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Updated products divided by spatial

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docs/source/products/data/external_ace_swepam_timeseries.rst deleted 100644 → 0
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====================
ACE Solar Wind 1 min
====================
.. contents:: Table of contents
qui dovra' esserci la descrizione del prodotto
References
~~~~~~~~~~
qui invece la bibliografia
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- external_ace_swepam_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 101A
* - **id_tmp:**
- 101
* - **short_name:**
- ace_1minute
* - **identifier:**
- aspis:///external/ace_swepam_timeseries
* - **dynamic:**
- Approx 2MB every week
* - **size:**
- 100kB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 21599
* - **time_start:**
- 2016-12-14
* - **time_stop:**
- 2020-12-31
* - **spatial:**
- L1
* - **messenger:**
- protons,electrons
* - **spectral_min:**
- 0.26
* - **spectral_max:**
- 36
* - **spectral_units:**
- keV
* - **observable:**
- CME,SW,SEP
* - **latest update:**
- 2024-03-29 12:01:32
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC
* - 2
- ProtonDensity
- p/cc
- double
- p/cm^3
* - 3
- BulkSpeed
- km/s
- double
- km/s
* - 4
- IonTemperature
- K
- double
- K
docs/source/products/data/external_flux_goes_timeseries.rst deleted 100644 → 0
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===============
GOES X-ray Flux
===============
.. contents:: Table of contents
not available in DBF
References
~~~~~~~~~~
not available in DBF
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- external_flux_goes_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 102A
* - **id_tmp:**
- 102
* - **short_name:**
- goesx1min
* - **identifier:**
- aspis:///external/flux_goes_timeseries
* - **dynamic:**
- Approx 1MB every week
* - **size:**
- 5MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 21599
* - **time_start:**
- 2016-12-14
* - **time_stop:**
- 2020-12-31
* - **spatial:**
- L1
* - **messenger:**
- photons
* - **spectral_min:**
- 1
* - **spectral_max:**
- 8
* - **spectral_units:**
- Angstrom
* - **observable:**
- flare
* - **latest update:**
- 2024-03-28 05:08:04
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC
* - 2
- Short_Wave
- Watts/m^2
- double
- W/m^2
* - 3
- Long_Wave
- Watts/m^2
- double
- W/m^2
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================
GOES proton Flux
================
.. contents:: Table of contents
not available in DBF
References
~~~~~~~~~~
not available in DBF
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- external_part_goes_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 103A
* - **id_tmp:**
- 103
* - **short_name:**
- GOES_particle1min
* - **identifier:**
- aspis:///external/part_goes_timeseries
* - **dynamic:**
- Approx 2MB every week
* - **size:**
- 2MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 4319
* - **time_start:**
- 2016-12-14
* - **time_stop:**
- 2020-12-31
* - **spatial:**
- L1
* - **messenger:**
- protons,electrons
* - **spectral_min:**
- 1
* - **spectral_max:**
- 100
* - **spectral_units:**
- MeV
* - **observable:**
- flare,SEP,CME,ESP,SW
* - **latest update:**
- 2024-03-28 05:08:04
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC
* - 2
- P1
- Protons/cm^2 - s^-1 - sr
- double
- >=1Mev integral proton flux 5min average
* - 3
- P5
- Protons/cm^2 - s^-1 - sr
- double
- >=5Mev integral proton flux 5min average
* - 4
- P10
- Protons/cm^2 - s^-1 - sr
- double
- >=10Mev integral proton flux 5min average
* - 5
- P30
- Protons/cm^2 - s^-1 - sr
- double
- >=30Mev integral proton flux 5min average
* - 6
- P50
- Protons/cm^2 - s^-1 - sr
- double
- >=50Mev integral proton flux 5min average
* - 7
- P100
- Protons/cm^2 - s^-1 - sr
- double
- >=100Mev integral proton flux 5min average
* - 8
- E_8
- Electrons/cm^2 - s^-1 - sr
- double
- >=0.8Mev integral electron flux 5min average
* - 9
- E2_0
- Electrons/cm^2 - s^-1 - sr
- double
- >=2Mev integral electron flux 5min average
* - 10
- E4_0
- Electrons/cm^2 - s^-1 - sr
- double
- >=4Mev integral electron flux 5min average
docs/source/products/data/inaf_cpcp_superdarn_datacube.rst deleted 100644 → 0
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=============================
SuperDARN Polar Cap Potential
=============================
.. contents:: Table of contents
The Super Dual Auroral Radar Network (SuperDARN) is an international network of
High Frequency coherent scatter radars. A map of the fields of view of the radars
currently in operation can be seen in Figure 1: INAF-IAPS manages the radar pair of
Dome C East (DCE) and Dome C North (DCN) located at the Concordia station, in
Antarctica, whose fields of view are shaded in green in the figure.
The SuperDARN concept is described in detail in [2]. A SuperDARN radar is a bistatic
apparatus (i.e. the same antennae and the same electronics are used to both transmit
and receive signals to/from the ionosphere), which works in the 8-20 MHz frequency
range: coded sequences of radio pulses are steered through a field of view several tens
degrees wide along a number of “beams” (directions), so that the whole field of view
is covered in one or two minutes, depending on the operating mode. Along each beam,
the pulse sequence defines from 75 to 100 range gates, from 180 km up to 3000 km
from the radar site, where the radio signals encounter plasma density irregularities in
the ionosphere, which cause such signals to be scattered back along the same direction.
As ionospheric irregularities are dragged in the large scale convection at high latitudes, the measure of the Doppler phase shift between the emitted and backscattered waves
allows to infer the velocity of the ambient plasma with respect to the sounded direction
and gate.
References
~~~~~~~~~~
https://www.sciencedirect.com/science/article/abs/pii/S136468260600263X
[1] SuperDARN Data Analysis Working Group, Thomas, E. G., Reimer, A. S., Bland,
E. C., Burrell, A. G., Grocott, A., Ponomarenko, P. V., Schmidt, M. T., Shepherd, S. G.,
Sterne, K. T., and Walach, M.-T, SuperDARN Radar Software Toolkit (RST) 5.0 (v5.0).
