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Title:
Mid- and far-infrared fine-structure-line sensitivities to hypothetical variability of the fine-structure constant
Authors:
Kozlov, M. G.; Porsev, S. G.; Levshakov, S. A.; Reimers, D.; Molaro, P.
Affiliation:
AA(Petersburg Nuclear Physics Institute, Gatchina, 188300, Russia), AB(Petersburg Nuclear Physics Institute, Gatchina, 188300, Russia), AC(Ioffe Physico-Technical Institute, Politekhnicheskaya Street 26, 194021 St. Petersburg, Russia), AD(Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, D-21029 Hamburg, Germany), AE(Osservatorio Astronomico di Trieste, Instituto Nazionale di Astrofisica, Via G. B. Tiepolo 11, 34131 Trieste, Italy)
Publication:
Physical Review A, vol. 77, Issue 3, id. 032119 (PhRvA Homepage)
Publication Date:
03/2008
Origin:
APS
PACS Keywords:
Determination of fundamental constants, Radio-frequency, microwave, and infrared spectra, Fine and hyperfine structure
DOI:
10.1103/PhysRevA.77.032119
Bibliographic Code:
2008PhRvA..77c2119K

Abstract

Sensitivity coefficients to temporal variation of the fine-structure constant α for transitions between the fine-structure (FS) sublevels of the ground states of C I, Si I, S I, Ti I, Fe I, N II, Fe II, O III, S III, Ar III, Fe III, Mg V, Ca V, Na VI, Fe VI, Mg VII, Si VII, Ca VII, Fe VII, and Si IX are calculated. These transitions lie in the mid- and far-infrared regions and can be observed in spectra of high-redshift quasars and infrared bright galaxies with active galactic nuclei. Using FS transitions to study α variation over cosmological time scales allows one to improve the limit on Δα/α by several times as compared to contemporaneous optical observations (|Δα/α|<10‑5) , and to suppress considerably systematic errors of the radial velocity measurements caused by the Doppler noise. Moreover, the far infrared lines can be observed at redshifts z≳10 , far beyond the range accessible to optical observations (z≲4) . We have derived a simple analytical expression which relates the FS intervals and the sensitivity of the FS transitions to the change of α .
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