Pluto

@ARTICLE{asteriks,
               author = {{Hedges}, C. and Co},
                title = "{}",
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            archivePrefix = "arXiv",
               eprint = {},
             primaryClass = "",
             keywords = {},
                 year = ,
                month = ,
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                pages = {},
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@MISC{2014ktwo.propGO7012,
	author = {{Benecchi}, B. and {Schwamb}, S. and {Binzel}, B. and {Lisse}, L.},
	title = {The Lightcurve of Pluto Post New Horizons},
	abstract = {Discovered in 1930, Pluto is a unique dwarf planet that has chal
		lenged and inspired the minds of many. It is a key object in the
		 third zone out from our Sun and provides important insight to f
		ormation and collisional processes that were at work in the orig
		inal solar nebula. In July 2015 the New Horizons spacecraft (a N
		ASA mission) will encounter this small, dark, icy world and the 
		family of objects that orbit it providing a once-in-a-lifetime o
		pportunity to directly link our Earth-based view of Pluto with g
		round truth provided by in situ measurements. However, this enco
		unter will be short-lived compared to other planetary voyages be
		cause it is unfeasible to slow the spacecraft down to orbit with
		in the Pluto system; instead this visit will be a flyby. Studies
		 from Earth-based or Earth-orbit facilities prior to and post en
		counter will provide critical baseline and context information f
		or optimal interpretation of the valuable flyby science data. Pl
		uto is known to be a constantly changing world due to the solar 
		energy being received decreasing by ~2% per year on account of i
		ts eccentric orbit now carrying it rapidly away from perihelion.
		  Whats more, the orientation of Pluto's spin axis and the sub-s
		olar latitude (the height of the "midday Sun") changes by more t
		han 1 degree per Earth year, bringing 100,000 square kilometers 
		of new surface area into sunlight for the first time in a centur
		y (while casting an equal and opposite polar area into a century
		 long arctic winter). These orbit-related effects on the atmosph
		ere and surface of Pluto are on top of the well-known longitudin
		al variations measurable over the course Plutos 6.387 day rotati
		on. Observations of Pluto one year prior-to and post-flyby will 
		allow us to identify evolving trends in the system which could b
		e missed if we focused on only the flyby dataset. Our ultimate g
		oal is to better understand Pluto, its family of satellites and 
		their evolution since formation. We propose to observe the Pluto
		 system, which is on silicon in the selected Campaign 7 K2 field
		. These observations will take place after New Horizons has comp
		leted its flyby and will provide a key baseline of photometric o
		bservations that are not available from ground-based observatori
		es because of Pluto's position relative to Sun during the timefr
		ame of this campaign (Oct-Dec 2015).  Pluto is relatively bright
		, MV~14, but not overly bright, so it is an ideal object for the
		 K2 set-up. The positional uncertainty of Pluto over the observi
		ng period is less than a Kepler pixel providing starlike PRFs in
		 a single K2 observation. Therefore, monitoring Pluto, which mov
		es only a few arcminutes per night, requires a target pixel mask
		 over its path on the FOV. Pluto's rotation period is 6.387 days
		 so the collected 30-min integration "long cadence" datapoints w
		ill provide measurements of nearly 12 full rotations of Pluto an
		d its companions. Likewise, the 3-month baseline also allows us 
		to sample seasonal variations and solar phase angles ranging fro
		m 1.7°-0.2° during Campaign 7. The continuous 30-minute sampling
		 interval provides a time resolution not possible from any other
		 observatory. Some complications for interpreting the dataset wi
		ll result from the large pixel scale, but the high sampling dens
		ity will allow for disentanglement of the individual Pluto-Charo
		n lightcurves.  This will be the highest resolution Earth-center
		ed dataset of the Pluto system ever collected and will provide c
		ritical long time baseline photometry for tying the New Horizons
		 sub-disk photometry to disk integrated observations. This datas
		et is critical for our continued study of Pluto's evolving surfa
		ce-atmosphere interaction as it recedes from the Sun and of the 
		influence of Pluto and Charon on each other. It will also provid
		e insight for interpretation of other dwarf planets and Kuiper B
		elt objects in the third zone of our Solar System.}
	howpublished = {K2 Proposal},
	year = {2014},
	month = {October},
	url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO7012.txt},
	notes = {K2 Proposal GO7012}
}

                    Acknowledgement:
                    This work uses...