Polarization measurements of stars in the Magellanic Clouds.

Mathewson, D. S.; Ford, V. L.

doi:10.1086/111024

Cited by 90 publications

(98 citation statements)

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“…This small dispersion indicates that the data are collinearly distributed in the (Ç) -U) plane during this observing epoch. The blue-band polarization values reported by Mathewson and Ford (1970) and Behr (1959) lie very close to the straight line fit appearing in Figure 1. The value reported by Poeckert et al (1979) departs from this line by about 4 a.…”

Section: Discussionsupporting

confidence: 82%

A search for linear polarization variability in pole-on Be stars

Hayes¹

1980

PASP

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Section: Discussionsupporting

confidence: 82%

A search for linear polarization variability in pole-on Be stars

Hayes¹

1980

PASP

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“…This mechanism is believed to cause the interstellar polarization observed toward many stars in our Galaxy and has been used to map out the Galactic magnetic field (Mathewson & Ford 1970). In this scenario, the linear polarization of TVLM 513−46 would lie parallel to the magnetic field direction, which is 31 ± 10 • .…”

Section: Discussionmentioning

confidence: 98%

Rotational modulation of the linear polarimetric variability of the cool dwarf TVLM 513−46546

Miles-Páez

Osorio

Πάλλη

2015

A&A

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Aims. We aim to monitor the optical linear polarimetric signal of the magnetized, rapidly rotating M8.5 dwarf TVLM 513−46546. Methods. R-and I-band linear polarimetry images were collected with the Andalucía Faint Object Spectrograph and Camera (ALFOSC) instrument of the 2.56-m Nordic Optical Telescope (NOT) on two consecutive nights, covering about 0.5 and four rotation cycles in the R and I filters, respectively. We also obtained simultaneous intensity curves by means of differential photometry. The typical precision of the data is ±0.46% (R), ±0.35% (I) in the linear polarization degree and ±9 mmag (R), ±1.6 mmag (I) in the differential intensity curves. Results. Strong and variable linear polarization is detected in the R and I filters, with values of maximum polarization (p * = 1.30 ± 0.35 %), that are similar for both bands. The intensity and the polarimetric curves present a sinusoid-like pattern with a periodicity of ∼1.98 h, which we ascribe to structures in the surface of TVLM 513−46546 synchronized with its rotation. We found that the peaks of intensity and polarimetric curves occur with a phase difference of 0.18 ± 0.01 and that the maximum of the linear polarization occurs nearly half a period (0.59 ± 0.03) after the radio pulse. We discuss different scenarios to account for the observed properties of the light curves.

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“…In addition, for local detections of O VI near the galactic plane a sight-line must either cross or be located at the edge of a neutral cloud at the Local Bubble boundary. Plots of the E-vector polarization of starlight by dust in the interstellar medium presented by Mathewson and Ford (1970) show that, for sight-lines < 50pc, optical polarization is minimal in all galactic directions with no preferential polarization vector angle. However, the polarization for stars in the 50 -100pc range clearly exhibits large features in the longitude range l = 0 to 60° reaching up from the galactic plane to high +ve latitudes.…”

Section: Towards An Understanding Of the O Vi-sxrbmentioning

confidence: 94%

O VI in the local interstellar medium

Barstow¹,

Boyce²,

Barstow³

et al. 2008

Space Astronomy

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We report the results of a search for O VI absorption in the spectra of 80 hot DA white dwarfs observed by the FUSE satellite. We have carried out a detailed analysis of the radial velocities of interstellar and (where present) stellar absorption lines for the entire sample of stars. In approximately 35% of cases (where photospheric material is detected), the velocity differences between the interstellar and photospheric components were beneath the resolution of the FUSE spectrographs. Therefore, in 65% of these stars the interstellar and photospheric contributions could be separated and the nature of the O VI component unambiguously determined. Furthermore, in other examples, where the spectra were of a high signal-to-noise, no photospheric material was found and any O VI detected was assumed to be interstellar. Building on the earlier work of Oegerle et al. (2005) and Savage & Lehner (2006), we have increased the number of detections of interstellar O VI and, for the first time, compared their locations with both the soft X-ray background emission and new detailed maps of the distribution of neutral gas within the local interstellar medium. We find no strong evidence to support a spatial correlation between O VI and SXRB emission. In all but a few cases, the interstellar O VI was located at or beyond the boundaries of the local cavity. Hence, any T ~ 300,000K gas responsible for the O VI absorption may reside at the interface between the cavity and surrounding medium or in that medium itself. Consequently, it appears that there is much less O VI-bearing gas than previously stated within the inner rarefied regions of the local interstellar cavity.

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Polarization measurements of stars in the Magellanic Clouds.

Cited by 90 publications

References 0 publications

A search for linear polarization variability in pole-on Be stars

A search for linear polarization variability in pole-on Be stars

Rotational modulation of the linear polarimetric variability of the cool dwarf TVLM 513−46546

O VI in the local interstellar medium

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