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Near-Infrared Spectral Monitoring of Pluto's Ices: Spatial Distribution and Secular Evolution

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Near-Infrared Spectral Monitoring of Pluto's Ices: Spatial Distribution and Secular Evolution Near-Infrared Spectral Monitoring of Pluto's Ices: Spatial Distribution and Secular Evolution W.M. Grundy1,2, C.B. Olkin2,3, L.A. Young2,3, M.W. Buie2,3, and E.F. Young2,3. 1. Lowell Observatory, 1400 W. Mars Hill Rd., Flagstaff AZ 86001. 2. Visiting or remote observer at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NNX-08AE38A with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. 3. Southwest Research Institute, 1050 Walnut St. #300, Boulder CO 80302. Ð Published in 2013 in Icarus Vol. 223, pp. 710-721 Ð ABSTRACT We report results from monitoring Pluto's 0.8 to 2.4 µm reflectance spectrum with IRTF/SpeX on 65 nights over the dozen years from 2001 to 2012. The spectra show vibrational absorption features of simple molecules CH4, CO, and N2 condensed as ices on Pluto's surface. These absorptions are modulated by the planet's 6.39 day rotation period, enabling us to constrain the longitudinal distributions of the three ices. Absorptions of CO and N2 are concentrated on Pluto's anti-Charon hemisphere, unlike absorptions of less volatile CH4 ice that are offset by roughly 90° from the longitude of maximum CO and N2 absorption. In addition to the diurnal variations, the spectra show longer term trends. On decadal timescales, Pluto's stronger CH4 ab- sorption bands have been getting deeper, while the amplitude of their diurnal variation is dimin- ishing, consistent with additional CH4 absorption at high northern latitudes rotating into view as the sub-Earth latitude moves north (as defined by the system's angular momentum vector). Un- like the CH4 absorptions, Pluto's CO and N2 absorptions appear to be declining over time, sug- gesting more equatorial or southerly distributions of those species. Comparisons of geometri- cally-matched pairs of observations favor geometric explanations for the observed secular changes in CO and N2 absorption, although seasonal volatile transport could be at least partly re- sponsible. The case for a volatile transport contribution to the secular evolution looks strongest for CH4 ice, despite it being the least volatile of the three ices. 1 1. Introduction Reflectance spectroscopy has had a remarkable record of revealing the surface composi- tions of icy solar system bodies, ranging from satellites of the four giant planets to icy dwarf planets beyond Neptune's orbit (see reviews by Cruikshank et al. 1998a,b; Clark et al. 2013; and de Bergh et al. 2013; and references therein). In addition to nearly ubiquitous water ice, more ex- otic ices of methane, ethane, nitrogen, oxygen, hydrogen cyanide, ammonia, carbon monoxide, carbon dioxide, and sulfur dioxide have been identified on outer solar system bodies from their characteristic patterns of absorption bands imprinted on visible to infrared reflectance spectra. Several of these ices are highly volatile (e.g., Brown and Zeigler 1980; Fray and Schmitt 2009) and could be mobilized on seasonal timescales, even at the cryogenic temperatures prevalent in the outer solar system (Hansen and Paige 1996; Spencer et al. 1997; Trafton et al. 1998; Young 2012a). In addition to discovering the existence of such