The Enigma of the Open Cluster M29 (Ngc 6913) Solved

Straižys, V.; Milašius, K.; Boyle, R. P.; Vrba, F. J.; Munari, U.; Walborn, N. R.; Cernis, K.; Kazlauskas, A.; Zdanavičius, K.; Janusz, Robert; Zdanavicius, J.; Laugalys, V.

doi:10.1088/0004-6256/148/5/89

Cited by 17 publications

(11 citation statements)

References 41 publications

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“…for B-and A-type stars, as described in Straižys et al (2014). In the IC 4996 area, this is very close to the coefficient obtained for the direction to the cluster M29.…”

Section: Interstellar Extinctions and Distancessupporting

confidence: 87%

Young open cluster IC 4996 and its vicinity: multicolor photometry and Gaia DR2 astrometry

Straižys

Boyle

Milašius

et al. 2019

A&A

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The open cluster IC 4996 in Cygnus and its vicinity are investigated by applying a two-dimensional photometric classification of stars measured in the Vilnius seven-color photometric system. Cluster members are identified by applying distances based on the Gaia DR2 parallaxes and the point vector diagram of the Gaia DR2 proper motions. For some B-type stars, spectroscopic MK types are also obtained from the Asiago spectra and collected from the literature. New parameters of the cluster are derived. The interstellar extinction A V covers a wide range of values, from 1.3 to 2.4 mag; the mean value in the central part of the cluster is 1.8 mag. The cluster distance is 1915 ± 110 pc, and its age is within 8-10 Myr. The cluster exhibits a long sequence from early-B to G stars, where stars cooler than B8 are in the pre-main-sequence stage. The plot of extinction versus distance shows a steep rise of A V up to 1.6 mag at 700-800 pc, which is probably related to dust clouds at the edge of the Great Cygnus Rift. The next increase in extinction by an additional 0.8 mag at d ≥ 1.7 kpc is probably related to the associations Cyg OB1 and Cyg OB3. The cluster IC 4996 does not belong to the Cyg OB1 association, which is located closer to the Sun, at 1682 ± 116 pc. It seems likely that the cluster and the surrounding O-B stars have a common origin with the nearby association Cyg OB3 since Gaia data show that these stellar groups are located at a similar distance.

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“…for B-and A-type stars, as described in Straižys et al (2014). In the IC 4996 area, this is very close to the coefficient obtained for the direction to the cluster M29.…”

Section: Interstellar Extinctions and Distancessupporting

confidence: 87%

Young open cluster IC 4996 and its vicinity: multicolor photometry and Gaia DR2 astrometry

Straižys

Boyle

Milašius

et al. 2019

A&A

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“…A proof of this has been reported by Straizys et al (2014) analysing the distance distribution of the stellar population in the M29 cluster area, where the stars are in the field range of between a few hundred parsecs up to more than 2 kpc. M29 (NGC 6913) forms part of the Cygnus OB1 association, which also contains five other young clusters.…”

Section: Introductionmentioning

confidence: 87%

Analysis of the kinematic structure of the Cygnus OB1 association

Costado¹,

Alfaro²,

González³

et al. 2016

Mon. Not. R. Astron. Soc.

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The main objective of this study is the characterization of the velocity field in the Cygnus OB1 association using the radial velocity data currently available in the literature. This association is part of a larger star-forming complex located in the direction of the Cygnus region, but whose main subsystems may be distributed at different distances from the sun. We have collected radial velocity data for more than 300 stars in the area of 5 x 5 square degrees centred on the Cygnus OB1 association. We present the results of a kinematic clustering analysis in the subspace of the phase space formed by angular coordinates and radial velocity using two independent methodologies. We have found evidence of structure in the phase space with the detection of two main groups, corresponding to different radial velocity and distance values, belonging to the association, and associated with two main shells defined by the Hα emission. A third grouping well separated from the other two in velocity appears to occupy the whole region associated with what has been called "common shell".

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“…The photometric data were used to classify about 70% of these stars into spectral and luminosity classes. In the next paper (Straižys et al 2014, Paper II), we investigated the cluster M29 applying the catalog of stars from Paper I and the MK spectral types of nine brightest O9-B2 stars. The distance (1.54 ± 0.15 kpc) and the age (5 ± 1 Myr) of the cluster were determined (3σ errors).…”

Section: Introductionmentioning

confidence: 99%

Interstellar Extinction in the Direction of the Open Cluster M29

Straižys

Vrba

Boyle

et al. 2015

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The interstellar extinction is investigated in a 1.5 deg 2 area in the direction of the open cluster M29 (NGC 6913) in Cygnus, centered at R.A. = 20 h 24 m , decl. = +38°30′. The study is based on photometric classification of 1110 stars in spectral and luminosity classes down to V = 19 mag using photometry in the Vilnius seven-color system published in Paper I (Milašius et al. 2013). Additionally, in the same area the extinction is investigated using 1147 red clump giants (RCGs), identified by combining selected two-color diagrams of the 2MASS and Spitzer surveys. The investigated area is divided into three parts with different obscuration and in these directions the extinction versus distance plots up to 5 kpc are presented. In the whole area a steep rise of the extinction is observed at a distance of ∼800 pc; it should be related to dust clouds in the Great Cygnus Rift obscuring the stars behind it by A V = 4.0-4.7 mag. RCGs exhibit much larger extinction values, up to A K s = 1.2-1.3 mag in the more transparent areas and 1.45 mag in the northeastern part of the area and above it, where the dust cloud TGU H466 is located. These values of A K s correspond to A V = 10-12 mag. We do not exclude the possibility that the largest values of the extinction belong not to RCGs but to some contaminating intrinsically red AGB stars penetrated through the applied RCG selection constraints. The extinction in the TGU H466 cloud probably originates in two cloud systems-the Great Cygnus Rift at 800 pc and the Cygnus X complex of dust and molecular clouds at 1.3-1.5 kpc.

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The Enigma of the Open Cluster M29 (Ngc 6913) Solved

Cited by 17 publications

References 41 publications

Young open cluster IC 4996 and its vicinity: multicolor photometry and Gaia DR2 astrometry

Young open cluster IC 4996 and its vicinity: multicolor photometry and Gaia DR2 astrometry

Analysis of the kinematic structure of the Cygnus OB1 association

Interstellar Extinction in the Direction of the Open Cluster M29

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