Rosetta
Mars Express
Venus Express
MaRS/ RSI/ VeRa
Archive Generation, Validation and Transfer Plan
Issue: 5
Revision: 29
Date: 29.04.2016
Document: MEX-MRS-IGM-IS-3019
ROS-RSI-IGM-IS-3079
VEX-VRA-IGM-IS-3007
Prepared by
___________________________________________
Markus Fels
Approved by
___________________________________________
Martin Paetzold (MaRS Principal Investigator)
page left free
Document Change Record
DISTRIBUTION LISTS
Recipient Institution No. Of Copies
MaRS Team
Martin Paetzold RIU 1
Bernd Haeusler Universitaet der Bundeswehr Muenchen 2
Richard Simpson Stanford University 2
ESA/ ESOC/ ESTEC
Agustin Chicarro ESA 1
Patrick Martin ESA 1
Michel Denis ESA 1
Joe Zender ESA 1
Adriana Ocampo ESTEC 1
RSI Team
Martin Paetzold RIU 1
Bernd Haeusler UBW 2
ESA/ ESOC/ ESTEC
Gerhard Schwehm ESA 1
Rita Schulz ESA 1
Detlef Koschny ESA 1
Joe Zender ESA 1
Mark Sweeney ESOC 1
VeRa Team
Bernd Haeusler UBW 2
Martin Paetzold RIU 1
ESA/ ESOC/ ESTEC
Hakan Svedhem ESTEC 1
Adriana Ocampo ESTEC 1
ACRONYMS
A/D Analog/Digital
AGC Automatic Gain Control
AGVTP Archive Generation, Validation and Transfer Plan
AOL Amplitude Open Loop
ATDF Archival Tracking Data Format
CD-ROM Compact Disk - Read Only Memory
CL Closed-Loop
DDS Data Delivery System
DSN Deep Space Network
DVD Digital Versatile Disk
ESA European Space Agency
ESOC European Space Operation Center
ESTEC European Space Technology Center
FOL Frequency Open Loop
G/S Ground Station
HGA High Gain Antenna
IFMS Intermediate Frequency Modulation System
JPL Jet Propulsion Laboratory
LCP Left Circular Polarization
LGA Low Gain Antenna
LOS Line Of Sight
MaRS Mars Express Radio Science Experiment
MGA Medium Gain Antenna
MGS Mars Global Surveyor
MSP Master Science Plan
NASA National Aeronautics and Space Administration
NNO New Norcia
ODF Orbit Data File
ODR Original Data Record
OL Open-Loop
ONED one-way dual-frequency mode
ONES One-way single-frequency mode
PDS Planetary Data System (NASA)
POL Polarization Open Loop
PSA Planetary Science Archive (ESA).
RCP Right Circular Polarization
RSI Rosetta Radio Science Investigation
RSR Radio Science Receiver
RX Receiver
S/C Spacecraft
SIS Software Interface Specification
S-TX S-Band Transmitter
SPICE Space Planet Instrument C-Matrix Events
TBC To Be Confirmed
TBD To Be Determined
TNF Tracking and Navigation File
TWOD Two-way dual-frequency mode
TWOS Two-way single-frequency mode
UBW Universitaet der Bundeswehr Muenchen
USO Ultra Stable Oszillator
VeRa Venus Express Radio Science Experiment
VEX Venus Express
X-TX X-band Transmitter
1. Introduction
1.1. Scope
This document and its content are consistent with the Experimenter to Archive
Interface Control Document (EAICD) of ESAs Planetary Science Archive
(PSA). It presents the Archive Generation, Validation and Transfer Plan
(AGVTP) for the Rosetta Orbiter Radio Science (RSI) Experiment, the Mars
Express Orbiter Radio Science (MaRS) Experiment and the Venus Express Radio
Science Experiment (VeRa).
It describes the data flow, the different data types and levels, the directory
structures for the different data volumes, and the delivery and distribution
plans. Further it contains information about the Volume, Dataset and File
Formats, the used Standards in Data Product Generation
(PDS, Time, Coordinates), the process of Data Validation, the Volume and
Dataset Name Specifications and finally there are shown some Example PDS
Label files for the different Data types of data level 1a, 1b and 2.
1.2. Referenced Documents
The following documents are referenced in the AGVTP and may be referred to if
more information is needed.
Reference Number Title Issue_Number Date
ESA-MEX-TN-4008 Mars Express Archive Generation, Validation and Transfer
Plan 1 12.6.2001
RO-EST-TN-3372 ROSETTA Archive Generation, Validation and Transfer Plan
2.0 27.10.2003
VEX-EST-TN-036 VEX Archive Conventions
MEX-MRS-IGM-IS-3016
ROS-RSI-IGM-IS-3087 Radio Science File Naming Convention
VEX-VRA-IGM-IS-3009 and Radio Science File Formats 3.0 4.6.2003
JPL D-7669, Part 2 Planetary Data System, Standards Reference 3.5
15.10.2002
GRST-TTC-GS-ICD-0518-TOSG IFMS-to-OCC Interface Control Document 1.0
14-Mar-2000
JPL D-16765
(159-SCIENCE) Radio Science Receiver RSR Draft 5.2.2001
TRK-2-34 DSMS Tracking System Data Archival Data
(Description of the TNF data files) B 30.4.2000
TRK-2-18 Orbit Data File Interface change 3 15.06.2000
RO-UoB-IF-1234 Experimenter To Planetary Science Archive Interface
Control
Document (EAICD) Draft 5 7.11.2003
VEX-VERA-UBW-TN-3040 Reference Systems and Techniques Used for the
Simulation and Prediction of
Atmospheric and Ionospheric Sounding Measurements at Planet Venus
2.3 12.11.2003
1.3. Document Overview
The AGVTP consists of ten major sections with several subsections that follow
the introduction.
Section 2 Describes instruments and the science objectives
Section 3 Operational scenarios
Section 4 Data flow
Section 5 Archive structure and formats
Section 6 Data Delivery Schedules
Section 7 Standards used in Data Product Generation
Section 8 Data Validation
Section 9 MaRS, RSI and VeRa Volumes and Datasets Organization, Formats and
Name Specification
2. Instrument Overviews
2.1. Mars Express Orbiter Radio Science Experiment
MaRS makes use of the onboard radio subsystem, which is primarily responsible
for the communication link between the S/C and the ground stations on Earth.
Mars Express Orbiter is capable of receiving and transmitting radio signals
via two dedicated antenna systems:
High Gain Antenna (HGA), a fixed parabolic dish of 1.80m diameter and two Low
Gain Antennas (LGA), front and rear, S- Band only. The transponders consist of
an S- band and X- band receiver and transmitter each. The S/C is capable of
receiving two uplink signals at S- band (2100 MHz) via the LGAs , or
non-simultaneously at either X- Band (7100 MHz) or S- Band via the HGA and
transmit simultaneously two downlink signals at S- Band (2300 MHz) and X- Band
(8400 MHz) or at S- Band only via the LGAs.
The HGA is the main antenna for receiving telecommands from and transmitting
telemetry to the ground. The LGAs are used during the commissioning phase just
after launch and for emergency operations.
A simultaneous and coherent dual-frequency downlink at X-band and S-band via
the High Gain Antenna (HGA) is required to separate the contributions from
the classical Doppler shift and the dispersive media effects caused by the
motion of the spacecraft with respect to the Earth and the propagation of
the signals through the dispersive media, respectively.
The experiment relies on the observation of the phase, amplitude, polarization
and propagation times of radio signals transmitted from the spacecraft and
received with ground station antennas on Earth. The radio signals are affected
by the medium through which the signals propagate (atmospheres, ionospheres,
interplanetary medium, solar corona), by the gravitational influence of the
planet on the spacecraft and finally by the performance of the various systems
involved both on the spacecraft and on ground.
2.1.1. Science objectives
As part of the Mars Express Orbiter payload, the Mars Express Orbiter Radio
Science experiment (MaRS) will perform the following experiments:
radio sounding of the neutral Martian atmosphere (occultation experiment) to
derive vertical density, pressure and temperature profiles as a function of
height (height resolution better than 100 meter)
radio sounding of the ionosphere (occultation experiment) to derive vertical
ionospheric electron density profiles and to derive a description of the
global behavior of the Martian ionosphere through its diurnal and seasonal
variations depending also on solar wind conditions
determination of dielectric and scattering properties of the Martian surface
in specific target areas by a bistatic radar experiment
determination of gravity anomalies in conjunction with simultaneous
observations using the camera HRSC as a base for three dimensional (3D)
topography for the investigation of the structure and evolution of the
Martian crust and lithosphere
radio sounding of the solar corona during the superior conjunction of the
planet Mars with the Sun
the determination of the mass of Phobos
2.1.2. Instrument Modes
The MaRS experiment has four different operational modes:
TWOD : two-way, dual-frequency coherent mode:
X- band uplink or S-band uplink
S- and X- band downlink simultaneously.
Applicable for science objective a), b), d),e)
TWOS : two-way, single-frequency mode:
X- band uplink
X- band downlink
Applicable for science objective d), e) and f)
ONED : One-way, dual frequency mode:
No uplink
S- and X- band downlink simultaneously
Applicable for science objective c)
ONES : One-way, single frequency mode:
No uplink
X- band downlink
Applicable for science objective c)
The dual-frequency downlink at X-band and S-band is used to separate classical
and dispersive Doppler shifts and therefore to correct the observed frequency
shift by the plasma contribution due to the propagation through the
interplanetary medium.
The different kind of data types with respect to the two different ground
station systems are shown in the Table 2.1.
Ground_station_systems Description
IFMS (ESA) CL Closed-loop data: Doppler and
Ranging at selected sample rates
OL Open-loop data: Downconverted
received sky frequency A/D
converted at very high sample
rates
RCP at two frequencies
RCP and LCP at one frequency
DSN (NASA) ODF Orbit Data File (Closed-loop)
Doppler and Ranging
RSR Radio- Science Receiver (Open-loop)
2 or 4 channels
LCP & RCP polarizations
Table 2.1: MaRS, RSI and VeRa data types
2.2. Rosetta Radio Science Investigation (RSI)
RSI makes use of the onboard radio subsystem, which is primarily responsible
for the communication link between the s/c and the ground stations on Earth.
The Rosetta radio subsystem is especially equipped with an Ultra- Stable
Oscillator (USO), which significantly improves the sensitivity and accuracy
of the one-way radio link measurements.
