The VMC Survey - XXIV. Signatures of tidally stripped stellar populations from the inner Small Magellanic Cloud

Smitha Subramanian*, Stefano Rubele, Ning-Chen Sun, Léo Girardi, Richard de Grijs, Jacco Th. van Loon, Maria-Rosa L. Cioni, Andrés E. Piatti, Kenji Bekki, Jim Emerson, Valentin D. Ivanov, Leandro Kerber, Marcella Marconi, Vincenzo Ripepi, Benjamin L. Tatton

*Corresponding author for this work

Research output: Contribution to journalArticlepeer-review

36 Citations (Scopus)


We study the luminosity function of intermediate-age red clump stars using deep, near-infrared photometric data covering similar to 20 deg² located throughout the central part of the Small Magellanic Cloud (SMC), comprising the main body and the galaxy's eastern wing, based on observations obtained with the VISTA Survey of the Magellanic Clouds (VMC). We identified regions that show a foreground population (similar to 11.8 ± 2.0 kpc in front of the main body) in the form of a distance bimodality in the red clump distribution. The most likely explanation for the origin of this feature is tidal stripping from the SMC rather than the extended stellar haloes of the Magellanic Clouds and/or tidally stripped stars from the Large Magellanic Cloud. The homogeneous and continuous VMC data trace this feature in the direction of the Magellanic Bridge and, particularly, identify (for the first time) the inner region (similar to 2-2.5 kpc from the centre) from where the signatures of interactions start becoming evident. This result provides observational evidence of the formation of the Magellanic Bridge from tidally stripped material from the SMC.

Original languageEnglish
Pages (from-to)2980-2995
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Issue number3
Publication statusPublished - Jun 2017
Externally publishedYes


  • stars: individual: red clump stars
  • galaxies: interactions
  • Magellanic Clouds


Dive into the research topics of 'The VMC Survey - XXIV. Signatures of tidally stripped stellar populations from the inner Small Magellanic Cloud'. Together they form a unique fingerprint.

Cite this