I hope you enjoyed the article and learned something about spectrometers from it! You can email me at amesett@gmail.com or find me on LinkedIn at (here: ) for more discussion on the mysterious world of spectrometry!

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So to break it down: because we are able to point the existence of lines on atoms, we are able to determine similarities between the laws and chemicals in what we know to be the universe.

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Side note — the measurements taken with spectrometers suggest the existence of dark matter to equate for the consistent velocity curve demonstrated on the orbital speeds.

In the same way that every person has their own special signature that’s unique to themselves, every element has its own light “image” that belongs exclusively to itself.

However, modern spectroscopy has given us the ability to see more of these lines. We can now also use them to determine certain elemental compositions. The black lines here represent emissions and the color represents the absorption points. When looking at the chart to determine elements based on their emission and absorption amounts, the points which appear black on the chart appear in color on a black background in the reading image.

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For example, Carbon-12 is an isotope that has 6 neutrons and 6 protons. You could also find more elements like this one, just with different values of neutrons and protons (c13, c14, c15, etc). In the sun, all of these atoms are ionized, where each carbon ion (c4+, c5+) will fall into a different chemical species because of its different electric charge.

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Spectrometry can also be used to measure gamma-ray bursts and their intensity. A spectrometer can take the absorption measurements from one of these short blasts of radiation and determine the general composition of the star from which the blast came from. Thanks to this scanning ability, we now are able to figure out the composition of outer portions of our known Universe.

The light is patched through diffraction grating inside the spectrometer, which activates the absorption (the black Fraunhofer lines we see over the spectrum images). The emissions are what we see as lines of color over the black background, and they always are the sheer opposite of what we see in the absorption lines. So to sum it up:

Each ion generates a different point on the absorption spectrum when they are crossed by the light coming directly from the center of the sun. So when we see a chemical through the spectrometer, its crossed by a white light which helps us see it after diffraction.

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In order to pick up where the element is on the light spectrum, there’s first a process which occurs within the spectrometer. Let’s start on the sun.

A rotation curve (also called a velocity curve) is just a line plot that charts the orbital speeds of visible stars or gas in that galaxy versus the radial distance from the center of the galaxy.

Spectroscopes can be used to “read” the different element signatures by taking in the type of light that is reflected from it. In this way, scientists determined that many of the same elements we have on Earth (i.e. cesium) are also found in the sun!

Usually, we measure light on the light spectrum. We split it up by what we see as colors. Of course, we can’t see the whole spectrum; in fact, we’re only able to see a small portion of it. Light is also a wave, transmitted by wavelengths projected from the light source.

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The first idea of a spectroscope was invented by a German optician/scientist, Joseph Von Fraunhofer, who remarked that there must be a way to measure the different types of light. He determined the idea of Fraunhofer lines, which are spectral lines of points on the spectrum. Initially, the visible light spectrum had ten of these lines.

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In every galaxy, the stars have a higher concentration nearer to the center of the galaxy, and the speed toward the outside of the galaxy is pretty consistent. This confirms the existence of an unknown substance. This is rendered on a scanner as the black.

By measuring the emission lines and seeing where they appear and in what quantities, it becomes clear what element one is looking at or scanning with the spectrometer.

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In the infographic above, there are two different sides of what we’re able to see in terms of visible light. After a certain point, there are two reasons the color is essentially invisible to our eyes:

Spectrometry has more uses than just scanning. One of these alternate uses is being able to study the rotation curve of a galaxy.

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First of all, all the elements on the sun (to our current knowledge) are isotopes. An isotope is an atom that has a different number of neutrons than the typical number for that element. That’s like having a series of pencils and erasers, but having a number of writable tips and erasers that don’t line up, either because you have more writable tips or more erasers. However, looking back on the isotopes in the sun, they don’t necessarily have to be stable.

These parts of a spectrometer are able to interact together and result in a clear reading of various elements. Every part of the spectrometer is essential for it to work. Understanding this, there are two ways in which readings can be taken on a spectrometer (based on the type of diffraction grating used).

Humans on earth have only been able to create from x-rays to AM radio waves. Gamma rays are incredibly volatile and dangerous, usually emitted from celestial events such as stars going supernova. On the other hand, an AM radio wave is completely harmless.