Show simple item record

Authordc.contributor.authorMuñoz Vidal, Ricardo Rodrigo 
Authordc.contributor.authorPadmanabhan, Nikhil es_CL
Authordc.contributor.authorGeha, Marla es_CL
Admission datedc.date.accessioned2012-06-21T19:43:23Z
Available datedc.date.available2012-06-21T19:43:23Z
Publication datedc.date.issued2012-02-01
Cita de ítemdc.identifier.citationASTROPHYSICAL JOURNAL Volume: 745 Issue: 2 Article Number: 127 Published: FEB 1 2012es_CL
Identifierdc.identifier.otherDOI: 10.1088/0004-637X/745/2/127
Identifierdc.identifier.urihttps://repositorio.uchile.cl/handle/2250/125653
General notedc.descriptionArtículo de publicación ISIes_CL
Abstractdc.description.abstractThe discovery of ultra-faint dwarf (UFD) galaxies in the halo of the Milky Way extends the faint end of the galaxy luminosity function to a few hundred solar luminosities. This extremely low luminosity regime poses a significant challenge for the photometric characterization of these systems. We present a suite of simulations aimed at understanding how different observational choices related to the properties of a low-luminosity system impact our ability to determine its true structural parameters such as half-light radius and central surface brightness. We focus on estimating half-light radii (on which mass estimates depend linearly) and find that these numbers can have up to 100% uncertainties when relatively shallow photometric surveys, such as the Sloan Digital Sky Survey, are used. Our simulations suggest that to recover structural parameters within 10% or better of their true values: (1) the ratio of the field of view to the half-light radius of the satellite must be greater than three, (2) the total number of stars, including background objects should be larger than 1000, and (3) the central to background stellar density ratio must be higher than 20. If one or more of these criteria are not met, the accuracy of the resulting structural parameters can be significantly compromised. In the context of future surveys such as Large Synoptic Survey Telescope, the latter condition will be closely tied to our ability to remove unresolved background galaxies. Assessing the reliability of measured structural parameters will become increasingly critical as the next generation of deep wide-field surveys detects UFDs beyond the reach of current spectroscopic limits.es_CL
Patrocinadordc.description.sponsorshipNational Science Foundation AST-0908752 GEMINI-CONICYT 32080010 CONICYT 15010003 BASAL PFB-06es_CL
Lenguagedc.language.isoenes_CL
Publisherdc.publisherIOP PUBLISHING LTDes_CL
Keywordsdc.subjectgalaxies: dwarfes_CL
Títulodc.titleMEASURING SIZES OF ULTRA-FAINT DWARF GALAXIESes_CL
Document typedc.typeArtículo de revista


Files in this item

Icon

This item appears in the following Collection(s)

Show simple item record