This catalog has a list of interplanetary coronal
mass ejections (ICME) observed by STEREO-A and/or STEREO-B between
December 2006 and March 2009. For each of the 24 observations, the
following information is given: event start time, start time of the
"magnetic obstacle (~flux rope)," event end time, maximum values of
thermal pressure, magnetic field magnitude and flow speed, a measure of
speed change over the event, a three-fold event characterization based
on the pressure profile, and a comment. It is expected that this list,
given in both PDF and Excel formats, will be updated periodically.

STEREO spacecraft, A or/and B

Magnetic obstacle (~flux rope) start time: if it is different from the ICME start time, there is a sheath region. NaN indicates there is no clear magnetic obstacle, possibly because of a glance through of the sheath region.

∆V: temporal variation of solar wind speed over one event, negative value indicating solar wind is expanding, and "~" means the solar wind speed remains almost constant or does not change systematically over the event despite back-and-forth changes.

Group: We sort ICMEs into 3 groups depending on their temporal profiles of Pt. Corresponding to the Group 1, 2, and 3 ICMEs, the Pt profile, excluding any shock and/or sheath region (if present), respectively, has a central pressure maximum, a steady plateau, or a gradual decay. In the hypothesis that all ICMEs have a central flux rope, these three groups of Pt profiles are due to different approach distances to the central flux rope. Group 1 ICMEs are assumed to be the ones penetrated by spacecraft near the flux rope axis, and they usually present signatures of magnetic clouds. See Jian et al. (2006) for more detail.