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Asteroid 216 Kleopatra

Alternate IDs:
A905 OA, A910 RA
Asteroid 216 Kleopatra (top)

24-Color Asteroid Survey (1 data product)

thumbnail for data2/216kleopatra.tab

216KLEOPATRA

time: N/A      file: data2/216kleopatra.tab      dataset: 24-Color Asteroid Survey

This file contains the spectrum of the asteroid specified in TARGET NAME, as part of the 24-color Asteroid Survey.
Asteroid 216 Kleopatra (top)

2MASS Asteroid and Comet Survey V2.0 (1 data product)

J MAGNITUDE 2MASS * J band selected magnitude in the 2MASS survey, or if the source is not detected in the J-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the first character of the rd_flg value.
(MAGNITUDE)
J MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the J-band magnitude in the 2MASS survey. If rd_flg[1]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[1]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If J_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[1]=0 or 6) or if the source is not measurable (rd_flg[1]=9).
(MAGNITUDE)
H MAGNITUDE 2MASS * H band selected magnitude in the 2MASS survey, or if the source is not detected in the H-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the second character of the rd_flg value.
(MAGNITUDE)
H MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the H-band magnitude in the 2MASS survey. If rd_flg[2]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[2]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If H_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[2]=0 or 6) or if the source is not measurable (rd_flg[2]=9).
(MAGNITUDE)
KS MAGNITUDE 2MASS * Ks band selected magnitude in the 2MASS survey, or if the source is not detected in the Ks-band, the 95% confidence upper limit derived from a 4 arcsec radius aperture measurement taken at the position of the source on the Atlas Image. (The Atlas Images are quick-look images suitable for deriving positional information but not accurate photometry.) The origin of the magnitude is given by the third character of the rd_flg value.
(MAGNITUDE)
KS MAGNITUDE 2MASS UNC * Corrected photometric uncertainty for the Ks-band magnitude in the 2MASS survey. If rd_flg[3]=2, this is the measurement error from the profile-fitting procedure, corrected to be consistent with observed repeatability statistics. If rd_flg[3]=1 or 4, this is the RMS of the brightness measured in aperture photometry on the individual frames. If rd_flg=3, the uncertainty is derived from the residuals to the 1-d radial profile fit (averaging over azimuth) to the unsaturated wings of the bright source. If KS_MAG_SIG > 8.0, it is a flag value indicating that a meaningful uncertainty could not be determined for the source. This column is null if the magnitude is a 95% confidence upper limit (rd_flg[3]=0 or 6) or if the source is not measurable (rd_flg[3]=9).
(MAGNITUDE)
8.855 0.015 8.534 0.027 8.306 0.027
8.914 0.016 8.546 0.021 8.367 0.023
8.916 0.018 8.550 0.027 8.352 0.024
8.917 0.025 8.513 0.026 8.361 0.022
8.918 0.011 8.535 0.051 8.349 0.021
8.920 0.029 8.546 0.030 8.359 0.021
8.927 0.027 8.564 0.049 8.343 0.019
8.943 0.021 8.581 0.024 8.436 0.018
8.949 0.013 8.583 0.027 8.416 0.023
8.966 0.015 8.555 0.019 8.417 0.018
8.978 0.007 8.594 0.019 8.445 0.020
8.987 0.017 8.611 0.027 8.449 0.021
9.011 0.020 8.571 0.045 8.453 0.019
9.223 0.015 8.824 0.025 8.698 0.019

Asteroid 216 Kleopatra (top)

Asteroid Lightcurve Derived Data V16.0 (2 data products)

