Secchirh

SolO surveys

Renaud Romagnan — 2022-05-30T08:42:28Z

The composite survey SolO 8h covers the 08-16 UT time range (1pixel/60sec) and zooms are 1 hour long (1pixel/10sec).
The composite survey SolO 24h covers the 00-24 UT time range (1pixel/180sec) and zooms are 3 hours long (1pixel/22.5sec).

It is composed of

EPD : the time histories of protons and electrons (A).
a spectrum (B)
NRH : a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time at 150 MHz (C)
STIX : the count time histories (D)

EPD : The time histories of protons and electrons (A)

the time histories of protons (energy ranges 7.075-28.33 MeV, 47.05-104.8 MeV) and electrons (energy ranges 53-73 and 282-397 keV), drawn from low-latency data.

Multi-instrument spectrum (B)

Frequency range 600 MHz-20 kHz. Logarithmic scale.
Combines data obtained with :

Instrument	Fmin	Fmax	Time resolution
Waves RAD1	20 KHz	1 MHz	1 min
Waves RAD2	1.04 MHz	13.8 MHz	16 sec
NDA	20 MHz	70 MHz	1 sec
ORFEES	144 MHz	1000 MHz	1 sec

NRH : EW and NS brightness distribution versus time at 150 MHz (C)

Integration time : 10s (1 point/ 60s)
Each frame contains a display of brightness distribution projected onto the heliocentric East/West or North/South direction versus time ; the units of the vertical axis are solar radius.

STIX : The count time histories (D)

the count time histories in 20s time intervals in three photon energy channels (4-10, 10-15, 15-25 keV).

Solar Orbiter

Renaud Romagnan — 2022-05-30T08:37:42Z

The Radio/Solar Orbiter (SolO) pages combine radio observations from ground and space with quick-look plots of X-ray light curves at selected photon energies from Solar Orbiter / STIX and time histories of the intensities of energetic electrons and protons in selected energy ranges from Solar Orbiter / EPD.

The plot on the top right indicates the relative position of Solar Orbiter with respect to the Sun-Earth axis on the given day. Please be aware that during certain periods, the view of the Sun provided by ground-based instruments cannot be directly compared to the observations from Solar Orbiter.

The Spectrometer/Telescope for Imaging X-rays (STIX) is described at https://datacenter.stix.i4ds.net/. The quick-look plots on the present web site are produced from low-latency data (not science data). They show the count time histories in 20s time intervals in three photon energy channels (4-10, 10-15, 15-25 keV). The time axis is the arrival time of photons at 1 AU, corrected from the light propagation time between the satellite and the earth using the coordinates of the spacecraft provided by the SPICE kernels.
The Energetic Particle Detector EPD is described at https://espada.uah.es/epd/ . The quick-look plots on the present web site show the time histories of protons (energy ranges 7.075-28.33 MeV, 47.05-104.8 MeV) and electrons (energy ranges 53-73 and 282-397 keV), drawn from low-latency data. The intensities are averages over the four viewing directions of EPD. The time axis is the time at the spacecraft.
The Radio and Plasma Waves instrument (RPW) is described at https://rpw-datacenter.obspm.fr/. The quick-look plots on this website are produced from calibrated science data products (L2), which include dynamical spectra acquired by the RPW TNR-HFR radio receivers between 4 kHz and 16.4 MHz. They show the power spectral density (in log scale) measured at the receiver level, as functions of UTC time and frequency (in MHz).

The data shown are quicklook-data, used for giving an overview of observations and a first guide to the event selection for scientific investigations. They are not suited for scientific publications. Please refer to the instrument web sites for advise on the recovery and use of science-ready data.

Spectrum gui

Renaud Romagnan — 2020-08-26T08:00:33Z

General Introduction
Readable data
Main Window
Using mouse in the Main Window
Auxiliary Window
Profiles
Background substraction

General Introduction

Spectrum_gui is a software designed to display and analyse dynamic radio spectra from various solar spectrographs. It is designed for ease of use.

Through Spectrum_gui, the user reads and displays the input data, selects and substracts a backgroud, selects time and frequency intervals of interest, displays an Intensity vs frequency profile at a selected time or an Intensity vs time profile at a selected frequency. All plot windows can be saved as png, postscript or eps file.

Data from solar spectrographs are distributed in various file formats requiring different software for each source. Spectrum_gui lets the user analyse data from various solar spectrographs( please see Data Help for more information). without caring for the file format.

Overview of what the user can do with Spectrum_gui :

display adynamic spectrum
plot an intensity-vs-frequency profile at a selected time
plot an intensity-vs-time profile at a selected frequency
display several auxiliary windows for various operations like zooming or background subtraction
save the plot windows in a png, ps or eps file

Install software

Requierements
Spectrum_gui is a software developped with IDL (https://www.harrisgeospatial.com/Software-Technology/IDL).
You need the following softwares to use Spectrum_gui :

IDL 8.5
solarsoft (https://sohowww.nascom.nasa.gov/solarsoft/).