Zenodo (2022). https://doi.org/10.5281/zenodo.7467337
[2] Greenwald, R.A., Baker, K.B., Dudeney, J.R. et al., DARN/SuperDARN, A global
view of the dynamics of high-latitude convection, Space Sci Rev, 71, 761–796 (1995).
https://doi.org/10.1007/BF00751350
[3] Ruohoniemi, J.M., and K.B. Baker, Large-scale imaging of high-latitude
convection with Super Dual Auroral Radar Network HF radar observations, J. Geophys. Res., Space Physics, 103, 20797-20811 (1998).https://doi.org/10.1029/98JA01288
[4] Thomas, E. G., and S. G. Shepherd, Statistical Patterns of Ionospheric Convection
Derived From Mid-latitude, High-Latitude, and Polar SuperDARN HF Radar
Observations, J. Geophys. Res., Space Physics, 123(4), 3196-3216 (2018).
https://doi.org/10.1002/2018JA025280
[5] Baker, K. B., and S. Wing, A new coordinate system for conjugate studies at high latitudes, J. Geophys. Res., 94(A7), 9139 (1989).https://doi.org/10.1029/JA094iA07p09139
[6] Shepherd, S. G., Altitude-Adjusted Corrected Geomagnetic Coordinates: Definition
and Functional Approximations, J. Geophys. Res., Space Physics, 119(9), 7501-7521
(2014). https://doi.org/10.1002/2014JA020264
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_cpcp_superdarn_datacube
* - **publisher:**
- INAF
* - **alph_code:**
- 31
* - **id_tmp:**
- 71
* - **short_name:**
- SuperDARN CPCP
* - **identifier:**
- aspis://inaf/cpcp_superdarn_datacube
* - **dynamic:**
- static
* - **size:**
- 200MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 1515672
* - **time_start:**
- 2015-06-21
* - **time_stop:**
- 2017-09-11
* - **spatial:**
- IONO
* - **messenger:**
- electrons,
* - **spectral_min:**
- 0
* - **spectral_max:**
- 1
* - **spectral_units:**
- dimensionless
* - **observable:**
- IMF,GEOINDEX
* - **latest update:**
- 2024-04-04 01:53:25
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- Time representation ISO8601: YYYY-MO-DYTHR:MN:SC
* - 2
- hem
-
- string
- Flag identifying the hemisphere where data are taken for a given record. “N”=North; “S”=South
* - 3
- ndata
- counts
- int
- Number of velocity vectors actually measured by the radars in the given time interval
* - 4
- minlat
- deg
- int
- Low latitude limit for the convection: it is the 0 described in Section 2.
* - 5
- latpole
- deg
- float
- Geographic latitude of the AACGM pole (North or South). It can be useful for coordinate transformations.
* - 6
- lonpole
- deg
- float
- Geographic longitude of the AACGM pole (North or South). It can be useful for coordinate transformations.
* - 7
- radpole
- Earth radii (Re=6371.2 km)
- float
- Distance from the centre of the Earth of the AACGM pole.
* - 8
- imfbx
- nT
- float
- GSM* x component of the interplanetary magnetic field. Data are taken from DSCOVR spacecraft, ballistically propagated to the centre of the Earth, median filtered and averaged in the 2 minutes time intervals of the radar scans. IMF is used to select the model patterns to be added to the measured vectors in order to reconstruct convection in the whole polar cap.
* - 9
- imfby
- nT
- float
- GSM* y component of the interplanetary magnetic field.
* - 10
- imfbz
- nT
- float
- GSM* z component of the interplanetary magnetic field.
* - 11
- imfbt
- nT
- float
- IMF strength. Btot = sqrt(Bx^2 + By^2 + Bz^2)
* - 12
- kpr
-
- string
- Range of geomagnetic Kp index during the given time interval. This parameter is used to select the model patterns to be added to the measured vectors in order to reconstruct convection in the whole polar cap. This field represents an information useful to be reported in the convection maps.
* - 13
- cpcp
- V
- float
- Cross Polar Cap Potential: Maximum potential difference through the polar cap.
* - 14
- maxpot
- V
- float
- Maximum positive value of the electric potential.
* - 15
- minpot
- V
- float
- Minimum negative value of the electric potential.
* - 16
- l
- counts
- int
- l-order of the harmonic expansion of the potential.
* - 17
- m
- counts
- int
- m-order of the harmonic expansion of the potential. -l ≤ m ≤ l
* - 18
- coef
- V
- float
- Alm coefficient of the harmonic expansion of the potential. If m<0, then the coefficient is the Blm in Eq. 2.
docs/source/products/data/inaf_data_solopas_timeseries.rst deleted 100644 → 0
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================================
INAF-IAPS Solar Orbiter-PAS data
================================
.. contents:: Table of contents
The product contains density N, speed vector V, pressure tensor P, temperature components (Tx, Ty, Tz), and the velocity of the satellite V_solo, computed using the data collected by the Proton-Alpha Sensor (PAS) onboard Solar Orbiter.
PAS measures the 3D distribution functions of the dominant ions of the solar wind, from 200 eV to 20 KeV, without mass and charge selection. In practice, this concerns mostly the proton and alfa populations (unseparated). At full resolution, PAS collects the 3D ion distribution function in about 1 second, even though the moments have a cadence of 4 seconds, while in “snapshot” mode the phase space sampling is reduced, allowing a greater cadence for the moments.
Data is hosted on http://soar.esac.esa.int/soar/
References
~~~~~~~~~~
R. D’Amicis et al, Astronomy &Astrophysics 656, A21 (2021)
B. Lavraud et al, Astronomy &Astrophysics 656, A37 (2021)
D. Perrone et al, Astronomy &Astrophysics 668, A189 (2022)
R. De Marco et al, Astronomy &Astrophysics, 669, A108 (2023)
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_data_solopas_timeseries
* - **publisher:**
- INAF-IAPS, Plasma & Space Weather Group
* - **alph_code:**
- 14
* - **id_tmp:**
- 72
* - **short_name:**
- SolO-PAS_data
* - **identifier:**
- aspis://inaf/data_solopas_timeseries
* - **dynamic:**
- a file each day (file size between 3 and 4 Mb). As a general rule, one month of data is uploaded each month, generally relating to 3 months before the upload date
* - **size:**
- 2GB
* - **format:**
- dsv
* - **type:**
- timeseries
* - **records_number:**
- 38653
* - **time_start:**
- 2020-07-06
* - **time_stop:**
- 2022-01-31
* - **spatial:**
- IP
* - **messenger:**
- Protons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- SW,SEP
* - **latest update:**
- 2024-04-04 01:54:59
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- Datetime [UTC ]
* - 2
- N
- cm^-3
- float
- Protono Density [cm^-3]
* - 3
- VR
- Km/s
- float
- Proton Velocity along the R direction [Km/s]
* - 4
- VT
- Km/s
- float
- Proton Velocity along the T direction [Km/s]
* - 5
- VN
- Km/s
- float
- Proton Velocity along the N direction [Km/s]
* - 6
- T
- eV
- float
- Proton Temperature [eV]
* - 7
- VR_SolO
- Km/s
- float
- Spacecraft Velocity along the R direction [Km/s]
* - 8
- VT_SolO
- Km/s
- float
- Spacecraft Velocity along the T direction [Km/s]
* - 9
- VN_SolO
- Km/s
- float
- Spacecraft Velocity along the N direction [Km/s]
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=============================================
SVIRCO Observatory - the Rome neutron monitor
=============================================
.. contents:: Table of contents
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 1h. Average intensity of January-February 1997 = 100%
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_flux1h_svirco_timeseries
* - **publisher:**
- INAF
* - **alph_code:**
- 42C
* - **id_tmp:**
- 73
* - **short_name:**
- flux1h_SVIRCO
* - **identifier:**
- inaf_flux1h_svirco_timeseries
* - **dynamic:**
- Data collection grows in time.
