Available parameters for Swarm data

Note

See also: Jupyter notebook about data and model availability - check out the other demo notebooks there too. If you can’t see a suitable recipe to help you get started, do get in touch (email ashley.smith@ed.ac.uk) and I will help you out.

You can check which parameters are available with:

from viresclient import SwarmRequest
request = SwarmRequest()
request.available_collections()
request.available_measurements("MAG")
request.available_measurements("SW_OPER_MAGA_LR_1B")
request.available_models()
request.available_auxiliaries()

The available measurements are segregated according to the “collection” (essentially Swarm products): each collection has a number of measurements associated with it, and the appropriate collection must be set in order to access the measurements. auxiliaries are available together with any set collection. models provide magnetic model evaluation on demand, at the locations of the time series which is being accessed (when accessing magnetic field data such as MAG or MAG_HR). Standard positional variables always returned, such as Timestamp, Spacecraft, geocentric Latitude, Longitude, Radius.


See the Swarm Data Handbook for details about the products and Swarm Product Demos (Jupyter notebooks) for basic recipes to get started.


collections

Collections are grouped according to a type containing similar measurements (i.e. the same product from different spacecraft). The collection type can be given to viresclient.SwarmRequest.available_collections() to retrieve the full collection names. These cover the Swarm data products as below (replace x with A, B, or C for Alpha, Bravo, or Charlie):

Collection full name Collection type Description
SW_OPER_MAGx_LR_1B MAG Magnetic field (1Hz) from VFM and ASM
SW_OPER_MAGx_HR_1B MAG_HR Magnetic field (50Hz) from VFM
SW_OPER_EFIx_LP_1B EFI Electric field instrument (Langmuir probe measurements at 2Hz)
SW_OPER_IPDxIRR_2F IPD Ionospheric plasma characteristics (derived quantities at 1Hz)
SW_OPER_TECxTMS_2F TEC Total electron content
SW_OPER_FACxTMS_2F FAC Field-aligned currents (single satellite)
SW_OPER_FAC_TMS_2F FAC Field-aligned currents (dual-satellite A-C)
SW_OPER_EEFxTMS_2F EEF Equatorial electric field
SW_OPER_IBIxTMS_2F IBI Ionospheric bubble index

The AEBS (auroral electrojets and boundaries) products are a bit more complicated:

Collection full name Collection type Description
SW_OPER_AEJxLPL_2F AEJ_LPL Auroral electrojets line profile - Line current method (LC)
SW_OPER_AEJxLPL_2F:Quality AEJ_LPL:Quality -> Quality indicators per orbital section from LC
SW_OPER_AEJxPBL_2F AEJ_PBL -> Peaks and boundaries from LC
SW_OPER_AEJxLPS_2F AEJ_LPS Auroral electrojets line profile - SECS method
SW_OPER_AEJxLPS_2F:Quality AEJ_LPS:Quality -> Quality indicators per orbital section from SECS
SW_OPER_AEJxPBS_2F AEJ_PBS -> Peaks and boundaries from SECS
SW_OPER_AEJxPBS_2F:GroundMagneticDisturbance AEJ_PBS:GroundMagneticDisturbance -> Location and strength of peak ground disturbance per pass
SW_OPER_AOBxFAC_2F AOB_FAC Auroral oval boundaries derived from FACs

The AUX_OBS collections contain ground magnetic observatory data from INTERMAGNET and WDC. Please note that these data are provided under different usage terms than the ESA data, and must be acknowledged accordingly.

Collection full name Collection type Description
SW_OPER_AUX_OBSH2_ AUX_OBSH Hourly values derived from both WDC and INTERMAGNET data
SW_OPER_AUX_OBSM2_ AUX_OBSM Minute values from INTERMAGNET
SW_OPER_AUX_OBSS2_ AUX_OBSS Second values from INTERMAGNET

The AUX_OBS collections contain data from all observatories together (distinguishable by the IAGA_code variable). Data from a single observatory can be accessed with special collection names like SW_OPER_AUX_OBSM2_:ABK where ABK can be replaced with the IAGA code of the observatory. Use viresclient.SwarmRequest.available_observatories() to find these IAGA codes.