Procedure

1) download the zip file named spectrum_gui.zip :
http://secchirh.obspm.fr/sites/secchirh/IMG/zip/spec_gui.zip
2) un-zip the file spec_gui.zip
3) the directory contain the following files :
spectrum_gui.sav : the software
spectrumGUI_config.xml : configuration file
spectrumGUI_instruments.xml : database file

Launch software

Go to the directory where you stored spectrum_gui.sav
With a shell, launch the following command :
link_to_your_idl_directory/idl -vm=spectrum_gui.sav

General software philosophy

Spectrum_gui is a multi-window software. The mandatory are :

The GUI is the first window which appeares when the software is launched
• The MAIN Window displays the dynamic spectrum. It appears after a file has been read. The user can interact with the Mouse on the MAIN window to visually select a time or a frequency.

The user can create an arbitrary number of AUXILLIARY windows to display the dynamic spectrum with alternative parameters (such as different types of background subtraction).

The user can create an arbitrary number of PROFILE windows to display Intensity vs Frenquency/Time at a selected Time/Frequency.

The GUI is composed of 4 panels.

General panel : date and instrument
Main window panel : manage parameters of the Main Window
Profile panel : manage parameters for displaying profiles
Auxiliary window panel : manage parameters for displaying profiles

Quick start

Read a file
File → Open file → select the file you want to read

Readables data

Data readble with SPECTRUM_GUI
Data	Website	Filename
ORFEES radio-spectrograph (http://secchirh.obspm.fr/spip.php?article19)	https://rsdb.obs-nancay.fr/	orfyyyymmdd_hhmmss.fts
WAVES The Radio and Plasma Wave Investigation on the WIND Spacecraft RAD1, RAD2 and TNR data (http://secchirh.obspm.fr/spip.php?article22)	https://solar-radio.gsfc.nasa.gov/data/wind/rad1/ or rad2	yyyymmdd.R1 or yyyymmdd.R2
Nancay Decameter Array	https://realtime.obs-nancay.fr/dam/data_dam_affiche/data_dam_affiche.php?planete=soleil&couleur=NoirBlanc&mode=fichier&an=2020 (choose RAW)	yymmdd.rt1
Bleien Solar Radio Data . PHOENIX-2 spectrometer	http://http://soleil.i4ds.ch/solarradio/data/2002-20yy_Callisto/	PHOENIX-2_yyyymmdd_hhmmssi.fit
USAF Radio Solar Telescope Network (RSTN) (https://www.sws.bom.gov.au/World_Data_Centre/2/8/9)	ftp://ftp.ngdc.noaa.gov/STP/space-weather/solar-data/solar-features/solar-radio/rstn-spectral/	IIyymmdd.SRS where II=station name
CALLISTO spectrometers.	http://http://soleil.i4ds.ch/solarradio/data/2002-20yy_Callisto/	*_yyyyymmdd_hhmmdd_ ??.fit
Culgoora Solar radiospectrograph	ftp://ftp-out.sws.bom.gov.au/wdc/wdc_spec/data/culgoora/raw/	SPECyymmdd
Swaves data	https://cdpp-archive.cnes.fr	ST ?_WAV_ ?FR_yyyymmdd.B3E

Main window

The tabs of the Main window panel lets you to manage the parameters of the Dynamic Spectrum.

The parameters are dispatched in the following tabs :

Hours tab : manage time limits of the dynamic spectrum in the Main Window
Frequencies tab : manage frequency limits and the frequency axis of the dynamic spectrum in the Main Window
Color tables : manage color table
Display size : manage display size of the Main Window

Buttons
Display Principal Window : to refresh the Main Window with the new parameters every time. To do so, change a parameter in the main window panel,
Save Principal Window : to Save the content of the main window in a file (png, ps or eps).
Adjust the the size of the Main Window with the button in the bottom right corner.

Using mouse in the Main Window

The user can use the mouse to visually select a Time or a Frequency on the Main window. Using the mouse will automatically fill some text areas of the GUI.

Left mouse button (LMB)

PRESS LMB to fill the bottom/left limits

X	Start hour of Intensity vs Time profile
Y	First frequency of intensity vs Frequency profile
X	Start hour of Auxiliary window
Y	First frequency hour of Auxiliary window

RELEASE LMB to fill the top/right limits :

X	End hour of Time vs Intensity profile
Y	End frequency of Frequency vs Intensity profile
X	End hour of Auxiliary window
Y	End Frequency hour of Auxiliary window

Right mouse button (RMB)

PRESS RMB :

X	Time of Frequency vs Intensity profile
Y	Frequency of Time vs Intensity profile
X	Hour taken for background when subtracting a backgroung on the Auxiliary window

Auxiliary window

The tabs of the Auxiliary Window panel lets you to manage the parameters of the Dynamic Spectrum in the Auxiliary Window.
The parameters are dispatched in the following tabs :

Hours tab : manage time limits of the dynamic spectrum in the Main Window
Frequencies tab : manage frequency limits and frequency axe of the dynamic spectrum in the Auxiliary Window
Background : manage background substraction in the Auxiliary Window (Please see Background Help for more details)
Display size : manage display size of the Auxiliary Window

Buttons
Display Auxiliary Window : Every time you change a parameter in the auxiliary window panel, click on Display Auxiliary Window to refresh the Auxiliary Window with the new parameters.
Save Auxiliary Window : Save the content of the auxiliary window in a png file.

