2001 DU87 (a.k.a. 63291) is a moving object from K2 campaign 111, 112. You can read more information about this object at the JPL Small-Body Database Browser here. Data was taken from 03 November 2016 to 07 December 2016.
2001 DU87 was proposed for by Pal, Parker, Ryan in GO11114, GO11100, GO11051. If you use this data, please cite their proposal. You can find the bibtex citation by clicking the button below.
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@MISC{2016ktwo.propGO11114,
author = {{Pal}, P. and {Szabo}, S. and {Mueller}, M. and {Kiss}, K. and {Kiss}, K.},
title = {K2 photometry of a large sample of trans-Neptunian objects},
abstract = {Our recent studies (Pal et al. 2015, 2016, Kiss et al 2016) have
demonstrated that the K2 mission is an excellent opportunity to
obtain rotational properties of trans-Neptunian objects (TNOs).
Using long-cadence Kepler photometry focusing on the stationary
points of the apparent tracks of these objects, light curves wi
th excellent quality can be obtained, from which one can constra
in the rotation period, surface inhomogeneities, the shape of th
e object and decide, whether the true rotation period correspond
s to a single-peaked or double-peaked solution.We propose to obs
erve 13+9+9 Centaurs and trans-Neptunian objects throughout the
Campaigns 11, 12 and 13, respectively, of the K2 programme. From
our list of proposed targets, 8 also have been observed in the
framework of the ``TNOs are Cool!'' open-time key programme of t
he Herschel Space Observatory (Muller et al. 2009), therefore an
unambiguous rotational characteristics can be combined with an
unambiguous diameter and surface albedo for these objects. This
sample of ours covers various dynamical types of the population
of objects outside the main asteroid belt, including 5 Centaurs,
13 classical objects, 4 scattered disk objects and 9 resonant o
bjects. One of the resonant objects has 1:1 mean-motion resonanc
e with Neptune (namely 2012 VU85, a Trojan of Neptune) as well a
s there are four Plutinos, i.e. objects in 2:3 mean-motion reson
ance with Neptune.None of targets having Herschel/PACS thermal p
hotometry have a currently known accurate rotation period (note:
2005 TB190 has ground-based observations confirming variability
but with several aliases, see also Thirouin et al. 2012). Hence
, the K2 time series also aids the proper interpretation of ther
mal emission measurements. All of the targets having Herschel ph
otometry fall on silicon for quite long time (60+ days) with the
exception of Borasisi. This object is a binary system with a pe
riod of 46.3 days (Noll et al. 2004). Hence, the total time of 1
3+10 days when K2 is capable to perform photometry would not cov
er the binary period, however, even this shorter track could con
firm or constrain whether the objects have a synchronous rotatio
n or not.Due to the number of these targets and the comparativel
y large pixel cost w.r.t the stellar sources, we prioritize our
targets according to their brightness (i.e. the effective S/N ra
tio of the rotational light curve) as well as the existence of t
hermal infrared data. Our top priority objects include all of th
e objects having Herschel/PACS photometry. We also indicated 201
2 VU85 with priority 1. Priority 2 objects are either bright or
have interesting dynamical properties. We note that even the fai
ntest (priority 3) objects have comparable brightness to that of
2002 GV31. This object was also successfully observed by K2, yi
elding a folded light curve with good signal-to-noise ratio and
an unambiguous rotation period (Pal et al. 2015). We also note t
hat the first minor body discovered in the outer Solar System, (
2060) Chiron fell on silicon during Campaign 12. Due to the diff
erent nature of K2 data acquisition, the science case of (2060)
Chiron is described in a separate proposal.Proposed targets:}
howpublished = {K2 Proposal},
year = {2016},
month = {Februrary},
url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO11114.txt},
notes = {K2 Proposal GO11114}
}
@MISC{2016ktwo.propGO11100,
author = {{Parker}, P. and {Howett}, H. and {Horst}, H. and {Ryan}, R.},
title = {Monitoring Solar System Ocean Worlds: Activity on Titan and Enceladus},
abstract = {Saturn's moons Titan and Enceladus are two of the solar system's
most intriguing bodies. Titan's thick atmosphere and complex hy
drologic and climatic cycles are rivaled only by Earth's, while
Enceladus' vast water plumes are a geophysical enigma and an ast
robiological opportunity rolled into one. Both are examples of t
he solar system's "ocean worlds" and stand as potential targets
for future New Frontiers-class missions due to their relevance t
o understanding the diversity of habitable environments within t
he solar system and the potential emergence of life beyond Earth
.We propose to target both Titan and Enceladus for photometric m
onitoring with K2. They are on silicon for over 5 days during K2
Campaign 11. Observations from K2 will allow us to probe global
atmospheric activity across Titan on short timescales continuou
sly over the period of observability. This will provide unique t
emporal sampling and may highlight as-yet unseen physics in Tita