The measurements, models, and auxiliaries chosen will match the cadence of the collection chosen.


measurements

Choose combinations of measurements from one of the following sets, corresponding to the collection chosen above. The collection full name or collection type can be given to viresclient.SwarmRequest.available_measurements() to retrieve the list of available measurements for a given collection (e.g. request.available_measurements("SW_OPER_MAGA_LR_1B"))

Collection type Available measurement names
MAG F,dF_AOCS,dF_other,F_error,B_VFM,B_NEC,dB_Sun,dB_AOCS,dB_other,B_error,q_NEC_CRF,Att_error,Flags_F,Flags_B,Flags_q,Flags_Platform,ASM_Freq_Dev
MAG_HR F,B_VFM,B_NEC,dB_Sun,dB_AOCS,dB_other,B_error,q_NEC_CRF,Att_error,Flags_B,Flags_q,Flags_Platform,ASM_Freq_Dev
EFI U_orbit,Ne,Ne_error,Te,Te_error,Vs,Vs_error,Flags_LP,Flags_Ne,Flags_Te,Flags_Vs
IPD Ne,Te,Background_Ne,Foreground_Ne,PCP_flag,Grad_Ne_at_100km,Grad_Ne_at_50km,Grad_Ne_at_20km,Grad_Ne_at_PCP_edge,ROD,RODI10s,RODI20s,delta_Ne10s,delta_Ne20s,delta_Ne40s,Num_GPS_satellites,mVTEC,mROT,mROTI10s,mROTI20s,IBI_flag,Ionosphere_region_flag,IPIR_index,Ne_quality_flag,TEC_STD
TEC GPS_Position,LEO_Position,PRN,L1,L2,P1,P2,S1,S2,Elevation_Angle,Absolute_VTEC,Absolute_STEC,Relative_STEC,Relative_STEC_RMS,DCB,DCB_Error
FAC IRC,IRC_Error,FAC,FAC_Error,Flags,Flags_F,Flags_B,Flags_q
EEF EEF,EEJ,RelErr,Flags
IBI Bubble_Index,Bubble_Probability,Flags_Bubble,Flags_F,Flags_B,Flags_q

AEBS products:

Collection type Available measurement names
AEJ_LPL Latitude_QD,Longitude_QD,MLT_QD,J_NE,J_QD
AEJ_LPL:Quality RMS_misfit,Confidence
AEJ_PBL Latitude_QD,Longitude_QD,MLT_QD,J_QD,Flags,PointType
AEJ_LPS Latitude_QD,Longitude_QD,MLT_QD,J_CF_NE,J_DF_NE,J_CF_SemiQD,J_DF_SemiQD,J_R
AEJ_LPS:Quality RMS_misfit,Confidence
AEJ_PBS Latitude_QD,Longitude_QD,MLT_QD,J_DF_SemiQD,Flags,PointType
AEJ_PBS:GroundMagneticDisturbance B_NE
AOB_FAC Latitude_QD,Longitude_QD,MLT_QD,Boundary_Flag,Quality,Pair_Indicator

AUX_OBS products:

Collection type Available measurement names
AUX_OBSH B_NEC,F,IAGA_code,Quality,SensorIndex
AUX_OBSM B_NEC,F,IAGA_code,Quality
AUX_OBSS B_NEC,F,IAGA_code,Quality

models

Models are evaluated along the satellite track at the positions of the time series that has been requested. These must be used together with one of the MAG collections, and one or both of the “F” and “B_NEC” measurements. This can yield either the model values together with the measurements, or the data-model residuals.

Note

For a good estimate of the ionospheric field measured by a Swarm satellite (with the core, crust and magnetosphere effects removed) use a composed model defined as: models=["'CHAOS-full' = 'CHAOS-Core' + 'CHAOS-Static' + 'CHAOS-MMA-Primary' + 'CHAOS-MMA-Secondary'"] (click for more info)

This composed model can also be accessed by an alias: models=["CHAOS"] which represents the full CHAOS model

See Magnetic Earth for an introduction to geomagnetic models.