Rosetta is capable of receiving and transmitting radio signals via three
dedicated antenna systems:
High Gain Antenna (HGA), a fully steer able parabolic dish of 2.20m diameter
Medium Gain Antenna (MGA), a fixed parabolic dish of 0.60m diameter
two Low Gain Antennas (LGA), front and rear, S- Band only
The transponders consist of an S- band and X- band receiver and transmitter
each. The s/c is capable of receiving two uplink signals at S- band (2100 MHz)
via the LGAs , or non-simultaneously at either X- Band (7100 MHz) or S- Band
via the HGA and transmit simultaneously two downlink signals at S- Band
(2300 MHz) and X- Band (8400 MHz) or at S- Band only via the LGAs.
The HGA is the main antenna for receiving telecommands from and transmitting
telemetry to the ground. The LGAs are used during the commissioning phase just
after launch and for emergency operations. The MGA is considered as a back-up.
2.2.1. Science objectives
The Rosetta RSI experiment has identified primary and secondary science
objectives at the comet, the asteroids flybys and during cruise.
The science objectives are divided into categories:
a) cometary gravity field investigations
b) comet nucleus investigations
c) cometary coma investigations
d) asteroid mass and bulk density
as the prime science objectives, and as the secondary science objectives:
e) solar corona sounding
f) a search for gravitational waves
2.2.2. Instrument modes
The Rosetta RSI experiment has four different operational modes:
TWOD : two-way, dual-frequency coherent mode:
X- band uplink; S-band uplink for objective e)
S- and X- band downlink simultaneously.
Applicable for science objective a), b), d),e) and f)
TWOS : two-way, single-frequency mode:
X- band uplink
X- band downlink
Applicable for science objective a)
ONED : One-way, dual frequency mode:
No uplink
S- and X- band downlink simultaneously
Applicable for science objective c) (plasma and dust investigations of
cometarys coma)
ONES : One-way, single frequency mode:
No uplink
X- band downlink
Applicable for the bistatic radar experiment to determine the surface
roughness of the comet
The different RSI data types are the same as for MaRS and VeRa and are
shown in the Table 2.1- 1 .
2.3. Venus Express Radio Science Experiment (VeRa)
VeRa makes use of the onboard radio subsystem, which is very similar to the
radio subsystem of Mars Express. The main difference is that Venus Express,
like Rosetta, is especially equipped with an Ultra- Stable Oscillator (USO).
2.3.1. Science objectives
As part of the Venus Express payload, the Venus Express Radio Science
experiment will perform the following experiments:
radio sounding of the neutral Venutian atmosphere (occultation experiment)
to derive vertical density, pressure and temperature profiles as a function of
height (height resolution better than 100 meter)
radio sounding of the ionosphere (occultation experiment) to derive vertical
ionospheric electron density profiles and to derive a description of the
global behavior of the Venutian ionosphere through its diurnal and seasonal
variations depending also on solar wind conditions
determination of dielectric and scattering properties of the Venutian
surface in specific target areas by a bistatic radar experiment
determination of gravity anomalies (tbc)
radio sounding of the solar corona during the superior conjunction of the
planet Venus with the Sun
2.3.2. Instrument Modes
The VeRa experiment has four different operational modes:
TWOD : two-way, dual-frequency coherent mode:
X- band uplink; S-band uplink
S- and X- band downlink simultaneously.
Applicable for science objective d) und e)
TWOS : two-way, single-frequency mode:
X- band uplink
X- band downlink
Applicable for science objective e)
ONED : One-way, dual frequency mode:
No uplink
S- and X- band downlink simultaneously
Applicable for science objective a) b) c)
ONES : One-way, single frequency mode:
No uplink
X- band downlink
Applicable for science objective c)
The dual-frequency downlink at X-band and S-band is used to separate
classical and dispersive Doppler shifts and therefore to correct the
observed frequency shift by the plasma contribution due to the propagation
through the interplanetary medium.
The different VeRa data types are the same as for MaRS and RSI and are shown
in the Table 2.1.
3. MaRS, RSI and VeRa Operational Scenarios
3.1. Data Processing
The MaRS, RSI and VeRa data processing depends on the ground station receiving
system (DSN or NNO) and its raw data type (closed-loop or open loop):
The IFMS data from New Norcia (NNO) will be transferred to ESOC and stored at
ESOC on the Data Delivery System (DDS). It will then be transferred via ftp
from the DDS in Darmstadt to Cologne . The closed-loop IFMS data files are raw
tracking data and contain Doppler and Ranging data recordings at selected
sample rates. The exact format of the open-loop IFMS data is still tbd, but
it consist of the down-converted and A/D converted received sky frequency at
very high sample rates.
The data from the three different DSN ground stations will be collected by the
JPL Radio-Science Group (RSG) and by the Stanford Radio Science Team for
delivery to Cologne (data delivery from Stanford to Cologne as soon as
available).
The DSN data are closed-loop Orbit Data Files (ODFs) and open-loop Radio-
Science Receiver (RSR) files. The latter are very similar to the IFMS
open-loop data files and consist of down-converted received sky frequency,
A/D converted at very high sample rates (up to 50000 Hz). These data files
will be sent via JPL to Stanford for processing up to level 2 and will be
collected in Cologne for further archiving. The processed RSR files consist
first of frequency resolution and intensity estimates probably at a
sub-second resolution for radio occultations and second for surface
scattering, there will be power spectra (and voltage cross-spectra when two
polarizations are collected), averaged over a few seconds, for each
band. All raw tracking data files and the processed data up to level 2 will
be collected in Cologne . After a final check the processed data will be
delivered to the Co-Is and after the propriety phase to PSA.
The following scientific analysis and interpretation of the processed data
product is up to the Co-I and his science objective. Lists of collaborating
institutes for MaRS, RSI and VeRa are shown in the Table 3.2-1 , Table 3.2-2
and Table 3.2-3 .
3.2. Collaborating Institutes
3.2.1. MaRS
Name Institute
---------------
M. Paetzold (PI) Rheinisches Institut fuer Umweltforschung an der
Universitaet zu Koeln, Germany
--------------------------------------------------------------
B. Haeusler,
S. Remus Institut fuer Raumfahrttechnik, Universitaet der Bundeswehr,
Munich, Germany
--------------------------------------------------------------
W. Ian Axford Max- Planck- Institut fuer Sonnensystemforschung,
Katlenburg- Lindau, Germany
--------------------------------------------------------------
J.-P. Barriot Observatoire Midi Pyrenees, Toulouse, France
Jean- Claude Cerisier CETP, 4 Ave. Neptune, Saint Maur Cedex, France
--------------------------------------------------------------
T. Hagfors Max- Planck- Institut fuer Sonnensystemforschung, Katlenburg-
Lindau, Germany
--------------------------------------------------------------
G.L. Tyler, R. Simpson, D. Hinson, Dep. of Electrical Engineering,
Stanford University , Palo Alto , USA
--------------------------------------------------------------
P. Janle Institut fuer Geophysik, Universitaet zu Kiel, Kiel, Germany
--------------------------------------------------------------
G. Kirchengast Institut fuer Geophysik u. Meteorologie,
Karl-Franzens-Universitaet,Graz, Austria
--------------------------------------------------------------
V. Dehant Observatoire Royale, Bruexelles
Table 3.2-1 : List of collaborating institutes for MaRS
3.2.2. RSI
Name Institute
---------------
M. Paetzold (PI) Rheinisches Institut fuer Umweltforschung
an der Universitaet zu Koeln, Germany
--------------------------------------------------------------
B. Haeusler,
S. Remus Institut fuer Raumfahrttechnik, Universitaet der Bundeswehr,
Munich, Germany
--------------------------------------------------------------
K. Aksnes Insitute for Theoretical Astrophysics, University of Oslo ,
Norway
--------------------------------------------------------------
J.D. Anderson
S.W. Asmar
B.T. Tsurutani Jet Propulsion Laboratory,California Institute of
Technology, Pasadena , USA
--------------------------------------------------------------
J.-P. Barriot Observatoire Midi Pyrenees, Toulouse, France
--------------------------------------------------------------
M.K. Bird Radioastronomisches Institut, Universitaet zu Bonn, Bonn,
Germany
--------------------------------------------------------------
H. Boehnhardt Max- Planck- Institut fuer Sonnensystemforschung,
Katlenburg- Lindau, Germany
--------------------------------------------------------------
N. Thomas Universitaet Bern, Berne, Swizerland
--------------------------------------------------------------
E. Gruen Max- Planck- Institut fuer Kernphysik, Heidelberg, Germany
--------------------------------------------------------------
W.H. Ip National Central University , Taipei , Taiwan
--------------------------------------------------------------
E. Marouf Dep. of Electrical Engineering,
San Jose State University , San Jose , California , USA
--------------------------------------------------------------
T. Morley ESA-ESOC, Darmstadt , Germany
Table 3.2-2 : List of collaborating institutes for RSI
3.2.3. VeRa
Name Institute
---------------
B. Haeusler (Principal Investigator),
S. Remus Institut fuer Raumfahrttechnik, Universitaet der Bundeswehr,
Munich, Germany
--------------------------------------------------------------
M. Paetzold (Co-PI) Rheinisches Institut fuer Umweltforschung
an der Universitaet zu Koeln, Germany
--------------------------------------------------------------
G.L. Tyler, R. Simpson, D. Hinson, Dep. of Electrical Engineering,
Stanford University , Palo Alto , USA
--------------------------------------------------------------
M. Bird Universitaet Bonn , Germany
--------------------------------------------------------------
R. Treumann Max-Planck Institut fuer Extraterrestrische Physik, Garching,
Germany
Table 3.2-3 : List of collaborating institutes for VeRa
4. MaRS, RSI and VeRA Data Flow
4.1. Data Flow
The data flow for the MaRS, RSI and VeRa experiments is shown in Figures 4-1
to 4-3 (not shown in Ascii version).
4.2. Points of contact
4.2.1. Point of contact for PSA archiving
Cologne is the single point of contact for the PSA archive team.
