Astrophysics (Index)About

spectral energy distribution

(SED)
(function or plot of brightness at each wavelength in the spectrum)

Electromagnetic radiation's spectral energy distribution (SED) is a function, i.e., plot of brightness or flux density (i.e., power) versus the frequency or wavelength (using frequency versus wavelength produces different results: see below) from a source. The shape of the continuum and any spectral signatures reveal information about the source.

A single instrument (e.g., a single spectrograph) always has bandwidth limitations, and overcoming that with multiple instruments leads to data-calibration challenges. If the SED of an astronomical object is measured from Earth, the effects of Earth atmosphere must be compensated for. Reddening requires similar compensation, even from space.

The alternate term, spectral power distribution (SPD), meaning the same thing, is used in some other (non-astronomy) fields.

Plotting by wavelength versus plotting by frequency has consequences: the peak wavelength differs in the two cases if each is plotted linearly, a consequence of plotting density functions over values that have a reciprocal relationship. Taking black-body spectrum as an example, plotting wavelengths by millimeter (0 mm, 1 mm, 2 mm, 3 mm, ...) crowds all the infrared, visible light, ultraviolet, etc., between 0 and 1 and spreads radio over a wide range. Plotting frequency by 100 GHz (0 GHz, 100 GHz, 200 GHz, 300 GHz, ...) crowds the radio into 0-300 GHz and spreads the others over the rest. The CMB (black-body) SED's peak is cited at various valid wavelengths and frequencies, though each SED is an accurate representation of the black-body spectrum for temperature 2.72548 K:

plotted by peak frequency peak wavelength peak photon energy
linear wavelength 282 GHz 1.063 mm 1.168 × 10-3 eV
linear frequency 160.23 GHz 1.871 mm 6.26 × 10-4 eV
log of either 222.6 GHz 1.347 mm 9.2 × 10-4 eV

Plots against the log of either produce an equivalent plot: 1 mm≡300 GHz, 10 mm≡30 GHz, 100 mm≡3 GHz, etc. The term spectral energy distribution (SED) is sometimes meant to imply this case: plotted against the log.

SED fitting (aka spectral energy distribution fitting) matches an observed SED with SEDs implying certain characteristics of the source. A common use is classifying distant galaxies, to help determine their age and degree of star formation. A challenge is that a young galaxy with dust has a SED across ultraviolet, visible light, and near infrared as an old galaxy. A fitting method is Markov chain Monte Carlo (MCMC), using random walks around a parameter-space to determine the degree of unique fit between a SED and a known type of object. GalMC is an example of software that takes this approach.


(EMR,physics,function,diagram)
Further reading:
https://en.wikipedia.org/wiki/Spectral_energy_distribution
https://coolwiki.ipac.caltech.edu/index.php/SED_plots_introduction
https://collegeofsanmateo.edu/astronomy/seds.asp
https://ui.adsabs.harvard.edu/abs/2012IAUS..284...42A/abstract

Referenced by pages:
A-type star (A)
AB system
angular power spectrum
B-type star (B)
Balmer jump (BJ)
black-body radiation
Catalog of Galaxies and Clusters of Galaxies (CGCG)
chemical tagging
chemically peculiar star (CP star)
Compton reflection
continuum
convolution
COSIE
CTIS
data cube
differential spectroscopy
dusty galaxy
F-type star (F)
filter bank
fine structure
FITS
fluorescence
G-type star (G)
galaxy SED
Hawking radiation
Herschel Orion Protostar Survey (HOPS)
K correction
K-type star (K)
L-type star (L)
linearly variable filter (LVF)
Lyman break (LB)
Lyman continuum (LyC)
M-type star (M)
MaNGA Stellar Library (MaStar)
non-thermal emission
O-type star (O)
Palomar 60-inch Telescope (P60)
Parkes Multibeam Pulsar Survey (PMPS)
radio galaxy (RG)
Rayleigh-Jeans law
rocky planet
sky subtraction
spaxel
spectral correlator
spectral line
spectral line energy distribution (SLED)
spectral line shape
spectral power distribution (SPD)
spectral resolution
spectral signature
spectral temperature
Spitzer Extended Deep Survey (SEDS)
stacking
stellar model atmosphere
Sunyaev-Zel'dovich effect (SZ effect)
supernova impostor
synchrotron self-Compton (SSC)
T-type star (T)
telluric line
templates
thermal bremsstrahlung
tip of the red-giant branch (TRGB)
transit spectroscopy
transition region
Type Ia supernova problem
vegetation red edge (VRE)
Wien's displacement law
Y-type star (Y)

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