IGRF,

# Comprehensive inversion (CI) models:
MCO_SHA_2C,                                # Core
MLI_SHA_2C,                                # Lithosphere
MMA_SHA_2C-Primary, MMA_SHA_2C-Secondary,  # Magnetosphere
MIO_SHA_2C-Primary, MIO_SHA_2C-Secondary,  # Ionosphere

# Dedicated inversion models:
MCO_SHA_2D,                                # Core
MLI_SHA_2D, MLI_SHA_2E                     # Lithosphere
MIO_SHA_2D-Primary, MIO_SHA_2D-Secondary   # Ionosphere
AMPS                                       # High-latitude ionosphere

# Fast-track models:
MMA_SHA_2F-Primary, MMA_SHA_2F-Secondary,  # Magnetosphere

# CHAOS models:
CHAOS-Core,                                # Core
CHAOS-Static,                              # Lithosphere
CHAOS-MMA-Primary, CHAOS-MMA-Secondary     # Magnetosphere

# Other lithospheric models:
MF7, LCS-1

# Aliases for compositions of the above models (shortcuts)
MCO_SHA_2X    # 'CHAOS-Core'
CHAOS-MMA     # 'CHAOS-MMA-Primary' + 'CHAOS-MMA-Secondary'
CHAOS         # 'CHAOS-Core' + 'CHAOS-Static' + 'CHAOS-MMA-Primary' + 'CHAOS-MMA-Secondary'
MMA_SHA_2F    # 'MMA_SHA_2F-Primary' + 'MMA_SHA_2F-Secondary'
MMA_SHA_2C    # 'MMA_SHA_2C-Primary' + 'MMA_SHA_2C-Secondary'
MIO_SHA_2C    # 'MIO_SHA_2C-Primary' + 'MIO_SHA_2C-Secondary'
MIO_SHA_2D    # 'MIO_SHA_2D-Primary' + 'MIO_SHA_2D-Secondary'
SwarmCI       # 'MCO_SHA_2C' + 'MLI_SHA_2C' + 'MIO_SHA_2C-Primary' + 'MIO_SHA_2C-Secondary' + 'MMA_SHA_2C-Primary' + 'MMA_SHA_2C-Secondary'

Custom (user uploaded) models can be provided as a .shc file and become accessible in the same way as pre-defined models, under the name "Custom_Model".

Flexible evaluation of models and defining new derived models is possible with the “model expressions” functionality whereby models can be defined like:

request.set_products(
  ...
  models=["Combined_model = 'MMA_SHA_2F-Primary'(min_degree=1,max_degree=1) + 'MMA_SHA_2F-Secondary'(min_degree=1,max_degree=1)"],
  ...
)

In this case, model evaluations will then be available in the returned data under the name “Combined_model”, but you can name it however you like.

NB: When using model names containing a hyphen (-) then extra single (') or double (") quotes must be used around the model name. This is to distinguish from arithmetic minus (-).


auxiliaries

SyncStatus, Kp10, Kp, Dst, IMF_BY_GSM, IMF_BZ_GSM, IMF_V, F107, F10_INDEX,
OrbitDirection, QDOrbitDirection,
OrbitSource, OrbitNumber, AscendingNodeTime,
AscendingNodeLongitude, QDLat, QDLon, QDBasis, MLT, SunDeclination,
SunHourAngle, SunRightAscension, SunAzimuthAngle, SunZenithAngle,
SunLongitude, SunVector, DipoleAxisVector, NGPLatitude, NGPLongitude,
DipoleTiltAngle

Note

  • Kp provides the Kp values in fractional form (e.g 2.2), and Kp10 is multiplied by 10 (as integers)
  • F107 is the hourly 10.7 cm solar radio flux value, and F10_INDEX is the daily average
  • QDLat and QDLon are quasi-dipole coordinates
  • MLT is calculated from the QDLon and the subsolar position
  • OrbitDirection and QDOrbitDirection flags indicate if the satellite is moving towards or away from each pole, respectively for geographic and quasi-dipole magnetic poles. +1 for ascending, and -1 for descending (in latitude); 0 for no data.

Note

Check other packages such hapiclient and others from PyHC for data from other sources.