* - **size:**
- 13MB
* - **format:**
- CSV
* - **type:**
- timeseries
* - **records_number:**
- 479976
* - **time_start:**
- 1966-04-01
* - **time_stop:**
- 2020-12-31
* - **spatial:**
- GROUND
* - **messenger:**
- Nucleons
* - **spectral_min:**
- 6.3
* - **spectral_max:**
- 9999
* - **spectral_units:**
- GeV
* - **observable:**
- GLE,GCR
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC - Time
* - 2
- I
- %
- float
- % - Normalized Intensity of the cosmic ray secondary nucleonic component measured by the Rome neutron monitor. The counting rates have been normalized to the reference value of January-February 1997 (= 100%).
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==============================================
SVIRCO Obser vatory - the Rome neutron monitor
==============================================
.. contents:: Table of contents
Intensity in percent of cosmic ray secondary nucleonic component of Rome neutron monitor. Data corrected for pressure with barometric coefficient variable with solar cycle and corrected for efficiency changes. Resolution: 5min Average intensity of January-February 1997 = 100%
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_flux5m_svirco_timeseries
* - **publisher:**
- INAF
* - **alph_code:**
- 42B
* - **id_tmp:**
- 74
* - **short_name:**
- flux5m_SVIRCO
* - **identifier:**
- inaf_flux5m_svirco_timeseries
* - **dynamic:**
- Data collection grows in time.
* - **size:**
- 80MB
* - **format:**
- CSV
* - **type:**
- timeseries
* - **records_number:**
- 2007072
* - **time_start:**
- 1997-05-21
* - **time_stop:**
- 2017-01-01
* - **spatial:**
- GROUND
* - **messenger:**
- Neutrons
* - **spectral_min:**
- 6.3
* - **spectral_max:**
- 9999
* - **spectral_units:**
- GeV
* - **observable:**
- GLE,GCR
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC - time
* - 2
- inc
- counts
- int
- Counting rates (not pressure corrected) of the cosmic ray secondary nucleonic component measured by the Rome neutron monitor
* - 3
- pressure
- hPa
- float
- Pressure measured at the SVIRCO Observatory
* - 4
- corr
- counts
- int
- Efficiency and pressure corrected counting rates of the cosmic ray secondary nucleonic component measured by the Rome neutron monitor
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=====================================================
IAPS Grad-Shafranov Reconstruction of Magnetic Clouds
=====================================================
.. contents:: Table of contents
Quasi 3-d magnetic field maps of magnetic field configuration within magnetic clouds for geoeffective target SWE events. Such maps will be estimated through the Grad-Shafranov reconstruction from single-spacecraft plasma and magnetic field data.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_gsmaps_datacube
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 25
* - **id_tmp:**
- 96
* - **short_name:**
- gsmaps-cubes
* - **identifier:**
- aspis://inaf/gsmaps_datacube
* - **dynamic:**
- static
* - **size:**
- 300kB
* - **format:**
- nc
* - **type:**
- spectrum
* - **records_number:**
- 3
* - **time_start:**
- 1997-01-01
* - **time_stop:**
- 2022-01-01
* - **spatial:**
- IP
* - **messenger:**
- Magnetic field,Magnetic vector potential,Flux rope coordinates
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- phys.magField,phys.potential,phys.size
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC - datetime - Time associated with the Grad-Shafranov reconstruction
* - 2
- data_name
- char
- string
- the name of the file with the data
* - 3
- prew_name
- char
- string
- the name of the full preview file
* - 4
- thumb_name
- char
- string
- the name of the thumbnail file
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==============================
IAPS ≥M2 SXR Flare Catalogue
==============================
.. contents:: Table of contents
The catalogue will contain the > M2 Soft X- Ray (SXR) flares from 1995 to 2017. The columns in the table are defined as follows: (1) event number (2) date of the SXR flare (3) peak time of SXR flare (4) peak SXR classification (saturated events flagged with an S in which case (3) refers to the onset of saturation), (5) flare location, (6) time-integrated SXR intensity (nominally between the 1/3 power points on rise and fall), (7) time-integrated 1 MHz Wind/WAVES intensity from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak, (8) Waves frequency used.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_m2flare_tableset
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 7
* - **id_tmp:**
- 75
* - **short_name:**
- IAPS-M2SXR
* - **identifier:**
- aspis://inaf/m2flare_tableset
* - **dynamic:**
- static
* - **size:**
- 100kB
* - **format:**
- xlsx
* - **type:**
- tableset
* - **records_number:**
- 1040
* - **time_start:**
- 1995-01-01
* - **time_stop:**
- 2017-05-03
* - **spatial:**
- SUN
* - **messenger:**
- Photons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- phys.flux
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- Onset date and time of each flare event
* - 2
- Date
- yyyy/mm/dd
- datetime
- Onset date of each flare event
* - 3
- SXR Peak Time
- hh:mm:ss XM
- datetime
- Time corresponding to the peak SXR flux
* - 4
- SXR Class
-
- string
- Classification of SXR bursts according to their peak intensities
* - 5
- SXR Class Label
-
- string
- Letter indicating the Peak SXR flux range, according to the standard SXR classification
* - 6
- SXR Class Intensity
- <unit>
- float
- Number indicating the factor for the flare within the class
* - 7
- Location Halpha-line
-
- string
- Averaged heliographic position of flare central region from observations on the H-alpha spectral line
* - 8
- HGS lat
- deg
- float
- Averaged heliographic latitude of flare central region from observations on the H-alpha spectral line
* - 9
- HGS lon
- deg
- float
- Averaged heliographic longitude of flare central region from observations on the H-alpha spectral line
* - 10
- SXR Fluence
- J/m^2
- float
- Time integrated SXR intensity between the 1/3 power points on rise and fall (J m^2)
* - 11
- Wind/Waves Fluence
- sfu*min
- float
- Time integrated 1 MHz intensity from Wind/Waves from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak (sfu x min)
* - 12
- Frequency
- kHz
- int
- Used Wind/Waves frequency close to 1 MHz (Hz)
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===============================================
INAF-bidimensional maps of Mercury Na exosphere
===============================================
.. contents:: Table of contents
Dataset of observations of Mercury's exosphere in the sodium D lines. Data are taken from the ground-based solar telescope THEMIS (years 2009-2013). They have been produced in both D1 and D2 lines (when both available) and converted into bi-dimensional maps of Rayleigh emission. Estimation of the “seeing” parameter is included in the jpeg files. Here the original fits files are given too for the whole data base (2007-2014), and it may be expanded to the most recent data from 2021 and 2022 (TBC). Data can be provided both uncalibrated and/or calibrated (TBD).
