User:Marshallsumter/Radiation astronomy/Chemicals

NGC 1087 is a spiral galaxy located approximately 80 million light-years from Earth in the constellation Cetus. The image is a combination of observations conducted at different wavelengths of light to map stellar populations and gas. ALMA’s observations are represented in brownish-orange tones and highlight the clouds of cold molecular gas that provide the raw material from which stars form. The MUSE data show up mainly in gold and blue. The bright golden glows map warm clouds of mainly ionised hydrogen, oxygen and sulphur gas, marking the presence of newly born stars, while the bluish regions reveal the distribution of slightly older stars. RA 2° 46' 25.16", Dec 0° 29' 56.26", field of view (FoV): 2.95 x 1.99 arcminutes. Orientation: North is 90.0° left of vertical.

Carbon has an emission line in plasmas at 529.053 nm from C VI.^[1]

"The [oxygen] green line occurs at 5577.339Å, in the middle of the strong C₂ (1,2) band, and thus has seldom been observed."^[2]

Carbon has one strong line in the red.

Carbon has three emission lines that occur in an electron cyclotron resonance (ECR) heated plasmas: 464.742, 465.025, and 465.147 nm from C III.^[1]

Carbon has an emission line that occurs in plasmas at 449.881 nm from C VI.^[1]

From the spectrum above, carbon has at least two lines in the violet.

"The Antennae Galaxies (also known as NGC 4038 and 4039) are a pair of distorted colliding spiral galaxies about 70 million light-years away, in the constellation of Corvus (The Crow). This view combines ALMA observations, made in two different wavelength ranges during the observatory’s early testing phase, with visible-light observations from the NASA/ESA Hubble Space Telescope."^[3]

"The Hubble image is the sharpest view of this object ever taken and serves as the ultimate benchmark in terms of resolution. ALMA observes at much longer wavelengths which makes it much harder to obtain comparably sharp images. However, when the full ALMA array is completed its vision will be up to ten times sharper than Hubble."^[3]

"Most of the ALMA test observations used to create this image were made using only twelve antennas working together — far fewer than will be used for the first science observations — and much closer together as well. Both of these factors make the new image just a taster of what is to come. As the observatory grows, the sharpness, speed, and quality of its observations will increase dramatically as more antennas become available and the array grows in size. This is nevertheless the best submillimetre-wavelength image ever taken of the Antennae Galaxies and opens a new window on the submillimetre Universe."^[3]

"While visible light — shown here mainly in blue — reveals the newborn stars in the galaxies, ALMA’s view shows us something that cannot be seen at those wavelengths: the clouds of dense cold gas from which new stars form. The ALMA observations — shown here in red, pink and yellow — were made at specific wavelengths of millimetre and submillimetre light (ALMA bands 3 and 7), tuned to detect carbon monoxide molecules in the otherwise invisible hydrogen clouds, where new stars are forming."^[3]

"Massive concentrations of gas are found not only in the hearts of the two galaxies but also in the chaotic region where they are colliding. Here, the total amount of gas is billions of times the mass of the Sun — a rich reservoir of material for future generations of stars."^[3]

RA: 12 1 52.55, Dec: -18° 52' 2.96".

"[A]irglow emissions [have been] measured by using vertical-viewing photometers [for the] O(¹S) green line at 557.7 nm [with a] background at 566 nm"^[4].

The O III emission lines are at 495.9 and 500.7 nm.^[5]

Oxygen has an emission line that occurs in plasmas at 527.62 nm from O IV.^[1]

Oxygen (O I) has two red lines at 630.0 and 636.4 nm. In the red there are the atomic oxygen transitions of the "forbidden oxygen red doublet at 6300.304 and 6363.776 Å (¹D - ³P)"^[6]. Atmospheric O₂ has a red line at 686.72 nm.

"The oxygen abundance [may be determined] using the oxygen forbidden line at 630nm"^[7]. "[R]atios [of] O/Fe ... are in agreement with the ratios found in the metal-poor red giants, suggesting that no real difference exists between dwarfs and giants."^[7]

"The forbidden oxygen line (λ 630.03nm) is weak in dwarf stars"^[7]

In the spectrum at right several red astronomy emission lines are detected and recorded at normalized intensities (to the oxygen III line) from the Ring Nebula. In the red are the two forbidden lines of oxygen ([O I], 630.0 and 636.4 nm), two forbidden lines of nitrogen ([N II], 654.8 nm and [N II], 658.4 nm), the hydrogen line (Hα, 656.3 nm) and a forbidden line of sulfur ([S II], 671.7 nm).

The spectrum above shows the lines in the visible due to emission from elemental oxygen.

Oxygen has several emission lines that occur in an electron cyclotron resonance (ECR) heated plasmas: 406.963, 406.99, 407.22, 407.59, 407.89, 408.51, 435.12, 441.489, and 441.697 nm from O II, and 434.045 nm from O VIII.^[1]

{{Chemistry resources}}