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Physical properties of star clusters in the outer LMC as observed by the Dark Energy Survey

Pieres, A, Santiago, B, Balbinot, E, Luque, E, Queiroz, ABA, Costa, LND, Maia, MAG, Drlica-Wagner, A, Roodman, A, Abbott, C , Allam, S, Benoit-Levy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Cunha, CE, Desai, S, Diehl, HT, Eifler, TF, Finley, DA, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, DW, Gruen, D, Gruendl, RA, Gutierrez, G, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Marshall, JL, Martini, P, Miller, CJ, Miquel, R, Nichol, RC, Nord, B, Ogando, R, Plazas, AA, Romer, AK, Sanchez, E, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thaler, J, Thomas, D, Tucker, D and Walker, AR (2015) Physical properties of star clusters in the outer LMC as observed by the Dark Energy Survey

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Abstract

The Large Magellanic Cloud (LMC) harbors a rich and diverse system of star clusters, whose ages, chemical abundances, and positions provide information about the LMC history of star formation. We use Science Verification imaging data from the Dark Energy Survey to increase the census of known star clusters in the outer LMC and to derive physical parameters for a large sample of such objects using a spatially and photometrically homogeneous data set. Our sample contains 255 visually identified cluster candidates, of which 109 were not listed in any previous catalog. We quantify the crowding effect for the stellar sample produced by the DES Data Management pipeline and conclude that the stellar completeness is < 10% inside typical LMC cluster cores. We therefore develop a pipeline to sample and measure stellar magnitudes and positions around the cluster candidates using DAOPHOT. We also implement a maximum-likelihood method to fit individual density profiles and colour-magnitude diagrams. For 117 (from a total of 255) of the cluster candidates (28 uncatalogued clusters), we obtain reliable ages, metallicities, distance moduli and structural parameters, confirming their nature as physical systems. The distribution of cluster metallicities shows a radial dependence, with no clusters more metal-rich than [Fe/H] ~ -0.7 beyond 8 kpc from the LMC center. The age distribution has two peaks at ~ 1.2 Gyr and ~ 2.7 Gyr.

Item Type: Article
Authors :
NameEmailORCID
Pieres, A
Santiago, B
Balbinot, Ee.balbinot@surrey.ac.uk
Luque, E
Queiroz, ABA
Costa, LND
Maia, MAG
Drlica-Wagner, A
Roodman, A
Abbott, C
Allam, S
Benoit-Levy, A
Bertin, E
Brooks, D
Buckley-Geer, E
Burke, DL
Rosell, AC
Kind, MC
Carretero, J
Cunha, CE
Desai, S
Diehl, HT
Eifler, TF
Finley, DA
Flaugher, B
Fosalba, P
Frieman, J
Gerdes, DW
Gruen, D
Gruendl, RA
Gutierrez, G
Honscheid, K
James, DJ
Kuehn, K
Kuropatkin, N
Lahav, O
Li, TS
Marshall, JL
Martini, P
Miller, CJ
Miquel, R
Nichol, RC
Nord, B
Ogando, R
Plazas, AA
Romer, AK
Sanchez, E
Scarpine, V
Schubnell, M
Sevilla-Noarbe, I
Smith, RC
Soares-Santos, M
Sobreira, F
Suchyta, E
Swanson, MEC
Tarle, G
Thaler, J
Thomas, D
Tucker, D
Walker, AR
Date : 3 December 2015
Uncontrolled Keywords : astro-ph.GA, astro-ph.GA
Related URLs :
Depositing User : Symplectic Elements
Date Deposited : 17 May 2017 13:46
Last Modified : 17 May 2017 15:12
URI: http://epubs.surrey.ac.uk/id/eprint/840280

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