References
~~~~~~~~~~
Leblanc, F., Doressoundiram, A., Schneider, N., Mangano, V., López Ariste, A., Lemen, C., Gelly, B., Barbieri, C. and Cremonese, G., 2008. High latitude peaks in Mercury's sodium exosphere: Spectral signature using THEMIS solar telescope. Geophysical Research Letters, 35(18).
Leblanc, F., Doressoundiram, A., Schneider, N., Massetti, S., Wedlund, M., López Ariste, A., Barbieri, C., Mangano, V. and Cremonese, G., 2009. Short‐term variations of Mercury's Na exosphere observed with very high spectral resolution. Geophysical research letters, 36(7).
Mangano, V., Massetti, S., Milillo, A., Mura, A., Orsini, S. and Leblanc, F., 2013. Dynamical evolution of sodium anisotropies in the exosphere of Mercury. Planetary and Space Science, 82, pp.1-10.
Mangano, V., Massetti, S., Milillo, A., Plainaki, C., Orsini, S., Rispoli, R. and Leblanc, F., 2015. THEMIS Na exosphere observations of Mercury and their correlation with in-situ magnetic field measurements by MESSENGER. Planetary and Space Science, 115, pp.102-109.
Massetti, S., Mangano, V., Milillo, A., Mura, A., Orsini, S. and Plainaki, C., 2017. Short‐term observations of double‐peaked Na emission from Mercury's exosphere. Geophysical Research Letters, 44(7), pp.2970-2977.
Orsini, S., Mangano, V., Milillo, A., Plainaki, C., Mura, A., Raines, J.M., De Angelis, E., Rispoli, R., Lazzarotto, F. and Aronica, A., 2018. Mercury sodium exospheric emission as a proxy for solar perturbations transit. Scientific reports, 8(1), p.928.
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_na_mercexo_image
* - **publisher:**
- Valeria Mangano, INAF-IAPS
* - **alph_code:**
- 57
* - **id_tmp:**
- 76
* - **short_name:**
- Merc_exos_Na_fts
* - **identifier:**
- aspis://inaf/na_mercexo_image
* - **dynamic:**
- period 2009-2013 is static, but if we decide to include also most recent data, it will grow in time.
* - **size:**
- 1GB
* - **format:**
- fits
* - **type:**
- image
* - **records_number:**
- 7
* - **time_start:**
- 2009-04-17
* - **time_stop:**
- 2013-05-25
* - **spatial:**
- Mercury
* - **messenger:**
- photons
* - **spectral_min:**
- 5890
* - **spectral_max:**
- 5896
* - **spectral_units:**
- Angstrom
* - **observable:**
- IMF,SW,CME
* - **latest update:**
- 2024-04-04 01:59:34
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- date and time of start of spectral scan
* - 2
- heliocentric_longitude
- deg
- float
- Mercury heliocentric longitude [deg]
* - 3
- heliocentric_latitude
- deg
- float
- Mercury heliocentric latitude [deg]
* - 4
- heliocentric_distance
- AU
- float
- Mercury heliocentric distance [AU]
* - 5
- true_anomaly_angle
- deg
- float
- Mercury True Anomaly Angle [deg]
* - 6
- phase_angle
- deg
- float
- Mercury Phase Angle [deg]
* - 7
- disk_visibility
- %
- float
- Percentage of Mercury disk lit by the Sun
* - 8
- seeing
- arcsec
- float
- estimated seeing during the spectral scan [arcsec]
* - 9
- seeing err
- arcsec
- float
- error associated with the seeing estimation [arcsec]
* - 10
- ave emission
- kR
- float
- Average value of the D2 Na emission [kR]
* - 11
- emission err
- kR
- float
- error associated with the Average value of the Na emission [kR]
* - 12
- type
- char
- string
- code for emission peaks morphology according to doi.org/10.1016/j.pss.2015.04.001
* - 13
- data_name
- char
- string
- the name of the file with the data
* - 14
- prew_name
- char
- string
- the name of the full preview file
* - 15
- thumb_name
- char
- string
- the name of the thumbnail file
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============================
IAPS S1 SEP events Catalogue
============================
.. contents:: Table of contents
The catalogue contains SEP events observed at the Earth of class S1, i.e. with flux in the range [10, 100) pfu, at >10 MeV from 1995 and their properties (onset, peak flux, fluence) as well as features of the associated flare (peak time, class, location), CME (lift off, position, angle width, speed) and radio burst (occurrence of type II or IV). The SEP events having flux >= 100 pfu at > 10 MeV are listed in the companion table S2 SEP Catalogue.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_s1sep_tableset
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 16A
* - **id_tmp:**
- 77
* - **short_name:**
- IAPS-S1 SEP events
* - **identifier:**
- aspis://inaf/s1sep_tableset
* - **dynamic:**
- static
* - **size:**
- 100kB
* - **format:**
- csv
* - **type:**
- tableset
* - **records_number:**
- 68
* - **time_start:**
- 1995-01-01
* - **time_stop:**
- 2014-09-10
* - **spatial:**
- Earth
* - **messenger:**
- Protons,Photons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- flare,CME,SEP
* - **latest update:**
- 2024-03-28 05:08:05
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- utc
- datetime
- UTC - Time of the peak of the SEP associated soft X -ray (SXR) flare. When the time coincides with that of the CME no information about the actual time was available.
