Open AccessMagnetic field in Cepheus A as deduced from OH maser polarimetric observations
Author(s) -
Bartkiewicz A.,
Szymczak M.,
Cohen R. J.,
Richards A. M. S.
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.09203.x
Subject(s) - physics , maser , zeeman effect , astrophysics , magnetic field , polarization (electrochemistry) , position angle , astronomy , circular polarization , line of sight , galaxy , chemistry , quantum mechanics
We present the results of MERLIN polarization mapping of OH masers at 1665 and 1667 MHz towards the Cepheus A star‐forming region. The maser emission is spread over a region of 6 × 10 arcsec 2 , twice the extent previously detected. In contrast to the 22‐GHz water masers, the OH masers associated with H ii regions show neither clear velocity gradients nor regular structures. We identified 10 Zeeman pairs which imply a magnetic field strength along the line of sight from −17.3 to +12.7 mG. The magnetic field is organized on the arcsecond scale, pointing towards us in the west and away from us in the east side. The linearly polarized components, detected for the first time, show regularities in the polarization position angles depending on their position. The electric vectors of OH masers observed towards the outer parts of H ii regions are consistent with the interstellar magnetic field orientation, while those seen towards the centres of H ii regions are parallel to the radio jets. A Zeeman quartet inside a southern H ii region has now been monitored for 25 years; we confirm that the magnetic field decays monotonically over that period.