The Mid-Infrared Extinction Law in the Large Magellanic Cloud

Jian, Gao; Jiang, Biwei; Li, Aigen; Xue, Mengyao

doi:10.1088/0004-637x/776/1/7

Cited by 40 publications

(35 citation statements)

References 60 publications

(134 reference statements)

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“…The latter is in excellent agreement with those listed in Table 6. As for the cluster distance moduli, we adopted the same distance modulus for all clusters (m − M) o = 18.49 ± 0.09 mag ) and Cardelli et al 1989;Gao et al 2013); by considering an average depth for the LMC disc of (3.44 ± 1.16) kpc (∆((m − M) o ) ∼ 0.15 mag Subramanian & Subramaniam 2009), we derived a smaller age difference than that resulting from the isochrones (characterised by the same metallicity) bracketing the observed cluster features in the CMD.…”

Section: Cluster Ages and Extinctionsmentioning

confidence: 99%

Extended main sequence turn-offs in low mass intermediate-age clusters

Piatti

Bastian

2016

A&A

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We present an imaging analysis of four low mass stellar clusters ( < ∼ 5000 M ) in the outer regions of the LMC in order to shed light on the extended main sequence turn-off (eMSTO) phenomenon observed in high mass clusters. The four clusters have ages between 1−2 Gyr and two of them appear to host eMTSOs. The discovery of eMSTOs in such low mass clusters -more than 5 times less massive than the eMSTO clusters previously studied -suggests that mass is not the controlling factor in whether clusters host eMSTOs. Additionally, the narrow extent of the eMSTO in the two older clusters (∼2 Gyr) is in agreement with predictions of the stellar rotation scenario, as lower mass stars are expected to be magnetically braked, meaning that their colour magnitude diagrams should be better reproduced by canonical simple stellar populations. We also performed a structural analysis on all the clusters and found that a large core radius is not a requisite for a cluster to exhibit an eMSTO.

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Section: Cluster Ages and Extinctionsmentioning

confidence: 99%

Extended main sequence turn-offs in low mass intermediate-age clusters

Piatti

Bastian

2016

A&A

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“…4 and 5). The reddening values were converted using the following equations: E(V −J)=1.80E(V −I); E(V −Ks)=2.24E(V −I) E(J−Ks)=0.43E(V −I) (Cardelli, Clayton, & Mathis 1989;Gao et al 2013). 7 The coefficients of the P W relations were calculated in a similar way.…”

Section: J Ks-band Period-luminosity Period-luminosity-colour and Pmentioning

confidence: 99%

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

Ripepi

Moretti

Marconi

et al. 2014

Monthly Notices of the Royal Astronomical Society

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The VISTA survey of the Magellanic Clouds System (VMC) is collecting deep K s -band time-series photometry of the pulsating variable stars hosted in the system formed by the two Magellanic Clouds and the Bridge connecting them. In this paper we have analysed a sample of 130 Large Magellanic Cloud (LMC) Type II Cepheids (T2CEPs) found in tiles with complete or near complete VMC observations for which identification and optical magnitudes were obtained from the OGLE III survey. We present J and K s light curves for all 130 pulsators, including 41 BL Her, 62 W Vir (12 pW Vir) and 27 RV Tau variables. We complement our near-infrared photometry with the V magnitudes from the OGLE III survey, allowing us to build a variety of PeriodLuminosity (P L), Period-Luminosity-Colour (P LC) and Period-Wesenheit (P W ) relationships, including any combination of the V, J, K s filters and valid for BL Her and W Vir classes. These relationships were calibrated in terms of the LMC distance modulus, while an independent absolute calibration of the P L(K s ) and the P W (K s , V ) was derived on the basis of distances obtained from Hubble Space T elescope parallaxes and Baade-Wesselink technique. When applied to the LMC and to the Galactic Globular Clusters hosting T2CEPs, these relations seem to show that: 1) the two population II standard candles RR Lyrae and T2CEPs give results in excellent agreement with each other; 2) there is a discrepancy of ∼0.1 mag between population II standard candles and Classical Cepheids when the distances are gauged in a similar way for all the quoted pulsators. However, given the uncertainties, this discrepancy is within the formal 1σ uncertainties.

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“…We adopted the same distance modulus for all clusters (m − M )0 = 18.49 ± 0.09 mag (de Grijs, Wicker & Bono 2014) and Ks − MK s = (m − M )0 + 0.372E(B − V ), for RV = 3.1 (Cardelli, Clayton & Mathis 1989;Gao et al 2013), since by considering an average depth for the LMC disc of (3.44±1.16) kpc ), we derived a smaller age difference than that resulting from the isochrones (characterized by the same metallicity) bracketing the observed cluster features in the CMD.…”

Section: Star Cluster Parametersmentioning

confidence: 99%

The VMC survey – XVI. Spatial variation of the cluster formation activity in the innermost regions of the Large Magellanic Cloud

Piatti

Grijs

Ripepi

et al. 2015

Mon. Not. R. Astron. Soc.

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We present results based on Y JK s photometry of star clusters in the Large Magellanic Cloud (LMC), distributed throughout the central part of the galaxy's bar and the 30 Doradus region. We analysed the field-star decontaminated colour-magnitude diagrams of 313 clusters to estimate their reddening values and ages. The clusters are affected by a mean reddening of E(B − V ) ∈ [0.2, 0.3] mag, where the average internal LMC reddening amounts to ∼ 0.1-0.2 mag. The region covering 30 Doradus includes clusters with reddening values in excess of E(B − V ) = 0.4 mag. Our cluster sample spans the age range 7.0 log(t yr −1 ) < 9.0, represents an increase of 30 per cent in terms of the number of clusters with robust age estimates and comprises a statistically complete sample in the LMC regions of interest here. The resulting cluster frequencies suggest that the outermost regions of the LMC bar first experienced enhanced cluster formation -log(t yr −1 ) ∈ [8.5, 9.0] -before the activity proceeded, although in a patchy manner, to the innermost regions, for log(t yr −1 ) < 7.7. Cluster frequencies in the 30 Doradus region show that the area is dominated by very recent cluster formation. The derived star-formation frequencies suggest that the cluster and field-star populations do not seem to have fully evolved as fully coupled systems during the last ∼ 100 Myr.

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The Mid-Infrared Extinction Law in the Large Magellanic Cloud

Cited by 40 publications

References 60 publications

Extended main sequence turn-offs in low mass intermediate-age clusters

Extended main sequence turn-offs in low mass intermediate-age clusters

The VMC Survey – XIII. Type II Cepheids in the Large Magellanic Cloud★

The VMC survey – XVI. Spatial variation of the cluster formation activity in the innermost regions of the Large Magellanic Cloud

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