Glossary

\(\Delta{\textrm{mag}}\)

Difference in magnitude between star and planet. Equal to \(\log_{10}\left(\frac{F_P}{F_S}\right)\) where \(F_P\) is the planet flux and \(F_S\) is the stellar flux.

completeness

Typically this refers to obsucrational and photometric completeness: the probability of observing a planet, belonging to a particular population, and with a particular instrument, given that one exists about a given target star, subject to both the photometric and geometric constraints of the instrument. That is, the integral over the joint probability density function of the population of \(\Delta{\textrm{mag}}\) and angular separation over the \(\Delta{\textrm{mag}}\) limits, and between the IWA and OWA of the instrument. For a full definition, see [Brown2005].

edge-on

Orbit with 90 degree inclination. The phase angle can be any value between 0 and 180 degrees.

face-on

Orbit with 0 inclination. The orbital radius vector always lays within the plane of the sky and the phase angle is always 90 degrees.

FWHM

Full-Width at Half-Maximum

IWA

Inner working angle. Minimum angular separation between an observable planet and its host star.

MCMS

Monte Carlo Mission Simulation. See [Savransky2010].

obscurational completeness

The probability of observing a planet, belonging to a particular population, and with a particular instrument, given that one exists about a given target star, subject only to the geometric constraints. That is, the integral over the probability density function of the population of angular separation between the IWA and OWA of the instrument.

OWA

Outer working angle. Maximum angular separation between an observable planet and its host star.

phase angle

The illuminant-object-observer angle. The angle between the planet-star and planet-observer vectors.

photometric completeness

The probability of observing a planet, belonging to a particular population, and with a particular instrument, given that one exists about a given target star, subject only to the photometric constraints (i.e., contrast capabilities of that instrument on that star within the allotted integration time). That is, the integral over the probability density function of the population of \(\Delta{\textrm{mag}}\) over the \(\Delta{\textrm{mag}}\) limits imposed by the instrument.

PSF

Point spread function. The impulse response of an optical system.

QE

Quantum Efficiency. The ratio of the number of charge carriers collected at the readout terminal to the number of photons hitting the detector surface.

SNR

Signal to noise ratio. Typically the estimated signal (i.e., planet flux) scaled by the variance of the estimated noise.