RADIO SCIENCE
Radio Science Cologne
Mars Express, Venus Express and ROSETTA
File Naming Convention and File Formats
of Higher Science Data Products
Issue: 4
Revision: 2
1 INTRODUCTION
1.1 SCOPE
This document defines the file naming convention and the file formats of the science
data products beyond data level 2 defined by the Radio Science Team in Cologne.
1.2 REFERENCED DOCUMENTS
- Radio Science File Naming
Convention and Radio
Science File Formats
MEX-MRS-IGM-IS-3016.PDF
- IFMS Doppler Processing
and Calibration Software:
Level 1a to Level 2
Software Design
Specifications
MEX-MRS-IGM-DS-
3035.PDF
1.3 APPLICABLE DOCUMENTS
Fjeldbo, , G., Kliore, A.J.,
and Eshleman, V.R.
The Neutral Atmosphere of Venus as Studied with the Mariner V
Radio Occultation Experiment, Astron. J. 76, 123-140,1971.
-------------------
Lipa, B. and Tyler, G.L.
Statistical and computational uncertainties in
atmospheric profiles from radio occultation: Mariner
10 at Venus, Icarus 39, 192-208, 1979.
-------------------
Eshleman, V.R.
The radio occultation method for the study of
planetary atmospheres, Planet. Space Sci. 21, 1521-1531,1973.
-------------------
Hinson, D.P., Tyler, G.L., Hollingsworth, J.L., and
Wilson, R.J.,
Initial results from radio occultation measurements
with Mars Global Surveyor,
J. Geophys. Res., 104, 26, 997-27, 012, 1999.
-------------------
Schaa, R.,
Abel-Inversion von Radio-
Okkultationsdaten,
Diplomarbeit, Institut fuer
Geophysik und Meteorologie, Universitaet
zu Koeln, 2005. (in german)
-------------------
Peter, K.,
Beobachtungen der Ionosphaeren- und
Ionopausenstrukturen des Mars mit dem
Radio Science Experiment MaRS auf Mars Express
Diplomarbeit,
Institut fuer Geophysik und
Meteorologie, Universitaet
zu Koeln, 2008. (in german)
------------------
Paetzold, M., Tellmann, S., Haeusler, B., Hinson, D.,
Schaa, R., Tyler, G.L.,
A Sporadic Layer in the Ionosphere of Mars,
Science 310, 5749, 837 - 839, 2005.
------------------
Paetzold, M., Haeusler, B., Bird, M.K., Tellmann, S.,
Mattei, R., Asmar,S.W., Dehant, V., Eidel, W., Imamura, T, Simpson,
R.A., Tyler, G.L.
The structure of Venus' middle atmosphere and ionosphere
Nature 450, 657660, 2007.
-----------------
Tellmann, S., Paetzold, M.,
Haeusler, B., Bird, M.K., Tyler, G.L.
The structure of the Venus neutral atmosphere as
observed by the Radio Science Experiment VeRa
on Venus Express, J. Geophys. Res.,114, E00B36, doi:
10.1029/2008JE003204,2009.
-----------------
Paetzold, M., Tellmann, S., Mendillo, M., Withers, P.,
Haeusler, B., Hinson, D.P., Tyler, G.L.,
The Martian Ionosphere as seen by Mars Express,Icarus, in prep
-----------------
2 OVERVIEW OF SCIENCE DATA LEVEL
2.1 DATA PROCESSING LEVELS
This document describes the Radio Science data formats beyond Level 2 (L02).
Level 1 (L01) data are raw data recorded at the ESA groundstations in New Norcia
(Australia), Cebreros (Spain) or at the NASA Deep Space Network (DSN). L02 data
contain the calibrated Radio Science data.
Calibrated received frequencies, predicted frequencies and resulting frequency
residuals (observed frequency minus predicted frequency) can be found in L02 data
files along with other relevant information about measurement time, measurement
geometry and received signal strength.
A detailed description of the L01 and L02 data can be found in [1] and [2]. Radio
Science L02 files can contain different measurement types:
- gravity measurements
- Radio occultation measurements
- Solar Corona data.
- Bistatic Radar
The L02 files build the input data base for the Level 3 (L03) & Level 4 (L04) data files.
2.2 SCIENCE DATA PROCESSING LEVELS
Level 3 (L03) files contain science information extracted from the Radio Science L02
data. Different output file types exists depending on the measurement type and
geometry. The six different measurement types are:
- Occultation measurements:
In a first step a refractivity profile is generated for each occultation
measurement (L03). These files contain information about the ray bending
of the radio link in the ionosphere and atmosphere. In a next computation
step these refractivity profiles are used to produce density, temperature
and pressure profiles of the neutral atmosphere and electron density
profiles of the ionosphere (Level 4 L04 files). The refractivity profile is the
main output for Level 3. It is included in the ionospheric L04 files and it can
be easily derived from the atmospheric Level 4 product because the
neutral number density in the L04 profiles is directly proportional to the
refractivity in the neutral atmosphere. (e.g. see [Hinson et al, 1999] for a
description and the proportionality factor).
- Gravity measurements.
- Phobos measurements.
- Atmospheric drag measurements.
- Solar Corona measurements.
- Bistatic Radar measurements.
Level 4 (L04) files
contain information calculated using the L03 output files. The data
processing levels 3 and 4 (L03 and L04) are identical to the CODMAC level 05.
The L03 occultation refractivity profiles are used to generate two different types of
L04 occultation (OCC) data:
- Atmospheric profiles of the neutral atmosphere containing vertical profiles
of temperature, pressure and neutral number density.
- Ionospheric files containing electron density profiles of the planets
ionosphere.
The Bistatic Radar L04 product contains information about the dielectric constant of the surface.
