SwePub - sökning: L773:9781583816622

Numrering	Referens	Omslagsbild	Hitta
1.	Beckman, John, et al. (författare) The Tremaine-Weinberg method for pattern speeds using H-alpha emission from ionized gas 2008 Ingår i: Formation and Evolution of Galaxy Disks. - : Astronomical Society of the Pacific. - 9781583816622 ; , s. 353- Konferensbidrag (populärvet., debatt m.m.)abstract The Fabry-Perot interferometer FaNTOmM was used at the 3.6m Canada France Hawaii Telescope and the 1.6m Mont Megantic Telescope to obtain data cubes in H-alpha of 9 nearby spiral galaxies from which maps in integrated intensity, velocity, and velocity dispersion were derived. We then applied the Tremaine-Weinberg method, in which the pattern speed can be deduced from its velocity field, by finding the integrated value of the mean velocity along a slit parallel to the major axis weighted by the intensity and divided by the weighted mean distance of the velocity points from the tangent point measured along the slit. The measured variables can be used either to make separate calculations of the pattern speed and derive a mean, or in a plot of one against the other for all the points on all slits, from which a best fit value can be derived. Linear fits were found for all the galaxies in the sample. For two galaxies a clearly separate inner pattern speed with a higher value, was also identified and measured.

Beckman, John, et al. (författare)
The Tremaine-Weinberg method for pattern speeds using H-alpha emission from ionized gas
2008
Ingår i: Formation and Evolution of Galaxy Disks. - : Astronomical Society of the Pacific. - 9781583816622 ; , s. 353-
Konferensbidrag (populärvet., debatt m.m.)abstract
- The Fabry-Perot interferometer FaNTOmM was used at the 3.6m Canada France Hawaii Telescope and the 1.6m Mont Megantic Telescope to obtain data cubes in H-alpha of 9 nearby spiral galaxies from which maps in integrated intensity, velocity, and velocity dispersion were derived. We then applied the Tremaine-Weinberg method, in which the pattern speed can be deduced from its velocity field, by finding the integrated value of the mean velocity along a slit parallel to the major axis weighted by the intensity and divided by the weighted mean distance of the velocity points from the tangent point measured along the slit. The measured variables can be used either to make separate calculations of the pattern speed and derive a mean, or in a plot of one against the other for all the points on all slits, from which a best fit value can be derived. Linear fits were found for all the galaxies in the sample. For two galaxies a clearly separate inner pattern speed with a higher value, was also identified and measured.

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