J/A+A/538/A136      OH 44.8-2.3 VLBA SiO maser maps          (Amiri+, 2012)
The following files can be converted to FITS (extension .fit or fit.gz)
	table1.dat maps.dat
Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/A+A/538/A136

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Beginning of ReadMe : J/A+A/538/A136 VLBA SiO maser maps of the star OH 44.8-2.3 (Amiri+, 2012) ================================================================================ VLBA SiO maser observations of the OH/IR star OH 44.8-2.3: magnetic field and morphology. Amiri N., Vlemmings W.H.T., Kemball A.J., van Langevelde H.J. <Astron. Astrophys. 538, A136 (2012)> =2012A&A...538A.136A ================================================================================ ADC_Keywords: Masers ; Magnetic fields ; Polarization Keywords: Stars - magnetic fields - polarization - masers Abstract: SiO maser emission occurs in the extended atmosphere of evolved stars and can be studied at high angular resolution. As compact, high-brightness components they can be used as important tracers of the dynamics at distances close to the central star. The masers also serve as probes of the evolutionary path from spherically symmetric AGB stars to aspherical PNe. Very long baseline interferometry (VLBI) observations of Mira variables indicate that SiO masers are significantly linearly polarized with linear polarization fractions up to 100%. However, no information is available at high angular resolution for SiO masers in higher mass loss OH/IR stars. Theory indicates a different SiO pumping mechanism in higher mass loss evolved stars. We extend the VLBI SiO maser studies to OH/IR stars. The observations enable us to understand the SiO pumping mechanisms in higher mass-loss evolved objects and to compare them with Mira variables. Additionally, polarimetric observations of SiO masers help us to understand the magnetic field strength and morphology and to distinguish between conflicting polarization theories. Description: The 43GHz SiO maser observations of the OH/IR star OH 44.8-2.3 were performed with the VLBA in full polarization spectral line mode. Auxiliary EVLA observations were performed to allow for the absolute calibration of the polarization angle. The Zeeman splitting was measured by cross correlating the right and left circular polarization spectra, as well as the S-curve fitting. Additionally, we analyzed the 1612MHz OH maser observations of OH 44.8-2.3 from the VLA archive. Objects: --------------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------------- 19 21 36.5 +09 27 56 OH 44.8-2.3 = IRAS 19192+0922 ---------------------------------------------------------

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