Light from a star surrounded by a cloud of gas often shows
absorption lines produced when starlight of a specific energy is absorbed by atoms in the gas cloud.
It was taken into account, that the curve must cross the origin of co-ordinate system because if there is no CO,
absorption line height is equal to 0.
The
absorption line actually appeared some months before the system's brightness started to drop.
Atmospheric gases absorb some of this light at specific wavelengths, adding very weak
absorption lines to the stellar spectrum.
The presence of many clouds at different distances creates a thicket of
absorption lines, called the Lyman alpha forest, within the spectrum of light emitted by the quasar.
The astronomers examined the Lyman-alpha hydrogen
absorption line and found evidence of several components of hydrogen along our line of sight to the star.
When astronomers see those fingerprints in a spectrum from Webb, they can then identify the molecule or family of molecules that created the
absorption lines.
First discovered in 1922, these
absorption lines (more than 400 of them) are seen any time astronomers look toward dust-reddened stars.
Based on the width of the
absorption lines and the intensity, the total pressure and the CO2 concentration in the package is determined.
While competitive laser-based instruments operate in the near-infrared range, the Delta Ray platform was designed to operate in the mid-infrared range because
absorption lines are about 8,000 times stronger than the NIR.
Characteristic narrow
absorption lines, observed at 380 and 435 nm, are most likely from forbidden spin transitions in ferrous iron.
We have analyzed Fe 11
absorption lines toward several of the reddened stars included in the FUSE survey of molecular hydrogen abundances in translucent clouds.
