dc.creator | Feinstein Baigorri, Carlos | |
dc.creator | Baume, Gustavo Luis | |
dc.creator | Vázquez, Rubén Ángel | |
dc.creator | Niemelä, Virpi Sinikka | |
dc.creator | Cerruti, Miguel Ángel | |
dc.date | 2000 | |
dc.date | 2019-11-05T13:40:40Z | |
dc.identifier | http://sedici.unlp.edu.ar/handle/10915/84909 | |
dc.identifier | issn:0004-6256 | |
dc.description | We have carried out multicolor linear polarimetry (U BV RI) of the brightest stars in the area of the open cluster Trumpler 27. Our data show a high level of polarization in the stellar light with a considerable dispersion, from P = 4% to P = 9.5%. The polarization vectors of the cluster members appear to be aligned. Foreground polarization was estimated from the data of some nonmember objects, for which two different components were resolved: the first one associated with a dust cloud close to the Sun producing P<SUB>λmax</SUB> = 1.3% and θ = 146°, and a second component, the main source of polarization for the cluster members, originating in another dust cloud, which polarizes the light in the direction of θ = 29°.5. From a detailed analysis, we found that the two components have associated values E<SUB>B-V</SUB> < 0.45 for the first one and E<SUB>B-V</SUB> > 0.75 for the other. Due the difference in the orientation of both polarization vectors, almost 90° (180° at the Stokes representation), the first cloud (θ ∼ 146°) depolarizes the light strongly polarized by the second one (θ ∼ 29°.5). | |
dc.description | Facultad de Ciencias Astronómicas y Geofísicas | |
dc.format | application/pdf | |
dc.format | 1906-1912 | |
dc.language | en | |
dc.rights | http://creativecommons.org/licenses/by-nc-sa/4.0/ | |
dc.rights | Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0) | |
dc.subject | Ciencias Astronómicas | |
dc.subject | Dust, extinction | |
dc.subject | Open clusters and associations: individual (Trumpler 27) | |
dc.title | The highly polarized open cluster Trumpler 27 | |
dc.type | Articulo | |
dc.type | Articulo | |