A stellar overdensity associated with the Small Magellanic Cloud | Zendy

A. Pieres | Zendy; B. X. Santiago | Zendy; A. Drlica-Wagner | Zendy; K. Bechtol | Zendy; Roeland P. van der Marel | Zendy; Gurtina Besla | Zendy; Nicolas F. Martin | Zendy; Vasily Belokurov | Zendy; Carme Gallart | Zendy; David MartínezDelgado | Zendy; J. L. Marshall | Zendy; N. E. D. Noël | Zendy; Steven R. Majewski | Zendy; Maria-Rosa L. Cioni | Zendy; T. S. Li | Zendy; W. G. Hartley | Zendy; E. Luque | Zendy; Blair C. Conn | Zendy; A. R. Walker | Zendy; E. Balbinot | Zendy; Guy S. Stringfellow | Zendy; Knut Olsen | Zendy; David L. Nidever | Zendy; L. N. da Costa | Zendy; R. L. C. Ogando | Zendy; M. A. G. Maia | Zendy; A. Fausti Neto | Zendy; T. Abbott | Zendy; F. B. Abdalla | Zendy; S. Allam | Zendy; J. Annis | Zendy; A. Benoit-Lévy | Zendy; A. Carnero Rosell | Zendy; M. Carrasco Kind | Zendy; J. Carretero | Zendy; C. E. Cunha | Zendy; C. B. D'Andrea | Zendy; S Desai | Zendy; H. T. Diehl | Zendy; P. Doel | Zendy; B. Flaugher | Zendy; P. Fosalba | Zendy; J. García-Bellido | Zendy; D. Gruen | Zendy; R. A. Gruendl | Zendy; J. Gschwend | Zendy; G. Gutierrez | Zendy; K. Honscheid | Zendy; D. J. James | Zendy; K. Kuehn | Zendy; N. Kuropatkin | Zendy; F. Menanteau | Zendy; R. Miquel | Zendy; A. A. Plazas | Zendy; A. K. Romer | Zendy; M. Sako | Zendy; E. Sánchez | Zendy; V. Scarpine | Zendy; M. Schubnell | Zendy; I. Sevilla-Noarbe | Zendy; R. C. Smith | Zendy; M. Soares-Santos | Zendy; F. Sobreira | Zendy; E. Suchyta | Zendy; M. E. C. Swanson | Zendy; G. Tarlé | Zendy; D. L. Tucker | Zendy; W. C. Wester | Zendy

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A stellar overdensity associated with the Small Magellanic Cloud

Author(s) -

A. Pieres,

B. X. Santiago,

A. Drlica-Wagner,

K. Bechtol,

Roeland P. van der Marel,

Gurtina Besla,

Nicolas F. Martin,

Vasily Belokurov,

Carme Gallart,

David MartínezDelgado,

J. L. Marshall,

N. E. D. Noël,

Steven R. Majewski,

Maria-Rosa L. Cioni,

T. S. Li,

W. G. Hartley,

E. Luque,

Blair C. Conn,

A. R. Walker,

E. Balbinot,

Guy S. Stringfellow,

Knut Olsen,

David L. Nidever,

L. N. da Costa,

R. L. C. Ogando,

M. A. G. Maia,

A. Fausti Neto,

T. Abbott,

F. B. Abdalla,

S. Allam,

J. Annis,

A. Benoit-Lévy,

A. Carnero Rosell,

M. Carrasco Kind,

J. Carretero,

C. E. Cunha,

C. B. D'Andrea,

S Desai,

H. T. Diehl,

P. Doel,

B. Flaugher,

P. Fosalba,

J. García-Bellido,

D. Gruen,

R. A. Gruendl,

J. Gschwend,

G. Gutierrez,

K. Honscheid,

D. J. James,

K. Kuehn,

N. Kuropatkin,

F. Menanteau,

R. Miquel,

A. A. Plazas,

A. K. Romer,

M. Sako,

E. Sánchez,

V. Scarpine,

M. Schubnell,

I. Sevilla-Noarbe,

R. C. Smith,

M. Soares-Santos,

F. Sobreira,

E. Suchyta,

M. E. C. Swanson,

G. Tarlé,

D. L. Tucker,

W. C. Wester

Publication year - 2017

Publication title -

monthly notices of the royal astronomical society

Language(s) - English

Resource type - Journals

SCImago Journal Rank - 2.058

H-Index - 383

eISSN - 1365-8711

pISSN - 0035-8711

DOI - 10.1093/mnras/stx507

Subject(s) - physics , small magellanic cloud , astrophysics , metallicity , stars , large magellanic cloud , radius , astronomy , computer security , computer science

International audienceWe report the discovery of a stellar overdensity 8° north of the centre of the Small Magellanic Cloud (SMC; Small Magellanic Cloud Northern Over-Density; SMCNOD), using data from the first 2 yr of the Dark Energy Survey (DES) and the first year of the MAGellanic SatelLITEs Survey (MagLiteS). The SMCNOD is indistinguishable in age, metallicity and distance from the nearby SMC stars, being primarily composed of intermediate-age stars (6 Gyr, Z=0.001), with a small fraction of young stars (1 Gyr, Z=0.01). The SMCNOD has an elongated shape with an ellipticity of 0.6 and a size of ∼ 6° × 2°. It has an absolute magnitude of M_V ≅ −7.7, r_h = 2.1 kpc, and μ_V(r < r_h) = 31.2 mag arcsec^−2. We estimate a stellar mass of ∼10^5 M_⊙, following a Kroupa mass function. The SMCNOD was probably removed from the SMC disc by tidal stripping, since it is located near the head of the Magellanic Stream, and the literature indicates likely recent Large Magellanic Cloud-SMC encounters. This scenario is supported by the lack of significant H i gas. Other potential scenarios for the SMCNOD origin are a transient overdensity within the SMC tidal radius or a primordial SMC satellite in advanced stage of disruption

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