Diffuse interstellar band


Diffuse interstellar band
Relative strengths of observed diffuse interstellar bands

Diffuse interstellar bands (DIBs) are absorption features seen in the spectra of astronomical objects in our galaxy. They are caused by the absorption of light by the interstellar medium. More than 200 bands are seen, in ultraviolet, visible and infrared wavelengths.

The origin of DIBs was unknown and hotly disputed for many years, and the DIBs were long believed to be due to polycyclic aromatic hydrocarbons and other large carbon-bearing molecules. However, no agreement of the bands could be found with laboratory measurements or with theoretical calculations.

Contents

Discovery and history

Much astronomical work relies on the study of spectra - the light from astronomical objects dispersed using a prism or, more usually, a diffraction grating. A typical stellar spectrum will consist of a continuum, containing absorption lines, each of which is attributed to a particular atomic energy level transition in the atmosphere of the star.

All astronomical objects are affected by extinction, the absorption of photons by the interstellar medium. Interstellar absorption predominantly affects the whole spectrum in a continuous way, rather than causing absorption lines, but in 1922 astronomer Mary Lea Heger[1] first observed a number of line-like absorption features which seemed to be interstellar in origin.

Their interstellar nature was shown by the fact that the strength of the observed absorption was roughly proportional to the extinction, and that in objects with widely differing radial velocities the absorption bands were not affected by Doppler shifting, implying that the absorption was not occurring in or around the object concerned.[2][3][4] The name Diffuse Interstellar Band, or DIB for short, was coined to reflect the fact that the absorption features are much broader than the normal absorption lines seen in stellar spectra.

The first DIBs observed were those at wavelengths 578.0 and 579.7 nanometres. Other strong DIBs are seen at 628.4, 661.4 and 443.0 nm. The 443.0 nm DIB is particularly broad at about 1.2 nm across - typical intrinsic stellar absorption features are 0.1 nm or less across.

Later spectroscopic studies at higher spectral resolution and sensitivity revealed more and more DIBs; a catalogue of them in 1975 contained 25 known DIBs, and a decade later the number known had more than doubled. The first detection-limited survey was published by Peter Jenniskens and Xavier Desert in 1994 (see Figure above),[5] which led to the first conference on The Diffuse Interstellar Bands at the University of Colorado in Boulder on May 16–19, 1994. Today over 300 have been detected.

In recent years, very high resolution spectrographs on the world's most powerful telescopes have been used to observe and analyse DIBs.[6] Spectral resolutions of 0.005 nm are now routine using instruments at observatories such as the European Southern Observatory at Cerro Paranal, Chile, and the Anglo-Australian Observatory in Australia, and at these high resolutions, many DIBs are found to contain considerable sub-structure.[7][8]

The nature of the carrier

The great problem with DIBs, apparent from the earliest observations, was that their central wavelengths did not correspond with any known spectral lines of any ion or molecule, and so the material which was responsible for the absorption could not be identified. A large number of theories were advanced as the number of known DIBs grew, and determining the nature of the absorbing material (the 'carrier') became a crucial problem in astrophysics.

One important observational result is that the strengths of most DIBs are not correlated with each other. This means that there must be many carriers, rather than one carrier responsible for all DIBs. Also significant is that the strength of DIBs is broadly correlated with the extinction. Extinction is caused by dust in the interstellar medium, and so DIBs are likely to be also due to dust or something related to it.

The existence of sub-structure in DIBs supports the idea that they are caused by molecules. Substructure results from band heads in the rotational band contour and from isotope substitution. In a molecule containing, say, three carbon atoms, some of the carbon will be in the form of the carbon-13 isotope, so that while most molecules will contain three carbon-12 atoms, some will contain two C12 atoms and one C13 atom, much less will contain one C12 and two C13s, and a very small fraction will contain three C13 molecules. Each of these forms of the molecule will create an absorption line at a slightly different rest wavelength.

The most likely candidate molecules for producing DIBs are thought to be large carbon-bearing molecules, which are common in the interstellar medium. Polycyclic aromatic hydrocarbons, long carbon-chain molecules, and fullerenes are all potentially important.[9][10]

References

  1. ^ Heger, Mary Lea (1922). "Further study of the sodium lines in class B stars ; The spectra of certain class B stars in the regions 5630A-6680A and 3280A-3380A ; Note on the spectrum of [gamma] Cassiopeiae between 5860A and 6600A". Lick Observatory Bulletin 10 (337): 146. Bibcode 1922LicOB..10..141H. 
  2. ^ Herbig, G. H. (1995), The Diffuse Interstellar Bands, Annual Review of Astronomy and Astrophysics, v.33, pp. 19-74.
  3. ^ Krelowski, J., Diffuse interstellar bands - an observational review, Universitaet Jena, Jena Conference on Physics and Properties of Interstellar Matter Related to the Formation and Evolution of Stars, German Democratic Republic, May 2–7, 1988, Astronomische Nachrichten (ISSN 0004-6337), vol. 310, no. 4, 1989, p. 255-263
  4. ^ Sollerman, J.; Cox, N.; Mattila, S.; Ehrenfreund, P.; Kaper, L.; Leibundgut, B.; Lundqvist, P., (2005), Diffuse Interstellar Bands in NGC 1448, Astronomy and Astrophysics, v.429, p.559-567
  5. ^ Jenniskens, P., Desert, X.; Desert, F.-X. (1994). "A survey of diffuse interstellar bands (3800-8680 A)". Astron. Astrophys. Suppl. Ser. 106: 39–78. Bibcode 1994A&AS..106...39J. 
  6. ^ Fossey S.J., Crawford I.A. (2000), Observing with the Ultra-High-Resolution Facility at the Anglo-Australian Telescope: Structure of Diffuse Interstellar Bands, Bulletin of the American Astronomical Society, v.32, p.727
  7. ^ Jenniskens P., Desert F.-X. (1993), Complex structure in two diffuse interstellar bands. Astronomy and Astrophysics, v. 274, p. 465-477
  8. ^ Galazutdinov G., Stachowska W., Musaev F., Moutou C., Lo Curto G., Krelowski J (2002), Fine structure of profiles of weak diffuse interstellar bands, Astronomy and Astrophysics, v.396, p.987-991
  9. ^ Herbig, G. H. (1995), The Diffuse Interstellar Bands, Annual Review of Astronomy and Astrophysics, v.33, pp. 19-74
  10. ^ Ehrenfreund P. (1999), The Diffuse Interstellar Bands as evidence for polyatomic molecules in the diffuse interstellar medium, Bulletin of the American Astronomical Society, v.31, p.880

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