Profiles

Frequency VS Intensity profile

The « Frequency profile » tab lets you display an Intensity vs Frequency profile at a selected time.

Time of profile :selected time of the profile.
First frequency/End frequency of profile : limits of the profile.
Xsize/Ysize : size of the window.
You can choose the orientation of the frequency axis (frequency increasing upwards or downwards)..
Buttons
DISPLAY : Display the Intensity vs Frequency profile.
SAVE : Save the Intensity vs Frequency profile.

Time VS Intensity profile

The « Time profile » tab lets you to display a Time VS Intensity profile of a selected time.

Frequency of profile : selected frequency of the profile.
Starthour/Endhour of profile : limits of the profile.
Xsize/Ysize : size of the window.
Buttons
DISPLAY : Display the Intensity vs Time profile.
SAVE : Save the Intensity vs Time profile.

Background Substraction in Auxiliary Window

The user can subtract a background in the Auxiliary Window.
2 methods are availables :

1 Subtract a spectrum at a user-defined time
2/3 Use a sliding window with a chosen time interval

Subtract the same chosen background

The user chooses a time where the spectrum is considered as a background (A ). This background is subtracted from the entire dynamic spectrum.

Using a sliding window with a chosen time interval

The user chooses an interval duration DELTA( B ).
The background at a certain time is calculated with the Mean (2) or Median (3) of the points in the time interval form (T-DELTA_T)/2 to (T+DELTA_T)/2

ORFEES Real Time

Renaud Romagnan — 2018-10-23T07:02:48Z

- Data products / ouvrir_dans_autre_fenetre

Welcome

Abdallah Hamini — 2018-10-02T14:25:52Z

The present web site is brought to you by the LESIA , UMR 8109, Observatoire de Paris-Meudon and is made possible thanks to a grant from the french Space Agency CNES.

This radio survey project is a joint effort of the Paris Observatory, the Yunnan Observatory (China), the University of Sydney (Australia), the University of Athens, the University of Ioannina (Greece), the Solar Physics Branch of the Naval Research Laboratory (USA), The Royal Observatory of Belgium and the Indian Institute of Astrophysics (Gauribidanur).

The primary goal of the project is to support multi-wavelength data analysis and space missions dedicated to research on solar activity and on solar-terrestrial relationships, more particularly the SOHO, STEREO, SDO and Solar Orbiter missions.

This site provides daily surveys which include :

Radio spectra covering a large frequency range obtained by combining data sets from : Orfees and NDA (Nançay France), YNAO (Yunnan,China), Culgoora or Learmonth (Australia), Artemis (Thermopyle, Greece), GLOSS (Gauribidanur, India), ARCAS and HSRS (Humain, Belguim), spectrographs from WIND and STEREO missions.
Processed Radio imaging at two frequencies and access to multi-frequency data from the Nançay Radioheliograph (NRH) providing files readable by Solar Soft.
Coronal Mass Ejections (CMEs) occurrences observed by SOHO and STEREO.

Artemis

Renaud Romagnan — 2018-09-24T13:13:10Z

Direct access to the Quicklook Artemis data.

Please note that these data are not in our reponsability.
So if you have questions about them, please adress your requests to the Artemis Science Group.

NDA

Renaud Romagnan — 2018-09-24T13:10:25Z

Direct access to the Nancay Decameter Array data.

Please note that these data are not in our reponsability.
So if you have questions about them, please adress your requests to the NDA science group.

ORFEES

Florence HENRY — 2018-09-24T09:43:33Z

The process to request ORFEES data has been changed.
After clicking on Get Nancay Data button on the survey page you will be redirected on the Solar Radio Data Base @ Nancay webpage. This data base provides more flexibility and efficiency for data request.

NRH Data

Florence HENRY — 2018-09-24T09:38:22Z

The process to request NRH data has been changed.
After clicking on Get Nancay Data button on the survey page you will be redirected on the Solar Radio Data Base @ Nancay webpage. This data base provides more flexibility and efficiency for data request.

High Resolution Image

Renaud Romagnan — 2018-07-23T08:47:00Z

You can view here Rotational synthesis images.

Their advantages, when compared to snapshot images, are :

A better sensitivity and a strong reduction of interferences, both resulting from the long observation time.
A better spatial resolution (respectively about 3 and 2 times better in the EW and NS directions) and a field of view wider by a factor 1.5 in the EW direction, due to a much more complete uv-coverage.

The dynamical range in images of the quiet corona is much larger than in snapshot images, with a sensitivity of a few kK and a mean accuracy of 15 kK. The counterpart is that the sun must be quiet, or with a low-level time-varying activity, which excludes active days.

You can download PDF yearly quicklook.