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Asteroid 2867 Steins

Alternate IDs:
1979 FJ4, 1980 VV1, 1969 VC, 1980 WB, 1954 QL
Asteroid 2867 Steins (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)
14.481 0.029 14.083 0.040 14.067 0.060
16.033 0.097 15.444 0.145 15.605 0.191

Asteroid 2867 Steins (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 6.04681 0.00002 3 H Jorda 2012
. I WISE
6.0443 0.0006 0.31 0.05 2 Behrend 2005web
. I Mainzer 2011
. N Veres 2015
6.0488 0.0046 0.18 2 Waszczak 2016
6.054 0.003 0.25 0.04 3 H Jorda 2008
0.31 0.01 . H Lamy 2008c
. N Lamy 2008b
6.049 0.3 3 Weissman 2005
6.06 0.05 0.2 . N Hicks 2004
6.057 0.003 0.20 0.02 3 Dotto 2009
6.052 0.007 0.23 . H Kuppers 2007
S 6.0467905 0.29 0.01 . H Lamy 2008c
6.05 0.01 0.30 0.03 3- Warner 2004c
S 6.04681 0.00002 . Lamy 2008a
. S Fornasier 2006
6.048 0.007 0.29 0.04 3 Weissman 2007

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+ 6.049 0.30
Lamy 2008a 3 250.0 -89.0 6.04681 Y
Lamy 2008c 9+ 94.0 -86.0 6.0467905 Y
Jorda 2012 9+ 95.0 -85.0 6.04681 Y

Asteroid 2867 Steins (top)

Asteroid Names and Discovery V12.0 (1 data product)

Asteroid 2867 Steins (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 2867 Steins (top)

Kharkiv Asteroid Magnitude-Phase Relations V1.0 (1 data product)

OBSERVATION DATE * Date of observation MAGPHASE U MAG * U magnitude as reported in the Kharkiv Magnitude-Phase Relations Database, in the Johnson-Cousins system, for the maximum of the lightcurve, corrected for unit distance to the Sun and the Earth.
(MAGNITUDE)
MAGPHASE B MAG * B magnitude as reported in the Kharkiv Magnitude-Phase Relations Database, in the Johnson-Cousins system, for the maximum of the lightcurve, corrected for unit distance to the Sun and the Earth.
(MAGNITUDE)
MAGPHASE V MAG * V magnitude as reported in the Kharkiv Magnitude-Phase Relations Database, in the Johnson-Cousins system, for the maximum of the lightcurve, corrected for unit distance to the Sun and the Earth.
(MAGNITUDE)
MAGPHASE R MAG * R magnitude as reported in the Kharkiv Magnitude-Phase Relations Database, in the Johnson-Cousins system, for the maximum of the lightcurve, corrected for unit distance to the Sun and the Earth.
(MAGNITUDE)
MAGPHASE I MAG * I magnitude as reported in the Kharkiv Magnitude-Phase Relations Database, in the Johnson-Cousins system, for the maximum of the lightcurve, corrected for unit distance to the Sun and the Earth.
(MAGNITUDE)
MAGPHASE REFERENCE * Short reference for the reported observation in the Kharkiv Magnitude-Phase Relations Database. The full references are given in the file magphaseref.tab.
2008-04-11 13.672 13.151 Dotto et al. (2009)
2008-04-17 13.650 13.130 Dotto et al. (2009)
2008-04-17 13.640 13.110 Dotto et al. (2009)
2008-04-19 13.640 13.120 Dotto et al. (2009)
2008-04-19 13.660 13.120 Dotto et al. (2009)
2008-05-01 13.732 13.228 Dotto et al. (2009)
2008-05-03 13.763 13.268 Dotto et al. (2009)
2008-05-09 13.812 13.345 Dotto et al. (2009)
2008-05-10 13.830 13.361 Dotto et al. (2009)
2008-06-30 14.070 13.553 Dotto et al. (2009)
2008-06-01 14.065 13.533 Dotto et al. (2009)
2008-06-02 14.045 13.543 Dotto et al. (2009)

Asteroid 2867 Steins (top)

Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0 (5 data products)

time: 2008-09-05T13:31:55.729      file: spectroscopic/miro_3_cts_20082491331.dat      dataset: Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0

time: 2008-09-05T18:29:45.086      file: spectroscopic/miro_3_cts_20082491829.dat      dataset: Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0

time: 2008-09-05T18:51:36.203      file: spectroscopic/miro_3_cts_20082491851.dat      dataset: Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0

time: 2008-09-05T13:31:20.243      file: continuum/miro_3_mm_20082491331.dat      dataset: Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0

time: 2008-09-05T13:31:20.243      file: continuum/miro_3_submm_20082491331.dat      dataset: Rosetta-Orbiter Steins MIRO 3 AST1 Steins V1.0

Asteroid 2867 Steins (top)

Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0 (42 data products)

time: 2008-09-01T00:11:10.239      file: resampled/2008/sep/level_f/ib/rpcmag080901_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-01T00:10:46.489      file: resampled/2008/sep/level_f/ob/rpcmag080901_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-01T00:11:10.239      file: resampled/2008/sep/level_g/ib/rpcmag080901_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-01T00:10:46.489      file: resampled/2008/sep/level_g/ob/rpcmag080901_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-02T00:00:42.713      file: resampled/2008/sep/level_f/ib/rpcmag080902_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-02T00:00:18.963      file: resampled/2008/sep/level_f/ob/rpcmag080902_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-02T00:00:42.713      file: resampled/2008/sep/level_g/ib/rpcmag080902_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-02T00:00:18.963      file: resampled/2008/sep/level_g/ob/rpcmag080902_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-03T00:00:57.700      file: resampled/2008/sep/level_f/ib/rpcmag080903_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-03T00:00:33.950      file: resampled/2008/sep/level_f/ob/rpcmag080903_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-03T00:00:57.700      file: resampled/2008/sep/level_g/ib/rpcmag080903_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-03T00:00:33.950      file: resampled/2008/sep/level_g/ob/rpcmag080903_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-04T00:00:47.252      file: resampled/2008/sep/level_f/ib/rpcmag080904_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-04T00:00:23.502      file: resampled/2008/sep/level_f/ob/rpcmag080904_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-04T00:00:47.252      file: resampled/2008/sep/level_g/ib/rpcmag080904_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-04T00:00:23.502      file: resampled/2008/sep/level_g/ob/rpcmag080904_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-05T04:38:54.371      file: resampled/2008/sep/level_h/ob/rpcmag080905t0438_clh_ob_m3.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. LAP DISTURBANCE OCCURRING AT CONSTANT FREQUENCIES HAS BEEN ELIMINATED. DYNAMIC REACTION WHEEL DISTURBANCE SIGNATURE ELIMINATED IN SPECTRUM.

time: 2008-09-05T00:01:11.156      file: resampled/2008/sep/level_f/ib/rpcmag080905_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-05T00:00:47.406      file: resampled/2008/sep/level_f/ob/rpcmag080905_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-05T00:01:11.156      file: resampled/2008/sep/level_g/ib/rpcmag080905_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-05T00:00:47.406      file: resampled/2008/sep/level_g/ob/rpcmag080905_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-06T00:00:19.292      file: resampled/2008/sep/level_h/ob/rpcmag080906t0000_clh_ob_m3.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. LAP DISTURBANCE OCCURRING AT CONSTANT FREQUENCIES HAS BEEN ELIMINATED. DYNAMIC REACTION WHEEL DISTURBANCE SIGNATURE ELIMINATED IN SPECTRUM.

time: 2008-09-06T00:00:35.742      file: resampled/2008/sep/level_f/ib/rpcmag080906_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-06T00:00:19.792      file: resampled/2008/sep/level_f/ob/rpcmag080906_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-06T00:00:35.742      file: resampled/2008/sep/level_g/ib/rpcmag080906_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-06T00:00:19.792      file: resampled/2008/sep/level_g/ob/rpcmag080906_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-07T00:00:48.171      file: resampled/2008/sep/level_f/ib/rpcmag080907_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-07T00:00:24.421      file: resampled/2008/sep/level_f/ob/rpcmag080907_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-07T00:00:48.171      file: resampled/2008/sep/level_g/ib/rpcmag080907_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-07T00:00:24.421      file: resampled/2008/sep/level_g/ob/rpcmag080907_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-08T00:01:09.728      file: resampled/2008/sep/level_f/ib/rpcmag080908_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-08T00:00:45.978      file: resampled/2008/sep/level_f/ob/rpcmag080908_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-08T00:01:09.728      file: resampled/2008/sep/level_g/ib/rpcmag080908_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-08T00:00:45.978      file: resampled/2008/sep/level_g/ob/rpcmag080908_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-09T00:00:59.287      file: resampled/2008/sep/level_f/ib/rpcmag080909_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-09T00:00:35.537      file: resampled/2008/sep/level_f/ob/rpcmag080909_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-09T00:00:59.287      file: resampled/2008/sep/level_g/ib/rpcmag080909_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-09T00:00:35.537      file: resampled/2008/sep/level_g/ob/rpcmag080909_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-10T00:00:52.747      file: resampled/2008/sep/level_f/ib/rpcmag080910_clf_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-10T00:00:28.997      file: resampled/2008/sep/level_f/ob/rpcmag080910_clf_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO S/C-COORDS COORDINATES.DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-10T00:00:52.747      file: resampled/2008/sep/level_g/ib/rpcmag080910_clg_ib_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE INBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.

