2010A&A...516A.113L


Query : 2010A&A...516A.113L

2010A&A...516A.113L - Astronomy and Astrophysics, volume 516, A113-113 (2010/6-3)

Searching for spatial variations of alpha2/µ in the Milky Way.

LEVSHAKOV S.A., MOLARO P. and REIMERS D.

Abstract (from CDS):

We probe the dependence of α2/µ on the ambient matter density by means of spectral observations in submm- and mm-wave bands. A procedure is suggested for exploring the value of F=α2/µ, where µ=me/mp is the electron-to-proton mass ratio, and α=e2/((h/2π)c) is the fine-structure constant. The fundamental physical constants, which are measured in different physical environments of high (terrestrial) and low (interstellar) densities of baryonic matter are supposed to vary in chameleon-like scalar field models, which predict that both masses and coupling constant may depend on the local matter density. The parameter ΔF/F=(Fobs-Flab)/Flab can be estimated from the radial velocity offset, ΔV=Vrot-Vfs, between the low-laying rotational transitions in carbon monoxide 13CO and the fine-structure transitions in atomic carbon [CI]. A model-dependent constraint on Δα/α can be obtained from ΔF/F using Δµ/µ independently measured from the ammonia method. Currently available radio astronomical datasets provide an upper limit on |ΔV|<110m/s (1σ). When interpreted in terms of the spatial variation of F, this gives |ΔF/F|<3.7x10–7. An order of magnitude improvement in this limit will allow us to independently test a non-zero value of Δµ/µ=(2.2±0.4stat±0.3sys)x10–8, recently found with the ammonia method. Considering that the ammonia method restricts the spatial variation of µ at the level of |Δµ/µ|≤3x10–8 and assuming that ΔF/F is the same in the entire interstellar medium, one obtains that the spatial variation of α does not exceed the value |Δα/α|< 2x10–7. Since extragalactic gas clouds have similar densities to those in the interstellar medium, the bound on Δα/α is also expected to be less than 2x10–7 at high redshift if no significant temporal dependence of α is present.

Abstract Copyright:

Journal keyword(s): line: profiles - ISM: molecules - techniques: radial velocities - cosmology: observations

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 NAME Per Arm PoG 03 30 +45.0           ~ 1432 0
2 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1267 0
3 QSO B0347-383 QSO 03 49 43.6603590912 -38 10 30.825444900     17.3     ~ 188 0
4 QSO J0407-4410 QSO 04 07 18.0880236912 -44 10 13.983623724   17.6 17.6     ~ 95 0
5 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4099 0
6 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1568 0
7 4C -02.19 QSO 05 01 12.80988538 -01 59 14.2564557   19.1 18.4 19.04   ~ 557 1
8 NAME Ori A MoC 05 38 -07.1           ~ 2899 0
9 NAME Ori B MoC 05 41 43.0 -01 54 44           ~ 1303 0
10 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 729 1
11 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 378 1
12 SDSS J212329.46-005052.9 QSO 21 23 29.4639412848 -00 50 52.916363736   16.91 16.62     ~ 113 0
13 NAME Cep B cor 22 57 07.00 +62 37 22.3           ~ 86 0
14 NAME III CEP ASSOC As* 23 04.2 +63 24           ~ 315 0
15 NAME Cas A SNR 23 23 24.000 +58 48 54.00     14.30     ~ 2669 1
16 QSO J2340-0053 QSO 23 40 23.6700032496 -00 53 27.001299696   18.26 17.93     ~ 95 0
17 NAME Ori Arm PoG ~ ~           ~ 196 0

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2023.02.04-19:18:29

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