LC PERIOD FLAG * Flag referring to the sidereal period given in the asteroid lightcurve parameters file, taking the following values: > - less than LC PERIOD NOTE * Note with further information about the period given in the asteroid lightcurve parameters file. LC PERIOD * Rotation period of the asteroid about its axis, in hours, in the asteroid lightcurve parameters file. The period given is synodic unless the S flag (sidereal) is set in P_FLAG.
(HOUR)
LC PERIOD ERR * Error in the rotational period given in the asteroid lightcurve parameters file.
(HOUR)
LC AMPLITUDE FLAG * A flag pertaining to the amplitude of the lightcurve in the asteroid lightcurve parameters file, given in AMP_MIN and AMP_MAX. - greater than LC AMPLITUDE MINIMUM * Lightcurve amplitude minimum, in the asteroid lightcurve parameters file. In the cases where a range of amplitude is given, this is the lower limit of the range. For individual observations for which a single value of the amplitude is given, this field contains a null value.
(MAGNITUDE)
LC AMPLITUDE MAXIMUM * Lightcurve amplitude maximum in the asteroid lightcurve parameters file. In cases where a range of amplitudes is given, this field is the upper limit of the range. In cases where a single value is given for the amplitude, this field is that value and a null value is given for AMP_MIN. Both AMP_MIN and AMP_MAX contain a null value if the publication did not include an amplitude.
(MAGNITUDE)
LC AMPLITUDE ERR * Error in the lightcurve amplitudes given in the asteroid lightcurve parameters file.
(MAGNITUDE)
LC QUALITY CODE * This code describes the reliability of the lightcurve results in the asteroid lightcurve parameters file, and takes the following values: 0 - Result later proven incorrect. This appears only on records of individual observations. 1 - Result based on fragmentary lightcurve(s), may be completely wrong. 2 - Result based on less than full coverage, so that the period may be wrong by 30 percent or so. Also, a quality of 2 is used to note results where an ambiguity exists as to the number of extrema per cycle or the number of elapsed cycles between lightcurves. Hence the result may be wrong by an integer ratio. 3 - Denotes a secure result with no ambiguity and full lightcurve coverage. 4 - In addition to full coverage, denotes that a pole position is reported. In some cases, the numerical quality code may be followed by a plus or minus sign, indicating that the reliability is judged somewhat better (+) or worse (-) than implied by an un-signed number alone. This refinement in scale has been only recently added, and not yet retroactively, so most entries don't have signs, even in some cases where they would be appropriate. LC NOTES * Notes pertaining to the lightcurve reported in the asteroid lightcurve parameters file. These are one-letter flags, one or more of which may appear in the column. ? - Usually tied with 'T' to indicate uncertainty. 1 - Monomodal curve (one min/max per rotation) 3 - Trimodal curve (three min/max per rotation) 4 - Quadrimodal curve (four min/max per rotation) A - Ambiguous period D - Period determined by us that differs from that given in the original publication E - Occultation observation H - Space telescope observations I - IR/Thermal observations M - Polarimetric observation N - No lightcurve published O - Adaptive optics observation P - Photographic photometry R - Radar observation T - Tumbling (Non-principal axis rotation - see lc_npa.tab for details) V - Visual photometry Additional flags associated with the T flag are as follows: None after the T - The asteroid is definitely tumbling ? : Possible tumbler 0 : The tumbling damping timescale is long enough that tumbling might be expected, but observations are not sufficient to substantiate either tumbling or not tumbling. - : The tumbling damping timescale is long enough that tumbling might be expected, but observations indicate the object is NOT tumbling. + : The tumbling damping timescale is short enough that tumbling would not seem likely, however, observations indicate that it may be tumbling or actually is tumbling. LC BINARY FLAG * Note regarding binarity in the asteroid lightcurve parameters file: ? - Possible, usually due to lacking mutual eclipse/occultation events B - Binary system M - Multiple system, more than two LC REFERENCE ID * A short version of the reference citation for the published paper in which the values in this entry (in the asteroid lightcurve parameters file) were reported. The full citations may be found in the file lc_references.tab.
5.379 0.002 0.36 0.02 3 Warner 2006m
. Frank 1988
0.58 . Gil-Hutton 1990b
0.87 . Grossman 1981
0.13 . Dotto 1992a
S 5.38528 . Drummond 1991
5.385 0.8 3 V Pilcher 1982
1.2 . Tholen 1980
5.394 0.40 3 Scaltriti 1978b
0.12 . N Takahashi 2003
0.30 0.02 . Foglia 2000a
5.386 0.003 0.9 0.02 3 Fauvaud 2001
5.386 0.001 0.93 0.03 3 Alton 2009a
S 5.38529 . Drummond 1988a
5.38 0.05 0.66 0.07 2 Behrend 2003web
S 5.38528 . Magnusson 1986
1.1 . Carlsson 1983
0.12 0.84 . Weidenschilling 1990
S 5.38528 . Magnusson 1990
S 5.385263 . Lupishko 1987a
5.376 0.006 0.12 0.01 3 Behrend 2002web
. I SIMPS
0.68 . N Harris 1989b
S 5.385277 . De Angelis 1995a
5.3848 0.0003 0.33 0.01 3 Behrend 2004web
. O M Marchis 2008e
S 5.38527 . Magnusson 1983
. Shevchenko 2006
5.399 0.73 1.18 . Zappala 1983b
5.394 0.13 1.07 . Weidenschilling 1987
5.386 0.70 3 Kennedy 1982
. I Masiero 2012
5.385414 0.000006 0.80 1.00 0.03 3 Behrend 2015web
5.41 0.05 0.13 0.01 3- Shevchenko 2014
. Pravec 2012b
S 5.38528 0.00001 . Kaasalainen 2012
5.386 0.001 0.97 0.03 3 Garlitz 2008web
. I AKARI
5.39 0.05 1.22 0.03 3- Behrend 2010web
. I WISE