time: 2008-09-10T00:00:28.997      file: resampled/2008/sep/level_g/ob/rpcmag080910_clg_ob_a1.tab      dataset: Rosetta-Orbiter Steins RPCMAG 4 AST1 Resampled V3.0

THIS FILE CONTAINS CALIBRATED MAGNETIC FIELD VECTOR DATA OBTAINED BY THE OUTBOARD MAGNETOMETER ABOARD THE ROSETTA S/C. GROUND CALIBRATION RESULTS HAVE BEEN APPLIED TO THE RAW DATA. FIELD IS ROTATED TO ECLIPJ2000 COORDINATES. THE S/C POSITION IS GIVEN IN ECLIPJ2000 COORDINATES AS WELL. DATA ARE AVERAGED TO 1 S MEANS.
Asteroid 2867 Steins (top)

Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0 (35 data products)

thumbnail for 2008/09/ra_080904094502_his3_lin.fit

time: 2008-09-04T09:45:01.948      file: 2008/09/ra_080904094502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904104503_his3_lin.fit

time: 2008-09-04T10:45:02.909      file: 2008/09/ra_080904104503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904114503_his3_lin.fit

time: 2008-09-04T11:45:02.921      file: 2008/09/ra_080904114503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904124503_his3_lin.fit

time: 2008-09-04T12:45:02.939      file: 2008/09/ra_080904124503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904134502_his3_lin.fit

time: 2008-09-04T13:45:02.001      file: 2008/09/ra_080904134502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904144502_his3_lin.fit

time: 2008-09-04T14:45:02.025      file: 2008/09/ra_080904144502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904154502_his3_lin.fit

time: 2008-09-04T15:45:01.944      file: 2008/09/ra_080904154502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904164503_his3_lin.fit

time: 2008-09-04T16:45:02.929      file: 2008/09/ra_080904164503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904174503_his3_lin.fit

time: 2008-09-04T17:45:02.946      file: 2008/09/ra_080904174503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904184502_his3_lin.fit

time: 2008-09-04T18:45:02.012      file: 2008/09/ra_080904184502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904194502_his3_lin.fit

time: 2008-09-04T19:45:01.938      file: 2008/09/ra_080904194502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904204502_his3_lin.fit

time: 2008-09-04T20:45:01.971      file: 2008/09/ra_080904204502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904214503_his3_lin.fit

time: 2008-09-04T21:45:02.960      file: 2008/09/ra_080904214503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904224502_his3_lin.fit

time: 2008-09-04T22:45:02.026      file: 2008/09/ra_080904224502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080904234502_his3_lin.fit

time: 2008-09-04T23:45:01.965      file: 2008/09/ra_080904234502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905004502_his3_lin.fit

time: 2008-09-05T00:45:01.996      file: 2008/09/ra_080905004502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905014502_his3_lin.fit

time: 2008-09-05T01:45:02.028      file: 2008/09/ra_080905014502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905024502_his3_lin.fit

time: 2008-09-05T02:45:01.958      file: 2008/09/ra_080905024502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905034502_his3_lin.fit

time: 2008-09-05T03:45:01.987      file: 2008/09/ra_080905034502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905084501_his3_lin.fit

time: 2008-09-05T08:45:01.204      file: 2008/09/ra_080905084501_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905094502_his3_lin.fit

time: 2008-09-05T09:45:01.975      file: 2008/09/ra_080905094502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905104503_his3_lin.fit

