2010A&A...512A..44L


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.20CET01:10:19

2010A&A...512A..44L - Astronomy and Astrophysics, volume 512, A44-44 (2010/3-1)

Searching for chameleon-like scalar fields with the ammonia method.

LEVSHAKOV S.A., MOLARO P., LAPINOV A.V., REIMERS D., HENKEL C. and SAKAI T.

Abstract (from CDS):

We probe the dependence of the electron-to-proton mass ratio, µ=me/mp, on the ambient matter density by means of radio astronomical observations. The ammonia method, which has been proposed to explore the electron-to-proton mass ratio, is applied to nearby dark clouds in the Milky Way. This ratio, which is measured in different physical environments of high (terrestrial) and low (interstellar) densities of baryonic matter is supposed to vary in chameleon-like scalar field models, which predict strong dependences of both masses and coupling constant on the local matter density. High resolution spectral observations of molecular cores in lines of NH3 (J,K)=(1,1), HC3N J=2-1, and N2H+ J=1-0 were performed at three radio telescopes to measure the radial velocity offsets, ΔV=Vrot-Vinv, between the inversion transition of NH3 (1,1) and the rotational transitions of other molecules with different sensitivities to the parameter Δµ/µ=(µobslab)/µlab. The measured values of ΔV exhibit a statistically significant velocity offset of 23±4stat±3sysm/s. When interpreted in terms of the electron-to-proton mass ratio variation, this infers that Δµ/µ=(2.2±0.4stat±0.3sys)x10–8. If only a conservative upper bound is considered, then the maximum offset between ammonia and the other molecules is |ΔV|≤30m/s. This provides the most accurate reference point at z=0 for Δµ/µ of |Δµ/µ|≤3x10–8.

Abstract Copyright:

Journal keyword(s): line: profiles - ISM: molecules - radio lines: ISM - techniques: radial velocities

Simbad objects: 54

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Number of rows : 54

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 933 2
2 LDN 1355 DNe 02 52.7 +69 02           ~ 15 0
3 [RPF2008] NH3SRC 8 PoC 03 25 26.3 +30 45 05           ~ 2 0
4 [RPF2008] NH3SRC 28 PoC 03 27 26.4 +29 51 08           ~ 2 0
5 [RPF2008] NH3SRC 36 PoC 03 27 55.9 +30 06 18           ~ 2 0
6 [RPF2008] NH3SRC 91 PoC 03 30 15.2 +30 23 39           ~ 2 0
7 [RPF2008] NH3SRC 95 PoC 03 30 32.1 +30 26 19           ~ 2 0
8 [RPF2008] NH3SRC 97 PoC 03 30 50.5 +30 49 17           ~ 2 0
9 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1019 0
10 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 190 0
11 LDN 1400K DNe 04 10 48.6 +54 53 14           ~ 30 0
12 NAME [BM89] L1498 PoC 04 10 51.4 +25 09 58           ~ 187 0
13 LDN 1498 DNe 04 11.0 +24 58           ~ 242 0
14 NAME [BM89] L1495 PoC 04 14 08.2 +28 09 31           ~ 170 0
15 LDN 1495 DNe 04 18.1 +27 37           ~ 280 1
16 NAME [BM89] B217 PoC 04 27 46.4 +26 17 52           ~ 3 0
17 LDN 1524 DNe 04 27 57.7 +24 39 18           ~ 71 0
18 LDN 1521F DNe 04 28 39.3 +26 51 43           ~ 177 1
19 Bad 16 Y*O 04 30 50.280 +23 00 08.85   18.08   14.95   F1 132 0
20 NAME Kutner's Cloud MoC 04 32 44.6 +24 23 13           ~ 209 0
21 NAME [BM89] TMC-2 PoC 04 32 44.7 +24 25 13           ~ 186 0
22 LDN 1536 DNe 04 33 24.6 +22 43 29           ~ 93 0
23 LDN 1503 DNe 04 40.4 +29 56           ~ 23 0
24 NAME Taurus Dark Cloud SFR 04 41.0 +25 52           ~ 3352 0
25 Barnard 220 DNe 04 41 38.8 +26 00 42           ~ 120 0
26 TMC-1 MoC 04 41 45.9 +25 41 27           ~ 1332 0
27 LDN 1507 MoC 04 43 32 +29 40.0           ~ 32 0
28 NAME [BM89] L1517B cor 04 55 18.8 +30 38 04           ~ 128 0
29 LDN 1512 MoC 05 04 09.7 +32 43 09           ~ 159 0
30 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 660 0
31 NAME [BM89] L1544 cor 05 04 22.5 +25 11 36           ~ 434 1
32 HE 0515-4414 QSO 05 17 07.6239672230 -44 10 55.578294294 14.74 15.49 15.16     ~ 95 0
33 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3643 1
34 LDN 134A DNe 15 53 36.4 -04 35 26           ~ 48 0
35 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 675 1
36 LDN 43 DNe 16 34 29.3 -15 47 11           ~ 132 1
37 LDN 260 DNe 16 46 58.2 -09 36 20           ~ 41 0
38 LDN 234A DNe 16 48 06.9 -10 51 48           ~ 23 0
39 NAME [LM99] L234E-S cor 16 48 08.6 -10 57 25           ~ 13 0
40 LDN 63 DNe 16 50 15.5 -18 06 06           ~ 74 0
41 LDN 146 MoC 16 57 17.5 -16 09 18           ~ 67 1
42 NAME the Pipe Nebula DNe 17 30 -25.0           ~ 323 1
43 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11155 0
44 LDN 492 DNe 18 15 51 -03 44.4           ~ 43 0
45 LDN 778 DNe 19 26 32.5 +23 58 42           ~ 50 1
46 LDN 663 DNe 19 36 55 +07 34.4           ~ 544 0
47 [LM99] L694-2 cor 19 41 04.6 +10 57 02           ~ 58 0
48 [LM99] L1049-2 cor 20 41 30.6 +57 33 44           ~ 6 0
49 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2305 1
50 IRAS 22290+7458 Y*O 22 29 59.537 +75 14 04.41           ~ 21 1
51 [KP93] 3-5 Y*O 22 30 31.3 +75 13 38           ~ 6 0
52 [TW96] T1 PoC 22 31 02.4 +75 13 39           ~ 5 0
53 LDN 1251C DNe 22 35 40.0 +75 18 06           ~ 22 1
54 LDN 1197 DNe 22 37 20 +58 56.1           ~ 29 0

    Equat.    Gal    SGal    Ecl

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2020.01.20-01:10:19

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