LC REFERENCE ID * A short version of the reference citation for the published paper in which the values in this entry (in the asteroid lightcurve parameters file) were reported. The full citations may be found in the file lc_references.tab. LC SPINAXIS QUALITY CODE * The Q value gives our assessment of the quality of the pole solution. 0 Either wrong or very uncertain determination 1 Possible but not certain pole determination. This will most often appear when a limited number of data sets is used, especially if methods other than lightcurve inversion are involved. 2 Good determination, based on large dataset. The solution consists of one or two solutions (and possibly their 180 degree mirrors). If two solutions, they may differ in both longitude and latitude but not by the simple 180 degree mirror. 3 Very good determination, based on large dataset, an ambiguity of about 180 degrees in pole longitude might appear. 4 Excellent determination, pole position confirmed by methods based on independent datasets (for example, lightcurves and radar data, lightcurves and spacecraft fly-by). P A prograde rotation has been determined but no specific pole position has been determined. This will be followed by a 0 or 1, indicating the quality of the determination. R A retrograde rotation has been determined by no specific pole position has been determined. This will be followed by a 0 or 1, indicating the quality of the determination. In some cases, the numerical quality code is followed by a plus or minus sign, indicating that the reliability is judged somewhat better (+) or worse (-) than implied by an un-signed number alone. If the Q value is blank, the given pole solution has not yet been reviewed under the new rating system. LC PERIOD * Rotation period of the asteroid about its axis, in hours, in the asteroid lightcurve parameters file. The period given is synodic unless the S flag (sidereal) is set in P_FLAG.
(HOUR)
LC AMPLITUDE MAXIMUM * Lightcurve amplitude maximum in the asteroid lightcurve parameters file. In cases where a range of amplitudes is given, this field is the upper limit of the range. In cases where a single value is given for the amplitude, this field is that value and a null value is given for AMP_MIN. Both AMP_MIN and AMP_MAX contain a null value if the publication did not include an amplitude.
(MAGNITUDE)
LC SPINAXIS ECLIPTIC LONGITUDE 1 * Ecliptic longitude of the first solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LATITUDE 1 * Ecliptic latitude of the first solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LONGITUDE 2 * Ecliptic longitude of the second solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LATITUDE 2 * Ecliptic latitude of the second solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LONGITUDE 3 * Ecliptic longitude of the third solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LATITUDE 3 * Ecliptic latitude of the third solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LONGITUDE 4 * Ecliptic longitude of the fourth solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS ECLIPTIC LATITUDE 4 * Ecliptic latitude of the fourth solution in the spinaxis file of the asteroid derived lightcurve data set
(DEGREE)
LC SPINAXIS SIDEREAL PERIOD * Sidereal period of the spinaxis solution in the spinaxis file of the asteroid derived lightcurve data set.
(HOUR)
LC SPINAXIS SHAPE FLAG * Flag for shape model in the spinaxis file of the asteroid derived lightcurve data set: Y = shape model exists
summary 9+ 5.385 1.22
Magnusson 1983 2 71.0 21.0 234.0 38.0 5.38527 Y
Zappala 1983b 2 67.0 15.0 231.0 31.0 51.0 -31.0 247.0 -15.0 5.399 Y
Magnusson 1986 3 72.0 20.0 235.0 34.0 5.38528 Y
Lupishko 1987a 9+ 5.385263
Drummond 1988a 3 69.0 10.0 5.38529 Y
Magnusson 1990 3 71.0 19.0 236.0 34.0 5.38528 Y
Drummond 1991 3 69.0 10.0 5.38528 Y
Dotto 1992a 2 78.0 25.0 229.0 45.0 49.0 -45.0 258.0 -25.0 Y
De Angelis 1995a 3 72.0 18.0 5.385277 Y
Kaasalainen 2012 9+ 73.0 21.0 5.38528 Y

