SOHO UVCS CME CATALOG: A Brief Description 

Detailed desciption can be found in 
Giordano, S.; Ciaravella, A.; Raymond, J. C.; Ko, Y. -K.; Suleiman, R., 2013, JGR, 118, 3
"UVCS/SOHO catalog of coronal mass ejections from 1996 to 2005: Spectroscopic proprieties"
https://ui.adsabs.harvard.edu/abs/2013JGRA..118..967G/abstract              

This catalog contains 1059 CMEs manually identified since 1996 to 2005 from the 
UltraViolet Coronagraph Spectrometer (UVCS) on board the Solar and Heliospheric 
Observatory (SOHO) mission. 
The LASCO CME Catalog available at CDAW Data Center has been used as baseline to 
search CME signatures on UVCS data. 
All the UVCS events are available on LASCO catalog too.

For each event in the LASCO CME catalog we systematically searched in the entire UVCS 
observations catalog the data in a time window covering from one hour prior to the CME 
onset time, estimated from LASCO C2 coronal observations, to 4 hours after the time when 
the CME is expected to leave the UVCS field of view, (in some case this time window has 
been extended to include long lifetime CME-related features, such as the current sheets).
Then we select observations pointing within the latitudinal region spanned by the 
expanding plasma, determined by the angular width parameter in the LASCO catalog. 
Once the UVCS data potentially containing a CME observation have been selected, a 
specially designed software tool was used to look for temporal changes in line strengths, 
line widths and line centroids associated with the CME. 
The software produced height-time intensity, width, centroid and running difference maps, 
which made it easy to detect changes in any chosen spectral line. 
When temporal variations of a spectral parameter are identified, the event is listed as 
a UVCS CME in the catalog and the software allows to create an httl page with embedded 
a LASCO movie of the event with the UVCS slit positions superposed. 
For each UVCS CME identified, by using the NGDC/NOAA events catalogs 
(ftp.ngdc.noaa.gov/STP/SOLAR_DATA), we checked, in the time spent by the CME to expand 
into solar corona, the detection of a type II radio burst, signature of CME-driven shock, 
and the detection of a X-flare in a short time window around the CME onset. 
Then the likely association between CME in UVCS catalog and type II radio burst and 
X flare is recorded into the single event pages.
Almost all the CME identified in UVCS data have been detected also by LASCO, therefore, 
they are recorded with a same identification number which allow to link each other 
the two catalogs. 
However, a small number of CMEs without correspondence to a LASCO event were discovered 
in UVCS data and included in our catalog. 

As with the LASCO catalog, the UVCS CME catalog is a living document, which can have some 
minor revisions in the future to include new events discovered or in case of more detailed 
analysis of known events which can provide new interpretation of observed features.

The catalog of CMEs observed by UVCS is on-line available at the URL: 
http://solarweb.oato.inaf.it/UVCS_CME. 
The main page of the catalog is a matrix of year and month of observation. 
By clicking on a month in that matrix a list of the events is displayed, then 
by clicking on a single date the user opens a page containing some general information 
on the CME and a tutorial on the UVCS instrument and spectral analysis. 
It lists the UVCS data files, the time of first detection by UVCS, the heights at which 
the CME was observed, the maximum blue and red shift in km/s, the wavelength ranges 
covered in the UVCS spectra and the lines in which the CME is detected. 
Each event page contains a frame from a movie of LASCO C2 difference images with 
the UVCS slit superimposed is also shown. 
A set of 2D images of the CME in selected lines give the line intensity during the 
observation as a function of time and the polar angle position along the slit measured 
counterclockwise from north pole. 
Doppler velocity images can also be included, and they give the Doppler shift from the 
variation of centroid for selected spectral lines with respect to the background corona 
as a function of the time and position along the slit. 
In general the Doppler velocity maps from line centroid represent a lower limit of the 
line of sight velocity determined by computing the maximum Doppler shift of the observed 
feature with respect the central wavelength value of the pre-CME spectral line emission. 

The interpretation section of each event in the catalog draws a preliminary interpretation 
of the UVCS observations listing whether the front, void, shock, current sheet, prominence, 
flare O~VI, leg or helix were detected in the spectra. 
Finally the list of publications related to the event and some comments are included in 
each single event page. 

All information contained in the online UVCS CME catalog is also included in the 
CDAW LASCO CME catalog, available at the URL: http://cdaw.gsfc.nasa.gov/CME_list 
In the page with the monthly list of LASCO CMEs UVCS is listed in the next to last column 
for the events detected. By clicking on UVCS the user will get the same page as in the 
UVCS CME catalog, described so far.

The online catalog can also be searched to select events in a user--given range of dates, 
velocities, latitudes and Doppler shifts, and/or to select events probably connected to 
X flares and type II radio burst, or interpreted as signature of, for example, shock, 
current sheet, O~VI flare etc., the catalog returns the list of the only CMEs meeting the 
search criteria in a table similar to the monthly list in the catalog.

Last update: Oct 30, 2020