Pismis 20: One or two clusters?

Orsatti, A. M.; Vega, E. I.; Marraco, H. G.

doi:10.1051/0004-6361:20030919

Cited by 2 publications

(2 citation statements)

References 15 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Also, the combination of both dust layers could lead to an increase in the polarization or in a depolarization depending on the orientation of the dust grains between both dust clouds. This kind of analysis has been successfully applied by Feinstein et al (2003b), Orsatti et al (2003), and Martínez et al (2004) (#39, 56, 61, 62, 102, 111) is so similar in the Q − U space that its weight average is Q = −0.64 ± 0.12, U = 0.11 ± 0.2, (P = 0.65% , θ = 84.8…”

Section: Resultsmentioning

confidence: 99%

Optical multicolor polarization observations in the region of the open cluster NGC 5749

Vergne¹,

Feinstein²,

Martinez³

2006

A&A

View full text Add to dashboard Cite

We present (UBVRI) multicolor linear polarimetric data for 31 of the brightest stars in the area of the open cluster NGC 5749 considered to study the properties of the interstellar medium (ISM) towards the cluster. Our data yield a mean polarization percentage of P V ∼ 1.7%, close to the polarization value produced by the ISM with normal efficiency (P(%) = 3.5E (B−V) 0.8 ) for a mean color excess of E B−V = 0.42. The mean angle of polarization vectors, θ = 74• , agrees quite well with the expected angle produced by dust particles aligned in the direction of the galactic disk (and the magnetic field) in the region. Our analysis indicates that the visual absorption affecting the stars in NGC 5749 is partially produced by a dust layer located up to 300 pc from the Sun and also by a second layer of dust closer to the cluster (located at least at 700 pc). The observed photometry and our polarization data are consistent with the existence of dust within the cluster. We also show in this work how polarimetry could be an excellent technique for identifying nonmember stars.

show abstract

Section: Resultsmentioning

confidence: 99%

Optical multicolor polarization observations in the region of the open cluster NGC 5749

Vergne¹,

Feinstein²,

Martinez³

2006

A&A

View full text Add to dashboard Cite

show abstract

“…When the light passes through multiple dust layers, the resultant polarization may increase or decrease depending upon the orientation of the magnetic field in each dust layer (see e.g. Feinstein et al 2003; Orsatti, Vega & Marraco 2003; Martínez et al 2004; Vergne et al 2007, 2010; E11). The observed polarization and extinction data towards a particular direction of the Galaxy provide important input to test the models dealing with the extinction and alignment of the grains.…”

Section: Dust Propertiesmentioning

confidence: 99%

Broad-band optical polarimetric studies towards the Galactic young star cluster Berkeley 59

Eswaraiah

Pandey

Maheswar

et al. 2011

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present multiwavelength optical linear polarimetric observations of 69 stars towards the young open cluster Berkeley 59. The observations reveal the presence of three dust layers located at distances of ∼300, ∼500 and ∼700 pc. The dust layers produce a total polarization PV∼ 5.5 per cent. The mean values of polarization and polarization angles due to the dust layers are found to increase systematically with distance. We show that polarimetry in combination with the (U−B)–(B−V) colour–colour diagram yields a better identification of cluster members. The polarization measurements suggest that the polarization due the intracluster medium is ∼2.2 per cent. An anomalous reddening law exists for the cluster region, indicating a relatively larger grain size than that in the diffuse interstellar medium. The spatial variation of polarization and colour excess E(B−V) are found to increase with radial distance from the cluster centre, whereas θV and λmax are found to decrease with increasing radial distance from the cluster centre. About 40 per cent of cluster members show the signatures of either intrinsic polarization or rotation in their polarization angles. There is an indication that the starlight of the cluster members might have been depolarized because of non‐uniform alignment of dust grains in the foreground dust layers and in the intracluster medium.

show abstract

Pismis 20: One or two clusters?

Cited by 2 publications

References 15 publications

Optical multicolor polarization observations in the region of the open cluster NGC 5749

Optical multicolor polarization observations in the region of the open cluster NGC 5749

Broad-band optical polarimetric studies towards the Galactic young star cluster Berkeley 59

Contact Info

Product

Resources

About