Asteroid 216 Kleopatra (top)

Asteroid Masses V3.0 (1 data product)

Asteroid 216 Kleopatra (top)

Asteroid Occultations V14.0 (1 data product)

OBSERVATION DATE * Date of observation OCC MAJOR AXIS * Major axis of best-fit ellipse derived from stellar occultation observations
(KILOMETER)
OCC MINOR AXIS * Minor axis of best-fit ellipse derived from stellar occultation observations
(KILOMETER)
OCC MAJOR AXIS POSITION ANGLE * Position angle of major axis of best-fit ellipse derived from stellar occultation observations
(DEGREE)
OCC FIT QUALITY CODE * Quality code for occultation fit: 0 - no fit, no position; 1 - no fit, but observations sufficiently reliable to derive an astrometric position of the asteroid relative to the star; 2 - poor fit; 3 - good fit; 4 - excellent fit OCC MAJOR AXIS UNC * Standard deviation of major axis of best-fit ellipse derived from stellar occultation observations
(KILOMETER)
OCC MINOR AXIS UNC * Standard deviation of minor axis of best-fit ellipse derived from stellar occultation observations
(KILOMETER)
OCC MAJOR AXIS POSITION ANGLE UNC * Standard deviation of position angle of major axis of best-fit ellipse derived from stellar occultation observations
(DEGREE)
1980-10-10 123.7 88.2 -81.7 3 7.0 5.6 7.0
1991-01-19 264.0 60.0 43.0 2
2000-03-07 135.0 135.0 0.0 0
2001-02-03 141.0 128.0 0.0 0
2003-08-10 222.3 93.9 -63.0 2 22.3 16.0
2005-01-18 135.0 135.0 0.0 1
2006-04-22 135.0 135.0 0.0 1
2008-09-26 98.0 57.0 -55.5 1 8.1 15.5
2009-12-24 254.9 62.9 38.5 4 2.9 0.7
2015-03-12 130.5 73.4 37.5 4 5.8 2.4 1.8

Asteroid 216 Kleopatra (top)

Asteroid Photometric Catalog V1.1 (54 data products)

More products were returned than can be displayed. Click for the full list. Which may take a while to load.
Asteroid 216 Kleopatra (top)

Asteroid Polarimetric Database V1.0 (1 data product)

APD Table

time: 1959-02-17Z      file: apd.csv      dataset: Asteroid Polarimetric Database V1.0

Asteroid Polarimetry Database
Asteroid 216 Kleopatra (top)

Asteroid Polarimetric Database V8.0 (1 data product)

APD POLARIMETRY TABLE

time: 1958-10-22      file: apd.tab      dataset: Asteroid Polarimetric Database V8.0

This file contains the Asteroid Polarimetry Database (APD) compiled by D.F. Lupishko and S.V. Vasilyev of Karazin Kharkiv National University, Ukraine. It contains the majority of asteroid polarimetry published by Feb. 10, 2014. The APD includes data in the form of complete polarization curves (degree of polarization vs. phase angle) as well as the polarization and position angle reduced to the proper coordinate system, where available.
Asteroid 216 Kleopatra (top)

