Sign on

SAO/NASA ADS Astronomy Abstract Service

· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· Full Refereed Journal Article (PDF/Postscript)
· arXiv e-print (arXiv:astro-ph/0405240)
· References in the article
· Citations to the Article (21) (Citation History)
· Refereed Citations to the Article
· SIMBAD Objects (7)
· NED Objects (1)
· Also-Read Articles (Reads History)
· HEP/Spires Information
·
· Translate This Page
Title:
A Laboratory for Constraining Cosmic Evolution of the Fine-Structure Constant: Conjugate 18 Centimeter OH Lines toward PKS 1413+135 at z = 0.24671
Authors:
Darling, Jeremy
Affiliation:
AA(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101; )
Publication:
The Astrophysical Journal, Volume 612, Issue 1, pp. 58-63. (ApJ Homepage)
Publication Date:
09/2004
Origin:
UCP
ApJ Keywords:
Cosmology: Observations, Galaxies: Individual: Alphanumeric: PKS 1413+135, Galaxies: ISM, Masers, Galaxies: Quasars: Absorption Lines, Radiation Mechanisms: Nonthermal
DOI:
10.1086/422450
Bibliographic Code:
2004ApJ...612...58D

Abstract

We report the detection of the satellite 18 cm OH lines at 1612 and 1720 MHz in the z=0.24671 molecular absorption system toward the radio source PKS 1413+135. The two OH lines are conjugate; the 1612 MHz line is seen in absorption while the 1720 MHz line is seen in weak maser emission of equal but negative optical depth. We do not detect the main 18 cm OH lines at 1667 and 1665 MHz down to 1.1 mJy rms in 4.0 km s-1 channels. The detected and undetected 18 cm OH lines support a scenario of radiatively pumped stimulated absorption and emission with pumping dominated by the intraladder 119 μm line of OH, suggesting a column density N(OH)~=1015-1016 cm-2. Combined with simultaneous H I 21 cm observations and published CO data, we apply the OH redshifts to measurements of cosmic evolution of the fine-structure constant (α≡e2/ℏc). We obtain highly significant (~25 σ) velocity offsets between the OH and H I lines and the OH and CO lines, but measurements of α-independent systematics demonstrate that the observed velocity differences are entirely attributable to physical velocity offsets between species rather than a change in α. The OH alone, for which conjugate line profiles guarantee that both lines originate in the same molecular gas, provides a weak constraint of Δα/α0=(+0.51+/-1.26)×10-5 at z=0.24671. Higher frequency OH line detections can provide a larger lever arm on Δα and can increase precision by an order of magnitude. The OH molecule can thus provide precise measurements of the cosmic evolution of α that include quantitative constraints on systematic errors. Application of this technique is limited only by the detectability of |τ|~0.01 OH lines toward radio continuum sources and may be possible to z~5.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)
   

Find Similar Abstracts:

Use: Authors
Title
Keywords (in text query field)
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints