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The LMC geometry and outer stellar populations from early DES data

Balbinot, E, Santiago, BX, Girardi, L, Pieres, A, Costa, LND, Maia, MAG, Walker, RAGAR, Yanny, B, Drlica-Wagner, A, Benoit-Levy, A, Abbott, TMC, Allam, SS, nnis, JA, Bernstein, JP, Bernstein, RA, Bertin, E, Brooks, D, Buckley-Geer, E, Rosell, AC, Cunha, CE, DePoy, DL, Desai, S, Diehl, HT, Doel, P, Estrada, J, Evrard, AE, to, AFN, Finley, DA, Flaugher, B, Frieman, JA, Gruen, D, Honscheid, K, James, D, Kuehn, K, Kuropatkin, N, Lahav, O, March, M, Marshall, JL, Miller, C, Ogando, RMR, Peoples, J, Plazas, A, Scarpine, V, Schubnell, M, Sevilla-Noarbe, I, Smith, RC, Soares-Santos, M, Suchyta, E, Swanson, MEC, Tarle, G, Tucker, DL, Wechsler, R and Zuntz, J (2015) The LMC geometry and outer stellar populations from early DES data Monthly Notices of the Royal Astronomical Society.

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Abstract

The Dark Energy Camera has captured a large set of images as part of Science Verification (SV) for the Dark Energy Survey. The SV footprint covers a lar ge portion of the outer Large Magellanic Cloud (LMC), providing photometry 1.5 magnitudes fainter than the main sequence turn-off of the oldest LMC stel lar population. We derive geometrical and structural parameters for various stellar populations in the LMC disk. For the distribution of all LMC stars, we find an inclination of $i=-38.14^{\circ}\pm0.08^{\circ}$ (near side in the North) and a position angle for the line of nodes of $\theta_0=129.51^{\circ}\pm0.17^{\circ}$. We find that stars younger than $\sim 4$ Gyr are more centrally concentrated than older stars. Fitting a projected exponential disk shows that the scale radius of the old populations is $R_{>4 Gyr}=1.41\pm0.01$ kpc, while the younger population has $R_{<4 Gyr}=0.72\pm0.01$ kpc. Howe ver, the spatial distribution of the younger population deviates significantly from the projected exponential disk model. The distribution of old stars suggests a large truncation radius of $R_{t}=13.5\pm0.8$ kpc. If this truncation is dominated by the tidal field of the Galaxy, we find that the LMC is $\simeq 24^{+9}_{-6}$ times less massive than the encircled Galactic mass. By measuring the Red Clump peak magnitude and comparing with the best-fit LM C disk model, we find that the LMC disk is warped and thicker in the outer regions north of the LMC centre. Our findings may either be interpreted as a warped and flared disk in the LMC outskirts, or as evidence of a spheroidal halo component

Item Type: Article
Authors :
NameEmailORCID
Balbinot, Ee.balbinot@surrey.ac.ukUNSPECIFIED
Santiago, BXUNSPECIFIEDUNSPECIFIED
Girardi, LUNSPECIFIEDUNSPECIFIED
Pieres, AUNSPECIFIEDUNSPECIFIED
Costa, LNDUNSPECIFIEDUNSPECIFIED
Maia, MAGUNSPECIFIEDUNSPECIFIED
Walker, RAGARUNSPECIFIEDUNSPECIFIED
Yanny, BUNSPECIFIEDUNSPECIFIED
Drlica-Wagner, AUNSPECIFIEDUNSPECIFIED
Benoit-Levy, AUNSPECIFIEDUNSPECIFIED
Abbott, TMCUNSPECIFIEDUNSPECIFIED
Allam, SSUNSPECIFIEDUNSPECIFIED
nnis, JAUNSPECIFIEDUNSPECIFIED
Bernstein, JPUNSPECIFIEDUNSPECIFIED
Bernstein, RAUNSPECIFIEDUNSPECIFIED
Bertin, EUNSPECIFIEDUNSPECIFIED
Brooks, DUNSPECIFIEDUNSPECIFIED
Buckley-Geer, EUNSPECIFIEDUNSPECIFIED
Rosell, ACUNSPECIFIEDUNSPECIFIED
Cunha, CEUNSPECIFIEDUNSPECIFIED
DePoy, DLUNSPECIFIEDUNSPECIFIED
Desai, SUNSPECIFIEDUNSPECIFIED
Diehl, HTUNSPECIFIEDUNSPECIFIED
Doel, PUNSPECIFIEDUNSPECIFIED
Estrada, JUNSPECIFIEDUNSPECIFIED
Evrard, AEUNSPECIFIEDUNSPECIFIED
to, AFNUNSPECIFIEDUNSPECIFIED
Finley, DAUNSPECIFIEDUNSPECIFIED
Flaugher, BUNSPECIFIEDUNSPECIFIED
Frieman, JAUNSPECIFIEDUNSPECIFIED
Gruen, DUNSPECIFIEDUNSPECIFIED
Honscheid, KUNSPECIFIEDUNSPECIFIED
James, DUNSPECIFIEDUNSPECIFIED
Kuehn, KUNSPECIFIEDUNSPECIFIED
Kuropatkin, NUNSPECIFIEDUNSPECIFIED
Lahav, OUNSPECIFIEDUNSPECIFIED
March, MUNSPECIFIEDUNSPECIFIED
Marshall, JLUNSPECIFIEDUNSPECIFIED
Miller, CUNSPECIFIEDUNSPECIFIED
Ogando, RMRUNSPECIFIEDUNSPECIFIED
Peoples, JUNSPECIFIEDUNSPECIFIED
Plazas, AUNSPECIFIEDUNSPECIFIED
Scarpine, VUNSPECIFIEDUNSPECIFIED
Schubnell, MUNSPECIFIEDUNSPECIFIED
Sevilla-Noarbe, IUNSPECIFIEDUNSPECIFIED
Smith, RCUNSPECIFIEDUNSPECIFIED
Soares-Santos, MUNSPECIFIEDUNSPECIFIED
Suchyta, EUNSPECIFIEDUNSPECIFIED
Swanson, MECUNSPECIFIEDUNSPECIFIED
Tarle, GUNSPECIFIEDUNSPECIFIED
Tucker, DLUNSPECIFIEDUNSPECIFIED
Wechsler, RUNSPECIFIEDUNSPECIFIED
Zuntz, JUNSPECIFIEDUNSPECIFIED
Date : 17 February 2015
Identification Number : https://doi.org/10.1093/mnras/stv356
Uncontrolled Keywords : astro-ph.GA, astro-ph.GA
Related URLs :
Depositing User : Symplectic Elements
Date Deposited : 17 May 2017 13:34
Last Modified : 17 May 2017 15:11
URI: http://epubs.surrey.ac.uk/id/eprint/839686

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