Function Name Adress E-mail Telephone/Fax
--------------------------------------------------------------
Principal Investigator Martin Paetzold Rheinisches Insitut fuer
Umweltforschung an der Universitaet zu Koeln, Aachenerstr. 201-209,
D-50931 Koeln, Germany mpaetzol@uni-koeln.de phone:
(49)-221-27781810 Fax: (49)-221-400-2320
--------------------------------------------------------------
Data Manager Christina Stanzel Rheinisches Insitut fuer
Umweltforschung an der Universitaet zu Koeln, Aachenerstr. 201-209,
D-50931 Koeln, Germany christina.stanzel@uni-koeln.de phone:
(49)-221-27781812 Fax: (49)-221-400-2320
4.2.2. Points of contact for data forwarding
site Name Adress E-mail Telephone/ Fax
--------------------------------------------------------------
Stanford University Richard A. Simpson Dept. of Electrical Engineering,
Stanford University, Packard Building 350, Serra Mall, Stanford, CA
94305-9515, USA
rsimpson@magellan.stanford.edu phone: (1)-650-723-3525
Fax: (1)-650-723-9251
--------------------------------------------------------------
JPL Sami W. Asmar Jet Propulsion Laboratory, California Institute of
Technology, 4800 Oak Grove Drive, Pasadena CA 91009 , USA
sami.w.asmar@jpl.nasa.gov phone: (1)-818-354-6288 Fax: (1)-818-393-9282
--------------------------------------------------------------
ESOC DDS TBD Esoc, Robert- Bosch- Str. 5, Darmstadt, Germany
mex.dds@esa.int (Mars Express)
rosetta.dds@esa.int (Rosetta)
TBD (Venus Express)
4.2.3. Points of contact for data distribution
Function Name Adress E-mail Telephone/ Fax
--------------------------------------------------------------
Data Manager Christina Stanzel Rheinisches Insitut fuer
Umweltforschung an der Universitaet zu Koeln, Aachenerstr. 201-209,
D-50931 Koeln, Germany cstanzel@uni-koeln.de phone: (49)-221-27781812
Fax: (49)-221-400-2320
4.3. Data Level Definition
4.3.1. Level 1a data
Level 1a raw tracking data (closed-loop and open-loop) will be recorded
directly in the ground stations.
New Norcia (NNO):
Closed-loop IFMS data will be forwarded to the DDS at ESOC and ftped to the
home institute in Cologne .
The open-loop IFMS data is retrieved also via ftp from DDS at ESOC.
Deep Space Network (DSN):
ODF (closed-loop) and RSR (open-loop) data will be collected by JPL and
transferred to Stanford University and finally send to Cologne on CD-ROMs or via
ftp.
4.3.2. Level 1b and 2 data
Level 1b data are processed from level 1a (raw tracking data) into an ASCII
formatted file. Cologne is processing IFMS and ODF data, Stanford University
processes RSR data up to level 2 and forwards raw and processed data to
Cologne for archiving.
Level 2 data are calibrated data after further processing. The file format is
in ASCII. This data level can be used for further scientific interpretation
and will be available to the Co-Is along with the required ancillary data as
soon as available with a propriety phase of at least six months.
Level 1a to level 2 data will be archived in Cologne once all tracking and
ancillary data of a campaign are available. Target date for PDS delivery is
six months after the last data of a specific campaign have been recorded.
4.3.3. Level 3 data
Derived scientific data products (see Table 4.1) by the Co-Is will be
archived in Cologne . A certain scientific data set will be available to the
public on request after the first major publication of this data set.
4.3.4. CODMAC level definition
In the keywords DATA_SET_ID and PROCESSING_LEVEL_ID within the data labels,
CODMAC level are used instead of PSA level. In all other file names and
documents we keep the PSA data level definition as described above. For a
comparison between the two data level definition see Table 4.2.
MaRS
--------------------------------------------------------------
Science Data Product Description
--------------------------------------------------------------
Gravity LOS accelerations
Occultations Atmospheric profiles
Ionospheric profiles
Bistatic radar dielectric constant
surface roughness
Solar Corona Doppler or phase time series
Total electron content
Change in electron content
Electron density
--------------------------------------------------------------
RSI
--------------------------------------------------------------
Science Data Product Description
--------------------------------------------------------------
Gravity Low orbit LOS accelerations
Gravity field coefficients
LOS accelerations (asteroids)
Mass flux Doppler time series
LOS accelerations
Derived mass flux
Occultations Dust scatter spectra
Ionospheric profiles
Bistatic radar dielectric constant
surface roughness
refractivity
Solar Corona Doppler or phase time series
Total electron content
Change in electron content
Electron density
--------------------------------------------------------------
VeRa
--------------------------------------------------------------
Science Data Product Description
--------------------------------------------------------------
Gravity LOS accelerations
Occultations Atmospheric profiles
Ionospheric profiles
Bistatic radar dielectric constant
surface roughness
Solar Corona Doppler or phase time series
Total electron content
Change in electron content
Electron density
Table 4.1 : Examples for Science Data products (Data Level 3)
CODMAC level PSA level Description
--------------------------------------------------------------
1 | 1a | raw data
2 | 1b | edited raw data
3 | 2 | calibrated data
5 | 3 | derived scientific data
Table 4.2 : Comparison between CODMAC level and PSA level
4.4. MaRS, RSI and VeRA Archiving Functions
4.4.1. Archive Content
The complete data set size of each investigation is expected to be
approximately 200GB for MaRS, 1000GB for RSI and tbd for VeRa. The storage
media of the archival data set are CD-ROMs and DVD-ROMs. The data set will be
divided in single volumes with respect to the science objectives. Level 1a,
level1b and level 2 data will be stored on the same medium (if medium space
allows), separated into special data directories. All these directories will
be separated again into directories for different types of data, e.g. open
loop separate from closed loop and so on. Within directories, the data will
be ordered by time. Please note that not all possible directories have to be
present. For example, one data set may contain closed loop data but no open
loop data thus there is no need for an open loop subdirectory. The same is true
for data coming from IFMS and DSN. Level 3 and higher Level data will be stored
on separate data volumes.
4.4.2.Expected Number of file products
The following lists can only give an estimate and overview of the to be
archived file products and file numbers. The MEX commissioning has shown that
operational constraints and events will change the operations plan and will
have an impact on the actual number of data takings.
Mars Express MaRS
ESA IFMS
Total number of data files to be archived
-----------------------------------------
Commissioning 1: 1620
Commissioning 2: 324
Gravity: 24900
Occultation: 311250
Solar Corona: 18960
Rosetta RSI
ESA IFMS
Total number of data files to be archived
-----------------------------------------
Commissioning 1: 5940
Commissioning 2: 768
Passive Checkout: 1362 (so far)
Solar Conjunction: 12480 (so far)
Venus Express VeRa
ESA IFMS (only Closed_Loop)
Total number of data files to be archived
-----------------------------------------
Commissioning 2005: 672
Commissioning 2006: 3024
Occultation: 34656 (planned so far)
4.4.3. Single Raw Data File (level 1a) Volume
Closed-loop
IFMS Calculation (bytes) One_hour_data_recording@1_second_sampling_time
Overhead 18 kBytes
Ranging 110 x number of samples /hour 396 kBytes
Doppler 220 x number of samples/hour 792 kBytes
Meteo 100 x number of samples/hour 6 kbytes
(1 min sampling time)
DSN
ODF One_hour_data_recording@1_second_sampling_time
1.11 MB/hour
Open-Loop
IFMS Calculation (bytes) Event volume
Occultation 6 bytes*5000 samples/s 54 Mbyte (2x15 min)
Bistatic radar 6 bytes*50000 samples/s 2160 Mbyte (2 hours)
Solar corona 6 bytes*5000 samples/s(*) 648 MByte (6 hours)
RSR Calculation (bytes) Event volume (tracking pass)
Occultations 0.5 Mbytes / minute 15 Mbytes total
each channel (duration 2x 15 minutes)
each channel
Bistatic radar 12.5 Mbytes / minute 750 Mbytes total
each channel (duration 1 hour)
each channel
Solar corona 0.5 Mbytes / minute 195 Mbytes total
each channel (6.5 hours)
each channel
(*)1000 samples/s implemented in the Rosetta RSI user manual, but 5000 samples/s
aspired
The number of available tracking passes for each science objective is given in
Table 4.3.
Investigation Science_Objective #_of_tracking_passes duration Total_data
volume
MaRS Gravity TBD
Occultations 1500
Bistatic radar 200
Solar Corona 240
RSI Gravity TBD
Mass flux TBD
Occultations TBD
Bistatic radar TBD
Solar Corona TBD
VeRa Gravity TBD
Occultations TBD
Bistatic radar TBD
Solar Corona TBD
Table 4.3: Estimate for available tracking passes for each science objective
5. Archive Structure and Formats
MaRS, RSI and VeRA will issue two kinds of data volumes:
Data level 1a and 1b: Observational data (level 1b) processed from the raw
data (level 1a) as received and structured by the receiving system of the
ground stations
Data level 2: Calibrated data derived from the processed data files (level 1b)
Data Level 3: Science Data derived from Level 2 data
Data of levels 1a, 1b and 2 will be stored on the same data volume separated
into different subdirectories, if enough free capacity on the data volume is
available. Level 3 and higher Level data will be stored on separate data
volumes.
Subdirectories appearing in Table 5.1 to 5.1 but in practice will not
contain observed data or ancillary data of any level on the physical archive
volume, will not be created.
The documents listed in Table 5.1-1 to 5.1-3 represent the maximum of available
documents. Not all have to be present for one specific measurement. For IFMS
(NNO) measurements refer mainly to MRS/RSI/VRA_DOC, for DSN measurements to
DSN_DOC.
