using
led to
based on spectral lines that appear due to a particular stellar atmosphere
usually dimmer than
did not match observations for low-frequency light
can be derived from Planck's law for high frequencies
measured with
did not match observations for high-frequency light because we are still alive
isolates light for
derived from
need spectroscopy equipment to measure spectra for analysis
scatters into wavelength for viewing or measurement by

Astronomical spectroscopy

Spectral modeling

Other
approximations

Wien's approximation

Rayleigh-Jean's law

Ultraviolet catastrophe

Planck's law

Spectral analysis

Capturing spectrum
data for analysis

Analyzing spectra for
stellar properties

Spectral lines

Composition of
stellar atmospheres

Doppler shift using
spectral line offsets

Peak intensity
wavelength

Temperature of
celestial object

Wien's displacement

Spectroscopy equipment

Types

Spectroscopes

Spectrometers

Components

Light-dispersing
component

Diffraction grating

Glass prism

Light isolation
mechanism

Slit

Hole

Fibre-optic
cables

Light observation
component

Simple viewing hole

Photometer

Optical sensor
(camera sensor)