* - 2
- SXR_class
- char
- char
- Char - Class of the SEP associated flare according to their peak intensities
* - 3
- Flare_Latitude
- deg
- float
- Degrees - Averaged heliographic latitude of the SEP associated flare central region from observations of the H-alpha spectral line
* - 4
- Flare_Longitude
- deg
- float
- Degrees - Averaged heliographic longitude of the SEP associated flare central region from observations of the H-alpha spectral line. The value 180 indicates longitudes >90, when it cannot be better determined. The value -180 indicates longitudes >90, when
* - 5
- CME_NOAA_date
- utc
- datetime
- UTC - Date and time of the associated CME from the NOAA list (https://umbra.nascom.nasa.gov/SEP/)
* - 6
- CME_SOHO_date
- utc
- datetime
- UTC - In case the CME NOAA Date was not present or not considered reliable in the previous column, the date and time of the associated CME from the SOHO list (https://cdaw.gsfc.nasa.gov/CME_list/UNIVERSAL_ver1/1998_05/univ1998_05.html) is given in this c
* - 7
- CME_central_PA
- deg
- float
- Degrees - CME position angle measured from Solar North in degrees (counter-clockwise). The value 360 indicates a halo CME.
* - 8
- Halo_CME_type
- char
- char
- Char - Halo CMEs are indicated in the 'CME_Central_PA' column with 360. In this column the letters ('S', 'BA', 'OA') in the brackets show type of halo CMEs. Halo CMEs can be symmetric (S) or asymmetric with respect to the occulting disk. Brightness asymme
* - 9
- CME_angular_width
- deg
- float
- Degrees - Angular width of the CME. For values =361 more information are available in the sOHO LASCO CME catalogue (https://cdaw.gsfc.nasa.gov/CME_list/).
* - 10
- CME_Speed_Art1
- km/s
- float
- km/s - CME speed from catalogue of article 1 (Art1) Papaioannou et a. 2016 (doi: 10.1051/swsc/2016035)
* - 11
- Radio_burst_type_II
- char
- int
- Int - Occurrence of type II radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 12
- Radio_burst_type_IV
- char
- int
- Int - Occurrence of type IV radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 13
- CME_Speed_Art2
- km/s
- float
- km/s - CME speed from catalogue of article2 (ART2) Gopalswamy et al. 2015 (doi: 10.48550/arXiv.1509.04216)
* - 14
- SOHO_CME_linear_speed
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through linear fit of height-time measurements
* - 15
- SOHO_CME_speed_2nd
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated at the time of final height measurement
* - 16
- SOHO_CME_speed_20_Rs
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated when the CME is at a height of 20 solar radii
* - 17
- CME_acceleration
- km/s^2
- float
- km/s^2 - Acceleration of the CME
* - 18
- SXR_Fluence
- J/m^2
- float
- J m^2 - Time integrated SXR intensity between the 1/3 power points on rise and fall (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 19
- Radio_Fluence
- sfu*min
- float
- sfu*min - Time integrated 1 MHz intensity from Wind/Waves from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 20
- Frequency
- kHz
- float
- kHz - Used Wind/Waves frequency close to 1 MHz in computing the Radio_Fluence in the previous column
* - 21
- SEP_onset
- utc
- datetime
- UTC - SEP onset time
* - 22
- SEP_threshold
- utc
- datetime
- UTC - Time at which the >10 MeV proton flux exceeds the 10 pfu threshold
* - 23
- SEP_Peak_time
- utc
- datetime
- UTC - Peak proton flux time at >10 MeV energies
* - 24
- SEP_end
- utc
- datetime
- UTC - Time at the end of the SEP event at >10 MeV energies
* - 25
- Peak_proton_flux
- pfu
- float
- pfu=1/(cm^2 s sr) - Peak proton flux at >10 MeV energies
* - 26
- Proton_fluence
- #/(cm^2*sr)
- float
- #/(cm^2 sr) - Time integrated proton flux in the onset-end time interval
* - 27
- GLE
- char
- char
- Char - YES or NO flag indicating the presence or the absence of a Ground Level Enhancement event, respectively.
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============================
IAPS S2 SEP events Catalogue
============================
.. contents:: Table of contents
The catalogue contains SEP events observed at the Earth of class S2, i.e. with flux >100 pfu, at >10 MeV from 1995 and their properties (onset, peak flux, fluence) as well as features of the associated flare (peak time, class, location), CME (lift off, position, angle width, speed) and radio burst (occurrence of type II or IV). The SEP events having flux in the interval [10, 100) pfu at > 10 MeV are listed in the companion table S1 SEP Catalogue.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_s2sep_tableset
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 16B
* - **id_tmp:**
- 78
* - **short_name:**
- IAPS-S2 SEP events
* - **identifier:**
- aspis://inaf/s1sep_tableset
* - **dynamic:**
- static
* - **size:**
- 100kB
* - **format:**
- csv
* - **type:**
- tableset
* - **records_number:**
- 60
* - **time_start:**
- 1995-01-01
* - **time_stop:**
- 2014-09-10
* - **spatial:**
- Earth
* - **messenger:**
- Protons,Photons
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- flare,CME,SEP
* - **latest update:**
- 2024-03-28 05:08:06
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- utc
- datetime
- UTC - Time of the peak of the SEP associated soft X -ray (SXR) flare. When the time coincides with that of the CME no information about the actual time was available.
* - 2
- SXR_class
- char
- char
- Char - Class of the SEP associated flare according to their peak intensities
* - 3
- Flare_Latitude
- deg
- float
- Degrees - Averaged heliographic latitude of the SEP associated flare central region from observations of the H-alpha spectral line
* - 4
- Flare_Longitude
- deg
- float
- Degrees - Averaged heliographic longitude of the SEP associated flare central region from observations of the H-alpha spectral line. The value 91 indicates longitudes >90 the value 121 indicates longitudes >120 the value -91 indicates longitudes<-90.
* - 5
- CME_NOAA_date
- utc
- datetime
- UTC - Date and time of the associated CME from the NOAA list (https://umbra.nascom.nasa.gov/SEP/)
* - 6
- CME_SOHO_date
- utc
- datetime
- UTC - In case the CME NOAA Date was not present or not considered reliable in the previous column, the date and time of the associated CME from the SOHO list (https://cdaw.gsfc.nasa.gov/CME_list/UNIVERSAL_ver1/1998_05/univ1998_05.html) is given in this c
* - 7
- CME_central_PA
- deg
- float
- Degrees - CME position angle measured from Solar North in degrees (counter-clockwise). The value 360 indicates a halo CME.
* - 8
- Halo_CME_type
- char
- char
- Char - Halo CMEs are indicated in the 'CME_Central_PA' column with 360. In this column the letters ('S', 'BA', 'OA') in the brackets show type of halo CMEs. Halo CMEs can be symmetric (S) or asymmetric with respect to the occulting disk. Brightness asymme
* - 9
- CME_angular_width
- deg
- float
- Degrees - Angular width of the CME. For values =-361 more information are available in the sOHO LASCO CME catalogue (https://cdaw.gsfc.nasa.gov/CME_list/).