time: 2008-09-05T10:45:02.948      file: 2008/09/ra_080905104503_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905114502_his3_lin.fit

time: 2008-09-05T11:45:02.008      file: 2008/09/ra_080905114502_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905181918_his3_lin.fit

time: 2008-09-05T18:19:18.066      file: 2008/09/ra_080905181918_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905183118_his3_lin.fit

time: 2008-09-05T18:31:18.043      file: 2008/09/ra_080905183118_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905184418_his3_lin.fit

time: 2008-09-05T18:44:18.022      file: 2008/09/ra_080905184418_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905190819_his3_lin.fit

time: 2008-09-05T19:08:18.968      file: 2008/09/ra_080905190819_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905193819_his3_lin.fit

time: 2008-09-05T19:38:18.940      file: 2008/09/ra_080905193819_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905200819_his3_lin.fit

time: 2008-09-05T20:08:18.914      file: 2008/09/ra_080905200819_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905203818_his3_lin.fit

time: 2008-09-05T20:38:18.023      file: 2008/09/ra_080905203818_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905210819_his3_lin.fit

time: 2008-09-05T21:08:18.961      file: 2008/09/ra_080905210819_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905213818_his3_lin.fit

time: 2008-09-05T21:38:17.981      file: 2008/09/ra_080905213818_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905220819_his3_lin.fit

time: 2008-09-05T22:08:18.915      file: 2008/09/ra_080905220819_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905223818_his3_lin.fit

time: 2008-09-05T22:38:18.032      file: 2008/09/ra_080905223818_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
thumbnail for 2008/09/ra_080905230818_his3_lin.fit

time: 2008-09-05T23:08:18.008      file: 2008/09/ra_080905230818_his3_lin.fit      dataset: Rosetta-Orbiter Steins/Cal ALICE 4 Ast1 V1.0

HEADER: FITS header for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. IMAGE: FITS image for Rosetta-Alice calibrated (CODMAC Data Level 3) histogram observation. Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second ERROR_IMAGE_HEADER: FITS extension header ERROR_IMAGE: FITS extension containing the statistical uncertainty associated with each pixel in the primary extension. This is derived by assuming Gaussian statistics, such that for a given number of detected counts, N, the corresponding uncertainty is sqrt(N). Units are photons cm**-2 s**-1 Data are in units of photons per square centimeter per second WAVELENGTH_HEADER: FITS extension header WAVELENGTH_TABLE: FITS extension containing the wavelength vector in units of Angstroms. PULSE_HEIGHT_HEADER: FITS extension header PULSE_HEIGHT_TABLE: The pulse height distribution (PHD) is a one-dimensional histogram, that bins each of the detected events (pulses) based on their 'amplitude'. Detected events are those that are larger than the discriminator setting, which is an analog (voltage) value. Of the 16 PHD bins, both the top and bottom 3 bins don't get any events (this is caused by the digitization of this amplitude information), so only 10 bins contain non-zero values. The sampling parameter interval is effectively unknown and somewhat arbitrary anyway since only the relative shape and stability of the distribution is of interest. COUNT_RATE_HEADER: FITS extension header COUNT_RATE_SERIES: These count rate data are a vector that gives the measured count rate from the observation. Units are counts per time hack interval
Asteroid 2867 Steins (top)

SDSS Moving Object Catalog V3.0 (1 data product)

