2000 UX34 (a.k.a. 193354) is a moving object from K2 campaign 13. You can read more information about this object at the JPL Small-Body Database Browser here. Data was taken from 08 March 2017 to 08 May 2017.
2000 UX34 was proposed for by Ryan in GO13051. If you use this data, please cite their proposal. You can find the bibtex citation by clicking the button below.
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author = {{Hedges}, C. and Co},
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@MISC{2016ktwo.propGO13051,
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/GO13051.txt},
notes = {K2 Proposal GO13051}
}
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