n's utterly unique atmosphere. Similarly, observations from K2 w
ill allow us to search for photometric indications of Enceladus'
plumes in backscattered light, and monitor them for variability
on timescales much shorter than those probed by Cassini. These
observations will constrain the size distribution of particles i
n Enceladus' plumes and may provide hints toward the sources of
energy powering the plumes.Both observations can serve as unique
proofs of concept for space-based photometric monitoring of the
se outer solar system worlds, and will support the development o
f future missions to characterize them.}
howpublished = {K2 Proposal},
year = {2016},
month = {Februrary},
url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO11100.txt},
notes = {K2 Proposal GO11100}
}
@MISC{2016ktwo.propGO11051,
author = {{Ryan}, R. and {Woodward}, W.},
title = {Lightcurves of Trojan and Hilda asteroids: Insight into Planetary Migration in the Early Solar System},
abstract = {Studies of the small bodies of the solar system reveal important
clues about the condensation and formation of planetesimal bodi
es, and ultimately planets in planetary systems. Dynamics of sma
ll bodies have been utilized to model giant planet migration wit
hin our solar system, colors have been used to explore compositi
onal gradients within the protoplanetary disk, & studies of
the size-frequency distribution of main belt asteroids may revea
l compositional dependences on planetesimal strength limiting mo
dels of planetary growth from collisional aggregration. Studies
of the optical lightcurves of asteroids also yield important inf
ormation on shape and potential binarity of asteroidal bodies. L
ightcurves of Hilda and Trojan asteroids populations yield key i
nformation about the primordial shape and binary fraction of the
se small body populations and their origins. Milli-mag Kepler ph
otometry will tightly constrain both of the latter characteristi
cs. These 2 populations are in resonances with Jupiter & col
lisional frequencies within these populations are the lowest wit
hin inner solar system small body populations. Results from the
WISE survey suggest that ~20% of Trojans & ~40% of Hildas ar
e either extremely elongated objects or binaries. Kepler optical
light curves are required to confirm these controversial findin
gs. Ground based surveys are not optimal for this type of photom
etric variability study due to large amounts of observing time r
equired & nightly aliasing effects on lightcurves. Kepler ho
wever is ideal for this type of photometric survey of asteroid v
ariability due to the photometric stability of the observing pla
tform and the correspondence between the C11 field and the L4 Tr
ojan cloud. Methodology: We have identified 100 objects for stud
y in the Hilda and Trojan asteroids to be studied with Kepler in
C11-13 with magnitudes of m_V < 20. Due to the overlap betwe
en the Campaign 11 field and the L4 Trojan cloud, our request fo
r data represents 70 objects Campaign 11, 23 objects in Campaign
12 & 7 objects in Campaign 13. These objects are not statio
nary within the Kepler fields, rather they move across the field
, resulting in a mean time in the Kepler field of view on active
silicon of 24 days. Due to the motion of these targets, the Kep
ler Science Center assesses solar system program as containing m
ore targets than proposed number of objects, (In C8, 6 Hilda tar
gets are assessed as 4847 targets by the Kepler Science Center),
thus THIS PROPOSAL SHOULD BE CONSIDERED A LARGE PROPOSAL. We wi
ll utilize data obtained with the 30 minute Kepler cadence to de
termine rotational periods for our selected targets. The ratio o
f lightcurve amplitudes will subsequently be utilized to determi
ne body elongation and/or binarity.Relevance to K2:This study wi
ll obtain high fidelity lightcurves for solar system objects in
the Kepler field of view during campaigns 11-13 to determine if
these objects originated in the Kuiper Belt and later migrated
and are amenable to the operational characteristics and constrai
nts of the mission and defined observing fields.}
howpublished = {K2 Proposal},
year = {2016},
month = {Februrary},
url = {https://keplerscience.arc.nasa.gov/data/k2-programs/GO11051.txt},
notes = {K2 Proposal GO11051}
}
Acknowledgement:
This work uses...
If only want the light curve of the object with the optimal aperture, download this product. This will give you one .fits file with several extensions. The first extension is the optimal apertures determined for this target. Further extensions contain a range of aperture sizes. You can read more in our readme.
Our code asteriks creates Moving Target Pixel Files, which are similar to Kepler/K2 TPFs, and contain stacks of images from the telescope. Moving TPFs track the motion of solar system objects, so that they are always centered in every image. Moving TPFs are background subtracted. The movie above shows a Moving TPF with background subtraction on the right.
You can run our code asteriks to regenerate any of these light curves yourself, or generate light curves of other objects. You can read more about our code at our GitHub Page and you can read more about how the code works in our recent paper