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Morphologies and ages of star cluster pairs and multiplets in the Small Magellanic Cloud
Astrophysics · Submitted 26 Jun 2000
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find evidence that star cluster pairs and multiplets may have had an important role in the dynamical history of clusters presently seen as large single objects.
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The abstract, sentence by sentence
An isophotal atlas of 75 star cluster pairs and multiplets in the Small Magellanic Cloud is presented, comprising 176 objects. They are concentrated in the SMC main body. The isophotal contours were made from Digitized Sky Survey images and showed relevant structural features possibly related to interactions in about 25% of the sample. Previous N-body simulations indicate that such shapes could be due to tidal tails, bridges or common envelopes. The diameter ratio between the members of a pair is preferentially in the range 1 - 2, with a peak at 1. The projected separation is in the range ~ 3 - 22 pc with a pronounced peak at ~ 13 pc. For 91 objects it was possible to derive ages from Colour-Magnitude Diagrams using the OGLE-II photometric survey. The cluster multiplets in general occur in OB stellar associations and/or HII region complexes. This indicates a common origin and suggests that multiplets coalesce into pairs or single clusters in a short time scale. Pairs in the SMC appear to be mostly coeval and consequently captures are a rare phenomenon. We find evidence that star cluster pairs and multiplets may have had an important role in the dynamical history of clusters presently seen as large single objects.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | An isophotal atlas of 75 star cluster pairs and multiplets in the Small Magellanic Cloud is presented, comprising 176 objects. | contribution 1.00 | 0.95 | 0.04 | asserted 1.00 |
| s1 | They are concentrated in the SMC main body. | result 1.00 | 0.78 | 0.03 | asserted 1.00 |
| s2 | The isophotal contours were made from Digitized Sky Survey images and showed relevant structural features possibly related to interactions in about 25% of the sample. | result 0.74 | 0.94 | 0.04 | hedged possibility 0.94 |
| s3 | Previous N-body simulations indicate that such shapes could be due to tidal tails, bridges or common envelopes. | background 0.85 | 0.04 | 0.03 | hedged possibility 0.99 |
| s4 | The diameter ratio between the members of a pair is preferentially in the range 1 - 2, with a peak at 1. | result 1.00 | 0.90 | 0.04 | asserted 0.99 |
| s5 | The projected separation is in the range ~ 3 - 22 pc with a pronounced peak at ~ 13 pc. | result 1.00 | 0.90 | 0.04 | asserted 1.00 |
| s6 | For 91 objects it was possible to derive ages from Colour-Magnitude Diagrams using the OGLE-II photometric survey. | method 0.90 | 0.94 | 0.03 | asserted 0.99 |
| s7 | The cluster multiplets in general occur in OB stellar associations and/or HII region complexes. | result 0.99 | 0.76 | 0.06 | asserted 0.99 |
| s8 | This indicates a common origin and suggests that multiplets coalesce into pairs or single clusters in a short time scale. | interpretation 1.00 | 0.46 | 0.21 | hedged possibility 0.98 |
| s9 | Pairs in the SMC appear to be mostly coeval and consequently captures are a rare phenomenon. | interpretation 0.66 | 0.79 | 0.18 | hedged possibility 0.89 |
| s10 | We find evidence that star cluster pairs and multiplets may have had an important role in the dynamical history of clusters presently seen as large single objects. | interpretation 0.88 | 0.93 | 0.66 | hedged possibility 0.93 |
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Original abstract
An isophotal atlas of 75 star cluster pairs and multiplets in the Small Magellanic Cloud is presented, comprising 176 objects. They are concentrated in the SMC main body. The isophotal contours were made from Digitized Sky Survey images and showed relevant structural features possibly related to interactions in about 25% of the sample. Previous N-body simulations indicate that such shapes could be due to tidal tails, bridges or common envelopes. The diameter ratio between the members of a pair is preferentially in the range 1 - 2, with a peak at 1. The projected separation is in the range ~ 3 - 22 pc with a pronounced peak at ~ 13 pc. For 91 objects it was possible to derive ages from Colour-Magnitude Diagrams using the OGLE-II photometric survey. The cluster multiplets in general occur in OB stellar associations and/or HII region complexes. This indicates a common origin and suggests that multiplets coalesce into pairs or single clusters in a short time scale. Pairs in the SMC appear to be mostly coeval and consequently captures are a rare phenomenon. We find evidence that star cluster pairs and multiplets may have had an important role in the dynamical history of clusters presently seen as large single objects.
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