A deep wide-field optical survey in the young open cluster Collinder 359

Lodieu, N.; Bouvier, J.; James, D. J.; Wit, W. J. de; Palla, F.; McCaughrean, M. J.; Cuillandre, Jean-Charles

doi:10.1051/0004-6361:20054105

Cited by 10 publications

(7 citation statements)

References 77 publications

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“…Collinder 359, located at a distance of 551 pc, is visually separated by 85 pc on the sky from the northern clusters of Serpens. Given the relative proper motions (Cantat-Gaudin et al 2018a), the cluster would have overlapped with Serpens Northeast (in projected space) 16 Myr ago, which is likely younger than the cluster age, estimated to be ∼ 60 Myr by Lodieu et al (2006). IC 4665, located at 350 pc, is a less promising candidate.…”

Section: The Star Formation History Of the Serpensmentioning

confidence: 99%

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An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Herczeg

Kuhn

Zhou

et al. 2019

ApJ

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The dense clusters within the Serpens Molecular Cloud are among the most active regions of nearby star formation. In this paper, we use Gaia DR2 parallaxes and proper motions to statistically measure ∼ 1167 kinematic members of Serpens, few of which were previously identified, to evaluate the star formation history of the complex. The optical members of Serpens are concentrated in three distinct groups located at 380-480 pc; the densest clusters are still highly obscured by optically-thick dust and have few optical members. The total population of young stars and protostars in Serpens is at least 2000 stars, including past surveys that were most sensitive to protostars and disks, and may be far higher. Distances to dark clouds measured from deficits in star counts are consistent with the distances to the optical star clusters. The Serpens Molecular Cloud is seen in the foreground of the Aquila Rift, dark clouds located at 600-700 pc, and behind patchy extinction, here called the Serpens Cirrus, located at ∼ 250 pc. Based on the lack of a distributed population of older stars, the star formation rate throughout the Serpens Molecular Cloud increased by at least a factor of 20 within the past ∼ 5 Myr. The optically bright stars in Serpens Northeast are visible because their natal molecular cloud has been eroded and not because they were flung outwards from a central factory of star formation. The separation between subclusters of 20-100 pc and the absence of an older population leads to speculation that an external forcing was needed to trigger the active star formation.

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Section: The Star Formation History Of the Serpensmentioning

confidence: 99%

“…Searching for clusters from 500 to 600 pc yields Collinder 359 (e.g. Lodieu et al 2006;Cantat-Gaudin et al 2018a), a young cluster located ∼ 551 pc that may be related a previous epoch of star formation in Serpens.…”

Section: Searching For Isolated Groups Of Starsmentioning

confidence: 99%

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Herczeg

Kuhn

Zhou

et al. 2019

ApJ

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“…At an assumed distance to the cluster of 0r = 352 pc, it is ≈ 6 pc. However, the stars with a common proper motion occupy an area of ≈ 100 square degrees on the celestial sphere (Lodieu et al 2006) and, hence, the coronal radius of IC 4665 is ≈ 30 pc. As can be seen from Table 2, the error in the spatial position of the center of IC 4665 is about ±50 pc; its spatial displacement in 2 Myr is insignificant.…”

Section: Resultsmentioning

confidence: 99%

Open Clusters IC 4665 and Cr 359 and a Probable Birthplace of the Pulsar PSR B1929+10

Bobylev

2008

Preprint

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Based on the epicyclic approximation, we have simulated the motion of the young open star clusters IC 4665 and Collinder 359. The separation between the cluster centers is shown to have been minimal 7 Myr ago, 36 pc. We have established a close evolutionary connection between IC 4665 and the Scorpius-Centaurus association -the separation between the centers of these structures was ≈ 200 pc 15 Myr ago. In addition, the center of IC 4665 at this time was near two well-known regions of coronal gas: the Local Bubble and the North Polar Spur. The star HIP 86768 is shown to be one of the candidates for a binary (in the past) with the pulsar PSR B1929+10. At the model radial velocity of the pulsar V r = 2 ± 50 km s −1 , a close encounter of this pair occurs in the vicinity of IC 4665 at a time of −1.1 Myr. At the same time, using currently available data for the pulsar B1929+10 at its model radial velocity V r = 200 ± 50 km s −1 , we show that the hypothesis of Hoogerwerf et al. (2001) about the breakup of the ζOph-B1929+10 binary in the vicinity of Upper Scorpius (US) about 0.9 Myr ago is more plausible.Note. The velocities of the pulsar B1929+10 were calculated for its radial velocity V r = 2 ± 50 km s −1 ; the velocities of the pulsar RX J185635.3754were calculated for V r = −50 ± 50 km s −1 .

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“…hard to distinguish from field stars on a few year baseline. For example, we can mention Orionis [8,13], IC 4665 [12], NGC 2547 [26], IC2391 [4], Collinder 359 [35], to cite only a few.…”

Section: Wide-field Surveysmentioning

confidence: 99%

Brown dwarfs in wide-field surveys

Lodieu

2011

EPJ Web of Conferences

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Abstract. In this invited talk, I briefly summarise early photometric and proper motion surveys carried out in the nearest and youngest open clusters to introduce the motivation behind the Galactic Cluster component of the UKIRT Infrared Deep Sky Survey. Afterwards, I focus on the latest results that we obtained in the Upper Sco association and in the Pleiades. To finish, I show a comparison of the luminosity and mass functions obtained in the Upper Sco association, the Pleiades cluster, and Orionis from the homogeneous set of data publicly available from the Galactic Clusters Survey.

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A deep wide-field optical survey in the young open cluster Collinder 359

Cited by 10 publications

References 77 publications

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

An Initial Overview of the Extent and Structure of Recent Star Formation within the Serpens Molecular Cloud Using Gaia Data Release 2

Open Clusters IC 4665 and Cr 359 and a Probable Birthplace of the Pulsar PSR B1929+10

Brown dwarfs in wide-field surveys

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