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dc.creatorEskew, Michaelen_US
dc.creatorZaritsky, Dennisen_US
dc.creatorMeidt, Sharonen_US
dc.date.accessioned2016-04-22T19:48:25Z
dc.date.available2016-04-22T19:48:25Z
dc.date.issued2012-06en
dc.identifierdoi:10.15781/T2RJ72
dc.identifier.citationEskew, Michael, Dennis Zaritsky, and Sharon Meidt. >Converting from 3.6 and 4.5 micron Fluxes to Stellar Mass.> The Astronomical Journal, Vol. 143, No. 6 (Jun., 2012): 139.en_US
dc.identifier.issn0004-6256en_US
dc.identifier.urihttp://hdl.handle.net/2152/34542
dc.description.abstractWe use high spatial resolution maps of stellar mass and infrared flux of the Large Magellanic Cloud (LMC) to calibrate a conversion between 3.6 and 4.5 mu m fluxes and stellar mass, M-* = 10(5.65) F-3.6(2.85) F-4.5(-1.85) (D/0.05)(2) M-circle dot,where fluxes are in Jy and D is the luminosity distance to the source in Mpc, and to provide an approximate empirical estimate of the fractional internal uncertainty in M* of 0.3 root N/10(6), where N is the number of stars in the region. We find evidence that young stars and hot dust contaminate the measurements, but attempts to remove this contamination using data that are far superior to what are generally available for unresolved galaxies resulted in marginal gains in accuracy. The scatter among mass estimates for regions in the LMC is comparable to that found by previous investigators when modeling composite populations, and so we conclude that our simple conversion is as precise as possible for the data and models currently available. Our results allow for a reasonably bottom-heavy initial mass function, such as Salpeter or heavier, and moderately disfavor lighter versions such as a diet-Salpeter or Chabrier initial mass function.en_US
dc.language.isoEnglishen_US
dc.rightsAdministrative deposit of works to Texas ScholarWorks: This works author(s) is or was a University faculty member, student or staff member; this article is already available through open access or the publisher allows a PDF version of the article to be freely posted online. The library makes the deposit as a matter of fair use (for scholarly, educational, and research purposes), and to preserve the work and further secure public access to the works of the University.en_US
dc.subjectgalaxies: fundamental parametersen_US
dc.subjectgalaxies: stellar contenten_US
dc.subjectmagellanicen_US
dc.subjectcloudsen_US
dc.subjectlarge-magellanic-clouden_US
dc.subjectstar-formation historyen_US
dc.subjectspitzer-space-telescopeen_US
dc.subjecthigh-redshift galaxiesen_US
dc.subjectinfrared array cameraen_US
dc.subjectnearby galaxiesen_US
dc.subjectdwarfen_US
dc.subjectgalaxiesen_US
dc.subjecttp-agben_US
dc.subjectpopulationen_US
dc.subjectevolutionen_US
dc.subjectastronomy & astrophysicsen_US
dc.titleConverting From 3.6 And 4.5 Micron Fluxes To Stellar Massen_US
dc.typeArticleen_US
dc.description.departmentAstronomyen_US
dc.identifier.doi10.1088/0004-6256/143/6/139en_US
dc.contributor.utaustinauthorEskew, Michaelen_US
dc.relation.ispartofserialAstronomical Journalen_US


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