2010A&A...524A..32L


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET17:45:59

2010A&A...524A..32L - Astronomy and Astrophysics, volume 524, A32-32 (2010/12-1)

Searching for chameleon-like scalar fields with the ammonia method. II. Mapping of cold molecular cores in NH3 and HC3N lines.

LEVSHAKOV S.A., LAPINOV A.V., HENKEL C., MOLARO P., REIMERS D., KOZLOV M.G. and AGAFONOVA I.I.

Abstract (from CDS):

In our previous work we found a statistically significant offset ΔV≃27 m/s between the radial velocities of the HC3N J=2-1 and NH3 (J,K)=(1, 1) transitions observed in molecular cores from the Milky Way. This may indicate that the electron-to-proton mass ratio, µ=me/mp, increases by ∼3x10–8 when measured under interstellar conditions with matter densities of more than 10 orders of magnitude lower than with laboratory (terrestrial) environments. We map four molecular cores L1498, L1512, L1517, and L1400K selected from our previous sample to estimate systematic effects in ΔV due to possible velocity gradients or other sources across the cloud and to check the reproducibility of the velocity offsets on the year-to-year time base. We use the ammonia method, which involves observations of inversion lines of NH3 complemented by rotational lines of other molecular species and allows us to test changes in µ caused by a higher sensitivity of the inversion frequencies to the µ-variation than with the rotational frequencies. We find that in two cores L1498 and L1512 the NH3 (1, 1) and HC3N (2-1) transitions closely trace the same material and show an offset of ΔV=Vlsr(HC3N)-Vlsr(NH3)=26.9±1.2stat±3.0sysm/s throughout the entire clouds. The offsets measured in L1517B and L1400K are 46.9±3.3stat±3.0sysm/s and 8.5±3.4stat±3.0sysm/s, respectively, and are, probably, subject to Doppler shifts due to spatial segregation of HC3N versus NH3. We also determine frequency shifts caused by external electric and magnetic fields and by the cosmic black body radiation-induced Stark effect and find that they are less than 1m/s. The measured velocity offset in L1498 and L1512, when interpreted in terms of Δµ/µ=(µobslab)/µlab, gives Δµ/µ=(26±1stat±3sys)x10–9. Although this estimate is based on a limited number of sources and molecular pairs used in the ammonia method, it demonstrates a high accuracy with which the fundamental physics can be tested by means of radio observations. The non-zero signal in Δµ/µ should be further examined as larger and more accurate data sets become available.

Abstract Copyright:

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

Simbad objects: 13

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Number of rows : 13

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 QSO B0218+357 QSO 02 21 05.5 +35 56 14   20.0 20.0 19.60   ~ 489 3
2 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 929 2
3 LDN 1400K DNe 04 10 48.6 +54 53 14           ~ 30 0
4 NAME [BM89] L1498 PoC 04 10 51.4 +25 09 58           ~ 187 0
5 LDN 1498 DNe 04 11.0 +24 58           ~ 241 0
6 NAME Tau-Aur Region SFR 04 30 +25.0           ~ 1182 1
7 NAME [BM89] L1517B cor 04 55 18.8 +30 38 04           ~ 127 0
8 LDN 1517 DNe 04 55 45 +30 33.0           ~ 93 0
9 LDN 1512 MoC 05 04 09.7 +32 43 09           ~ 159 0
10 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3618 1
11 LDN 183 MoC 15 54 12.2 -02 49 42           ~ 674 1
12 QSO B1830-211 QSO 18 33 39.92 -21 03 39.9     18.70 21   ~ 536 6
13 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2303 1

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2019.11.17-17:45:59

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