The Phobos, Solar Corona and Atmospheric Drag L04 data product are TBD.
2.3 GENERAL FILE NAME FORMAT
The file names of all higher science products generated from Level 2 data will follow
the following file name format:
rggttttlll_sss_yydddhhmm_qq.eee
See Table 2-1 for explanation.
2.4 DATA FILE NAMES
All tabulated ASCII data files of each processing level will have the extension eee =
TAB.
2.5 DESCRIPTIVE FILE NAMES
Descriptive files contain information in order to support the content of data files. The
following file types are defined as descriptive files with extension eee =
- *.LBL PDS label files
- *.TXT Information (text) files
- *.LOG additional processing information
Table 2-1: Data file naming convention:
Acronym | Description | Examples
-----------------------------------------------
r |Spacecraft (Raumsonde) name |
|R = Rosetta |
|M = Mars Express |
|V = Venus Express |M
-----------------------------------------------
gg |Ground station ID: | 00
|00 = valid for all ground |
|stations or independent of |
|ground station or not |
|feasible to appoint to a |
|specific ground station or |
|complex DSN complex 40 |
|Canberra |
| 34 = 34 m BWG |
| 40 = complex |
| 43 = 70 m |
| 45 = 34 m HEF |
| ESA |
| Cebreros antenna: |
| xx = 35 m |
| New Norcia antenna |
| 32 = 35 m |
| DSN complex 10 Goldstone: |
| 10 = complex |
| 14 = 70 m |
| 15 = 34 m HEF |
| 24 = 34 m BWG |
| 25 = 34 m BWG |
| 26 = 34 m BWG |
| 27 = 34 m HSBWG |
| DSN complex 60 Madrid: |
| 54 = 34 m BWG |
| 55 = 34 m BWG |
| 60 = complex |
| 63 = 70 m |
| 65 = 34 m HEF |
-------------------------------------------------
tttt | data source identifier |ODF0
| Level 3 & 4 |
| ICL1 = IFMS 1 closed loop |
| ICL2 = IFMS 2 closed loop |
| ICL3 = IFMS RS (IFMS 3) |
| closed-loop |
| IOL1 = IFMS 1 open loop |
| IOL2 = IFMS 2 open loop |
| IOL3 = IFMS RS (IFMS 3) |
| open loop |
| ODFX = DSN ODF |
| closed-loop file (X-band) |
| ODFS = DSN ODF closed-loop |
| file (S-band) |
| T000 T017 = DSN TNF |
| closed-loop file |
| RSR0 = DSN RSR open-loop |
| file |
| SUMM = summary table |
-------------------------------------------------
lll |Data processing level |
|L03 = Level 3 |
|L04 = Level 4 |
|L03 |
-------------------------------------------------
sss |data type |AIX
|Science data level 3: |
|-------------------- |
|OCx summary for occultation |
|season |
|x=1,2,3,... |
| |
|STC solar corona total |
|electron content data |
| |
|SEC solar corona change of |
|electron content data |
| |
|RIX ionospheric refractivity|
|profile from X-band |
| |
|RIS ionospheric refractivity|
|profile from S-band |
| |
|RNX refractivity profile for|
|neutral atmosphere from |
| X-band |
| |
|RNS refractivity profile for|
|neutral atmosphere from |
|S-band |
| |
|RDX refractivity profile |
|from differential Doppler |
|from X-band |
| |
|RDS refractivity profile |
|from differential Doppler |
|from S-band |
| |
|GRV gravity LOS acceleration|
|data |
| |
|PHB Phobos measurement |
| |
|DRG atmospheric drag |
|measurement |
| |
|PXR bistatic radar echo |
|power X-band, right circular|
|polarized |
| |
|PXL bistatic radar echo |
|power X-band, left circular |
|polarized |
| |
|PSR bistatic radar echo |
|power S-band, right circular|
|polarized |
| |
|PSL bistatic radar echo |
|power S-band, left circular |
|polarized |
| |
|Science data level 4: |
|-------------------- |
|IIX ionosphere electron |
|density profiles from X-band|
|data (ingress measurement) |
| |
|IIS ionosphere electron |
|density profiles from S-band|
|data (ingress measurement) |
| |
|IID ionosphere electron |
|density profiles from diff. |
|Doppler data (ingress |
|measurement) |
| |
|IIO ionospheric files |
|containing additional |
|information about the |
|geometry of the OCC |
|measurement (ingress) and |
|the data processing |
| |
|IEX ionosphere electron |
|density profiles from X-band|
|data (egress measurement) |
| |
|IES ionosphere electron |
|density profiles from S-band|
|data (egress measurement) |
| |
|IED ionosphere electron |
|density profiles from diff. |
|Doppler data (egress |
|measurement) |
| |
|IEO ionospheric files |
|containing additional |
|information about the |
| geometry of the OCC |
|measurement (egress) and the|
|data processing |
| |
|AIX atmospheric profiles |
|generated from X-band data |
|(ingress measurement) |
| |
|AIS atmospheric profiles |
|generated from S-band data |
|(ingress measurement) |
| |
|AIO atmospheric files |
|containing additional |
|information about the |
|geometry of the OCC |
|measurement (ingress) and |
|the data processing |
| |
|AEX atmospheric profiles |
|generated from X-band data |
|(egress measurement) |
| |
|AES atmospheric profiles |
|generated from S-band data |
|(egress measurement) |
| |
|AEO atmospheric files |
|containing additional |
|information about the |
|geometry of the OCC |
|measurement (egress) and the|
|data processing |
| |
|PHB Phobos measurement |
| |
|DRG atmospheric drag |
|measurement |
| |
|DEX dielectric constant |
|X-band from bistatic radar |
|measurement |
| |
|DES dielectric constant |
|S-band from bistatic radar |
|measurement |
| |
------------------------------------------------
yy |Year of the measurement. | 04
| For the summary tables |
|(sss = OCx yy describes the |
|year of the first |
|occultation measurement |
|in the file.) |
------------------------------------------------
ddd |Day of the year of the |153
|measurement. For the summary|
|tables (sss = OCx ddd |
|describes the day of year of|
|the first occultation |
|measurement in the file.) |
------------------------------------------------
hhmm |Sample hour ,minute (Start |1135
|time of Doppler recording at|
|the Ground station for all |
|measurement types except |
|bistatic radar. |
|Set to 'N/A' for bistatic |
|radar) |
------------------------------------------------
qq |Sequence or version number |01
------------------------------------------------
eee |.TAB ASCII data files |TAB
|.LBL PDS label files |
|.TXT information files |
|.LOG processing information |
|files |
3 LEVEL 3 SCIENCE DATA PRODUCTS
3.1 LEVEL 3 DATA PRODUCTS: OCCULTATIONS
3.1.1 Summary Table Occultation Season
One summary table is provided for each occultation season. It contains the basic
information relevant for the occultation season.
