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Deep Subaru Hyper Suprime-Cam Observations of Milky Way Satellites Columba I and Triangulum II

Authordc.contributor.authorCarlin, Jeffrey L 
Authordc.contributor.authorSand, David J. 
Authordc.contributor.authorMuñoz Vidal, Ricardo Rodrigo 
Authordc.contributor.authorSpekkens, Kristine 
Authordc.contributor.authorWillman, Beth 
Authordc.contributor.authorCrnojevic, Denija 
Authordc.contributor.authorForbes, Duncan A. 
Authordc.contributor.authorHargis, ,Jonathan 
Authordc.contributor.authorKirby, Evan 
Authordc.contributor.authorPeter, Annika H. G. 
Authordc.contributor.authorRomanowsky, Aaron J. 
Authordc.contributor.authorStrader, Jay 
Cita de ítemdc.identifier.citationThe Astronomical Journal, 154:267 (10pp), 2017 Decemberes_ES
Abstractdc.description.abstractWe present deep, wide-field Subaru Hyper Suprime-Cam photometry of two recently discovered satellites of the Milky Way (MW): Columba. I (Col I) and Triangulum. II (Tri II). The color-magnitude diagrams of both objects point to exclusively old and metal-poor stellar populations. We re-derive structural parameters and luminosities of these satellites, and find M-V,M-Col I = -4.2 +/- 0.2 for Col. I and M-V,M-Tri II = -1.2 +/- 0.4 for Tri. II, with corresponding half-light radii of r(h,Col I)= 117 +/- 17 pc and rh,T-ri II = 21 +/- 4 pc. The properties of both systems are consistent with observed scaling relations for MW dwarf galaxies. Based on archival data, we derive upper limits on the neutral gas content of these dwarfs, and find that they lack H I, as do the majority of observed satellites within the MW virial radius. Neither satellite shows evidence of tidal stripping in the form of extensions or distortions in matched-filter stellar density maps or surface-density profiles. However, the smaller Tri. II system is relatively metal-rich for its luminosity (compared to other MW satellites), possibly because it has been tidally stripped. Through a suite of orbit simulations, we show that Tri. II is approaching pericenter of its eccentric orbit, a stage at which tidal debris is unlikely to be seen. In addition, we find that Tri. II may be on its first infall into the MW, which helps explain its unique properties among MW dwarfs. Further evidence that Tri. II is likely an ultra-faint dwarf comes from its stellar mass function, which is similar to those of other MW dwarfs.es_ES
Patrocinadordc.description.sponsorshipNSF Faculty Early Career Development (CAREER) award, AST1151462 / NSF, AST-1412504, AST-1514763, AST-1616710/ Packard Fellowship / Research Corporation for Science Advancement Cottrell Scholar / Instituto de Astrofisica de Canarias / NASA, NAS5-26555 / NASA Office of Space Science, NNX09AF08G / National Aeronautics and Space Administration, NNX08AR22G / National Science Foundation, AST-1238877es_ES
Publisherdc.publisherIOP Publishinges_ES
Type of licensedc.rightsAttribution-NonCommercial-NoDerivs 3.0 Chile*
Link to Licensedc.rights.uri*
Sourcedc.sourceThe Astronomical Journales_ES
Keywordsdc.subjectGalaxies dwarfes_ES
Keywordsdc.subjectGalaxies individual (Columba I, Triangulum II)es_ES
Keywordsdc.subjectGalaxies photometryes_ES
Keywordsdc.subjectGalaxy haloes_ES
Keywordsdc.subjectLocal Groupes_ES
Títulodc.titleDeep Subaru Hyper Suprime-Cam Observations of Milky Way Satellites Columba I and Triangulum IIes_ES
Document typedc.typeArtículo de revistaes_ES
Indexationuchile.indexArtículo de publicación ISIes_ES

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Except where otherwise noted, this item's license is described as Attribution-NonCommercial-NoDerivs 3.0 Chile