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The Young Stellar Population of the Cygnus-X DR15 Region
Solar and Stellar Astrophysics · Submitted 9 Oct 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The presence of other groups with slightly older ages, associated with much less prominent gaseous structures may imply that the evolution of young clusters in this part of the complex proceeds in periods that last 3 to 5 Myr, perhaps after a slow dissipation of their dense molecular cloud birthplaces.
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We present a multi-wavelength study of the young stellar population in the Cygnus-X DR15 region. We studied young stars forming or recently formed at and around the tip of a prominent molecular pillar and an infrared dark cloud. Using a combination of ground based near-infrared, space based infrared and X-ray data, we constructed a point source catalog from which we identified 226 young stellar sources, which we classified into evolutionary classes. We studied their spatial distribution across the molecular gas structures and identified several groups possibly belonging to distinct young star clusters. We obtained samples of these groups and constructed K-band luminosity functions that we compared with those of artificial clusters, allowing us to make first order estimates of the mean ages and age spreads of the groups. We used a $^{13}$CO(1-0) map to investigate the gas kinematics at the prominent gaseous envelope of the central cluster in DR15, and we infer that the removal of this envelope is relatively slow compared to other cluster regions, in which gas dispersal timescale could be similar or shorter than the circumstellar disk dissipation timescale. The presence of other groups with slightly older ages, associated with much less prominent gaseous structures may imply that the evolution of young clusters in this part of the complex proceeds in periods that last 3 to 5 Myr, perhaps after a slow dissipation of their dense molecular cloud birthplaces.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present a multi-wavelength study of the young stellar population in the Cygnus-X DR15 region. | contribution 1.00 | 0.95 | 0.03 | asserted 0.94 |
| s1 | We studied young stars forming or recently formed at and around the tip of a prominent molecular pillar and an infrared dark cloud. | contribution 0.99 | 0.95 | 0.03 | asserted 0.98 |
| s2 | Using a combination of ground based near-infrared, space based infrared and X-ray data, we constructed a point source catalog from which we identified 226 young stellar sources, which we classified into evolutionary classes. | method 0.97 | 0.98 | 0.04 | asserted 1.00 |
| s3 | We studied their spatial distribution across the molecular gas structures and identified several groups possibly belonging to distinct young star clusters. | result 0.66 | 0.97 | 0.06 | hedged possibility 0.57 |
| s4 | We obtained samples of these groups and constructed K-band luminosity functions that we compared with those of artificial clusters, allowing us to make first order estimates of the mean ages and age spreads of the groups. | method 0.85 | 0.98 | 0.08 | asserted 0.85 |
| s5 | We used a $^{13}$CO(1-0) map to investigate the gas kinematics at the prominent gaseous envelope of the central cluster in DR15, and we infer that the removal of this envelope is relatively slow compared to other cluster regions, in which gas dispersal timescale could be similar or shorter than the circumstellar disk dissipation timescale. | result 0.58 | 0.96 | 0.28 | hedged possibility 0.79 |
| s6 | The presence of other groups with slightly older ages, associated with much less prominent gaseous structures may imply that the evolution of young clusters in this part of the complex proceeds in periods that last 3 to 5 Myr, perhaps after a slow dissipation of their dense molecular cloud birthplaces. | interpretation 1.00 | 0.82 | 0.49 | hedged possibility 0.99 |
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Original abstract
We present a multi-wavelength study of the young stellar population in the Cygnus-X DR15 region. We studied young stars forming or recently formed at and around the tip of a prominent molecular pillar and an infrared dark cloud. Using a combination of ground based near-infrared, space based infrared and X-ray data, we constructed a point source catalog from which we identified 226 young stellar sources, which we classified into evolutionary classes. We studied their spatial distribution across the molecular gas structures and identified several groups possibly belonging to distinct young star clusters. We obtained samples of these groups and constructed K-band luminosity functions that we compared with those of artificial clusters, allowing us to make first order estimates of the mean ages and age spreads of the groups. We used a $^{13}$CO(1-0) map to investigate the gas kinematics at the prominent gaseous envelope of the central cluster in DR15, and we infer that the removal of this envelope is relatively slow compared to other cluster regions, in which gas dispersal timescale could be similar or shorter than the circumstellar disk dissipation timescale. The presence of other groups with slightly older ages, associated with much less prominent gaseous structures may imply that the evolution of young clusters in this part of the complex proceeds in periods that last 3 to 5 Myr, perhaps after a slow dissipation of their dense molecular cloud birthplaces.
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How the literature uses it
1 arXiv paper cite this in 2 sentences
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Cites it as support 1 paper
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In our simulation, this is manifested in the hierarchical membership of the stellar units that conform a cluster; 3) that the clusters appear to consist of subunits of slightly different ages that merge to form larger structures ( [ref] ; [ref] ).
Cluster Assembly in Hierarchically Collapsing Clouds · Discussion · 0.97
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As shown in recent studies like those of [ref] and [ref] the mass loss rates in pillars due to photoevaporation are of the order of $∼10^2 M_⊙ Myr^-1$, not too different from our estimations in the expanding gas shell.
The Pillars of Creation revisited with MUSE: gas kinematics and high-mass stellar feedback traced by optical spectroscopy · Discussion · 0.89
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