3.1.1.1 File name format
The file name follows the definition of section 2.1 and Table 2-1
r00SUMML03_OCx_yyddd0000_qq.TAB
The source identifier is set to tttt = SUMM, sss = OCx is for occultation season x = 1,
2, 3, 4, 5, or 6, respectively. yyddd describe the year (yy) and the day of year (ddd)
of the first occultation measurement in the summary table.
3.1.1.2 File format
This file contains some information about the geometrical occultation (OCC) point.
The geometrical OCC point is the point where the radio link would disappear behind
the planetary disc if the atmospheric and ionospheric bending would be absent. The
geometrical OCC point might differ from the real OCC point due to the atmospheric
and ionospheric bending of the radio link, especially for Venus. The radio link can not
reach the surface at Venus due to the critical refraction below ca. 32 km. The
information given in these files is provided to give the user a first approximate
information about the location and local time of the measurements. More detailed
information about the measurement can be found in the *.TXT files described below.
1 Occultation number in season x
2 Orbit number
3 Day of year
4 Date [dd/mm/yy]
5 Start time of Doppler recording in hh:mm:ss
6 Stop time of Doppler recording in hh:mm:ss
7 Ground station
8 Longitude of occultation coordinate (east) at
ingress [deg]
9 Longitude of occultation coordinate (west) at
ingress [deg]
10 Latitude of occultation coordinate at ingress [deg]
11 Solar longitude at ingress [deg]
12 Solar elevation at ingress [deg]
13 Solar zenith angle at ingress [deg]
14 Local time on planet in fraction of hours at ingress hours
15 Local radius based on
For Mars: the MOLA model at ingress location [km]
For Venus: mean radius of 6051.8 km used [km]
16 Topographic elevation at ingress [km]
17 Longitude of occultation coordinate (east) at
egress [deg]
18 Longitude of occultation coordinate (west) at
egress [deg]
19 Latitude of occultation coordinate at egress [deg]
20 Solar longitude at egress [deg]
21 Solar elevation at egress [deg]
22 Solar zenith angle at egress [deg]
23 Local time on planet in fraction of hours at egress hours
24 Local radius based on
For Mars: the MOLA model at egress location
For Venus: mean radius of 6051.8 km used [km]
25 Topographic elevation at egress [km]
Note: no egress observations with MEX. Egress columns for MEX are not included.
3.1.2 Occultation measurement information file
3.1.2.1 File name format: information file (*.TXT-file)
The file name follows the definition of section 2.1 and Table 2.1
rggttttL03_sss_yydddhhmm_qq.TXT
The source identifier is set to tttt = RSR0/ODFX/ODFS or tttt =
ICL1/ICL2/ICL3/IOL1/IOL2/IOL3 either the data have been processed through data
recorded at the DSN stations or at the ESA stations in closed loop recording (CL) or
open loop recording (OL) on the IFMSs 1,2 or 3. The data type identifier is set to sss
= RIX or RIS for X-band or S-band atmospheric profile data, respectively.
1 Start time: Earth Received Time (ERT) at which the first
radio occultation data sample was acquired.
2 Stop time: ERT at which the last radio occultation data
sample was acquired.
3 Occultation time: time at the planet when the geometrical
ray path grazed the limb. This is computed by substracting
the limb-to-Earth light time from the appropriate ERT.
4 Orbit number
5 ground station DSS number
6 Ray path direction: The angle between local north and the
tangent to the ray path at occultation point, measured
positive from local north toward local east. The tangent
to the ray path indicates the direction of signal
propagation. A signal travelling from west toward
east as it grazed the surface would have a ray-pathdirection
of 90 degrees. [deg]
7 Angle from diametric: Angle at which the spacecraft rises or
sets behind the planet limb, measured clockwise from the
planet radial direction as viewed from Earth. An angle-from-
diametric equal to zero indicates a diametric occultation
with motion of the ray away from the surface
(e.g., occultation egress). A value of 180 degrees is a
nearly diametric ingress occultation. [deg]
8 Latitude at surface (North) [deg]
9 Longitude at surface (East) [deg]
10 Sub-solar latitude [deg]
11 Sub-solar longitude [deg]
12 Solar Longitude [deg]
13 For Mars:
MOLA radius: Radius at
Occultation point taken from a
0.25 x 0.25 grid. The given
value is the radius at the grid
point closest to the
measurement point.