5.1. Volume Format
5.1.1. MaRS
5.1.1.1. Top-Level Directory Structure for a MaRS level 1a, 1b and 2 data volume
5.1.1.1.1. Table
ROOT
|- AAREADME.TXT description of volume contents
|- ERRATA.TXT overview of anomalies and errors
|- VOLDESC.CAT description of the contents of the logical volume
|
|- BROWSE
| |- BROWINFO.TXT Description of the BROWSE directory which
| includes Quick Look Browse Plots of the data.
|
|
|- CATALOG
| |- CATINFO.TXT text description of the directory contents
| |- MISSION.CAT PDS catalog object for Mission
| |- INST.CAT brief description of the radio systems of the s/c and
| | the ground stations
| |- INSTHOST.CAT brief description of the Instrument Host
| |- DATASET.CAT brief description of the reduced MaRS data
| |- PERSON.CAT description of key persons involved in MaRS
| |- REF.CAT collection of references uses in the inst.cat and
| | dataset.cat
| |- SOFT.CAT Dummy software catalog
|
|- CALIB
| |- CALINFO.TXT text description of the directory contents
| |- CLOSED_ LOOP
| | |- DSN Closed-loop calibration data of the DSN ground stations
| | |- IFMS
| | |- RCL Range Calibration data files
| | |- DCL Doppler Calibration data files
| | |- MET Meteo data files
| |
| |- OPEN_LOOP
| | |- DSN
| | | |- BCAL System temperature calibration files
| | | |- ION Ionospheric Calibration files
| | | |- MET Meteo data files
| | | |- TRO Tropospheric Calibration files
| | | |- SRF Surface Reflection Filer Files
| | |
| | |- IFMS
| | |- RCL Range Calibration data files
| | |- DCL Doppler Calibration data files
| | |- MET Meteo data files
| |
| |- UPLINK_FREQ_CORRECT Folder includes files which indicate wrong
| and corrected uplink frequency and their
| corresponding files.
|- DOCUMENT
| |- DOCINFO.TXT description of contents the Document Directory
| |
| |- MEX_POINTING_MODE_DESC.TXT Description of pointing modes
| |
| |- MRS_DOC
| | |
| | |- M32ESOCL1b_RCL_021202_00.PDF/.ASC
| | | Group delay stability specifications & measurements at
| | | New Norcia
| | |
| | |- M32ESOCL1b_RCL_030522_00.PDF/.ASC
| | | Range calibrations at New Norcia and Kourou
| | |
| | |- M32UNBWL1b_RCL_030801_00.PDF/.ASC
| | | Transponder group velocities (original in german, Ascii in
| | | english)
| | |
| | |- MEX-MRS-IGM-IS-3019.PDF/.ASC MaRS Data Archive Plan
| | |
| | |- MEX-MRS-IGM-IS-3016.PDF/.ASC MaRS File Naming Convention
| | |
| | |- MEX-MRS-IGM-IS-3016_APP_A.ASC MaRS File Naming Convention
| | | Appendix A, Example PDS labels
| | |
| | |- MEX-MRS-IGM-MA-3008.PDF
| | | MaRS User Manual
| | |
| | |- MARS_OPS_LOGBOOK_04.PDF
| | | status of all planned radio science operations for year 2004
| | | (later for 2005, 2006, ...) or MARS_OPS_LOGBOOK_04_COM.PDF for
| | | commissioning
| | |
| | |- MEX_MRS_IGM_DS_3035.PDF
| | | IFMS Doppler Processing and Calibration Software
| | | Documentation: Level 1a to Level 2
| | |
| | |- MEX_MRS_IGM_DS_3036.PDF
| | | IFMS Ranging Processing and Calibration Software
| | | Documentation: Level 1a to Level 2.
| | |
| | |- MEX-MRS-IGM-DS-3037.PDF ODF Processing and Calibration
| | | Software: Level 1a to Level 1b
| | | Software Design Specifications
| | |
| | |- MEX-MRS-IGM-DS-3038.PDF ODF Doppler Processing and
| | | Calibration Software: Level 1b
| | | to Level 2 Software Design
| | | Specifications
| | |
| | |- MEX-MRS-IGM-DS-3039.PDF Radio Science Predicted and
| | | Reconstructed Orbit and
| | | Planetary Constellation Data:
| | | Specifications
| | |
| | |- MEX-MRS-IGM-DS-3043.PDF ODF Ranging Processing and
| | | Calibration Software: Level 1b
| | | to Level 2 Software Design
| | | Specifications
| | |
| | |- MEX-MRS-UBW-TN-3045.PDF Reference Systems and Techniques
| | | for Simulation and Prediction of
| | | atmospheric and ionospheric
| | | sounding measurements
| | |
| | |- MEX-MRS-IGM-DS-3046.PDF Radio Science Geometry and
| | | Position Index Software Design
| | | Specifications
| | |
| | |- MEX-MRS-IGM-LI-3028.PDF List of MaRS Team members.
| |
| |-ESA_DOC
| | |
| | |- IFMS_OCCFTP.PDF documentation of IFMS data
| | | format
| | |
| | |- MEX_ESC_ID_5003_FDSICD.PDF file format description of
| | | ESOC Flight Dynamics files
| | | (ancillary files)
| | |
| | |- MEX-ESC-IF-5003_APPENDIX_C.PDF PI Account Details
| | |
| | |- MEX-ESC-IF-5003_APPENDIX_I.PDF definition of XML-schema for
| | | the data delivery interface
| | |
| | |- MEX-ESC-IF-5003_APPENDIX_H.PDF content description of ESOC
| | | Flight Dynamics files
| | | (ancillary files)
| | |
| | |- MEX-ESC-IF-5003.PDF data delivery interface
| | | document
| | |
| | |- SOP-RSSD-TN-010.PDF Planetary Science Data Archive
| | | Technical Note Geometry
| | | and Position Information
| | |
| | |- ESA-MEX-TN-4009.PDF Mars Express Archive Conventions
| |
| |- DSN_DOC
| |
| |- DSN_DESIGN_HB
| | Technical information and near future configurations of NASA
| | DSN
| |
| |- DSN_ODF_TRK-2-18.PDF
| | Documentation of Tracking System Interfaces and Orbit
| | Data File Interface
| |
| |- HGA_CALA.ASC
| | High Gain Antenna calibration (only MEX)
| |
| |- HGA_SBDA.PDF
| | S-band antenna patterns (only MEX)
| |
| |- HGA_XBDA.PDF
| | X-band antenna patterns (only MEX)
| |
| |- JPL_D-16765_RSR.PDF
| | Documentation of RSR data format
| |
| |- LIT_SIS.HTM
| | Software Interface Specification: Light Time File
| |
| |- M00DSN0L1A_DKF_....TXT (optional)
| | DSN Keyword File derived from SOE file and models of
| | activities supported by the DSN
| |
| |- M00DSN0L1A_SOE_....TXT (optional)
| | Sequence of Events file
| |
| |- M00SUE0L1A_ENB_....TXT (optional)
| | SUE Experimenter Notes
| |
| |- M00SUE0L1A_HEA_....TXT (optional)
| | DSN MEX Data Collection
| |
| |- M43DSN0L1A_NMC_....TXT (optional)
| | Network Monitor and Control Logfile
| |
| |- M43SUE0L1A_MFT_....TXT (optional)
| | Mars/Venus Express Manifest file
| |
| |- MEDIASIS.HTM
| | Media Calibration data: formats and contents
| |
| |- MON0158.ASC/.DOC/.PDF (optional)
| | Definition of format and distribution of the real-time,
| | mission monitor data
| |
| |- NMC_SIS.TXT
| | Contents of Network Monitor and Control Log.
| |
| |- OCCLOGnn.TAB
| | Summary information of MEX radio science tests and
| | experiments. nn represents the sequence number (only MEX)
| |
| |- OPTG_SIS.TXT
| | Software Interface Specification for the Orbit Propagation
| | and Timing Geometry (OPTG) file.
| |
| |- Ryddd?.ASC/.DOC/.PDF (optional)
| | Set of notes describing tests before and during radio
| | science tests or operations or the progress of an
| | experiment itself. y represents the year, ddd the DOY.
| |
| |- JPEG (optional)
| | Folder with 4 sets of 24 jpeg-files, each from a
| | different receiver, showing circularly polarized received
| | power spectra averaged over 60 seconds. FILENAME:
| | Rydddbca.jpg with y:year, ddd:doy, b:X- or S-band, c: Left-
| | or Right-Hand circulation, a:alphabetic numbering for each
| | plot of 60s.
| |
| |- SRX.TXT (optional)
| | Software Interface Specification for Surface Reflection
| | investigation files.
| |
| |- SUE_DMP.ASC/.DOC
| | Data Management Plan (only MEX)
| |
| |- TNF_SIS.TXT
| | Deep Space Mission System External Interface Specification
| |
| |- TRK_2_21.TXT
| | Software Interface Specification
| |
| |- TRK_2_23.TXT / DSN_MEDIA_CAL_TRK_2_23.PDF
| | Specification of DSN media calibration data.
| |
| |- TRK_2_24.TXT / DSN_WEA_FORMAT_TRK_2_24.PDF
| | Specification of DSN weather file.
|
|- INDEX
| |- INDXINFO.TXT description of the contents of the Index Directory
| |- INDEX.LBL detached PDS label to describe INDEX.TAB
| |- INDEX.TAB PDS table, listing all data files included in the
| | volume
| |- BROWSE_INDEX.LBL Label to describe BROWSE_INDEX.TAB
| |- BROWSE_INDEX.TAB Table listing all files in the BROWSE directory
|
|- EXTRAS
| |- EXTRINFO.TXT text description of the directory contents
| |- ANCILLARY
| |
| |- ESOC Relevant DDS files to describe the observation
| | geometry
| |- SPICE Relevant SPICE Kernels to describe the observation
| | geometry
| |- UNI_BW Relevant PREDICT files from the Uni BW Munich
| |- MRS Log-files Logfiles of Level 2 processing
| |- SUE SPICE Modified Spice Kernels
| |- DSN
| |
| |- EOP Earth Orientation parameter files
| |- LIT Light Time File
| |- OPT Orbit Propagation and Timing Geometry File
|
|- DATA
| |- LEVEL1A
| | |- CLOSED_LOOP
| | | |- DSN
| | | | |- ODF Orbit Data Files
| | | | |- Tracking and Navigation Files
| | | |
| | | |- IFMS
| | | |- AG1 Auto Gain Control 1 data files
| | | |- AG2 Auto Gain Control 2 data files
| | | |- DP1 Doppler 1 data files
| | | |- DP2 Doppler 2 data files
| | | |- RNG Ranging data files
| | |
| | |- OPEN_ LOOP
| | |- DSN
| | | |- RSR Radio-Science Receiver data files
| | |
| | |- IFMS
| | |- AG1 Auto Gain Control 1 data files
| | |- AG2 Auto Gain Control 2 data files
| | |- DP1 Doppler 1 data files
| | |- DP2 Doppler 2 data files
| | |- RNG Ranging data files
| |
| |- LEVEL1B
| | |- CLOSED_ LOOP
| | | |- DSN
| | | | |- ODF Orbit Data Files
| | | |
| | | |- IFMS
| | | |- AG1 Auto Gain Control 1 data files
| | | |- AG2 Auto Gain Control 2 data files
| | | |- DP1 Doppler 1 data files
| | | |- DP2 Doppler 2 data files
| | | |- RNG Ranging data files
| | |
| | |- OPEN_LOOP
| | | |- IFMS
| | | |- AG1 Auto Gain Control 1 data files
| | | |- AG2 Auto Gain Control 2 data files
| | | |- DP1 Doppler 1 data files
| | | |- DP2 Doppler 2 data files
| | | |- RNG Ranging data files
| |
| |- LEVEL2
| |- CLOSED_ LOOP
| | |- DSN
| | | |- ODF Orbit Data Files
| | |
| | |- IFMS
| | |- DP1 Doppler 1 data files
| | |- DP2 Doppler 2 data files
| | |- RNG Ranging data files
| |
| |- OPEN_ LOOP
| |- DSN
| | |- BSR Bistatic radar power spectra
| | |- SRG Bistatic radar surface reflection
| | | geometry file
| | |- DPX Doppler X-Band files
| | |- DPS Doppler S-Band files
| |- IFMS
| |- DP1 Doppler 1 data files
| |- DP2 Doppler 2 data files
| |- RNG Ranging data files
Table 5-1 : Top-Level Directory Structure for a MaRS processed data volume
(level 1a, 1b, 2)
5.1.2 RSI
5.1.2.1 Top-Level Directory Structure for a RSI level 1a, 1b and 2 data volume
5.1.2.1.1. Table
The table 5-2 for RSI is identical to the MaRS table 5-1, but for the
DOCUMENT folder and the subfolders RSI_DOC, DSN_DOC and ESA_DOC. For this
reason these subfolders are presented here again with the right names.