SDSS U MAGNITUDE * SDSS u' psf magnitude. The SDSS u' filter has effective wavelength 3540 angstroms and FWHM 570 angstroms. The psf (point spread function) magnitude is calculated from the total flux determined by a point spread fuction fitting procedure.
(MAGNITUDE)
SDSS U ERROR * SDSS u' magnitude error.
(MAGNITUDE)
SDSS G MAGNITUDE * SDSS g' psf magnitude. The SDSS g' filter has effective wavelength 4770 angstroms and FWHM 1370 angstroms. The psf (point spread function) magnitude is calculated from the total flux determined by a point spread fuction fitting procedure.
(MAGNITUDE)
SDSS G ERROR * SDSS g' magnitude error.
(MAGNITUDE)
SDSS R MAGNITUDE * SDSS r' psf magnitude. The SDSS r' filter has effective wavelength 6230 angstroms and FWHM 1370 angstroms. The psf (point spread function) magnitude is calculated from the total flux determined by a point spread fuction fitting procedure.
(MAGNITUDE)
SDSS R ERROR * SDSS r' magnitude error.
(MAGNITUDE)
SDSS I MAGNITUDE * SDSS i' psf magnitude. The SDSS i' filter has effective wavelength 7630 angstroms and FWHM 1530 angstroms. The psf (point spread function) magnitude is calculated from the total flux determined by a point spread fuction fitting procedure.
(MAGNITUDE)
SDSS I ERROR * SDSS i' magnitude error.
(MAGNITUDE)
SDSS Z MAGNITUDE * SDSS z' psf magnitude. The SDSS z' filter has effective wavelength 9130 angstroms and FWHM 950 angstroms. The psf (point spread function) magnitude is calculated from the total flux determined by a point spread fuction fitting procedure.
(MAGNITUDE)
SDSS Z ERROR * SDSS z' magnitude error.
(MAGNITUDE)
SDSS A COLOR * SDSS a* color. See Ivezic et al. 2001 [IVEZICETAL2001] AJ 122, 2749-2784.
(MAGNITUDE)
SDSS A ERROR * SDSS a* color error
(MAGNITUDE)
SDSS V MAGNITUDE * Johnson V-band magnitude synthesized from SDSS colors using V = r + 0.44*(g-r) - 0.02
(MAGNITUDE)
SDSS B MAGNITUDE * Johnson B-band magnitude synthesized from SDSS colors using B = V + 1.04*(g-r) + 0.19
(MAGNITUDE)
19.19 0.03 17.78 0.03 17.03 0.01 16.86 0.02 16.75 0.01 0.17 0.03 17.34 18.31

Asteroid 2867 Steins (top)

Stooke Small Bodies Maps V3.0 (3 data products)

STOOKEMAPS FILENAME * The name of the file containing the map described by this entry. These files, which are jpg images of the map sheets, are located in the document directory of the Stooke Small Bodies Maps data set. STOOKEMAPS SOURCE FLAG * The type of image which forms the basis of this map in the Stooke Small Bodies Maps collection, as follows: P - photomosaic S - shaded relief Photomosaic maps are reprojections of photomosaics assembled from spacecraft images of the mapped body. Shaded relief maps are reproductions from airbrushed maps intended to show the topography. STOOKEMAPS MAP PROJECTION * Map projection used to create this map in the Stooke Small Bodies Maps collection. A description of the various map projections used can be found in the published papers cited in the data set catalog, and is also summarized in the file 'projections.asc' in the document directory of the data set. STOOKEMAPS GRID FLAG * Flag indicating whether the map is gridded or ungridded. G = gridded, U = ungridded. STOOKEMAPS SERIES INDICATOR * For maps in the Stooke Small Bodies Maps collection, if the map sheet is part of a multi-sheet map, this indicates the sheet number within the series, or in the case of pairs of maps representing the northern and southern hemisphere of a body, N or S indicate the north or south member of the pair. Maps which are not part of a series recieve the indicator '-'. Note that the complete series is not always available due to limited image coverage of the body. E.g. for the Mathilde azimuthal equidistant photomosaic set, the entire body would be covered by 14 sheets, of which only sheets 3-6 were prepared. STOOKEMAPS SOURCE MISSION * The spacecraft mission which was the source of the images used in preparing this map in the Stooke Small Bodies Maps collection. Abbreviations: NEAR - Near Earth Asteroid Rendezvous, VO - Viking Orbiter, MGS - Mars Global Surveyor, ME - Mars Express, MRO - Mars Reconnaissance Orbiter
2867steins/steins-cylindrical-mosaic.jpg P simple cylindrical U Rosetta
2867steins/steins-map-grid.jpg P simple cylindrical G Rosetta
2867steins/steins-map-names.jpg P simple cylindrical G Rosetta
2867steins/steins-stooke-global-mosaic.jpg P simple cylindrical U Rosetta

INDEX TO STOOKE SMALL BODIES MAPS

time:      file: mapindex.tab      dataset: Stooke Small Bodies Maps V3.0

This index lists the type, projection, target body, source mission, and other relevant parameters describing the maps of small solar system bodies prepared by Phil Stooke of the University of Western Ontario. The map sheets themselves are provided in the document directory in the form of jpeg files along with an html map guide called 00_map_guide.html.

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