For Venus: mean planetary
radius of 6051.8 km used [km]
14 Spacecraft to Limb distance [km]
15 Spacecraft to ground station distance [km]
16 Local True Solar Time of Occultation (LTST) [hour]
17 Solar Zenith Angle [deg]
18 Sun-Earth-Spacecraft-Angle:
Approximate angle between Sun and spacecraft as viewed
from Earth during experiment.[deg]
19 ground station elevation angle [deg]
20 PCK file name: file name of
the NAIF Planetary Constants
file used in this retrieval.
21 SPK file name: file name of
the NAIF Spacecraft dealing
with ephemeris data.
3.2 LEVEL 3 DATA PRODUCTS: GRAVITY
TBD
3.3 LEVEL 3 DATA PRODUCTS: BISTATIC RADAR
TBD
3.4 LEVEL 3 DATA PRODUCTS: SOLAR CORONA
TBD
3.5 LEVEL 3 DATA PRODUCTS: ATMOSPHERIC DRAG
TBD
3.6 LEVEL 3 DATA PRODUCTS: PHOBOS
TBD
4 LEVEL 4 SCIENCE DATA PRODUCTS
4.1 LEVEL 4 DATA PRODUCTS: NEUTRAL ATMOSPHERIC PROFILES
4.1.1 Introduction
Vertical profiles of number density, pressure and temperature of the neutral
atmosphere are derived from the L03 refractivity data file. The data products are
- a TXT-file containing background information about measurement location,
solar and geometrical conditions, and file names of relevant used SPICE files.
- The atmospheric profiles (*.TAB-files).
4.1.2 Atmospheric information file
4.1.2.1 File name information file (*.TXT-file)
The file name follows the definition of section 3.1 and Table 3.1
rggttttL04_sss_yydddhhmm_qq.TXT
The source identifier is set to tttt = RSR0/ODFX/ODFS or tttt =
ICL1/ICL2/ICL3/IOL1/IOL2/IOL3 either the data have been processed through data
recorded at the DSN stations or at the ESA stations in closed loop recording (CL) or
open loop recording (OL) on the IFMSs 1,2 or 3. The data type identifier is set to sss
= AIO/AEO for X-band or S-band atmospheric profile data (I=ingress, E=egress),
respectively.
4.1.2.2 File format information file (*.TXT-file)
1 Profile file name: Name of the corresponding atmospheric
profile file
2 Start time: The Earth Receive Time (GRT) at which the first
radio occultation data sample in the corresponding profile
file was acquired.
3 Stop time: The Earth Receive Time (GRT) at which the last
radio occultation data sample in the corresponding profile
file was acquired.
4 Measurement time (lowest sample): The Spacecraft Time
(GRT-OWLT) at which the lowest acceptable radio
occultation data sample was acquired.
5 Orbit number
6 DSN antenna number
7 Ray path direction:
The angle between local north and the tangent to the ray path at
occultation point, measured positive from local north
toward local east. The tangent to the ray path indicates the
direction of signal propagation. A signal travelling from west toward
east as it grazed the surface would have a ray-path direction of 90 degrees.
[deg]
8 Angle from diametric:
Angle at which the spacecraft rises or sets behind the planet limb,
measured clockwise from the planet radial direction as
viewed from Earth. An angle from-diametric equal to zero
indicates a diametric occultation with motion of the
ray away from the surface (e.g., occultation egress). A
value of 180 degress is a nearly diametric ingress occultation.
[deg]
9 Latitude of lowest acceptable sample (North) [deg]
10 Longitude of lowest acceptable sample (East) [deg]
11 Sub-solar latitude of lowest acceptable sample (North) [deg]
12 Sub-solar longitude of lowest acceptable sample (East) [deg]
13 Solar Longitude at lowest acceptable sample [deg]
14 For Mars:
MOLA radius: Radius at latitude and longitude of
lowest acceptable measurement point taken
from a 0.25 x 0.25 grid. The given value is the radius at the
grid point closest to the measurement point.
For Venus: mean planetary
radius of 6051.8 km used
[km]
15 For Mars:
MOLA areoid: Radius of areoid at latitude and
longitude of lowest acceptable measurement point taken
from a 0.25 x 0.25 grid. The given value is the radius at the
grid point closest to the4measurement point.
For Venus: set to -9999.99
[km]
16 Radius of the lowest acceptable measurement point [km]
17 Sigma Radius [km]
18 Pressure of lowest sample [Pa]
19 Sigma Pressure of lowest sample [Pa]
20 Temperature of lowest sample [K]
21 Sigma Temperature of lowest sample [K]
22 Upper boundary condition for Temperature: lowest value [K]
23 Upper boundary condition for Temperature: medium value [K]
24 Upper boundary condition for Temperature: upper value [K]
25 Spacecraft to Limb Distance at measurement time of
lowest acceptable sample [km]
26 Spacecraft to Groundstation Distance at measurement
time of lowest acceptable sample [km]
27 Local True Solar Time of Occultation (LTST) at
geolocation of lowest acceptable sample [hour]
28 Solar Zenith Angle at geolocation of lowest
acceptable sample [deg]
29 Sun-Earth-Spacecraft-Angle at measurement time of
lowest acceptable sample:
Approximate angle between Sun and spacecraft as viewed
from Earth during experiment. [deg]
30 Groundstation elevation angle at measurement time of
lowest acceptable sample [deg]
31 Gravity field model
32 Geopotential reference:
Reference value for
geopotential. Reference geoid
has mean equatorial radius of
3396 km. [m2/s2]
33 PCK file name: file name of the NAIF Planetary Constants
file used in this retrieval.
34 SPK file name: file name of the NAIF Spacecraft dealing
with ephemeris data.
