Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iii. The Small Magellanic Cloud

Grijs, Richard de; Bono, G.

doi:10.1088/0004-6256/149/6/179

Cited by 114 publications

(57 citation statements)

References 123 publications

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“…We also note that the theoretical slopes agree quite well with the empirical ones, for both F and FO pulsators. Moreover, the inferred intrinsic mean distance modulus is equal to µ0 = 19.01 mag and its standard deviation to 0.08 mag, in agreement with the most recent literature values (see de Grijs & Bono 2015;Ripepi et al 2016, and references therein).…”

Section: The Pl Relationssupporting

confidence: 90%

The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids

Marconi

Molinaro

Ripepi

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the results of the χ 2 minimization model fitting technique applied to optical and near-infrared photometric and radial velocity data for a sample of 9 fundamental and 3 first overtone classical Cepheids in the Small Magellanic Cloud (SMC). The nearinfrared photometry (JK filters) was obtained by the European Southern Observatory (ESO) public survey "VISTA near-infrared Y, J, K s survey of the Magellanic Clouds system" (VMC). For each pulsator isoperiodic model sequences have been computed by adopting a nonlinear convective hydrodynamical code in order to reproduce the multifilter light and (when available) radial velocity curve amplitudes and morphological details. The inferred individual distances provide an intrinsic mean value for the SMC distance modulus of 19.01 mag and a standard deviation of 0.08 mag, in agreement with the literature. Moreover the instrinsic masses and luminosities of the best fitting model show that all these pulsators are brighter than the canonical evolutionary MassLuminosity relation (MLR), suggesting a significant efficiency of core overshooting and/or mass loss. Assuming that the inferred deviation from the canonical MLR is only due to mass loss, we derive the expected distribution of percentage mass loss as a function of both the pulsation period and of the canonical stellar mass. Finally, a good agreement is found between the predicted mean radii and current Period-Radius (PR) relations in the SMC available in the literature. The results of this investigation support the predictive capabilities of the adopted theoretical scenario and pave the way to the application to other extensive databases at various chemical compositions, including the VMC Large Magellanic Cloud pulsators and Galactic Cepheids with Gaia parallaxes.

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Section: The Pl Relationssupporting

confidence: 90%

The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids

Marconi

Molinaro

Ripepi

et al. 2016

Mon. Not. R. Astron. Soc.

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“…These CMD regions were defined as in Cioni et al (2014) for the LMC and were adjusted to the different mean distance, extinction, and metallicity of the SMC by applying a shift in magnitude, K s = +0.6, and in colour, (J − K s ) = −0.04 (Cioni et al 2000b). The shift in magnitude is slightly larger than it appears in the latest studies; for example, we obtain ∼0.5 mag from de Bono (2015), but this difference does not influence our investigation. The proper motion of each region was derived from the median of the proper motion of the stars enclosed in the region after the application of a σ-clipping procedure.…”

Section: Smc Areacontrasting

confidence: 60%

“…The Small Magellanic Cloud (SMC), in particular, has an intriguing structure with a large extent along the line of sight (e.g. Subramanian & Subramaniam 2012;Nidever et al 2013;de Grijs & Bono 2015, and references therein) and a morphology that clearly depends on stellar population age (e.g. Cioni et al 2000a;Zaritsky et al 2000;Dobbie et al 2014;Subramanian & Subramaniam 2015;Deb et al 2015;Rubele et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The VMC survey

Cioni

Bekki

Girardi

et al. 2016

A&A

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Aims. In this study we use multi-epoch near-infrared observations from the VISTA survey of the Magellanic Cloud system (VMC) to measure the proper motions of different stellar populations in a tile of 1.5 deg 2 in size in the direction of the Galactic globular cluster 47 Tuc. We obtain the proper motion of the cluster itself, of the Small Magellanic Cloud (SMC), and of the field Milky Way stars. Methods. Stars of the three main stellar components are selected according to their spatial distributions and their distributions in colour−magnitude diagrams. Their average coordinate displacement is computed from the difference between multiple K s -band observations for stars as faint as K s = 19 mag. Proper motions are derived from the slope of the best-fitting line among ten VMC epochs over a time baseline of ∼1 yr. Background galaxies are used to calibrate the absolute astrometric reference frame. Results. The resulting absolute proper motion of 47 Tuc is (μ α cos(δ), μ δ ) = (+7.26 ± 0.03, −1.25 ± 0.03) mas yr −1 . This measurement refers to about 35 000 sources distributed between 10 and 60 from the cluster centre. For the SMC we obtain (μ α cos(δ), μ δ ) = (+1.16 ± 0.07, −0.81 ± 0.07) mas yr −1 from about 5250 red clump and red giant branch stars. The absolute proper motion of the Milky Way population in the line of sight (l = 305.9, b = −44.9) of this VISTA tile is (μ α cos(δ), μ δ ) = (+10.22 ± 0.14, −1.27 ± 0.12) mas yr −1 and has been calculated from about 4000 sources. Systematic uncertainties associated with the astrometric reference system are 0.18 mas yr −1 . Thanks to the proper motion we detect 47 Tuc stars beyond its tidal radius.

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“…The LMC and SMC are the two most extensively studied galaxies, and with more than 500 distance determinations from a variety of techniques (de Grijs et al 2014) they are a natural choice for studies aimed at testing the accuracy of the TRGB method. The recent very accurate 2.2% distance measurement to the LMC from eclipsing binaries gives us a unique opportunity to compare different methods, and use the LMC as a very accurate zero-point for distance calibrations.…”

Section: Introductionmentioning

confidence: 99%

The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

Górski

Pietrzyński

Gieren

et al. 2016

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We present a precise optical and near-infrared determination of the tip of the red giant branch (TRGB) brightness in the Large and Small Magellanic Clouds (respectively, LMC and SMC). The commonly used calibrations of the absolute magnitude of the TRGB lead to an overestimation of the distance to the LMC and SMC in the K band, and an underestimation of the distance in the optical I band for both galaxies. Reported discrepancies are at the level of 0.2 mag, with respect to the very accurate distance determinations to both MCs based on late-type eclipsing binaries. The differential distances between the LMC and SMC obtained in the J and K bands, and for the bolometric brightness are consistent with each other, and with the results obtained from eclipsing binaries and other distance indicators.

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Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iii. The Small Magellanic Cloud

Cited by 114 publications

References 123 publications

The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids

The VMC survey – XXIII. Model fitting of light and radial velocity curves of Small Magellanic Cloud classical Cepheids

The VMC survey

The Araucaria Project: On the Tip of the Red Giant Branch Distance Determination to the Magellanic Clouds

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