Asteroid Spin Vector Compilation V5.0 (1 data product)

SPIN DATA CODE * A set of single letter codes used in the asteroid spin vectors compilation, identifying the type of information on which the solutions and rejections of spurious solutions in this record are based. The codes used are: A = Amplitudes of lightcurves C = Close observations from spacecraft during fly-by or rendezvous D = Individual data-points of photometric lightcurves E = Epochs (e.g. times of lightcurve extrema) F = Fourier coefficients of photometric lightcurves I = Infrared pre- and post-opposition differences L = Lightcurve inversion M = Magnitudes (usually at maximum light) O = Occultation observations P = Infrared polarimetry R = Radar observations S = Surface resolved (e.g. speckle data, adaptive optics) V = Visual position angles Z = Zero and non-zero amplitude apparitions imply pole-on view in former case SPIN POLE 1 LONGITUDE * Ecliptic longitude (equinox B1950.0) of the first spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 1 LATITUDE * Ecliptic latitude (equinox B1950.0) of the first spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 2 LONGITUDE * Ecliptic longitude (equinox B1950.0) of the second spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 2 LATITUDE * Ecliptic latitude (equinox B1950.0) of the second spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 3 LONGITUDE * Ecliptic longitude (equinox B1950.0) of the third spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 3 LATITUDE * Ecliptic latitude (equinox B1950.0) of the third spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 4 LONGITUDE * Ecliptic longitude (equinox B1950.0) of the fourth spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN POLE 4 LATITUDE * Ecliptic latitude (equinox B1950.0) of the fourth spin vector solution in the asteroid spin vector compilation.
(DEGREE)
SPIN SIDEREAL PERIOD * Sidereal period used in the asteroid spin vector compilation. Only periods accurate enough to bridge inter-apparitional gaps and produce absolute rotational phases for the whole data set are included. Less accurate synodic period determinations exist for many more objects. As evident from the table, the agreement between sidereal period determinations tend to be either very good or very bad. This is due to the non-uniform time-distribution of the observations, which tend to give many well-defined local chi-square minima.
(DAY)
SPIN ALBEDO FLAG * An X in this column marks the presence of albedo variegation for this asteroid in the asteroid spin vectors compilation. SPIN REFERENCE CODE * Reference code for the spin vector determination. The reference codes are formed by 2-3 letters of the first author name, followed by '+' if there are more authors, and the last two digits of the publication year. Full expansions of the codes are given in the accompanying reference table in the spin vectors compilation data set, spinrefs.tab. An entry of "Synth." means that this entry is a best value chosen by the authors of the compilation as a synthesis of the published values.
EA 71 +21 234 +38 0.2243864 Mag83
A 67 +15 231 +31 51 -31 247 -15 Zap+84
E 71 +21 234 +38 Kos86
EA 72 +20 235 +34 0.2243865 Mag86
E 0.22438596 Lu+87a
EAM 69 +10 0.2243870 Dr+88b
EAM 71 +19 236 +34 0.2243868 Mag90a
EAM 69 +10 0.2243868 Dru+91
AM 78 +25 229 +45 49 -45 258 -25 Dot+92
EA 72 +8 0.22438654 DeA95
72 +16 232 +37 0.2243867 Synth.

Asteroid 216 Kleopatra (top)

Asteroid Taxonomy V6.0 (1 data product)

Asteroid 216 Kleopatra (top)

Binary Minor Planets V9.0 (1 data product)