ices, spectroscopy can be a powerful tool for monitoring their evolution over time. This prospect is especially enticing for Pluto's surface, where volatile N2, CH4, and CO ices are all known to exist (Owen et al. 1993; Douté et al. 1999). Having passed through both perihelion and equinox within the past few decades, Pluto's surface and atmosphere are thought to be undergoing seasonal evolution at an especially rapid pace, at least compared with aphelion. Stellar occultations indicate that the atmospheric pressure has been increasing (Elliot et al. 2003; Sicardy et al. 2003; Young 2012b and references therein) and photometric lightcurves and Hubble Space Telescope imagery show that Pluto's sur- face albedo patterns are not static (Buratti et al. 2003; Schaefer et al. 2008; Buie et al. 2010a,b). NASA's New Horizons spacecraft will return a detailed, up-close look at the system in 2015 (e.g., Young et al. 2008). Understanding how that brief snapshot fits into the broader, seasonal context is crucial for getting the most scientific understanding out of the New Horizons flyby. Various teams have been spectroscopically monitoring the Pluto system at near-infrared wavelengths to help constrain the spatial distribution and long term evolution of its surface ices (e.g., Rudy et al. 2003; Verbiscer et al. 2007; Merlin et al. 2010). From 1995 to 1998, we col- lected Pluto spectra on 83 nights at Lowell Observatory's 72" Perkins telescope (Grundy and Buie 2001). Over the past dozen years, our spectroscopic monitoring campaign has continued at NASA's InfraRed Telescope Facility (IRTF). This paper presents the ensemble of the IRTF data and discusses some patterns seen in the data. Companion papers will go into greater detail with radiative transfer models fitted to the Pluto spectra. 2. Data Acquisition and Reduction Spectra were recorded during a series of observing runs from 2001 through 2012 at NASA's 3 m IRTF, located at an altitude of 4168 m on the summit of Mauna Kea. Most observ- ing was done remotely by observers situated on the mainland as described by Bus et al. (2002), during scheduled telescope time allocations of typically two to four hours duration, although longer allocations were occasionally requested in order to obtain higher quality data. We used the short cross-dispersed mode of the SpeX spectrograph (Rayner et al. 1998, 2003). This mode divides the 0.8 to 2.4 µm wavelength range across five spectral orders, recorded on a 1024 × 1024 InSb detector array. Usable data were obtained on 65 nights, with circumstances described in Table 1. A few of the resulting spectra have been shown previously (Olkin et al. 2007; Protopapa et al. 2008; Tegler et al. 2012; plus several conference presentations), but this paper presents most of them for the first time, along with a full description of data acquisition and reduction procedures. 2 Table 1 Observational circumstances UT date of Slit H band Sub-Earth Phase Pluto observation Sky conditionsa width seeing longitudeb latitudeb angle integration mean-time (on site or remote) (″″) (″″) (°E) (°N) (°) (min) 2001/07/04 8h.98 Cirrus (HI) 0.5 1.1 196.5 27.7 0.99 120 2001/07/07 9h.20 Cirrus (HI) 0.5 1.0 26.9 27.6 1.06 147 2001/07/08 8h.30 Clear (HI) 0.5 1.1 332.7 27.6 1.09 192 2002/06/24 6h.54 Mostly clear (HI) 0.5 1.1 352.0 30.0 0.64 44 2002/06/25 6h.30 Cirrus (HI) 0.5 0.6 296.2 29.9 0.66 46 2002/06/26 6h.49 Clear (HI) 0.3 0.6 239.3 29.9 0.69 48 