* - 10
- CME_Speed_Art1
- km/s
- float
- km/s - CME speed from catalogue of article 1 (Art1) Papaioannou et a. 2016 (doi: 10.1051/swsc/2016035)
* - 11
- Radio_burst_type_II
- char
- int
- Int - Occurrence of type II radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 12
- Radio_burst_type_IV
- char
- int
- Int - Occurrence of type IV radio burst: the value 1 indicates that the burst occurred the value 2 indicates that the burst occurred with a probability >50% the value 3 indicates that the burst occurred with a probability <50 the value 0 indicates that th
* - 13
- CME_Speed_Art2
- km/s
- float
- km/s - CME speed from catalogue of article2 (ART2) Gopalswamy et al. 2015 (doi: 10.48550/arXiv.1509.04216)
* - 14
- SOHO_CME_linear_speed
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through linear fit of height-time measurements
* - 15
- SOHO_CME_speed_2nd
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated at the time of final height measurement
* - 16
- SOHO_CME_speed_20_Rs
- km/s
- float
- km/s - Speed from SOHO catalogue obtained through quadratic fit of height-time measurements. The speed is evaluated when the CME is at a height of 20 solar radii
* - 17
- CME_acceleration
- km/s^2
- float
- km/s^2 - Acceleration of the CME
* - 18
- SXR_Fluence
- J/m^2
- float
- J m^2 - Time integrated SXR intensity between the 1/3 power points on rise and fall (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 19
- Radio_Fluence
- sfu*min
- float
- sfu*min - Time integrated 1 MHz intensity from Wind/Waves from 10 minutes before the onset of integration for the SXR burst to 10 minutes after the SXR burst peak (see Laurenza et al., 2009, doi: 10.1029/2007SW000379)
* - 20
- Frequency
- kHz
- float
- kHz - Used Wind/Waves frequency close to 1 MHz in computing the Radio_Fluence in the previous column
* - 21
- SEP_onset
- utc
- datetime
- UTC - SEP onset time
* - 22
- SEP_threshold
- utc
- datetime
- UTC - Time at which the >10 MeV proton flux exceeds the 10 pfu threshold
* - 23
- SEP_Peak_time
- utc
- datetime
- UTC - Peak proton flux time at >10 MeV energies
* - 24
- SEP_end
- utc
- datetime
- UTC - Time at the end of the SEP event at >10 MeV energies
* - 25
- Peak_proton_flux
- pfu
- float
- pfu=1/(cm^2 s sr) - Peak proton flux at >10 MeV energies
* - 26
- Proton_fluence
- #/(cm^2*sr)
- float
- #/(cm^2 sr) - Time integrated proton flux in the onset-end time interval
* - 27
- GLE
- char
- char
- Char - YES or NO flag indicating the presence or the absence of a Ground Level Enhancement event, respectively.
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================================================
IAPS Test Particle Simulation on Magnetic Clouds
================================================
.. contents:: Table of contents
Galactic cosmic ray intensity variations associated to the passage of magnetic clouds. The particle intensity variation is estimated through a dedicated full-orbit test-particle simulation.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_tps_datacube
* - **publisher:**
- INAF - Istituto di Astrofisica e Planetologia Spaziali
* - **alph_code:**
- 51
* - **id_tmp:**
- 97
* - **short_name:**
- IAPS-TPS
* - **identifier:**
- aspis://inaf/tps_datacube
* - **dynamic:**
- static
* - **size:**
- 300kB
* - **format:**
- nc
* - **type:**
- spectrum
* - **records_number:**
- 3
* - **time_start:**
- 1997-01-01
* - **time_stop:**
- 2022-01-01
* - **spatial:**
- Interplanetary Space (not L1 and Planets),Sun-Earth L1
* - **messenger:**
- Particle intensity variation
* - **spectral_min:**
-
* - **spectral_max:**
-
* - **spectral_units:**
-
* - **observable:**
- phys.flux,phys.particle.proton
* - **latest update:**
- 2024-03-28 05:08:06
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- UTC - datetime - Time associated with the simulation
* - 2
- data_name
- char
- string
- the name of the file with the data
* - 3
- prew_name
- char
- string
- the name of the full preview file
* - 4
- thumb_name
- char
- string
- the name of the thumbnail file
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======================================================================================
IAPS - Wind velocity-magnetic field correlation coefficient data of solar wind streams
======================================================================================
.. contents:: Table of contents
The velocity - magnetic field (v-b) correlation coefficient unables to identify Alfvénic solar wind intervals (along with almost constant magnetic field magnitude and proton number density). It is derived as the ratio between the covariance of velocity and magnetic field (in Alfvén units) components and the product of their standard deviations, in a time window ranging between tens of minutes to hours. In principle, this formula should be applied to every component of the velocity (V_i) and magnetic fields (B_i) (with i = R, T, N in RTN coordinate system or i = X, Y, Z in GSE coordinate system). The total correlation coefficient is then derived as the average from the three components. However, for the sake of simplicity, we consider only the N component since more Alfvénic than the other two.