DYNAMICAL TYPE * A code for the dynamical type of the object, determined by its orbital elements SYSTEM SEMIMAJOR AXIS * Semimajor axis of binary system's heliocentric orbit
(ASTRONOMICAL_UNIT)
SYSTEM ECCENTRICITY * Eccentricity of binary system's heliocentric orbit SYSTEM INCLINATION * Inclination of binary system's heliocentric orbit
(DEGREE)
EFFECTIVE DIAMETER * Combined effective diameter of a binary asteroid system
(KILOMETER)
EFFECTIVE DIAMETER UNC * Uncertainty in the combined effective diameter of a binary asteroid system
(KILOMETER)
D2 T0 D1 RATIO * Secondary to primary diameter ratio for a binary asteroid system D2 TO D1 RATIO UNC * Uncertainty in the ratio of the secondary to primary diameter for a binary asteroid system PRIMARY DIAMETER * Diameter of the primary body of a binary asteroid system
(KILOMETER)
PRIMARY DIAMETER UNCERTAINTY * Uncertainty in the diameter of the primary body of a binary asteroid system
(KILOMETER)
SECONDARY DIAMETER * Diameter of the secondary body of a binary asteroid system
(KILOMETER)
SECONDARY DIAMETER UNCERTAINTY * Uncertainty in the diameter of the secondary body of a binary asteroid system
(KILOMETER)
PRIMARY ROTATIONAL PERIOD * Rotational period of the primary body of a binary asteroid system
(HOUR)
PRIMARY ROTATIONAL PERIOD UNCERTAINTY * Uncertainty in the rotational period of the primary body of a binary asteroid system
(HOUR)
BINARY SEMIMAJOR AXIS * Semimajor axis of a binary asteroid system
(KILOMETER)
BINARY SEMIMAJOR AXIS UNC * Uncertainty in the semimajor axis of a binary asteroid system
(KILOMETER)
BINARY ORBITAL PERIOD * Orbital period of a binary asteroid system
(DAY)
BINARY ORBITAL PERIOD UNC * Uncertainty in the orbital period of a binary asteroid system
(DAY)
BINARY ECCENTRICITY * Binary eccentricity of a binary asteroid system BINARY ECCENTRICITY UNC * Uncertainty in the binary eccentricity PRIMARY ALBEDO * Albedo of the primary in a binary system PRIMARY ALBEDO UNCERTAINTY * Uncertainty in the albedo of the primary in a binary system BINARY SYSTEM MASS * Total mass of a binary asteroid system
(KILOGRAM)
BINARY SYSTEM MASS UNC * Uncertainty in the total mass of a binary asteroid system
(KILOGRAM)
BINARY SYSTEM DENSITY * Density of an asteroid binary system
(GRAM_PER_CUBIC_CENTIMETER)
BINARY SYSTEM DENSITY UNC * Uncertainty in the density of an asteroid binary system
(GRAM_PER_CUBIC_CENTIMETER)
MB 2.79 0.25 13 135.00 5.80 0.066 0.012 135.00 5.80 8.90 1.60 5.385 0.000 6.780E+02 1.30E+01 2.320E+00 2.00E-02 0.000 0.087 0.007 4.64E+18 2.00E+16 3.60 0.40
MB 2.79 0.25 13 135.00 5.80 0.051 0.012 135.00 5.80 6.90 1.60 5.385 0.000 4.540E+02 6.00E+00 1.240E+00 2.00E-02 0.000 0.087 0.007 4.64E+18 2.00E+16 3.60 0.40

Asteroid 216 Kleopatra (top)

Eight Color Asteroid Survey V4.0 (2 data products)

