  Observations from the 2012 transit of Venus are used to derive empirical
formulae for long and short-range scattered light at locations on the solar
disk observed by the Hinode Extreme ultraviolet Imaging Spectrometer (EIS) and
the Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) instruments.
Long-range scattered light comes from the entire solar disk, while short-range
scattered light is considered to come from a region within 50" of the region of
interest. The formulae were derived from the Fe XII 195.12 A emission line
observed by EIS and the AIA 193 A channel. A study of the weaker Fe XIV 274.20
A line during the transit, and a comparison of scattering in the AIA 193 A and
304 A channels suggests the EIS scattering formula applies to other emission
lines in the EIS wavebands. Both formulae should be valid in regions of fairly
uniform emission such as coronal holes and quiet Sun, but not faint areas close
(around 100") to bright active regions. The formula for EIS is used to estimate
the scattered light component of Fe XII 195.12 for seven on-disk coronal holes
observed between 2010 and 2018. Scattered light contributions of 56% to 100%
are found, suggesting that these features are dominated by scattered light,
consistent with earlier work of Wendeln \& Landi. Emission lines from the S X
and Si X ions - formed at the same temperature as Fe XII and often used to
derive the first ionization potential (FIP) bias from EIS data - are also
expected to be dominated by scattered light in coronal holes.
