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Clues to the formation of spiral structure in M51 from the ages and locations of star clusters

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Abstract
We determine the spatial distributions of star clusters at different ages in the grand-design spiral galaxy M51 using a new catalog based on multi-band images taken with the Hubble Space Telescope (HST). These distributions, when compared with the spiral structure defined by molecular gas, dust, young and old stars, show the following sequence in the inner arms: dense molecular gas (and dust) defines the inner edge of the spiral structure, followed by an overdensity of old stars and then young stellar clusters. The offset between gas and young clusters in the inner arms is consistent with the expectations for a density wave. Clusters as old as a few hundred Myr remain concentrated close to the spiral arms, although the distributions are broader than those for the youngest clusters, which is also consistent with predictions from density wave simulations. The outermost portion of the west arm is different from the rest of the spiral structure in that it contains primarily intermediate-age (approximate to 100-400 Myr) clusters; we believe that this is a "material" arm. We have identified four "feathers," stellar structures beyond the inner arms that have a larger pitch angle than the arms. We do not find age gradients along any of the feathers, but the least coherent feathers appear to have the largest range of cluster ages.
Keywords
WHIRLPOOL SURVEY PAWS, PHOTOMETRIC PERFORMANCE, GALAXIES, CLOUD, CALIBRATION, RESOLUTION, SPURS, GAS, galaxies: individual (M51), galaxies: star clusters: general, galaxies: starburst, stars: formation

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MLA
Chandar, Rupali, et al. “Clues to the Formation of Spiral Structure in M51 from the Ages and Locations of Star Clusters.” ASTROPHYSICAL JOURNAL, vol. 845, no. 1, 2017.
APA
Chandar, R., Chien, L.-H., van der Wel, S. M., Querejeta, M., Dobbs, C., Schinnerer, E., … Regan, M. (2017). Clues to the formation of spiral structure in M51 from the ages and locations of star clusters. ASTROPHYSICAL JOURNAL, 845(1).
Chicago author-date
Chandar, Rupali, L-H Chien, Sharon Meidt van der Wel, Miguel Querejeta, Clare Dobbs, Eva Schinnerer, Bradley C Whitmore, et al. 2017. “Clues to the Formation of Spiral Structure in M51 from the Ages and Locations of Star Clusters.” ASTROPHYSICAL JOURNAL 845 (1).
Chicago author-date (all authors)
Chandar, Rupali, L-H Chien, Sharon Meidt van der Wel, Miguel Querejeta, Clare Dobbs, Eva Schinnerer, Bradley C Whitmore, Daniela Calzetti, Daiana Dinino, Robert C Kennicutt, and Michael Regan. 2017. “Clues to the Formation of Spiral Structure in M51 from the Ages and Locations of Star Clusters.” ASTROPHYSICAL JOURNAL 845 (1).
Vancouver
1.
Chandar R, Chien L-H, van der Wel SM, Querejeta M, Dobbs C, Schinnerer E, et al. Clues to the formation of spiral structure in M51 from the ages and locations of star clusters. ASTROPHYSICAL JOURNAL. 2017;845(1).
IEEE
[1]
R. Chandar et al., “Clues to the formation of spiral structure in M51 from the ages and locations of star clusters,” ASTROPHYSICAL JOURNAL, vol. 845, no. 1, 2017.
@article{8622221,
  abstract     = {We determine the spatial distributions of star clusters at different ages in the grand-design spiral galaxy M51 using a new catalog based on multi-band images taken with the Hubble Space Telescope (HST). These distributions, when compared with the spiral structure defined by molecular gas, dust, young and old stars, show the following sequence in the inner arms: dense molecular gas (and dust) defines the inner edge of the spiral structure, followed by an overdensity of old stars and then young stellar clusters. The offset between gas and young clusters in the inner arms is consistent with the expectations for a density wave. Clusters as old as a few hundred Myr remain concentrated close to the spiral arms, although the distributions are broader than those for the youngest clusters, which is also consistent with predictions from density wave simulations. The outermost portion of the west arm is different from the rest of the spiral structure in that it contains primarily intermediate-age (approximate to 100-400 Myr) clusters; we believe that this is a "material" arm. We have identified four "feathers," stellar structures beyond the inner arms that have a larger pitch angle than the arms. We do not find age gradients along any of the feathers, but the least coherent feathers appear to have the largest range of cluster ages.},
  articleno    = {78},
  author       = {Chandar, Rupali and Chien, L-H and van der Wel, Sharon Meidt and Querejeta, Miguel and Dobbs, Clare and Schinnerer, Eva and Whitmore, Bradley C and Calzetti, Daniela and Dinino, Daiana and Kennicutt, Robert C and Regan, Michael},
  issn         = {0004-637X},
  journal      = {ASTROPHYSICAL JOURNAL},
  keywords     = {WHIRLPOOL SURVEY PAWS,PHOTOMETRIC PERFORMANCE,GALAXIES,CLOUD,CALIBRATION,RESOLUTION,SPURS,GAS,galaxies: individual (M51),galaxies: star clusters: general,galaxies: starburst,stars: formation},
  language     = {eng},
  number       = {1},
  pages        = {12},
  title        = {Clues to the formation of spiral structure in M51 from the ages and locations of star clusters},
  url          = {http://dx.doi.org/10.3847/1538-4357/aa7b38},
  volume       = {845},
  year         = {2017},
}

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