DOCUMENT
|
|- DOCINFO.TXT Description of contents of the
| Document directory.
|
|- RSI_DOC
| |
| |- M32ESOCL1B_RCL_021202_00.PDF Group delay stability specification
| | and measurements at New Norcia.
| |
| |- M32ESOCL1B_RCL_021202_00.ASC Group delay stability specification
| | and measurements at New Norcia.
| |
| |- M32ESOCL1B_RCL_030522_00.PDF Range calibrations at New Norcia
| | and Kourou.
| |
| |- M32ESOCL1B_RCL_030522_00.ASC Range calibrations at New Norcia
| | and Kourou.
| |
| |- M32UNBWL1B_RCL_030801_00.PDF Transponder group velocities (in
| | german).
| |
| |- M32UNBWL1B_RCL_030801_00.ASC Transponder group velocities (in
| | english, translated).
| |
| |- ROS_RSI_IGM_IS_3079.PDF RSI Data Archive Plan.
| |
| |- ROS_RSI_IGM_IS_3079.ASC RSI Data Archive Plan.
| |
| |- ROS_RSI_IGM_IS_3087.PDF RSI File Naming Convention.
| |
| |- ROS_RSI_IGM_IS_3087.ASC RSI File Naming Convention.
| |
| |- ROS_RSI_IGM_IS_3087_APP_A.ASC RSI File Naming Convention
| | Appendix A: Example PDS labels
| |
| |- ROS_RSI_IGM_MA_3081.PDF RSI User Manual.
| |
| |- ROS_OPS_LOGBOOK_14.PDF Status of all planned radio science
| | operations in year 2014.
| |
| |- ROS_RSI_IGM_LI_3116.PDF List of RSI Team members.
| |
| |- ROS_RSI_IGM_DS_3118.PDF IFMS Doppler Processing Software
| | Documentation: Level 1a to Level 2.
| |
| |- ROS_RSI_IGM_DS_3119.PDF IFMS Ranging Processing Software
| | Documentation: Level 1a to Level 2.
| |
| |- ROS_RSI_IGM_DS_3121.PDF Radio Science Predicted and Recon-
| | structed Orbit and Planetary Con-
| | stellation Data: Specifications
| |
| |- ROS_RSI_IGM_DS_3126.PDF Radio Science Geometry and Position
| | Index Software Design
| | Specifications
| |
| |- ROS_RSI_IGM_DS_3127.PDF ODF Processing and Calibration
| | Software: Level 1a to Level 1b
| | Software Design Specifications
|
|- ESA_DOC
| |
| |- IFMS_OCCFTP.PDF Documentation of IFMS data format.
| |
| |- RO_ESC_ID_5003_FDSICD.PDF File format description of ESOC
| | Flight Dynamics files (ancillary
| | files).
| |
| |- RO_ESC_IF_5003_APPENDIX_C.PDF Documentation of DDS
| | configuration.
| |
| |- RO_ESC_IF_5003_APPENDIX_I.PDF Definition of XML-schema for the
| | data delivery interface.
| |
| |- RO_ESC_IF_5003_APPENDIX_H.PDF Description of content of ESOC
| | Flight Dynamics files (ancillary
| | files).
| |
| |- RO_ESC_IF_5003.PDF Data delivery interface document.
| |
| |- SOP_RSSD_TN_010.pdf Planetary Science Data Archive
| | Technical Note Geometry
| | and Position Information
| |
| |- RO_EST_TN_3372.PDF Rosetta Archive Convention
| |
| |- HGA_CALA.ASC High Gain antenna
| | calibration (optional).
| |
| |- HGA_SBDA.PDF S-band antenna patterns
| | (optional).
| |
| |- HGA_XBDA.PDF X-band antenna patterns
| (optional).
|
|- DSN_DOC
| |
| |- DSN_WEA_FORMAT_TRK_2_24.PDF Specification of DSN
| | weather file.
| |
| |- DSN_ODF_TRK-2_18.PDF Documentation of
| | Tracking System Interfaces
| | and Orbit Data File
| | Interface.
| |
| |- DSN_MEDIA_CAL_TRK_2_23.PDF Specifiaction of DSN media
| | calibration data.
| |
| |- JPL_D_16765_RSR.PDF Documentation of RSR data
| | format.
| |
| |- JPEG Zip-folder with 4 sets of
| | 24 jpeg-files, each from a
| | different receiver, showing
| | circularly polarized
| | received power spectra
| | averaged over 60 seconds.
| | FILENAME: Rydddbca.jpg with
| | y:year, ddd:doy, b:X- or
| | S-band, c: Left or
| | Right-Hand circulation,
| | a:alphabetic numbering for
| | each plot of 60s
| | (optional).
| |
| |- DSN_DESIGN_HB.ASC Technical information of
| | current and near future
| | configurations of NASA DSN
| | (ASCII version).
| |
| |- DSN_DESIGN_HB.PDF Technical information of
| | current and near future
| | configurations of NASA DSN
| | (PDF version).
| |
| |- LIT_SIS.HTM Softaware interface
| | specification Light time
| | file.
| |- M00DSN0L1A_DKF_yydddhhmm_vv.TXT (optional)
| | DSN Keyword File derived
| | from SOE file and models of
| | activities supported by the
| | DSN.
| |
| |- M00DSN0L1A_SOE_yydddhhmm_vv.TXT (optional)
| | Sequence of Events file.
| |
| |- MggDSN0L1A_NMC__yydddhhmm_vv.TXT (optional)
| | Network Monitor and Control
| | Logfile.
| |
| |- MEDIASIS.HTM Media calibration data:
| | formats and contents.
| |
| |- MON0158.ASC/.DOC/.PDF (optional)
| | Definition of format and
| | distribution of the
| | real-time, mission monitor
| | data.
| |
| |- NMC_SIS.TXT Contents of network monitor
| | and control log.
| |
| |- OPTG_SIS.TXT Software Interface
| | Specification for the Orbit
| | Propagation and Timing
| | Geometry (OPTG) file.
| |
| |- SRX.TXT (optional)
| | Software Interface
| | Specification for Surface
| | Reflection investigation
| | files.
| |
| |- TNF_SIS.TXT Deep space mission system
| | external interface
| | specification.
| |
| |- TRK_2_21.TXT Software interface
| | specification.
5.1.3 VeRa
5.1.3.1 Top-Level Directory Structure for a VeRa level 1a, 1b and 2 data volume
5.1.3.1.1. Table
The table 5-3 for VeRa is identical to the MaRS table 5-1, but for the
DOCUMENT folder and the subfolders VRA_DOC and ESA_DOC. For this reason these
subfolders are presented here again with the right names. The documents in the
subfolder DSN_DOC remain mainly the same, sometimes the first letter of the
filename is changed from M (for Mars Express) to V (Venus Express).
|-DOCUMENT
| |-DOCINFO.TXT description of contents the Document Directory
| |
| |- OBSERVATION_TYPE_DESC.TXT VEX Observation types
| |
| |- VEX_POINTING_MODE_DESC.TXT VEX pointing mode description
| |
| |- VRA_DOC
| | |
| | |- M32ESOCL1b_RCL_021202_00.PDF/.ASC
| | | Group delay stability specifications & measurements at
| | | New Norcia
| | |
| | |- M32ESOCL1b_RCL_030522_00.PDF/.ASC
| | | Range calibrations at New Norcia and Kourou
| | |
| | |- M32UNBWL1b_RCL_030801_00.PDF/.ASC
| | | Transponder group velocities (original in german, Ascii in
| | | english)
| | |
| | |- VEX-VRA-IGM-IS-3007.PDF/.ASC VeRA Data Archive Plan
| | |
| | |- VEX-VRA-IGM-IS-3009.PDF/.ASC VeRa File Naming Convention
| | |
| | |- VEX-VRA-IGM-IS-3009_APP_A.ASC VeRa File Naming Convention
| | | Appendix A, Example PDS labels
| | |
| | |- VEX-VRA-IGM-MA-3005.PDF
| | | MaRS User Manual
| | |
| | |- VeRa_OPS_LOGBOOK_06.PDF
| | | status of all planned radio science operations for year 2006
| | | (later for 2007, 2008, ...)
| | |
| | |- VEX-VRA_IGM_DS_3011.PDF
| | | IFMS Doppler Processing and Calibration Software
| | | Documentation: Level 1a to Level 2
| | |
| | |- VEX-VRA_IGM_DS_3012.PDF
| | | IFMS Ranging Processing and Calibration Software
| | | Documentation: Level 1a to Level 2.
| | |
| | |- VEX-VRA-IGM-DS-5008.PDF ODF Processing and Calibration
| | | Software: Level 1a to Level 1b
| | | Software Design Specifications
| | |
| | |- VEX-VRA-IGM-DS-5009.PDF ODF Doppler Processing and
| | | Calibration Software: Level 1b
| | | to Level 2 Software Design
| | | Specifications
| | |
| | |- VEX-VRA-IGM-DS-5010.PDF ODF Ranging Processing and
| | | Calibration Software: Level 1b
| | | to Level 2 Software Design
| | | Specifications
| | |
| | |- VEX-VRA-UBW-TN-3040.PDF Reference Systems and Techniques
| | | for Simulation and Prediction of
| | | atmospheric and ionospheric
| | | sounding measurements
| | |
| | |- VEX-VRA-IGM-DS-3014.PDF Radio Science Predicted and
| | | Reconstructed Orbit and
| | | Planetary Constellation Data:
| | | Specifications
| | |
| | |- VEX-VRA-IGM-DS-5007.PDF Radio Science Geometry and
| | | Position Index Software Design
| | | Specifications
| | |
| | |- VEX-VRA-IGM-LI-3013.PDF List of VeRa Team members.