2002/07/15 7h.24 Clear (HI) 0.3 0.6 246.8 29.5 1.19 60 2002/07/16 7h.29 Some clouds (HI) 0.3 0.7 190.4 29.5 1.21 80 2002/07/17 6h.94 Partly cloudy (HI) 0.3 0.8 134.8 29.4 1.23 96 2002/07/18 6h.81 Thin cirrus (HI) 0.3 0.8 78.8 29.4 1.26 88 2002/07/19 7h.06 Thin cirrus (HI) 0.3 0.7 21.8 29.4 1.28 78 2002/07/20 6h.80 Thin cirrus (HI) 0.3 0.8 326.1 29.4 1.30 92 2002/07/21 6h.81 Thin cirrus (HI) 0.3 0.6 269.7 29.4 1.33 96 2002/07/22 6h.72 Clear (HI) 0.3 0.7 213.6 29.4 1.35 104 2003/08/09 6h.82 Clear (r) 0.5 0.6 225.0 31.1 1.63 96 2005/04/15 13h.15 Thin cirrus (r) 0.3 0.5 103.0 37.1 1.59 176 2005/05/09 13h.06 Mostly clear (r) 0.3 0.7 190.7 36.8 1.10 188 2005/05/23 11h.27 Heavy cirrus (r) 0.3 0.7 125.9 36.5 0.73 184 2005/05/24 12h.03 Clear (r) 0.3 0.7 67.8 36.5 0.70 268 2006/07/19 8h.32 Clear (r) 0.3 0.8 106.7 37.0 1.01 148 2006/07/24 7h.83 Heavy cirrus (r) 0.3 1.5 186.1 37.0 1.14 100 2006/07/25 7h.73 Clear (r) 0.3 1.0 130.0 36.9 1.16 160 2006/07/26 7h.71 Clear (r) 0.3 0.9 73.7 36.9 1.19 168 2006/08/08 7h.13 Thin cirrus (r) 0.3 0.5 62.4 36.7 1.47 126 2006/08/25 6h.80 Clear (r) 0.3 0.7 185.1 36.5 1.72 136 2007/06/23 10h.78 Clear (r) 0.3 0.6 72.0 39.5 0.26 32 2007/06/25 10h.66 Clear (r) 0.3 0.5 319.5 39.4 0.30 36 2007/08/06 7h.27 Clear (r) 0.5 0.7 120.7 38.5 1.36 104 2007/08/07 7h.50 Clear (r) 0.5 0.6 63.8 38.5 1.39 80 2007/08/08 7h.06 Clear (r) 0.5 0.6 8.5 38.5 1.41 108 2007/08/09 6h.90 Clear (r) 0.5 0.6 312.5 38.5 1.42 112 2007/08/10 7h.07 A little cirrus (r) 0.5 0.6 255.7 38.5 1.44 116 2007/08/11 7h.65 Clear (r) 0.5 0.7 198.0 38.5 1.46 124 3 2008/06/16 10h.99 A little cirrus (r) 0.5 0.5 355.4 41.4 0.25 52 2008/06/17 10h.94 Clear (r) 0.5 0.5 299.1 41.4 0.23 64 2008/06/18 11h.10 Cirrus (r) 0.5 0.6 242.4 41.3 0.22 34 2008/06/19 10h.63 Cirrus (r) 0.5 0.5 187.2 41.3 0.21 84 2008/06/20 10h.67 Clear (r) 0.5 0.6 130.7 41.3 0.21 60 2008/06/21 10h.68 Clear (r) 0.5 0.5 74.3 41.3 0.21 60 2009/06/18 12h.52 Clear (r) 0.5 0.8 184.8 43.0 0.24 64 2009/06/19 12h.14 Clear, humid (r) 0.5 1.1 129.3 43.0 0.22 80 2009/06/20 12h.84 Clear, humid (r) 0.5 0.9 71.3 43.0 0.20 84 2009/06/21 12h.40 Clear (r) 0.5 1.1 16.0 43.0 0.19 58 2009/06/22 12h.62 Clear (r) 0.5 0.7 319.1 42.9 0.19 88 2010/05/08 14h.11 Clear (r) 0.5 0.6 277.1 45.5 1.34 80 2010/05/28 14h.01 Some clouds (r) 0.5 1.1 230.2 45.1 0.86 64 2010/06/24 10h.52 Clear (r) 0.5 0.7 157.0 44.5 0.17 92 2010/06/25 10h.25 Clear (r) 0.5 0.5 101.3 44.5 0.16 124 2010/06/30 10h.22 Fog (r) 0.5 0.7 179.6 44.4 0.22 96 2010/07/01 9h.99 Clear (r) 0.5 0.7 123.8 44.4 0.24 112 2011/05/22 14h.77 Clear (r) 0.5 0.7 152.1 46.8 1.07 52 2011/06/01 13h.96 Clear (r) 0.3 0.8 310.5 46.6 0.81 72 2011/06/02 13h.89 Trace of clouds (r) 0.3 0.7 254.3 46.6 0.78 76 2011/06/06 14h.43 Clear (r) 0.3 0.6 27.6 46.5 0.67 64 2011/06/07 13h.91 Clear (r) 0.3 0.6 332.5 46.5 0.64 40 2011/06/11 13h.82 Clear (r) 0.3 0.5 107.3 46.4 0.53 52 2011/06/12 11h.90 Partly cloudy (r) 0.3 0.4 55.5 46.4 0.50 64 2011/07/15 9h.02 Clear (r) 0.3 0.9 2.8 45.6 0.54 64 2012/05/12 13h.51 Clear (r) 0.3 0.5 247.7 48.4 1.32 104 2012/05/13 13h.83 Clear (r) 0.3 0.6 190.6 48.4 1.30 120 2012/05/14 13h.92 Trace of cirrus (r) 0.3 0.7 134.0 48.4 1.28 92 2012/05/15 14h.04 Clear (r) 0.3 0.5 77.3 48.4 1.25 120 2012/05/16 14h.03 Clear (r) 0.3 0.6 21.0 48.4 1.23 96 2012/05/17 13h.97 Clear (r) 0.3 0.6 324.8 48.4 1.21 104 2012/09/09 6h.19 Clear (r) 0.3 0.7 342.9 46.3 1.68 40 Table notes: a.
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