finding. It does, however, appear to be composed of two
data points and not one, thereby supplying some confidence as
to its reality. It is also in a very clean and unstructured part of
the atmospheric transmission window. We cannot, however, rule
out the possibility that the feature is merely a statistical artifact
in the noise.
The comet was only marginally detected at short wavelengths
where it shone by reflected sunlight and, as a result, we were
unable to compute parameters relating to reflectivity. The L and
[N] (9.9–10.2 µm) magnitudes were 8.45 ± 0.16 and 3.13 ±
FIG. 1. The spectrum shows a silicate emission feature extending from
0.02, respectively.
roughly 8.2 to 12 µm. Two features are evident at 10.3 and 11.2 µm (the feature
at 9.7 is spurious due to poor ozone cancellation). The first peak at 10.3 µm is Figure 2 shows the spectrum of the comet on the following
weak and, if real, is new. The second one at 11.2 µm has been seen in the spectra night, February 1, 2001 (12 spectra with 200-s integrations),
of many comets before and is likely due to crystalline olivine. along with a 280-K gray body fit to the spectrum through the236 LYNCH, RUSSELL, AND SITKO
regions 8 and 13 µm. Like many comets, Comet McNaught– does not produce a peak in another part of our observable spec-
Hartley changed overnight (compare Figs. 1 and 2). In addition trum, except perhaps at 11.2 µm, where its contribution would
to brightening slightly (L and [N] were 8.18 ± 0.1 and 2.98 ± blend with and be indistinguishable from that of olivine.
0.02, respectively), the possible emission feature at 10.3 µm Comets are composed largely of water, a volatile, and it would
has disappeared and the 11.2-µm emission feature’s contrast is seem reasonable to suppose that in the warm early presolar days
somewhat diminished, leaving a shoulder at 11.2 µm. The net when comets formed or with the chemical mobility that oc-
result is a spectrum showing a trapezoidal continuum that is curs with periodic heating of a comet as it passes perihelion,
reminiscent of many comets (Hanner et al. 1994). We believe some more complex and possibly even hydrated minerals could
that the difference in the spectra between the two nights is real. be produced. The possibility that hydrated minerals could be
The seeing was fairly good on both nights and the absolute signal found in comets has been touched upon by Campins and Swindle
levels of the calibrators were the same to within 1–2%. Neither (1998) and recently H. Campins and co-workers (private com-
the 10.3-µm nor the 11.2-µm feature is in a region of signi- munication) have found a spectral feature at 2.2 µm in Comet
ficant atmospheric attenuation. The telluric opacity here is due 28P/Neujmin 1 tentatively identified as the Al–OH bond that
primarily to water vapor, and the DC levels on the sky were the resembles a feature found in smectite, a hydrated silicate. Smec-
same on the two nights to within our ability to measure them. tite does not have an emission feature that matches the 10.3-µm
The January 31 spectrum was reasonably well fit by a sin- feature.
gle Planckian gray body whose color temperature TC was 260 ± Minerals, especially hydrated minerals with cosmically abun-
10 K, about 10% above the radiative equilibrium blackbody tem- dant compositions, that have single, isolated peaks at 10.3 µm in-
perature TBB of 235 K (=278/R 1/2 K) for a perfect blackbody clude natrolite [Na2 (Al2 Si3 O10 ) · 2H2 O], hackmanite [Na4 Al3 S
at a distance of R = 1.4 AU from the Sun. On the next night the (SiO4 )3 Cl], and sodalite (Na4 Al3 Si3 O12 Cl). Probably less likely
color temperature was 280 ± 10 K but owing to the increased but nonetheless spectrally similar minerals include crocidolite
water vapor that night, uncertainty in the 8-µm point raises the [Na2 Fe2+ 3 Fe3+ 2 Si8 O22 (OH)2 ], and carpholite [MnAl2 Si2 O6
error bars to ±25 K. Thus we could not be certain that any real (OH)4 ]. The features in both sodalite and natrolite are somewhat
change in the color temperature occurred between the two nights. wider than the 10.3-µm feature we report and are not at precisely
To the extent to which the “nonsilicate” continuum can be the same wavelength. In view of the fact that feature shapes and
characterized by a gray body that passes through the 8- and locations can vary according to particle size, we would not want
13-µm parts of the spectrum (Fig. 2), two aspects of the silicate to rule these out as candidate minerals. We caution, however,
emission can be seen: (1) It comes up slowly from around 8 µm that these possible identifications are based on a single spectral
and contains no features until the 10.3-µm feature, which itself feature.
begins to rise at around 10.1 µm., and (2) After the 11.2-µm
olivine feature, the silicate emission drops rapidly and essen-
V. THE COMET–DISK CONNECTION
tially disappears by 12 µm.
In the past few years, there has been a growing understanding
IV. POSSIBLE ORIGIN OF THE 10.3-µm FEATURE of the mineralogical and chemical connection between comets
and circumstellar disks, especially in young stars. Such a con-
The first possibility is that both peaks were produced by the nection is not, perhaps, unexpected because current thinking
same mineral. The likeliest candidates are those already be- suggests that comets either are a component of circumstellar
lieved to have been identified in comets: olivine and pyroxene disks or are one possible end product of the disks’ evolution. The
(Wooden et al. 1999). Both produce two features at about the most compelling chemical connection is found in the optical and
right wavelengths but neither mineral seems likely to be able to UV spectra of certain main sequence stars where there are rapid
produce a peak at precisely 10.3 µm. In most spectra their short- variations in absorption line spectra of neutral and singly ionized
wavelength peak is closer to 10.1 µm. Thus we can tentatively species (Grady et al. 2000). These rapid changes are most easily
rule out both minerals as the source of both features with one interpreted as follows: Comets that are falling into or passing
caveat: Both are actually “mineral groups” with a common un- close to the star begin to evaporate; as the molecules and miner-
derlying structure but with significant compositional and molec- als dissociate into their individual atomic components, it is these
ular disorder variations under the same name. When these varia- components that we are seeing in absorption. To cause hourly
tions are taken with the effects of particle size, there are usually or daily spectral variations, such stars must have a dynamic and
small but significant wavelength shifts that could account for the very extensive comet cloud.
10.3-µm feature. Such effects can be easily seen by looking at The other piece of evidence linking comets and disks together
spectra of the same mineral at different particle sizes. is found in their 10-µm spectra, such as the ones shown in Figs. 1
The other possibility is that two different minerals are respon- and 2. The silicate feature, at least in its unstructured form, has
sible for the two peaks, one for each. If we accept that olivine is been long known in both comets and circumstellar shells, but re-
producing the 11.2-µm peak, then we must find a mineral which cent advances in spectral resolution in the 10-µm window have
(1) produces a peak at 10.3 µm and with a suitable width and (2) allowed us to parse the silicate feature and discern narrower,INFRARED SPECTROSCOPY OF COMET C/1999 T1 237
ACKNOWLEDGMENTS
We are grateful to Dave Griep at the IRTF for expert telescope operation and
to Daryl Kim and Suellen Brafford for help in obtaining the observations. This
work was supported by the Aerospace Corporation’s Independent Research and
Development program and by the United States Air Force Space and Missile
Systems Center through the Mission Oriented Investigation and Experimentation
program, under Contract F4701-00-C-0009. The data shown in Figs. 1 and 2 are
available from the author as digital ASCII (text only) files.
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