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Asteroid 1036 Ganymed

Alternate IDs:
1954 HH, 1924 TD, 1952 BF
Asteroid 1036 Ganymed (top)

24-Color Asteroid Survey (1 data product)

thumbnail for data1/1036ganymed.tab

1036GANYMED

time: N/A      file: data1/1036ganymed.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 1036 Ganymed (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)
8.970 0.023 8.647 0.055 8.618 0.021

Asteroid 1036 Ganymed (top)

52-Color Asteroid Survey (2 data products)

thumbnail for data1/1036ganymed1.tab

1036GANYMED1

time: N/A      file: data1/1036ganymed1.tab      dataset: 52-Color Asteroid Survey

This table contains a 52-color IR spectrum of the asteroid specified in TARGET_NAME.
thumbnail for data1/1036ganymed2.tab

1036GANYMED2

time: N/A      file: data1/1036ganymed2.tab      dataset: 52-Color Asteroid Survey

This table contains a 52-color IR spectrum of the asteroid specified in TARGET_NAME.
Asteroid 1036 Ganymed (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 < - greater than D - no numeric value (see P_NOTE for details) S - sidereal period (default is synodic period) U - period uncertain This is not the same as ambiguous where one or more additional periods are reported. 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. < - less than > - 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.
S 10.31284 0.00005 . N Hanus 2015a
10.316 0.002 0.09 0.01 3 Warner 2015r
10.313 0.001 0.13 0.01 2+ Pilcher 2012g
10.304 . Lupishko 1988b
10.332 0.006 0.11 0.02 3 3 Pilcher 2012g
10.309 0.001 0.18 0.01 3 3 Pilcher 2012g
. I SIMPS
12. 0.3 2 N Harris 1985
10.280 0.005 0.11 0.01 2+ Pilcher 2012g
10.31 0.13 . Gaftonyuk 2004
10.31 0.12 0.45 3 Hahn 1989
. Chernova 1995
10.308 0.45 3 Lupishko 1987b
. Hoffmann 1986
10.31 0.05 0.25 0.37 0.02 3 Velichko 2013
10.345 0.008 0.12 0.01 3- Pilcher 2012g
. I AKARI
S 10.313 . Kaasalainen 2002a
. S Licandro 2008
. I WISE
10.32 0.02 0.07 0.01 3 Skiff 2012a
10.33 0.03 0.13 0.01 3 Skiff 2012a
10.325 0.003 0.15 0.02 2+ Pilcher 2012g
. Thomas 2014
0.10 . Nakayama 2000
10.309 0.003 0.25 0.01 3 Pilcher 2012g
10.305 0.001 0.34 0.02 3 Pilcher 2012g
10.301 0.001 0.27 0.01 3 Pilcher 2012g
10.297 0.001 0.31 0.02 3 Pilcher 2012g
10.301 0.001 0.31 0.02 3 Pilcher 2012g
10.311 0.003 0.10 0.01 3 3 Pilcher 2012g
20.6016 0.0001 0.30 0.02 2 Behrend 2011web
10.318 0.002 0.20 0.01 3 Pilcher 2012g
10.297 0.002 0.30 0.01 3 Pilcher 2012g
10.297 0.001 0.28 0.01 3- Pilcher 2012g

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+ 10.297 0.45
Lupishko 1987b P 10.308
Hahn 1989 R 10.31
Kaasalainen 2002a 3- 214.0 -73.0 10.313 Y
Hanus 2015a 9+ 190.0 -78.0 10.31284

Asteroid 1036 Ganymed (top)

Asteroid Photometric Catalog V1.1 (60 data products)

More products were returned than can be displayed. Click for the full list. Which may take a while to load.
Asteroid 1036 Ganymed (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 1036 Ganymed (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.
E 0.42951 Lu+87b
E Hah+89
L 208 -76 0.42967 Ka+02a
208 -76 0.42967 Synth.

Asteroid 1036 Ganymed (top)

Asteroid Taxonomy V6.0 (1 data product)

Asteroid 1036 Ganymed (top)

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

Asteroid 1036 Ganymed (top)

Fieber-Beyer IRTF Mainbelt Asteroid Spectra V3.0 (1 data product)

thumbnail for fieberbeyer_gaffey_abell2011/1036.tab

SPECTRUM 1036 GANYMED

time: 2006-05-18T06:23:00      file: fieberbeyer_gaffey_abell2011/1036.tab      dataset: Fieber-Beyer IRTF Mainbelt Asteroid Spectra V3.0

The data set contains observations obtained with the NASA IRTF SpeX instrument covering the 0.7-2.5 micron near-infrared portion of the spectrum. The data set archives reduced, calibrated spectra which were obtained and used in Sherry Fieber-Beyer's Ph.D. dissertation at the University of North Dakota. The research focused on asteroids in a zone centered on the 3:1 resonance. These spectra were used to mineralogically characterize asteroids in this zone in an attempt to identify their meteorite analogs.
Asteroid 1036 Ganymed (top)

Small Solar System Objects Spectroscopic Survey V1.0 (1 data product)

thumbnail for n01036_n01244/01036_ganymed.tab

GANYMED CCD SPECTRUM

time: 1998-12-20T04:31      file: n01036_n01244/01036_ganymed.tab      dataset: Small Solar System Objects Spectroscopic Survey V1.0

Visible reflectance spectrum normalized at 5500 angstroms.
Asteroid 1036 Ganymed (top)

Vilas Asteroid Spectra V1.1 (1 data product)

thumbnail for spectra/ganymed.tab

GANYMED

time: 1984-04-28      file: spectra/ganymed.tab      dataset: Vilas Asteroid Spectra V1.1

Asteroid reflectance spectrum by Vilas and collaborators

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