4.1.3 Atmospheric profiles data file
4.1.3.1 File name format: Atmospheric profiles data file (*.TAB-file)
The file name follows the definition of section 3.1 and Table 3.1
rggttttL04_sss_yydddhhmm_qq.TAB
The source identifier is set to tttt = RSR0/ODFX/ODFS or tttt =
ICL1/ICL2/ICL3/IOL1/IOL2/IOL3 either the data have been processed through data
recorded at the DSN stations or at the ESA stations in closed loop recording (CL) or
open loop recording (OL) on the IFMSs 1,2 or 3. The data type identifier is set to sss
= AIX/AEX or AIS/AES for X-band or S-band atmospheric profiles data (I=ingress,
E=egress), respectively.
4.1.3.2 File format: Atmospheric Profiles data file (*.TAB-file)
1 Sample Number
2 UTC Time
3 Ephemeris Seconds [s]
4 Radius [km]
5 Latitude [deg]
6 Longitude (East) [deg]
7 Geopotential: Geopotential at measurement location
(RADIUS, LATITUDE, LONGITUDE). A reference
value (GEOPOTENTIAL REFERENCE in TXT-file)
has been substracted. [m2/s2]
8 Geopotential height calculated from column 4 using a
reference radius of 3396.0 km (for Mars) or 6051.8 km
for Venus. [km]
9 Pressure with lowest upper boundary condition [Pa]
10 Sigma pressure with lowest upper boundary condition [Pa]
11 Pressure with medium upper boundary condition [Pa]
12 Sigma pressure with medium upper boundary condition [Pa]
13 Pressure with highest upper boundary condition [Pa]
14 Sigma pressure with highest upper boundary condition [Pa]
15 Temperature with lowest upper boundary condition [K]
16 Sigma temperature fit with lowest upper boundary condition [K]
17 Temperature with medium upper boundary condition [K]
18 Sigma temperature fit with medium upper boundary condition [K]
19 Temperature with highest upper boundary condition [K]
20 Sigma temperature fit with highest upper boundary condition [K]
21 Number Density [m-3]
22 Sigma Density [m-3]
4.2 LEVEL 4 DATA PRODUCTS: IONOSPHERIC ELECTRON DENSITY
PROFILES
4.2.1 Introduction
Vertical profiles of electron density of the ionosphere are derived from the refractivity
data file. The data products are
- a TXT-file containing background information about measurement location,
solar and geometrical conditions, and file names of relevant used SPICE files.
- The ionospheric electron density profile (*.TAB)
4.2.2 Electron density profile file
4.2.2.1 File name format: electron density profile (*.TAB)
The file name follows the definition of section 3.1 and Table 3.1
rggttttL04_sss_yydddhhmm_qq.TAB
The source identifier is set to tttt = RSR0/ODFX/ODFS or tttt =
ICL1/ICL2/ICL3/IOL1/IOL2/IOL3 either the data have been processed through data
recorded at the DSN stations or at the ESA stations in closed loop recording (CL) or
open loop recording (OL) on the IFMSs 1,2 or 3. The data type identifier is set to sss
= IIX/IEX or IIS/IES for X-band or S-band ionospheric profile data (I=ingress, E =
egress), respectively, or sss = IID/IED for differential Doppler data.
4.2.2.2 File format: electron density profile (*.TAB)
1 Sample number
2 Time in ISO format
3 Ephemeris time [sec]
4 Radius [km]
5 Geopotential height [km]
6 Latitude [deg]
7 Longitude East [deg]
8 Refractivity times
9 Received signal power level [dBm]
10 Electron Density [m-3]
11 Uncertainty electron density [m-3]
4.2.3 Ionospheric information file
4.2.3.1 File name information file (*.TXT-file)
The file name follows the definition of section 3.1 and Table 3.1
rggttttL04_sss_yydddhhmm_qq.TXT
The source identifier is set to tttt = RSR0/ODFX/ODFS or tttt =
ICL1/ICL2/ICL3/IOL1/IOL2/IOL3 either the data have been processed through data
recorded at the DSN stations or at the ESA stations in closed loop recording (CL) or
open loop recording (OL) on the IFMSs 1,2 or 3. The data type identifier is set to sss
= IIO/IEO for X-band or S-band ionoospheric profile data (I=ingress, E=egress),
respectively.
4.2.3.2 File format information file (*.TXT-file)
1 Profile file name: Name of the corresponding ionospheric profile file
2 Start time: The Earth Receive Time (GRT) at which the first
radio occultation data sample in the corresponding profile
file was acquired.
3 Stop time: The Earth Receive Time (GRT) at which the last
radio occultation data sample in the corresponding profile
file was acquired.
4 Measurement time of the sample with a ray periapsis of
100 km above MOLA surface given in Earth Receive Time (GRT).
5 Measurement time of the sample with a ray periapsis of
100 km above MOLA surface given in Spacecraft Time
(GRT - OWLT).
6 Orbit number
7 DSN antenna number
8 Ray path direction: The angle between local north and the
tangent to the ray path at occultation point, measured
positive from local north toward local east. The tangent
to the ray path indicates the direction of signal
propagation. A signal travelling from west toward
east as it grazed the surface would have a ray-path direction
of 90 degrees.[deg]
9 Angle from diametric: Angle at which the spacecraft rises or
sets behind the planet limb, measured clockwise from the
planet radial direction as viewed from Earth. An angle from-
diametric equal to zero indicates a diametric
occultation with motion of the ray away from the surface
(e.g., occultation egress). A value of 180 degress is a
nearly diametric ingress occultation. [deg]
10 Solar Longitude of geometrical OCC point. [deg]
11 Latitude (North) of the sample with a ray periapsis of 100 km
above MOLA surface for Mars and 115 km above mean
radius of 6051.8 km for Venus. [deg]
12 Longitude (East) of the sample with a ray periapsis of
100 km above MOLA surface for Mars and 115 km above
mean radius of 6051.8 km for Venus. [deg]
13 Sub-solar latitude (North) of the sample with a ray
periapsis of 100 km above MOLA surface and 115 km
above mean radius of 6051.8 km for Venus. [deg]
14 Sub-solar longitude (East) of the sample with a ray
periapsis of 100 km above MOLA surface and 115 km
above mean radius of 6051.8 km for Venus. [deg]
15 For Mars:
MOLA radius: Radius at latitude and longitude (given
in line 11 and 12) taken from a 0.25 x 0.25 grid. The given
value is the radius at the grid point closest to the
measurement point.
