Interstellar Extinction in the Direction of the Open Cluster M29

Straižys, V.; Vrba, F. J.; Boyle, R. P.; Milašius, K.; Cernis, K.; Zdanavičius, K.; Zdanavicius, J.; Kazlauskas, A.; Macijauskas, M.; Janusz, Robert

doi:10.1088/0004-6256/149/5/161

Cited by 9 publications

(4 citation statements)

References 37 publications

(42 reference statements)

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“…Most probably, this jump in extinction is related to the cloud system of the Great Cygnus Rift. A similar jump has been found in our earlier papers (Straižys et al 2014(Straižys et al , 2015 in the direction of the nearby cluster M29. The next increase in extinction is observed at d > 1.7 kpc.…”

Section: Interstellar Extinction In the Cluster Areasupporting

confidence: 90%

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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Section: Interstellar Extinction In the Cluster Areasupporting

confidence: 90%

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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“…It must be borne in mind that the distances to the Cygnus OB1 association clusters appear to show greater uncertainty than other clusters located in other Galactic regions for which the photometric parallax is more precise. The distribution of dust in the region could be the cause of this imprecision in the distance, as Straizys et al (2015) have recently concluded with their reanalysis of the cluster NGC 6913 (M29).…”

Section: Clustering In the Phase Space: Opticsmentioning

confidence: 91%

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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“…Red supergiants at distances comparable to those of the OB associations are expected to appear very bright at near-infrared wavelengths, and also have very red colors due both to their low photospheric temperatures and to the foreground extinction, mainly associated with the Cygnus Rift (Straižys et al 2015). We made an initial selection of all the stars in the 2MASS Point Source Catalog in the area defined above having K S < 4.0, J − K S > 1.1.…”

Section: Red Supergiants In Cygnusmentioning

confidence: 99%

The historical record of massive star formation in Cygnus

Comerón

Djupvik

Schneider

et al. 2020

A&A

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Context. The Cygnus region, which dominates the local spiral arm of the Galaxy, is one of the nearest complexes of massive star formation, extending over several hundred parsecs. Its massive stellar content, regions of ongoing star formation, and molecular gas have been studied in detail at virtually all wavelengths. However, little is known of the history of the region beyond the past 10 Myr. Aims. We use the correlations between age, mass and luminosity of red supergiants to explore the history of star formation in Cygnus previous to the formation of the present-day associations. The brightness and spectroscopic characteristics of red supergiants make it easy to identify them and build up a virtually complete sample of such stars at the distance of the Cygnus region, thus providing a record of massive star formation extending several tens of Myr into the past, a period inaccessible through the O and early B stars observable at present. Methods. We have made a selection based on the 2MASS colors of a sample of bright, red stars in an area of 84 square degrees covering the whole present extension of the Cygnus association in the Local Arm. We have obtained spectroscopy in the red visible range allowing an accurate, homogeneous spectral classification as well as a reliable separation between supergiants and other cool stars. Our data are complemented with Gaia Data Release 2 astrometric data. Results. We have identified 29 red supergiants in the area, 17 of which had not been previously classified as supergiants. Twenty-four of the 29 most likely belong to the Cygnus region and four of the remaining to the Perseus arm. We have used their derived luminosities and masses to infer the star formation history of the region. Intense massive star formation activity is found to have started approximately 15 Myr ago, and we find evidence for two other episodes, one taking place between 20 and 30 Myr ago and another one having ended approximately 40 Myr ago. There are small but significant differences between the kinematic properties of red supergiants younger or older then 20 Myr, hinting that stars of the older group were formed outside the precursor of the present Cygnus complex, possibly in the Sagittarius-Carina arm.

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Interstellar Extinction in the Direction of the Open Cluster M29

Cited by 9 publications

References 37 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

The historical record of massive star formation in Cygnus

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