References
~~~~~~~~~~
D’Amicis et al, GRL, 34, L05108, 2007; Frontiers in Physics, 8, 541, 2020
Telloni et al, ApJ, 916, 64, 2021
D’Amicis et al, A&A, 656, A21, 2021
Tu et al., JGR, 94, 11739, 1989
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- inaf_vbcorr_wind_tableset
* - **publisher:**
- INAF-IAPS, Fisica dei Plasmi Spaziali e Space Weather
* - **alph_code:**
- 24C
* - **id_tmp:**
- 98
* - **short_name:**
- wind_v-b_corr
* - **identifier:**
- aspis://inaf/vbcorr_wind_tableset
* - **dynamic:**
- static
* - **size:**
- 35MB
* - **format:**
- csv
* - **type:**
- tableset
* - **records_number:**
- 538
* - **time_start:**
- 1998-10-01
* - **time_stop:**
- 2022-05-06
* - **spatial:**
- L1
* - **messenger:**
- protons
* - **spectral_min:**
- 0
* - **spectral_max:**
- 0
* - **spectral_units:**
- -
* - **observable:**
- SW
* - **latest update:**
- 2024-04-04 02:05:02
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- 2017-03-25T00:00:06 [UTC] - the UTC time associated to the masure
* - 2
- vb_coeff_corr
- number
- float
- -0.98 [dimensionless] the Pearson's correlation coefficient between the normal components of velocity and magnetic field
* - 3
- sample
- number
- int
- 75 [samples] the number of observations available in the 30-min window
* - 4
- scale
- min
- int
- 30 [minutes] the length of the window, i.e. 30 min
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===============================================================================================
HEPD-01 time-integrated proton spectrum during the Ground-Level Enhancement of October 28, 2021
===============================================================================================
.. contents:: Table of contents
Time-integrated spectrum of solar protons measured by the HEPD-01 detector from space during the Ground-Level Enhancement of October 28, 2021
References
~~~~~~~~~~
https://agupubs.onlinelibrary.wiley.com/doi/full/10.1029/2022SW003191
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_cses_hepd_spectrum
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 44C
* - **id_tmp:**
- 106
* - **short_name:**
- HEPD-proton
* - **identifier:**
- aspis://infn/infn_cses_hepd_spectrum
* - **dynamic:**
-
* - **size:**
- 10kB
* - **format:**
- csv
* - **type:**
- spectrum
* - **records_number:**
- 1
* - **time_start:**
- 2021-10-28
* - **time_stop:**
- 2021-11-03
* - **spatial:**
- GEOMAG
* - **messenger:**
- protons
* - **spectral_min:**
- 55
* - **spectral_max:**
- 250
* - **spectral_units:**
- MeV
* - **observable:**
- GLE,flare,SEP,GCR,CME
* - **latest update:**
- 2024-04-04 02:08:35
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime (2021-10-28T00:00:00.000) (time.epoch) - Reference time of the event
* - 2
- start_time
- UTC
- datetime
- datetime (2021-10-28T00:00:00.000) (time.epoch) - Start time of the data integration
* - 3
- end_time
- UTC
- datetime
- datetime (2021-11-03T23:59:59.000) (time.epoch) - End time of the data integration
* - 4
- spacecraft
- char
- string
- the name of the spacecraft
* - 5
- data_name
- char
- string
- the name of the file with the data
* - 6
- prew_name
- char
- string
- the name of the full preview file
* - 7
- thumb_name
- char
- string
- the name of the thumbnail file
docs/source/products/data/infn_iss_ams_flux_timeseries.rst deleted 100644 → 0
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===========================================
INFN AMS daily proton time dependent fluxes
===========================================
.. contents:: Table of contents
Daily proton fluxes in cosmic rays were measured with the Alpha Magnetic Spectrometer aboard the International Space Station, from May 20, 2011 to October 29, 2019 (a total of 2824 days or 114 Bartels rotations) in the rigidity interval from 1 to 100 GV, based on 5.5×10^9 protons collected. Several Forbush decreases were also observed during the whole period, in connection with transient magnetic perturbations. The product provides these data as time-profiles from May 20, 2011 to October 29 2019 as a function of rigidity. In particular the daily proton fluxes are measured in 30 bins from 1.00 to 100 GV. The errors include statistics, time-dependent systematic errors and the total systematic error.
References
~~~~~~~~~~
https://doi.org/10.1103/PhysRevLett.127.271102
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_iss_ams_flux_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 50A
* - **id_tmp:**
- 89
* - **short_name:**
- AMS_daily_H
* - **identifier:**
- aspis:///infn/ams_protons
* - **dynamic:**
- static
* - **size:**
- 4.1MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 83757
* - **time_start:**
- 2011-05-20
* - **time_stop:**
- 2019-10-29
* - **spatial:**
- GEOMAG
* - **messenger:**
- Protons
* - **spectral_min:**
- 1
* - **spectral_max:**
- 100
* - **spectral_units:**
- GV
* - **observable:**
- GCR
* - **latest update:**
- 2024-04-04 02:10:23
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime (2011-05-20T12:00:00) - time UTC of the data-taking
* - 2
- rigidity_min
- GV
- float
- GV (10.1) - lower edge of the rigidity interval
* - 3
- rigidity_max
- GV
- float
- GV (16.6) - upper edge of the rigidity interval
* - 4
- proton_flux
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (259.9) - daily proton flux
* - 5
- proton_flux_error_statistical
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.11) - total statistical error
* - 6
- proton_flux_error_timedependent
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.07) - systematic error from the trigger and reconstruction efficiencies
* - 7
- proton_flux_error_systematic_total
- m^-2sr^-1s^-1GV^-1
- float
- m^-2sr^-1s^-1GV^-1 (0.24) - total systematic error (sum in quadrature of the time-indep and the time-dep systematic errors)
docs/source/products/data/infn_pamela_flux_timeseries.rst deleted 100644 → 0
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==========================================================
PAMELA time-profiles of protons during 4 Forbush Decreases
==========================================================
.. contents:: Table of contents
Time-profiles of galactic cosmic-ray protons measured by the PAMELA detector in space during 4 Forbush Decreases from March 2012 to June 2015 in various rigidity intervals. Each profile is scaled for a suitable period of quiet Sun, estimated about 10 days before each Forbush Decrease
References
~~~~~~~~~~
https://iopscience.iop.org/article/10.3847/1538-4357/aaa0c8
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_pamela_flux_timeseries
* - **publisher:**
- not available in DBF
* - **alph_code:**
- 50B
* - **id_tmp:**
- 90
* - **short_name:**
- PAMELA-proton
* - **identifier:**
- aspis://INFN-PAMELA/proton
* - **dynamic:**
- Data collected starts on March 1, 2012 and is increasing with a daily resolution up until July 17, 2015
* - **size:**
- 200kB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 2394
* - **time_start:**
- 2012-03-01
* - **time_stop:**
- 2015-07-17
* - **spatial:**
- GEOMAG
* - **messenger:**
- protons
* - **spectral_min:**
- 0.85
* - **spectral_max:**
- 8.68
* - **spectral_units:**
- GV
* - **observable:**
- GCR
* - **latest update:**
- 2024-04-04 02:12:29
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime (2012-03-01T12:00:00) - time UTC of the data-taking
* - 2
- rig_min
- GV
- float
- GV (0.85) - lower edge of the rigidity interval
* - 3
- rig_max
- GV
- float
- GV (1.04) - upper edge of the rigidity interval
* - 4
- flux
- none
- float
- none (0.949654) - cosmic-ray flux, normalized for a quiet period before the event generating the decrease
* - 5
- error_flux
- none
- float
- none (0.0326884) - error on the proton measurement (stat + syst)
* - 6
- num_event
- none
- int
- none (0) - Forbush decrease number
docs/source/products/data/infn_saandose_samadha_timeseries.rst deleted 100644 → 0
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=============================================
SAMADHA neutron dose rate at Mount Chacaltaya
=============================================
.. contents:: Table of contents
SAMADHA (South Atlantic Magnetic Anomaly Dosimetry at High Altitude) is an INFN project aimed to monitor the neutron dose rate due to cosmic rays at the Chacaltaya Station (Bolivia, 5200 m) inside the South Atlantic Anomaly region, to study possible correlation between space weather events and dose rate at the ground, considering the proximity of the Van Allen Belts to the Earth's surface in the SAA region.