| |
| |- ESA_DOC
| | |
| | |- IFMS_OCCFTP.PDF documentation of IFMS data
| | | format
| | |
| | |- VEX_ESC_ID_5003_FDSICD.PDF file format description of
| | | ESOC Flight Dynamics files
| | | (ancillary files)
| | |
| | |- VEX-ESC-IF-5003_APPENDIX_C.PDF PI Account Details
| | |
| | |- VEX-ESC-IF-5003_APPENDIX_I.PDF definition of XML-schema for
| | | the data delivery interface
| | |
| | |- VEX-ESC-IF-5003_APPENDIX_H.PDF content description of ESOC
| | | Flight Dynamics files
| | | (ancillary files)
| | |
| | |- VEX-ESC-IF-5003.PDF data delivery interface
| | | document
| | |
| | |- SOP-RSSD-TN-010.PDF Planetary Science Data Archive
| | | Technical Note Geometry
| | | and Position Information
| | |
| | |- VEX-EST-TN-036.PDF VEX Archive Conventions
| | |
| | |- VEX-RSSD-IF-0002.PDF Specifications of operational
| | | interfaces and procedures.
| | |
| | |- MISSION_PHASE.TXT VEX Mission Phases
| | |
| | |- VEX_ORIENTATION_DESC.TXT VEX Orientation description
| | |
| | |- VEX_SCIENCE_CASE_ID_DESC.TXT VEX description of the science cases
6. Standards Used in MaRS, RSI and VeRa Data Product Generation
6.1. PDS Standards
The Standards for generating and Validation of the Data Volumes and Datasets
are based on the standards provided by the JPL?s Planetary Data System
Version 3.5. For further informations see Document Planetary Data System,
Standards Reference, JPL D-7669, Part 2.
6.2. Time Standards
MaRS, RSI and VeRa data products makes use of different Time and Reference
system. For our data processing and archiving the most important Time Systems
are:
Coordinated Universal Time (UTC)
Ephemeris Time (ET)
The scientific success of a Radio Science Experiment depends critically on a
common understanding about the conventions for the reference and time systems.
The following sections give an overview of the time standards necessary to
understand the above mentioned Time systems and to convert to other common Time
Systems. It should be noted that radio science data are generated and recorded
at ground stations. Thus the times given in the data and label files are ground
station and not onboard time.
6.2.1. Coordinated Universal Time (UTC)
Coordinated Universal Time (UTC) is obtained from atomic clocks running at the
same rate as TT (see section 12.1.3.3 ) or TAI (see section 12.1.3.2 ). The UTC
time scale is always within 0.7 seconds of UT1 (see section 12.1.3.5 ). By the
use of leap seconds, care is taken to ensure that this difference is never
exceeded. However, because of the introduction of the leap seconds it becomes
clear that this time scale is not steady.
The International Earth Rotation Service (IERS) can add leap seconds and is
normally doing this at the end of June or December of each year if necessary.
The actual UTC can only be determined for a previous point in time but
predictions for the future are published by the IERS. This fact should be
noted when future missions are planned on the base of the UTC time standard.
UTC can be obtained by the difference of the predicted value DUT1 or the past
value D UT between UT1 and UTC published in the IERS Bulletin A
(http://maia.usno.navy.mil/) which contains previous leap seconds and
predictions :
or UTC = UT - D UT
This relation is needed to obtain UT1 (UT) from UTC.
6.2.2. Dynamical Time Scale T eph for the JPL DE 405 Ephemeris
In a general relativistic framework, time is not an absolute quantity but
depends on the location and motion of a clock. Therefor unlike UTC T eph is
not based on the rotation of the earth around its axis. T eph refers to the
center of mass of the solar system and is the independent variable of barycentric
planetary ephemerides. It should be noted that during the years 1984-2003 the
time scale of ephemerides referred to the barycenter of the solar system was
the relativistic time scale Barycentric Dynamic Time TDB
(see section 12.1.3.1 ). From 2004 onwards this time scale for the JPL DE 405
ephemeris will be replaced by T eph. For practical purposes the length of
the ephemeris second can be taken as equal to the length of the TDB second.
T eph is approximately equal to TDB, but not exactly. On the other hand,
T eph is mathematically and physically equivalent to the newly-defined TCB
(see section 12.1.3.7 ), differing from it by only an offset and a constant
rate. Within the accuracy required by MaRS, RSI and VeRa we use: T eph ~ TDB.
T eph is then defined as seconds past J2000, with J2000 being 12 h 1 January
TDB.
6.2.3. Other Time Standards
6.2.3.1. Barycentric Dynamic Time (TDB)
Since the differences compared to TT are fairly small, the corrections can be
determined by the following approximation :
TDB = TT + 0.001658 sec x sin g + 0.000014 sec x sin (2g)
with g being the mean anomaly of the Earth in its orbit given by
g=357.53 + 0.95856003 x (JD(UT1)-2451545.0) [deg]
6.2.3.2. International Atomic Time (TAI)
TAI provides the practical realization of a uniform time scale based on atomic
clocks. This time is measured at the surface of the Earth. Since this time
scale is a steady one, it differs from UTC by an integral number of leap
seconds introduced up the current point in time:
TAI = UTC + LS
where LS is the number of leap seconds. The unit of TAI is the SI second.
6.2.3.3.Terrestrial Dynamic Time (TT)
Terrestial Time (TT) ? formerly Terrestrial Dynamical Time (TDT) - is to be
understood as time measured on the geoid. It has conceptionally a uniform time
scale. TT is the independent variable of geocentric ephemerides. TT replaced
Ephemeris Time (ET) in 1984. The difference between TT and the atomic time
scale (TAI) is a constant value of 32.184 seconds:
TT=TAI+32.184 sec
One therefore obtains also the relationship:
UTC=TT-32.184 sec - LS
TT does not take into account relativistic corrections. It is used as an
independent argument of geocentric ephemeris.
6.2.3.4. GMT (UT)
Time is traditionally measured in days of 86400 SI seconds. Each day has 24
hours counted from 0 h at midnight . The motion of the real sun was replaced
by the concept of a fictitious mean sun that moves uniformly in right
ascension defining the Greenwich Mean Time (GMT) or Universal Time (UT).
Greenwich Mean Sidereal Time (GMST), however, is the Greenwich hour angle of
the vernal equinox, i. e. it denotes the angle between mean vernal equinox
of date and the Greenwich meridian.
The mean vernal equinox is based on a reference system which takes into
account the secular effects, i.e. the precession of the Earth?s equator but
not periodic effects such as the nutation of the Earth?s axis.
In terms of SI seconds, the length of a sidereal day (i. e. the Earths
spin period) amounts 23 h 56 m 4 s.091 ? 0 s.005 (corresponding to a factor
1/1.00273790935) making it about four minutes shorter than a 24 h solar day.
Hence, sidereal time and mean solar time have different rates.
6.2.3.5. Universal Time (UT1)
Universal Time UT1 is the presently adopted realization of a mean solar time
scale (constant average length of a solar day of 24 hours) with UT1 = UT. As a
result, the length of one second of UT1 is not constant because of the
apparent motion of the sun and the rotation of the Earth. UT1 is therefore
defined as a function of sidereal time.
For any particular day, 0 h UT1 is defined as the instant at which Greenwich
Mean Sidereal Time (GMST) has the value:
GMST(0h UT1) = 24110.54841 sec + 8640184.812866 sec x T_0 + 0.093104 x
T_0exp(2)-0.0000062 sec x T_0exp(3)
For an arbitrary time of the day, the expression may be generalized to obtain
the Greenwich hour angle GHA by multiplying this time with the factor
1.00273790935, adding this result to GMST and convert it into degrees (if so
desired)
GMST(UT1) = 24110.54841 sec + 8640184.812866 sec x T_0 + 1.00273790935 UT1 +
0.093104 sec x Texp(2) - 0.0000062 sec x Texp(3)
where T is the time in Julian centuries since the 1st of January 2000 , 12 h,
i.e. 2000 Jan. 1.5 :
T = (JD(UT1)-2451545)/36525
and JD is the Julian Date.
Ecliptic and Earth equator at 2000 Jan 1.5 define the J2000 system.
The most useful relation for computer software is one that uses only JD (UT1):
GMST(degree) = 280.46061837 + 360.98564736629 x (JD-2451545.0) + 0.000387933
Texp(2) - Texp(3) /38710000
The difference between UT1 and TT or TAI ( atomic clock time, to be explained
below) can only be determined retrospectively. This difference is announced by
the International Earth Rotation Service (IERS) and is handled in practice by
the implementation of leap seconds (maximum of two in one year).
The above formulae contain implicitly the Earth?s mean angular rotation
omega in degrees per second [3.15].
Omega (rad/sec)=(1.002737909350795+5.9006 x 10E-11 T -5.9 x 10E-15 Texp(2))
x 2 PI/86400 sec
6.2.3.6. Geocentric Coordinate Time (TCG)
Geocentric Coordinate Time TCG represents the time coordinate of a four
dimensional reference system and differs from TT by a constant scale factor
yielding the relation
TCG = TT + L_G (JD-2443144.5) x 86400 sec
L_G = 6.9692903 x 10E-10
For practical reasons this equation can also be put into the following
relation :
TCG = TT + 2.2 s/cy x (year-1977.0)
cy = century
6.2.3.7. Barycentric Coordinate Time (TCB)
The Barycentric Coordinate Time TCB has been introduced to describe the motion
of solar system objects in a non rotating relativistic frame centered at the
solar system barycenter. TCB and TCG exhibit a rate difference which depends
on the gravitational potential of the Sun at the mean Earth-Sun distance 1 AU
and the Earth?s orbital velocity. The accumulated TCB-TT time difference
amounts to roughly 11 s around epoch J2000.
TCB = TCG + L_C (JD-2443144.5) x 86400 sec +P
(Mc Carthy 1996) and
P approximately +0.0016568 sec x sin(35999.37 degree T + 357.5 degree)
+0.0000224 sec x sin(32964.5 degree T + 246 degree)
+0.0000138 sec x sin(71998.7 degree T + 355 degree) + 0.0000048 sec x
sin(3034.9 degree T +25 degree) +
+0.0000047 x sin (34777.3 degree T +230 degree)
T=(JD-2451545.0)/36525
L_c = 1.4808268457 x 10E-8
The largest contribution is given by the first term. When neglecting the other
terms we can approximate P by:
P = 0.001658 s sin(g) + 0.000014 s sin(2g)
6.2.3.8. Julian Date (JD)
In astronomical computations, a continuous day count is used which avoids the
usage of a calendar. The Julian Date (JD) is the number of days since noon
January 1, 4712 BC including fractions of the day.