For Venus: mean planetary radius of
6051.8 km used [km]
16 For Mars:
MOLA areoid: Radius of areoid at latitude and
longitude (given in line 11 and 12) taken from a 0.25 x 0.25
grid. The given value is the radius at the grid point closest
to the measurement point.
For Venus:
set to -9999.99 [km]
17 Electron density at 100 km above MOLA surface and 115
km above mean radius of 6051.8 km for Venus. [m-3]
18 Sigma electron density at 100 km above MOLA surface and
115 km above mean radius of 6051.8 km for Venus. [m-3]
19 Local True Solar Time of Occultation (LTST) at 100 km
above MOLA surface and 115 km above mean radius of
6051.8 km for Venus. [hour]
20 Solar Zenith Angle at 100 km above MOLA surface and 115
km above mean radius of 6051.8 km for Venus.[deg]
21 Latitude (North) of the sample with maximum of electron
density. [deg]
22 Longitude (East) of the sample with maximum of electron density.
[deg]
23 Sub-solar latitude (North) of the sample with maximum of
electron density. [deg]
24 Sub-solar longitude (East) of the sample with maximum of
electron density. [deg]
25 For Mars:
MOLA radius: Radius at latitude and longitude (given
in line 21 and 22) taken from a 0.25 x 0.25 grid. The given
value is the radius at the grid point closest to the
measurement point.
For Venus: mean planetary radius of 6051.8 km used [km]
26 For Mars:
MOLA areoid: Radius of areoid at latitude and
longitude (given in line 21 and 22) taken from a 0.25 x 0.25
grid. The given value is the radius at the grid point closest
to the measurement point.
For Venus: set to -9999.99 [km]
27 Maximum of electron density [m-3]
28 Sigma maximum of electron density [m-3]
29 Radius of maximum of electron density [km]
30 Geopotenial height of electron density maximum [km]
31 Altitude above reference areoid of electron density
maximum [km]
32 Solar Zenith Angle at geolocation of electron density
maximum [deg]
33 Distance between Planet and Sun [km]
34 Gravity field model
35 Geopotential reference:
Reference value for geopotential. Reference geoid
has mean equatorial radius of
3396 km for Mars and 6051.8 km for Venus.
[m2/s2]
36 PCK file name: file name of the NAIF Planetary Constants
file used in this retrieval.
37 SPK file name: file name of the NAIF Spacecraft dealing
with ephemeris data.
4.3 LEVEL 4 DATA PRODUCTS: GRAVITY
TBD
4.4 LEVEL 4 DATA PRODUCTS: BISTATIC RADAR
TBD
4.5 LEVEL 4 DATA PRODUCTS: SOLAR CORONA
TBD
4.6 LEVEL 4 DATA PRODUCTS: ATMOSPHERIC DRAG
TBD
4.7 LEVEL 4 DATA PRODUCTS: PHOBOS
TBD
5 VOLUMES AND DATASETS ORGANIZATIONS, FORMATS AND
NAME SPECIFICATIONS
5.1 DEFINITIONS AND GENERAL CONCEPT
5.1.1 Definitions
5.1.1.1 Data Product
A data product is a labeled grouping of data resulting from a scientific observation.
Examples of
data products include spectrum tables, and time series tables. A data product is a
component of a data set.
5.1.1.2 Data Set
The accumulation of data products, secondary data, software, and documentation,
that completely document and support the use of those data products. A data set is
part of a data set collection.
5.1.1.3 Data Set Collection
A data set collection consists of data sets that are related by observation type,
discipline, target, or time, and therefore are treated as a unit, archived and distributed
as a group (set) for a specific scientific objective and analysis.
5.1.1.4 Volume
A physical unit used to store or distribute data products (e.g. a CD_ROM or DVD
disk) which contain directories and files. The directories and files include
documentation, software, calibration and geometry information as well as the actual
science data. A volume is part of a volume set.
5.1.1.5
5.1.1.6 Volume Set
A volume set consists of one or more data volumes containing a single data set or
collection of related data sets. In certain cases, the volume set can consists of only
one volume.
5.2 DATA- AND VOLUME SET ORGANIZATION
The general concept for the MaRS, RSI and VeRa Data- and Volume Set Design:
Each data product is accompanied by a label and form a data product.
Data products + ancillary data + documentation form a data set. In this case a
level 5 data set. One data set equals a volume. Volumes are grouped in volume sets.
5.3 VOLUME AND DATASET NAME SPECIFICATION
5.3.1 Dataset
5.3.1.1 Dataset ID
The Data Set ID is a unique alphanumeric identifier for the MaRS, VeRa and RSI
data products. One data set corresponds to one physical data volume and both have
a four digit sequence number. For higher science data, both volume and data set,
have the same sequence number (see 5.3.3.1).For more information on the dataset
ID see Table 5-1.
