Variations in the width, density, and direction of the Palomar 5 tidal tails
Author
dc.contributor.author
Bonaca, Ana
Author
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Pearson, Sarah
Author
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Price-Whelan, Adrian
Author
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Dey, Arjun
Author
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Geha, Marla
Author
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Kallivayalil, Nitya
Author
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Moustakas, John
Author
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Muñoz Vidal, Ricardo
Author
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Myers, Adam
Author
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Schlegel, David
Author
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Valdés, Francisco
Admission date
dc.date.accessioned
2020-05-08T22:43:11Z
Available date
dc.date.available
2020-05-08T22:43:11Z
Publication date
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2020
Cita de ítem
dc.identifier.citation
Astrophysical Journal (2020) 889:artículo 1
es_ES
Identifier
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10.3847/1538-4357/ab5afe
Identifier
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https://repositorio.uchile.cl/handle/2250/174619
Abstract
dc.description.abstract
Stars that escape globular clusters form tidal tails that are predominantly shaped by the global distribution of mass in the Galaxy, but also preserve a historical record of small-scale perturbations. Using deep grz photometry from DECaLS, we present highly probable members of the tidal tails associated with the evaporating globular cluster Palomar 5. These data yield the cleanest view of a stellar stream beyond 20 kpc and reveal: (1) a wide, low surface-brightness extension of the leading tail; (2) significant density variations along the stream; and (3) sharp changes in the direction of both the leading and the trailing tail. In the fiducial Milky Way model, a rotating bar perturbs the Palomar 5 tails and can produce streams with similar width and density profiles to those observed. However, the deviations of the stream track in this simple model do not match those observed in the Palomar 5 trailing tail, indicating the need for an additional source of perturbation. These discoveries open up the possibility of measuring the population of perturbers in the Milky Way, including dark-matter subhalos, with an ensemble of stellar streams and deep photometry alone.
es_ES
Patrocinador
dc.description.sponsorship
United States Department of Energy (DOE)
DE-AC02-05CH1123
United States Department of Energy (DOE)
DE-AC02-05CH1123
National Science Foundation (NSF)
AST-0950945