6.2.3.9. Modified Julian Date (MJD)
Since the JD has become such a large number, the Modified Julian Date was
introduced for convenience. JD was reset at November 17 th 1858 which leads to
the following equation :
MJD=JD-2400000.5 days
Note that the count for MJD starts at midnight .
6.3. Coordinate Systems
MaRS, RSI and VeRa make use of different coordinate systems (so called frames
in SPICE) with respect to the Target body and different science objectives.
There are four different frames classes:
6.3.1. Inertial Frames
Inertial frames do not accelerate with respect to the star background. They
are the frames in which Newtons laws of motion apply.
SPICE ACRONYM DESCRIPTION
J2000 Earth mean equator, dynamical equinox of J2000
MARSIAU Mars Mean Equator and IAU vector of J2000. The IAU vector at
Mars is the point on the mean equator of Mars where the equator
ascends through the the eart mean equator. This vector is the
cross of Earth mean north with Mars mean north
Table 6-1 : Inertial Frames
6.3.2. Bodyfixed Frames
Body fixed frames are reference frames that do not move with respect to
surface features of an object, but do move with respect to inertial frames.
The orientation of this frame is typically determined from the International
Astronomical Union (IAU) model for the body in question.
SPICE ACRONYM DESCRIPTION
ITRF93 International Terrestrial Reference Frame 93
IAU_MARS Mars IAU frame
IAU_MARS_BARYCENTER Mars IAU frame (origin in barycenter)
IAU_VENUS Venus IAU frame
IAU_VENUS_BARYCENTER Venus IAU frame (origin in barycenter)
IAU_PHOBOS Phobos IAU frame
IAU_DEIMOS Deimos IAU frame
Table 6-2 : Bodyfixed Frames
6.4. Earth Ellipsoid - Ground Station Coordinates
For the Earth the WGS-84 system is used as a reference ellipsoid to define the
Ground Station coordinates. The equation below shows how to compute cartesian
coordinates if the geodetic (= geocentric) longitude lambda , the geodetic
latitude phi and altitude h above the reference ellipsoid with a radius R_ref
and a flattening f are given:
r_1= (N+h) cos phi cos lambda
r_2 = (N+h) cos phi sin lambda
r_3 = (1-f exp(2) N+h ) sin phi
where
N= R_ref/sqrt(1-f (2-f) (sin exp(2) (phi)) )
and 1/f = 298.257223563
The motion of a ground station in an inertial reference system is dominated by
the Earth rotation with a velocity of 460 m/s at the equator and the
translatory motion of the Earth around the solar system barycenter
(~ 30 km/s). When the motion of the ground station is modeled in the inertial
International Celestial Reference System ICRS, the position r ITRS of the
station in the International Terrestrial Reference System (ITRS) has to be
transformed using SPICE.
6.4.1. Venus and Mars Ellipsoids
Venus has a spherical shape with an equatorial radius and polar radius of
6051.8 km. For Mars we assume a rotational symmetric ellipsoid. The polar and
equatorial semi-major axis have a length of 3376.20 km and 3396.19 km,
respectively [3.13].
6.5. Planetary Ephemeris and Planetary Coodinates
The position of the planets are calculated using the JPL/DE405 ephemeris
model. The ephemeris data are given in the barycentric time basis TDB and in
either the heliocentric or the geocentric J2000 system in a pure geometrical
sense, i.e. assuming infinite speed of light.
7. Data Validation
7.1. PSA Validation Tools
ESA developed the 'PSA Volume Verifier' (PVV) tool which is used for the
validation and delivery of a scientific dataset for ingestion to the Planetary
Science Archive (PSA). The tool allows the instrument teams to check their
datasets before delivering them to the PSA database.
The labels are verified for PDS compliance reasons and all aspects of the
dataset structure/content are validated. The PSA team will systematically
use PVV as well, before the data is ingested to the PSA.
The PVV can be downloaded using anonymous ftp from the site:
gorilla.estec.esa.int
cd /pub/projects/pvv/
The latest updates of the software will be kept there, along with the document
SOP-RDDS-UM-004, the PVV User Manual. Please refer to this document for
further details.
7.2. Radio Science Validation Process
Several Quick-Look-plots of the retrieved data are generated during processing
to Level 2. These plots are investigated to validate the measurement. Possible
decisions are then to deliver the data to the official PSA Archive, to archive
the data only internally or regard the measurement as failed.
The following section gives a short description of the Quick-Look-Plots and
their meaning for the validation process. The plots can be found in the BROWSE
folder. For more details refer to BROWINFO.TXT, also located in this folder. For
the respective terms refer to the document MEX-MRS-IGM-DS-3035/
ROS-RSI-IGM-DS-3118/VEX-VRA-IGM-IS-3011 (Doppler Processing and Calibration
Software) in the DOCUMENT folder of this dataset.
7.2.1 Residuals: Frequency_observed - Frequency_predicted
The residual should fluctuate around 0 Hz with a maximum fluctuation range of
approximately 0.1 HZ and since 2010-10-13 with a maximum fluctuation range of
approximately 0.2 HZ. Steps, peaks or a gradient in the residual should be
investigated if the data can be used. But it depends on the individual
measurement, if the data set is severely influenced by such data problems,
and on the experienced user if he accepts the data.
The time measuring device at the IFMS ground station may produce so-called
cycle-slips which can be seen in the observed frequency. This results in huge
peaks in the residuals and the data can not be used, if the number of cycle-
slips is too large.
7.2.2 AGC
The noise level of the data and the associated signal level (AGC) is dependent
on the distance between the spacecraft and the Earth. For X-Band we usually
have values of about -50/-70 dBm, for S-Band of about -70/-80 dBm. The
fluctuation range should not exceed 1 dBm. If there is a high noise-level or
the signal level is extremely low, the ground station receiver might have been
unlocked or the spacecraft operated in a non-coherent mode. No gradient or
peaks should be visible in the data. Steps can be seen if telemetry is
switched on/off, but this is not a sign for a measurement error. In case of
VEX occultations both, ingress and egress phases, can occur in one plot. A
drop of about 40 dB representing the occultation then appears in the middle
of the time interval.
7.2.3 Differential Doppler
The data should fluctuate around 0 Hz with a maximum fluctuation range of 0.1
Hz, depending on the distance between spacecraft and Earth. The Differential
Doppler is important in solar corona sounding measurements especially.
7.2.4 Calibration
7.2.4.1 Occultation
Calibration is done for occultation measurements using a Klobuchar model for
the Earth ionosphere. Besides, Meteo-files derived at the groundstation are
used for the tropospheric correction. The calibration data should show a
smooth curve with small values without any steps.
7.2.4.2 Gravity
Until begin of 2007 calibration of gravity measurements is done using the
Differential Doppler data. This calibration step corrects the effects induced
by the interplanetary plasma . This can only be done if two downlink
frequencies have been recorded. The Meteo-files derived at the groundstation
are used for the tropospheric correction. If the Differential Doppler noise is
too high, Earth ionosphere calibration is done via the Klobuchar-Coefficients.
The calibration data should then show a smooth curve of small values without
any steps. If the Differential Doppler is used, the high frequency plasma
noise superposes the calibration curve. The overall appearance depends on
the observation geometry.
Since begin of 2007 calibration is always done using the Klobuchar model for
Earth ionosphere. The Meteo-files derived at the groundstation are used for
the tropospheric correction. The calibration data should show a smooth curve
without steps and small values.
7.2.4.3 Solar Conjunction
Calibration is done for Solar Conjunction measurements with Klobuchar-
Coefficients for the Earth Ionosphere. The Meteo-files derived at the
groundstation are used for the tropospheric correction. The calibration data
should show a smooth curve with small values without any steps.
8. MaRS, RSI and VeRa Volumes and Datasets Organization, Formats and Name
Specification
8.1 Definitions and General Concept
8.1.1. Definitions
Data Product
A labelled 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.
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.
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.
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.
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.
8.1.2. Data- and Volume Set Organization
The general concept for the MaRS, RSI and VeRa Data- and Volume Set Design is
shown in Figure 8-1.
Figure 9-1 is not available in Ascii document.
8.2. Volume and Dataset Name Specification
8.2.1. Dataset
8.2.1.1. 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 the same four digit sequence number. See Table 8-1 for more information.
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 checkout, Sun)
| | CAL (for calibration)
-------------------------------------------------------------------
ZZZ | Instrument ID | MRS / RSI /VRA
-------------------------------------------------------------------
U | Data level (here | 1 raw data/ESOC/DDS
| CODMAC levels are used) | 2 edited raw data
| (*) | 3 calibrated data
| | 5 derived/scientific data
| | 1/2/3 (Data set contains raw,
| | edited and calibrated data)
--------------------------------------------------------------------
VVV | Data description | MCO
| (mission phases) | (for values see below)
--------------------------------------------------------------------
NNNN | 4 digit sequence number | 0123
|(Radio Science Volume_id)|
| |
--------------------------------------------------------------------
WWW | Version number | V1.0
Table 8-1: Dataset ID
Examples:
MEX-M-MRS-1/2/3-PRM-1144-V1.0
RO-C-RSI-1/2/3-PRL-0099-V2.0
VEX-V-VRA-1/2/3-VOI-0124-V1.0
It should be noted that the MaRS mission phase names used in the data_set_id do
not correspond to the mission phase names as defined from ESA for Mars Express.
However, since the radio science team tries to archive data for Mars Express
as well as for Venus Express and Rosetta, it was granted the use of
spacecraft-independent mission phase names which can be used for all three
missions. Nevertheless, for Venus Express the ESA-defined mission phases will be
used.
