extinction curve

Data interpretation The accompanying graph depicts immigration and extinction curves as a function of species diversity for two islands.

Astronomical observatories generally are able to characterise the local extinction curve very accurately, to allow observations to be corrected for the effect.

It is calculated by multiplying the standard atmospheric extinction curve by the mean airmass calculated over the duration of the observation.

The form of the standard extinction curve depends on the composition of the ISM, which varies from galaxy to galaxy.

To measure the extinction curve for a star, the star's spectrum is compared to the observed spectrum of a similar star known not to be affected by extinction (unreddened).

With the COS, we will be able to observe interstellar spectra in a new regime, translucent clouds, for atomic, ionic, and molecular lines and bands, and extinction curves.

One prominent feature in measured extinction curves of many objects within the Milky Way is a broad 'bump' at about 2175 Å, well into the ultraviolet region of the electromagnetic spectrum.

Given that we expect to find higher depletions, we should see an altered grain size distribution, which may show up in the extinction curves, probably as lower far-UV extinction than in diffuse clouds.

In the Local Group, the best-determined extinction curves are those of the Milky Way, the Small Magellanic Cloud (SMC) and the Large Magellanic Cloud (LMC).

"Given what the climate models predict for continuing warming and melting of sea ice, the whole thing leads to an extinction curve," said Peter Ewins, director of the World Wildlife Fund Canada's Arctic Conservation Program.