ECAS S V * Eight Color Asteroid Survey s-v color
(MAGNITUDE)
ECAS S V UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey s-v color
(MILLIMAGNITUDE)
ECAS U V * Eight Color Asteroid Survey u-v color
(MAGNITUDE)
ECAS U V UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey u-v color
(MILLIMAGNITUDE)
ECAS B V * Eight Color Asteroid Survey b-v color
(MAGNITUDE)
ECAS B V UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey b-v color
(MILLIMAGNITUDE)
ECAS V MAGNITUDE * v magnitude from the Eight Color Asteroid Survey
(MAGNITUDE)
ECAS V MAG UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey v magnitude
(MILLIMAGNITUDE)
ECAS V W * Eight Color Asteroid Survey v-w color
(MAGNITUDE)
ECAS V W UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey v - w color
(MILLIMAGNITUDE)
ECAS V X * Eight Color Asteroid Survey v-x color
(MAGNITUDE)
ECAS V X UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey v - x color
(MILLIMAGNITUDE)
ECAS V P * Eight Color Asteroid Survey v-p color
(MAGNITUDE)
ECAS V P UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey v - p color
(MILLIMAGNITUDE)
ECAS V Z * Eight Color Asteroid Survey v-z color
(MAGNITUDE)
ECAS V Z UNC * Uncertainty (standard deviation) in Eight Color Asteroid Survey v - z color
(MILLIMAGNITUDE)
0.108 10 0.067 5 0.036 3 11.830 23 0.063 4 0.121 7 0.144 8 0.176 11
0.120 8 0.043 5 0.010 2 10.713 20 0.072 8 0.138 6 0.177 11 0.198 13
0.110 21 0.082 17 0.041 14 10.284 13 0.054 15 0.116 14 0.136 19 0.165 14
0.111 34 0.065 20 0.009 23 10.264 26 0.064 25 0.114 19 0.163 31 0.187 41
0.071 10 0.055 12 0.023 10 10.202 13 0.078 12 0.121 28 0.164 24 0.224 24
0.067 38 0.036 32 0.003 26 12.229 42 0.077 20 0.079 34 0.108 38 0.211 44
0.117 18 0.072 16 0.043 9 11.997 27 0.083 14 0.135 19 0.173 17 0.203 5
0.079 25 0.054 17 0.026 13 12.890 13 0.079 11 0.106 15 0.184 18 0.222 21
0.090 33 0.050 38 0.027 29 12.859 45 0.059 13 0.108 14 0.163 22 0.200 18

Asteroid 216 Kleopatra (top)

Fornasier Spectra of M Asteroids V1.0 (4 data products)

thumbnail for compspectra/216kleopatra.tab

216KLEOPATRA

time: 2004-11-18      file: compspectra/216kleopatra.tab      dataset: Fornasier Spectra of M Asteroids V1.0

Composite spectrum of M asteroid from Fornasier et al. (2010). Individual spectra, which are in subdirectory 'indivspectra', were combined across instruments to produce a single composite spectrum for each target.
thumbnail for indivspectra/216kleopatra_dolores_lrr.tab

216KLEOPATRA_DOLORES_LRR

time: 2004-11-18T05:25      file: indivspectra/216kleopatra_dolores_lrr.tab      dataset: Fornasier Spectra of M Asteroids V1.0

Individual spectrum of M asteroid from Fornasier et al. (2010). Individual spectra were combined across instruments to produce a single composite spectrum for each target. The composite spectra are in the subdirectory 'compspectra'.
thumbnail for indivspectra/216kleopatra_dolores_mrb.tab

216KLEOPATRA_DOLORES_MRB

time: 2004-11-18T05:28      file: indivspectra/216kleopatra_dolores_mrb.tab      dataset: Fornasier Spectra of M Asteroids V1.0

Individual spectrum of M asteroid from Fornasier et al. (2010). Individual spectra were combined across instruments to produce a single composite spectrum for each target. The composite spectra are in the subdirectory 'compspectra'.
thumbnail for indivspectra/216kleopatra_nics.tab

216KLEOPATRA_NICS

time: 2004-11-19T04:45      file: indivspectra/216kleopatra_nics.tab      dataset: Fornasier Spectra of M Asteroids V1.0

Individual spectrum of M asteroid from Fornasier et al. (2010). Individual spectra were combined across instruments to produce a single composite spectrum for each target. The composite spectra are in the subdirectory 'compspectra'.
Asteroid 216 Kleopatra (top)

Hardersen IRTF Asteroid NIR Reflectance Spectra V1.0 (2 data products)

thumbnail for hardersen_et_al_2011/kleopatra1.tab

216 KLEOPATRA NIR SPECTRUM

time: 2001-04-29T06:00:00      file: hardersen_et_al_2011/kleopatra1.tab      dataset: Hardersen IRTF Asteroid NIR Reflectance Spectra V1.0

Near-infrared (0.7 to 2.5 microns) average normalized reflectance spectrum for (216) Kleopatra.
thumbnail for hardersen_et_al_2011/kleopatra2.tab

216 KLEOPATRA NIR SPECTRUM

time: 2001-05-04T06:19:00      file: hardersen_et_al_2011/kleopatra2.tab      dataset: Hardersen IRTF Asteroid NIR Reflectance Spectra V1.0