For the mission_phases definition see Table 8-2:
For Mars Express
MaRS mission name | abbreviation | time span
================================================================
Near Earth Verification | NEV | 2003-06-02 - 2003-07-31
----------------------------------------------------------------
Cruise 1 | CR1 | 2003-08-01 - 2003-12-25
----------------------------------------------------------------
Mission Comissioning | MCO | 2003-12-26 - 2004-06-30
----------------------------------------------------------------
Prime Mission | PRM | 2004-07-01 - 2005-12-31
----------------------------------------------------------------
Extended Mission 1 | EXT1 | 2006-01-01 - 2007-09-30
----------------------------------------------------------------
Extended Mission 2 | EXT2 | 2007-10-01 - 2009-12-31
----------------------------------------------------------------
Extended Mission 3 | EXT3 | 2010-01-01 - 2012-12-31
----------------------------------------------------------------
Extended Mission 4 | EXT4 | 2013-10-01 - 2014-12-31
----------------------------------------------------------------
Extended Mission 5 | EXT5 | 2015-01-01 - 2016-12-31
----------------------------------------------------------------
For Venus Express
VeRa mission name | abbreviation | time span
================================================================
Nominal Mission Phase | NMP | 2005-11-09 - 2007-10-02
----------------------------------------------------------------
Extended Mission 1 | EXT1 | 2007-10-03 - 2009-05-30
----------------------------------------------------------------
Extended Mission 2 | EXT2 | 2009-05-31 - 2010-08-21
----------------------------------------------------------------
Extended Mission 3 | EXT3 | 2010-08-22 - 2012-12-31
----------------------------------------------------------------
Extended Mission 4 | EXT4 | 2013-01-01 - 2015
----------------------------------------------------------------
Table 8-2: Mission phase description
The mission phases and their abbreviations for Venus Express will be used in
the DATA_SET_ID and DATA_SET_NAME. In the data labels, however, the value of
the keyword MISSION_PHASE_NAME is fixed and have other definitions, belonging
to defined subphases. These subphases can be found in the MISSION.CAT (CATALOG
folder of the Venus Express dataset) or in the MISSION_PHASE.TAB document
(DOCUMENT/ESA_DOC folder).
Rosetta mission phase definitions can be found in RO_EST_TN_3372.PDF in the
DOCUMENT/ESA_DOC directory.
For higher science data products data_set_id please refer to the higher
science file naming convention document MEX-MRS-RIU-IS-3050.
8.2.1.2 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. See Table 8-3 for more information.
Description | Example
==============================================================
Instrument Host Name | MARS EXPRESS
| ROSETTA ORBITER
| VENUS EXPRESS
--------------------------------------------------------------
Target name | Mars
| Venus
| 67P (for Comet Churyumov-Gerasimenko)
| Lutetia
| Steins
| Sky (commissioning VEX)
| Check (commissioning Rosetta)
--------------------------------------------------------------
Instrument id | MRS
| RSI
| VRA
--------------------------------------------------------------
CODMAC data level | 1/2/3
--------------------------------------------------------------
Data description | MISSION COMMISSIONING
mission phases for | CRUISE 1
level 1/2/3: | PRIME MISSION
(MaRS misson phases | NMP
can deviate from the | EXTENDED MISSION
MEX official phase |
names. See above) |
For higher science |
data: Measurement |
Measurement type |
--------------------------------------------------------------
A 4 digit sequence | 0123
number which is |
identical to the |
sequence number in |
the corresponding |
Radio Science |
VOLUME_ID |
--------------------------------------------------------------
Version number | V1.0
Table 8-3 : Dataset name
In order to not exceed 60 characters for the Dataset name during the Venus
Express nominal mission phase, the abbreviation 'NMP' will be used for the
mission phase within the Dataset name instead of 'NOMINAL MISSION PHASE'.
Examples:
Mars Express MARS MRS 1/2/3 Commissioning 0123 V1.0
Venus Express VENUS VRA 1/2/3 NMP 0099 V2.0
ROSETTA-ORBITER CHECK RSI 1/2/3 CRUISE 1 1144 V3.0
8.2.2. Dataset Collection
8.2.2.1. 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. See Table 8-4 for more information.
XXX_Y_ZZZ_U_VVV_IIIIIIIIII_TTT
Acronym | Description | Example
================================================================
XXX | Instrument HostID | MEX
| | RO
| | VEX
----------------------------------------------------------------
Y | Target ID | M (Mars)
| | V (Venus)
| | C (Comet 67P/Churyumov-Gerasimenko)
| | L (asteroid Lutetia)
| | S (asteroid Steins)
| | X (Sun)
-----------------------------------------------------------------
ZZZ | Instrument ID | MRS
| | RSI
| | VRA
----------------------------------------------------------------
U | Data Level(**) | 1 (Raw data)
| | 2 (Edited data)
| | 3 (Calibrated data)
| | 5 (Higher Science Data)
| | 1/2/3 (Data set contains raw, edited
| | and calibrated data)
----------------------------------------------------------------
VVV | Data Description | MCO commissioning
| (Acronym) | CR1 cruise first part
| | PRM prime mission
| | EXT extended mission
-----------------------------------------------------------------
IIIIIIIIII | Data Description |
| (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
-----------------------------------------------------------------
Table 8-4 : Dataset Collection ID
Examples:
MEX-M-MRS-1/2/3-PRM-ROCC-V1.0
ROS-W-RSI-1/2/3-MCO-GRAV-V2.0
VEX-V-VRA-1/2/3-PH5-BSR-V1.0
(*)In the keyword DATA_SET_ID the CODMAC-levels are used instead of PSA-level.
In all other file names and documents we keep PSA-level.
(**) In the keyword DATASET_COLLECTION_ID the CODMAC-levels are used instead of
PSA-level. In all other file names and documents we keep PSA-level.
8.2.3. Volume
8.2.3.1. 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. In the 4-digit number, the first one represents the volume set, the
remaining digits define the range of volumes in the volume set. For Mars
Express level 1/2/3 data and measurements taken before 1.1.2006 the first digit
U is not defined after the kind of measurement (see below for Rosetta and VEX),
but after the Mission phase (see Table 8-2).
0000: Commissioning
1000: Occultation
2000: Gravity
3000: Solar Conjunction
4000: Bistatic Radar
5000: Passive/Active Checkouts
6000: Swing-bys/Fly-bys
7000: Cometary Coma Observations
U =
0: Commissioning
1: Occultation
2: Gravity
3: Solar Conjunction
4: Bistatic Radar
5: Passive/Active Checkouts
6: Swing-bys/Fly-bys
7: Cometary Coma Observations
9: Higher Science data
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_4021, for example, denotes the 21th archived
Bistatic radar measurement recorded by the Mars Express MRS instrument since
implementation of this guideline. It is applied to measurements recorded after
the 1.1.2006. For measurements that were recorded earlier in general the radio
science volume_id was used.
XXXXXX_UZZZ
Acronym|Description |Example
=========================================
XXXXXX |Mission and Instrument ID|MEXMRS
| |ROSRSI
| |VEXVRA
------------------------------------------
UZZZ |4 digit sequence number |1001
Table 8-5 : Volume ID
Examples:
MEXMRS_1001
ROSRSI_2999
VEXVRA_3508
8.2.3.2 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.
Please note that the Volume_Version_ID is a independent
keyword and is not part of the actual Volume ID.
VV.V
Acronym | Description | Example
------------------------------------
VV.V | Volume Version ID | V1.0
Table 8-6: Volume Version ID
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.
8.2.3.3 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. Both the VOLUME ID and
the VOLUME NAME are printed on the CD-ROM or DVD label.
xxxxxx_zzzz_yyyy_ddd vv.v
Acronym| Description |Example
========================================
xxxxxx|Mission and Instrument ID|MEXMRS
| |RORSI
| |VEXVRA
---------------------------------------
zzzz |Radio Science Volume_Id |0001
---------------------------------------
yyyy |Year of the measurement |2004
----------------------------------------
ddd |Day of year of the |180
| measurement |
----------------------------------------
vv.v |Volume Version ID | V1.0
Table 8-7 : Volume name definition
Examples:
MEXMRS_0001_2003_180 V1.0
RORSI_0999_2016_355 V1.0
VEXVRA_0508_2008_190 V1.0
8.2.4. Volume Set
A volume set consists of a number of volumes.
8.2.4.1. 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. See
Table 8-8 for more information.
XXX_YYYY_ZZZ_WWW_UVVV
Acronym | Description | Example
========================================================
XXX | Abbreviation of the country of origin| GER
| | USA
--------------------------------------------------------
YYYY |The government branch | UNIK
| | NASA
--------------------------------------------------------
ZZZ | Discipline within branch | IGM
| | RIU
--------------------------------------------------------
WWW | Mission and Instrument ID | MEXMRS
| | RORSI
| | VEXVRA
-------------------------------------------------------
UVVV | A 4 digit sequence identifier | 0099
| The U digit is to 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 9.2.3.1 |
| The trailing V are wildcards that |
| represent the range of volumes in |
| the set
Table 8-8 : Volume Set ID
Examples:
GER_UNIK_IGM_MEXMRS_0099
USA_NASA_JPL_MEXMRS_0098
8.2.4.2. 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 COMMISSIONING
-----------------------------------------------------
Venus Express| VEX: RADIO SCIENCE OCCULTATION
| VEX: RADIO SCIENCE TARGET GRAVITY
| VEX: RADIO SCIENCE SOLAR CONJUNCTION
-----------------------------------------------------
Rosetta | RO: RADIO SCIENCE COMMISSIONING
Table 8-9: Volume Set Name
Examples:
MEX: RADIO SCIENCE OCCULTATION
MEX: RADIO SCIENCE GLOBAL GRAVITY
Both the VOLUME SET ID and the VOLUME SET NAME are printed on the CD-ROM or DVD
label.
8.2.5. Volume Series
A volume series consists of one or more volume sets that represent data from one
or more missions or campaigns.
8.2.5.1. 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. See Table 8-10 for details.
Spacecraft | Example
--------------------------------------
Mars Express | MISSION TO MARS
Venus Express| MISSION TO VENUS
Rosetta | MISSION TO SMALL BODIES
Table 8-10: Volume Series Name
8.3 Formats
8.3.1 Datasets
MaRS
See Document MEX-MRS-IGM-IS-3016 (Radio Science File Naming Convention and
Radio Science File Formats)
RSI
See Document ROS-RSI-IGM-IS-3087 (Radio Science File Naming Convention and
Radio Science File Formats)
VeRa
See Document VEX-VRA-IGM-IS-3009 (Radio Science File Naming Convention and
Radio Science File Formats)
8.3.2. Data Files
For information about the MaRS, RSI and VeRa Level 1a, 1b and 2 Data File
Formats see Document MEX-MRS-IGM-IS-3016/ ROS-RSI-IGM-IS-3087/
VEX-VRA-IGM-IS-3009 (Radio Science File Naming Convention and Radio Science File
Formats).