References
~~~~~~~~~~
http://samadha.to.infn.it
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_saandose_samadha_timeseries
* - **publisher:**
- SAMADHA
* - **alph_code:**
- 75A
* - **id_tmp:**
- 99
* - **short_name:**
- SAA_Ndose
* - **identifier:**
- aspis://infn/saandose_samadha_timeseries
* - **dynamic:**
- one dataset per day (50 kB/day)
* - **size:**
- 50kB
* - **format:**
- text
* - **type:**
- tableset
* - **records_number:**
- 2358
* - **time_start:**
- 2022-10-01
* - **time_stop:**
- 2023-12-31
* - **spatial:**
- Earth's Ground
* - **messenger:**
- neutrons
* - **spectral_min:**
- 0
* - **spectral_max:**
- 0
* - **spectral_units:**
- 0
* - **observable:**
-
* - **latest update:**
- 2024-04-04 02:14:12
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime of the measurement
* - 2
- dose_rate
- nSv/h
- float
- neutron ambient dose rate equivalent H*(10) average over 4 hours (nSv/h)
* - 3
- dose_rate_error
- nSv/h
- float
- neutron dose rate measure error (nSv/h)
docs/source/products/data/infn_tgndose_samadha_timeseries.rst deleted 100644 → 0
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=========================================
SAMADHA neutron dose rate at Testa Grigia
=========================================
.. contents:: Table of contents
Monitoring of the neutron dose rate due to cosmic rays at the Testa Grigia Station (3480 m, Cervinia, Italy), to study possible correlation between space weather events and dose rate at the ground. This measurement is part of the INFN project SAMADHA (South Atlantic Magnetic Anomaly Dosimetry at High Altitude) aimed to monitor the neutron dose inside the South Atlantic Anomaly (SAA) region in Bolivia. The data taken at Testa Grigia are a term of comparison for those collected in the SAA region.
References
~~~~~~~~~~
http://samadha.to.infn.it
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- infn_tgndose_samadha_timeseries
* - **publisher:**
- samadha
* - **alph_code:**
- 75B
* - **id_tmp:**
- 79
* - **short_name:**
- TG_Ndose
* - **identifier:**
- aspis://infn/tgndose_samadha_timeseries
* - **dynamic:**
- one dataset per day (50 kB/day)
* - **size:**
- 50kB
* - **format:**
- text
* - **type:**
- timeseries
* - **records_number:**
- 2835
* - **time_start:**
- 2021-09-01
* - **time_stop:**
- 2023-12-31
* - **spatial:**
- Earth's Ground
* - **messenger:**
- neutrons
* - **spectral_min:**
- 0
* - **spectral_max:**
- 0
* - **spectral_units:**
- 0
* - **observable:**
-
* - **latest update:**
- 2024-04-04 02:15:39
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- datetime of the measurement
* - 2
- dose_rate
- nSv/h
- float
- neutron ambient dose rate equivalent H*(10) average over 4 hours (nSv/h)
* - 3
- dose_rate_error
- nSv/h
- float
- neutron dose rate measure error (nSv/h)
docs/source/products/data/ingv_alert_aqu_timeseries.rst deleted 100644 → 0
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======================================================
INGV geomagnetic data, GIC indices and alert: L'Aquila
======================================================
.. contents:: Table of contents
From both components of GIC index for L'Aquila observatory it is possible to calculate an alert based on a risk scale that associates GIC index to the probability to observe damages to the power network. At present sample files are not available since so far this kind of computation has been performed all within a peculiar software environment (IgorPro), anyway if data were stored in txt files they would be arranged in 3-columns (1-minute data)
This tableset contains a set of data corresponding to products with ids 8, 47 and 48. In detail it contains the definitive values of the X,Y and Z components (in NEC coordinates) and of total intensity F of the geomagnetic field recorded at ground magnetic observatories managed by INGV. Besides, it contains the values of the GicX and GicY indices calculated from the Y and X components, respectively. To finish it contains values of the risk (i.e. alertX and alertY) , corresponding to the estimated values of the GicX and GicY indices.
Data sampling is of 1-minute.
References
~~~~~~~~~~
Dataset summary
~~~~~~~~~~~~~~~
.. list-table::
* - **internal_name:**
- ingv_alert_aqu_timeseries
* - **publisher:**
- INGV
* - **alph_code:**
- 48A
* - **id_tmp:**
- 80
* - **short_name:**
- INGV_AQU_alert
* - **identifier:**
- aspis:///ingv/INGV_AQU_alert
* - **dynamic:**
- This peculialiar version is static being data related only to the 6 CAESAR target events, otherwise it is expected to grow.
* - **size:**
- 10MB
* - **format:**
- csv
* - **type:**
- timeseries
* - **records_number:**
- 84960
* - **time_start:**
- 2012-03-07
* - **time_stop:**
- 2017-09-15
* - **spatial:**
- GROUND
* - **messenger:**
-
* - **spectral_min:**
- 1
* - **spectral_max:**
- 1
* - **spectral_units:**
- 1/minute
* - **observable:**
- GIC,GEOINDEX
* - **latest update:**
- 2024-04-04 02:27:54
Columns specification
~~~~~~~~~~~~~~~~~~~~~
.. list-table::
:widths: 7 20 15 10 48
:align: right
:header-rows: 1
* - progr
- column
- units
- type
- description
* - 1
- time
- UTC
- datetime
- no description
* - 2
- Geo_Lat
- deg
- float
- Geographic Latitude °
* - 3
- Geo_Lon
- deg
- float
- Geographic Longitude °
* - 4
- Altitude
- m
- float
- m
* - 5
- X
- nT
- float
- nT (X component in NEC frame)
* - 6
- Y
- nT
- float
- nT (Y component in NEC frame)
* - 7
- Z
- nT
- float
- nT (Z component in NEC frame)
* - 8
- F
- nT
- float
- nT total intensity
* - 9
- GICx
- dimensionless
- float
- no description
* - 10
- GICy
- dimensionless
- float
- no description
* - 11
- AlertX
- dimensionless
- integer
- Alert based on GicX index
* - 12
- AlertY
- dimensionless
- integer
- Alert based on GicY index
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