XXX-Y-ZZZ-U-VVV-NNNN-WWW
Acronym| Description |Example
XXX |Instrument Host ID |MEX RO VEX
------------------------------------------------------
Y |Target ID |M (Mars)
| |V (Venus)
| |C (Comet Churyumov-
| |Gerasimenko)
| |L (asteroid Lutetia)
| |S (asteroid Steins)
| |X (for others i.e. Sun)
------------------------------------------------------
ZZZ |Instrument ID |MRS RSI VRA
------------------------------------------------------
U | Data level |1
|(CODMAC Level) |
|derived higher |5
|science data |
------------------------------------------------------
VVV |For higher Sience |
|data the |
|measurement type |OCC
|Occultation |
------------------------------------------------------
NNNN |A 4 digit sequence |0123
|number |
------------------------------------------------------
WWW |Version number |V1.0
------------------------------------------------------
Note: In the keywords of the labels the CODMAC-levels are used instead of PSA-level. In all other file
names and documents we keep PSA-level.
Examples:
MEX-M-MRS-5-OCC-9101-V1.0
5.3.1.2 Dataset Name
The dataset name is the full name of the dataset already identifiable by a dataset id.
Dataset names shall be at most 60 characters in length and must be in upper case.
Description | Example
------------------------------------------------------
Instrument Host Name |MARS EXPRESS
|ROSETTA ORBITER
|VENUS EXPRESS
------------------------------------------------------
Target name |MARS
|VENUS
|67P (for Comet Churyumov-
|Gerasimenko)
|CHECKOUT (commissioning Rosetta)
|LUTETIA
|STEINS
|SKY (commissioning VEX)
------------------------------------------------------
Instrument id |MRS
|RSI
|VRA
------------------------------------------------------
data processing level |5
number in CODMAC level |
------------------------------------------------------
mission phases |MISSION COMMISSIONING
(MaRS misson phases |CRUISE 1
can deviate from the MEX |PRIME MISSION
official phase names. See |EXTENDED MISSION
above) |
For higher science data: |
Measurement type |OCCULTATION
------------------------------------------------------
A 4 digit sequence | 0123
number which is identical |
to the sequence number in |
the corresponding |
volume's Radio Science |
VOLUME_ID |
------------------------------------------------------
Version number |V1.0
------------------------------------------------------
Examples:
MARS EXPRESS MARS MRS 1/2/3 MISSION COMISSIONING 0123 V1.0
VENUS EXPRESS VENUS VRA 1/2/3 PRIME MISSION 0099 V2.0
ROSETTA ORBITER 67P RSI 1/2/3 CRUISE 1 1144 V3.0
MARS EXPRESS MARS MRS 5 OCCULTATION 9101 V2.0
5.3.2 Dataset Collection
5.3.2.1 Dataset Collection ID
The data set collection ID element is a unique alphanumeric identifier for a collection
of related data sets or data products. The data set collection is treated as a single
unit, whose components are selected according to a specific scientific purpose.
Components are related by observation type, discipline, target, time, or other
classifications.
XXX_Y_ZZZ_U_VVV_IIIIIIIIII_TTT
Acronym | Description |Example
------------------------------------------------------
XXX |Instrument Host ID |MEX
| | RO
| |VEX
------------------------------------------------------
Y |Target ID |M (Mars)
| |V (Venus)
| |C (Comet 67P/Churyumov-Gerasimenko tbc)
| |L (asteroid Lutetia tbc)
| |S (asteroid Steins tbc)
------------------------------------------------------
ZZZ |Instrument ID |MRS
| |RSI
| |VRA
------------------------------------------------------
U |Data Level |1 (Raw Data of level 1a and 1b)
| In the keyword |2 (Calibrated Data)
|DATA_COLLECTION_ID |5 (Higher Level Data)
|the CODMAC-levels |
|are used instead of |1/2/3 (Data set contains raw and
|PSA-level. In all other |calibrated data)
|file names and |
|documents we keep PSA-level|
------------------------------------------------------
VVV |Data Description |MCO
|(Acronym) |
|MCO commissioning |
|CR1 cruise first part |
|PRM prime mission |
|ENT extended mission |
------------------------------------------------------
IIIIIIIIII| Data Description |ROCC
|(Detailed) |
|ROCC Occulation Profiles |
|GRAV Gravity Data |
|RANG Apocenter Ranging |
|BSR Bistatic Radar Spectra |
|PHOBOS Phobos Flyby |
|SUPCON superior solar |
| conjunction |
|INFCON inferior solar |
| conjunction |
------------------------------------------------------
TTT |Version Number |V1.0
------------------------------------------------------
5.3.3 Volume
5.3.3.1 Volume ID
The Volume ID provides a unique identifier for a single MaRS, RSI or VeRa data
volume, typically a physical CD-ROM or DVD. The volume ID is also called 'volume
label' by the various CD-ROM recording software packages. The Volume ID is
formed using a mission identifier, an instrument identifier of 3 characters, followed by
an underscore character, followed by a 4 digit sequence number. For higher science
data in the 4-digit number, the first two digits UU represent the volume set, the
remaining digits define the range of volumes in the volume set.
Important note: the here defined ESA PSA Volume_Id is not identical with the
Radio Science Volume_Id. The Radio Science Volume_Id is a number which is
incremented measurement by measurement, independent what kind of
measurement was conducted. The Radio Science Volume_Id belonging to one
single measurement can be found in the Logbook, located in the folder
DOCUMENT/MRS_DOC (or RSI_DOC or VRA_DOC). The ESA PSA Volume_Id in
contrast is incremented by measurement types. MEXMRS_9121, for example,
denotes the 21th archived higher science occultation volume archived by the Mars
Express MRS team since implementation of this guideline.
For higher science data, i.e. level 3 and 4 data, the first digit in the sequence number
is set to 9. The second digit represents the type of measurement. The remaining
digits define the range of volumes in the higher science volume set.
