  Although advances in exoplanet detection techniques have seen an increase in
discoveries, observing a planet in the earliest stages of formation still
remains a difficult task. Here four epochs of spectra of the transitional disk
object T Cha are analysed to determine whether spectro-astrometry can be used
to detect a signal from its proposed protoplanet, T Cha b. The unique
properties of T Cha are also further constrained. H{\alpha} and [O I]{\lambda}
6300, the most prominent lines, were analysed using spectro-astrometry.
H{\alpha} being a direct accretion tracer is the target for the T Cha b
detection while [O I]{\lambda} 6300 is considered to be an indirect tracer of
accretion. [O I]{\lambda} 6300 is classified as a broad low velocity component
(BC LVC). The mass accretion rate was derived for all epochs using new [O
I]{\lambda} 6300 LVC relationships and the H{\alpha} line luminosity. It is
shown that a wind is the likely origin of the [O I]{\lambda} 6300 line and that
the [O I]{\lambda} 6300 line serves as a better accretion tracer than H{\alpha}
in this case. From the comparison between M acc([OI]) and M acc(H{\alpha}) it
is concluded that T Cha is not an intrinsically weak accretor but rather that a
significant proportion of the H{\alpha} emission tracing accretion is obscured.
T Cha b is not detected in the spectro-astrometric analysis yet a detection
limit of 0.5 mas is derived. The analysis in this case was hampered by
spectro-astrometric artefacts and by the unique properties of T Cha. While it
seems that spectro-astrometry as a means of detecting exoplanets in TDs can be
challenging it can be used to put an limit on the strength of the H{\alpha}
emission from accreting planetary companions and thus can have an important
input into the planning of high angular resolution observations.