Near-infrared (0.7 to 2.5 microns) average normalized reflectance spectrum for (216) Kleopatra.
Asteroid 216 Kleopatra (top)

IRTF Near-IR Spectroscopy of Asteroids V2.0 (1 data product)

thumbnail for clarketal2004/216_020617t065422.tab

NEAR-IR SPECTRUM OF ASTEROID 216 KLEOPATRA

time: 2002-06-17T06:54:22      file: clarketal2004/216_020617t065422.tab      dataset: IRTF Near-IR Spectroscopy of Asteroids V2.0

Asteroid spectrum obtained with SpeX at the NASA Infrared Telescope Facility (IRTF). Preprocessing of the SpeX data, as well as extraction of the 1-D spectrum and wavelength calibration was carried out using various tasks in IRAF. Telluric correction was achieved with IDL code that utilizes model atmospheric transmission spectra generated with ATRAN. Multiple solar-analog stars were used in calibrating this spectrum in units of relative reflectance. Spectrum has been normalized to 1.0 at ~ 1.215 microns (center of the J-band).
Asteroid 216 Kleopatra (top)

Rivkin Three Micron Asteroid Data V3.0 (1 data product)

thumbnail for 216kleopatra.tab

RIVKIN 3-MICRON DATA

time: 1991-12-30      file: 216kleopatra.tab      dataset: Rivkin Three Micron Asteroid Data V3.0

Spectrum of 216 Kleopatra. See accompanying index file for observational circumstances.
Asteroid 216 Kleopatra (top)

Small Body Radar Shape Models V2.0 (1 data product)

ASTEROID RADAR SHAPE MODELS, 216 KLEOPATRA

time: 1999-11-07T04:45:51      file: 216kleopatra.tab      dataset: Small Body Radar Shape Models V2.0

FACET_TABLE: The FACET_TABLE is the second part of the shape model file providing the linking of vertices into facets. The integers i1 j1 k1 are the indices of the 3 vertices that form triangular facet 1, and so on. VERTEX_TABLE: This shape file of asteroid 216 Kleopatra was created by Ostro et al. (2000) based on radar observations and has the format v x1 y1 z1 v x2 y2 z2 v x3 y3 z3 (etc.) f i1 j1 k1 f i2 j2 k2 (etc.) where the letter 'v' denotes a vertex and the letter 'f' denotes a triangular facet. The VERTEX_TABLE is the first part, describing the positions of the vertices of the shape model. The floating point numbers x1 y1 z1 are the coordinates of vertex 1, and so on (vertices are implicitly numbered beginning with 1). The origin is the center of mass, and the axes are the principle axes of the shape model. The units are kilometers. The linking of vertices into facets is provided in the FACET_TABLE. This format is identical to a Wavefront OBJ file. There is a freeware program called WCVT2POV that will convert this format into other formats such as POVray and DXF. Ostro, S.J., R.S. Hudson, M.C. Nolan, J.-L. Margot, D.J. Scheeres, D.B. Campbell, C. Magri, J.D. Giorgini, and D.K. Yeomans 2000. Radar observations of asteroid 216 Kleopatra. Science 288, 836-839. [OSTROETAL2000]
Asteroid 216 Kleopatra (top)

Small Main-belt Asteroid Spectroscopic Survey, Phase II (1 data product)

thumbnail for data08/216_01.tab

216 KLEOPATRA CCD SPECTRUM

time: 1994-11-05T03:28:06      file: data08/216_01.tab      dataset: Small Main-belt Asteroid Spectroscopic Survey, Phase II

Individual asteroid spectrum obtained during the Phase II Small Main-Belt Asteroid Spectroscopic Survey with the MDM telescopes at Kitt Peak National Observatory.
Asteroid 216 Kleopatra (top)

Torino Asteroid Polarimetry V1.0 (1 data product)

TORINO POLARIMETRY TABLE

time: 1995-01-01      file: torinopol.tab      dataset: Torino Asteroid Polarimetry V1.0

This table contains photopolarimetric measurements of Cellino et al. (2005), including all the data presented in Tables 1-4 of that paper.

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