UU:
90: Higher science data Commissioning
91: Higher science data occultation
92: Higher science data gravity
93: Higher science data solar conjunction
94: Higher science data bistatic radar
95: Higher science data checkout
96: Higher science data swing by
97: Higher science data cometary coma
XXXXXX_UUZZ
Acronym |Description |Example
--------------------------------------------------
XXXXXX |Missionhost and |MEXMRS
|Instrument ID |RORSI
| |VEXVRA
--------------------------------------------------
ZZZZ |4 digit sequence number| 9101
--------------------------------------------------
Examples:
MEXMRS_1001
RORSI_2999
VEXVRA_3508
MEXMRS_9101
5.3.3.2 Volume Version ID
There can be several version of the same volume, if for example the archiving
software changed during the archiving process or errors occurred during the initial
production. This is indicated by the Volume Version ID, a string, which consists of a
'V' for Version followed by a sequence number indicating the revision number.
VV.V
Acronym |Description |Example
-------------------------------------
VV.V |Volume Version ID |V1.0
-------------------------------------
If a volume is redone because of errors in the initial production or because of a
change in the archiving software during the archiving process, the volume ID remains
the same, and the Volume Version ID will be incremented.
5.3.3.3 Volume Name
The VOLUME NAME contains the name of the
physical data volume (typically a CD-ROM or DVD) already identifiable by its
VOLUME ID. Note that the volume naming for higher science data deviates from the
volume naming of level 1/2/3 (CODMAC level) i.e. level 1a/1b/2 (ESA PSA level)
data volumes (See document MEX_MRS_IGM_IS_3016 for more detail).
xxxxxx_zzzz_vv.v
Acronym |Description |Example
-----------------------------------------------------
xxxxxx |Missionhost and |MEXMRS
|Instrument ID |RORSI
| |VEXVRA
-----------------------------------------------------
zzzz |Radio Science Volume ID | 0001
|for data level 1/2/3 |
|ESA PSA volume id for |
|data level 5 |
-----------------------------------------------------
vv.v |Volume Version ID |V1.0
-----------------------------------------------------
Examples:
MEXMRS_9101_V1.0
RORSI_0999_V1.0
VEXVRA_9108_V1.0
5.3.4 Volume Set
A volume set consists of a number of volumes.
5.3.4.1 Volume Set ID
The VOLUME SET ID identifies a data volume or a set of volumes. Volume sets are
considered as a single orderable entity. VOLUME SET ID shall be at most 60
characters in length, must be in upper case and separated by underscores.
XXX_YYYY_ZZZ_WWW_UVVV
Acronym |Description |Example
------------------------------------------------------------
XXX |Abbreviation of the country of |GER
|origin |USA
------------------------------------------------------------
YYYY |The government branch |UNIK
| |NASA
------------------------------------------------------------
ZZZ |Discipline within branch |RIU (new, since
| |15.8.2007)
| |IGM (old)
------------------------------------------------------------
WWW |Mission and Instrument ID |MEXMRS
| |RORSI
| |VEXVRA
------------------------------------------------------------
UVVV | For Mex: | 0099
|A 4 digit sequence identifier |
|The 'U' digit is be used to |
|represent the volume set |
|Only MEX: |
|U = 0 commissioning / cruise |
| = 1 flybys |
| = 2 prime missions |
| = 3 extended missions |
|For ROS/VEX see chapter 5.3.3.1|
|the trailing 'V's are wildcards|
|that represent the range of |
|volumes in the set and are set |
|to X as long as the number of |
|volumes is not fixed |
------------------------------------------------------------
Examples:
GER_UNI_RIU_MEXMRS_91xx
USA_NASA_JPL_MEXMRS_0098
5.3.4.2 Volume Set Name
The VOLUME SET NAME provides the full, formal name of a group of data volumes
containing a data set or a collection of related data sets. Volume set names shall be
at most 60 characters in length and must be in upper case. Volume sets are
considered as a single orderable entity. In certain cases, the volume set name can be
the same as the volume name, such as when the volume set consists of only one
volume.
Spacecraft Example
Mars Express MEX: RADIO SCIENCE OCCULTATION
MEX: RADIO SCIENCE GLOBAL GRAVITY
MEX: RADIO SCIENCE TARGET GRAVITY
MEX: RADIO SCIENCE SOLAR CONJUNCTION
MEX: RADIO SCIENCE PHOBOS FLYBY
MEX: RADIO SCIENCE BISTATIC RADAR
MEX: RADIO SCIENCE OCCULTATION HIGHER
SCIENCE
MEX: RADIO SCIENCE GLOBAL GRAVITY HIGHER
SCIENCE
MEX: RADIO SCIENCE TARGET GRAVITY HIGHER
SCIENCE
MEX: RADIO SCIENCE SOLAR CONJUNCTION
HIGHER SCIENCE
MEX: RADIO SCIENCE PHOBOS FLYBY HIGHER
SCIENCE
MEX: RADIO SCIENCE BISTATIC RADAR HIGHER
SCIENCE
For Venus Express VEX: RADIO SCIENCE OCCULTATION
For Rosetta RO: RADIO SCIENCE COMMISSIONING
Examples:
MEX: RADIO SCIENCE OCCULTATION
MEX: RADIO SCIENCE GLOBAL GRAVITY
5.3.5 Volume Series
A volume series consists of one or more volume sets that represent data from one or
more missions or campaigns.
5.3.5.1 Volume Series Name
The volume_series_name element provides a full, formal name that describes a
broad categorization of data products or data sets related to a planetary body or a
research campaign.
Spacecraft Example
Mars Express MISSION TO MARS
Venus Express MISSION TO VENUS
Rosetta MISSION TO SMALL BODIES
Examples:
MISSION TO MARS
MISSION TO VENUS
MISSION TO SMALL BODIES