  We analyze the eruption of a coronal plasma channel (CPC) and an overlying
flux rope using \textit{Atmospheric Imaging Assembly/Solar Dynamic Observatory}
(AIA/SDO) and \textit{Solar TErrestrial RElations Observatory} (STEREO)-A
spacecraft data. The CPC erupted first with its low and very faint coronal
signature. Later, above the CPC, a diffuse and thin flux rope also developed
and erupted. The spreading CPC further triggered a rotating jet-like structure
from the coronal hole lying to its northward end. This jet-like eruption may
have evolved due to the interaction between spreading CPC and the open field
lines of the coronal hole lying towards its northward foot-point. The CPC
connected two small trans-equatorial coronal holes lying respectively in the
northern and southern hemisphere on either side of the Equator. These eruptions
were collectively associated with the stealth-type CMEs and CME associated with
a jet-like eruption. The source region of the stealth CMEs lay between two
coronal holes connected by a coronal plasma channel. Another CME was also
associated with a jet-like eruption that occurred from the coronal hole in the
northern hemisphere. These CMEs evolved without any low coronal signature and
yet were responsible for the third strongest geomagnetic storm of Solar cycle
24. These stealth CMEs further merged and collectively passed through the
interplanetary space. The compound CME further produced an intense geomagnetic
storm (GMS) with Dst index= -176 nT. The $z$-component of the interplanetary
magnetic field [$B_{z}$] switched to negative (-18 nT) during this interaction,
and simultaneous measurement of the disturbance in the Earth's magnetic field
(Kp=7) indicates the onset of the geomagnetic storm.
