Background galaxies as reddening probes throughout the Magellanic Clouds

Dutra, Carlos Maximiliano; Bica, E.; Clariá, J. J.; Piatti, A. E.; Ahumada, A. V.

doi:10.1051/0004-6361:20010467

Cited by 40 publications

(53 citation statements)

References 36 publications

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“…The remainder of the stars should be classified as outliers and need further careful inspection. Dutra et al (2001) find the Milky Way mean reddening in the direction of the LMC to be around 0.06 mag, and the internal LMC reddening to be E(B − V) = 0.05 ± 0.05. A similar result was obtained by Clementini et al (2003).…”

Section: Mean J and K S Magnitudes And Error Analysismentioning

confidence: 81%

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Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Borissova¹,

Rejkuba²,

Minniti

et al. 2009

A&A

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Context. RR Lyrae variable stars are the primary Population II distance indicator. Likewise, the Large Magellanic Cloud (LMC) constitutes a key step in the extragalactic distance scale. Aims. By combining near-IR photometry and spectroscopically measured metallicities for a homogeneous sample of 50 RR Lyr stars in the LMC, we investigate the metallicity dependence of the period-luminosity relation in the near-infrared (IR), use the newly derived relations to re-derive the distance to the LMC, and compare the distance moduli obtained from RR Lyr and red clump stars. Methods. This paper presents new (single-epoch) J-band and (multi-epoch) K s -band photometry of RR Lyr stars in 7 different LMC fields, observed with the near-IR camera SOFI at ESO's New Technology Telescope. Additional K s -band data for another two LMC fields were taken with the ISPI infrared array at CTIO's Blanco 4m telescope. The near-IR photometry was cross-correlated with the MACHO and OGLE databases, resulting in a catalog of 62 RR Lyr stars with BVRI JK s photometry. A subsample of 50 stars also has spectroscopically measured metallicities. Results. In the deep JK color-magnitude diagrams of 7 fields, red giant branch, red clump and RR Lyr stars are detected. The majority of RR Lyr stars are located within the instability strip with near-IR colors between 0.14 ≤ (J − K s ) 0 < 0.32. The period-luminosity relation only has a very mild dependence on metallicity in the K band, consistent with no dependence: M Ks = 2.11(±0.17) log P + 0.05(±0.07) [Fe/H] − 1.05. In the J band the currently available data do not allow firm conclusions regarding the metallicity dependence of the period-luminosity relation. Conclusions. The distance modulus of the LMC, derived using our near-IR period-luminosity-metallicity relation for RR Lyr stars, is (m − M) 0 = 18.53 ± 0.13, in very good agreement with the distance modulus from the red clump stars, 18.46 ± 0.07. However, LMC modulus derived from the RR Lyrae stars depends on the parallax of the star RR Lyrae.

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Section: Mean J and K S Magnitudes And Error Analysismentioning

confidence: 81%

“…Investigations of the LMC extinction, however, show that it is non-uniform and clumpy (see, for example, Udalski et al 2000;Dutra et al 2001;Zaritsky et al 2004). Therefore, it is necessary to calculate individual reddenings for each of the stars in our sample.…”

Section: Mean J and K S Magnitudes And Error Analysismentioning

confidence: 99%

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Borissova¹,

Rejkuba²,

Minniti

et al. 2009

A&A

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“…SFD found that at high-latitude regions, their dust maps correlate well with maps of H I emission, but deviations are coherent in the sky and are especially conspicuous in regions of saturation of HI emission towards denser clouds and of formation of H 2 in molecular clouds. The SMC is quite transparent, the average foreground and internal reddenings being 0.01 and 0.04, respectively (Dutra et al 2001). The typical …”

Section: Template Matching Methodsmentioning

confidence: 99%

Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud

Piatti

Santos²,

Clariá

et al. 2005

A&A

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Abstract. We present in this study flux-calibrated integrated spectra in the range (3600-6800) Å for 18 concentrated SMC clusters. Cluster reddening values were estimated by interpolation between the extinction maps of Burstein & Heiles (1982, AJ, 87, 1165 and Schlegel et al. (1998, ApJ, 500, 525). The cluster parameters were derived from the template matching procedure by comparing the line strengths and continuum distribution of the cluster spectra with those of template cluster spectra with known parameters and from the equivalent width (EW) method. In this case, new calibrations were used together with diagnostic diagrams involving the sum of EWs of selected spectral lines. A very good agreement between ages derived from both methods was found. The final cluster ages obtained from the weighted average of values taken from the literature and the present measured ones range from 15 Mr (e.g. L 51) to 7 Gyr (K 3). Metal abundances have been derived for only 5 clusters from the present sample, while metallicity values directly averaged from published values for other 4 clusters have been adopted. Combining the present cluster sample with 19 additional SMC clusters whose ages and metal abundances were put onto a homogeneous scale, we analyse the age and metallicity distributions in order to explore the SMC star formation history and its spatial extent. By considering the distances of the clusters from the SMC centre instead of their projections onto the right ascension and declination axes, the present age-position relation suggests that the SMC inner disk could have been related to a cluster formation episode which reached the peak ∼2.5 Gyr ago. Evidence for an age gradient in the inner SMC disk is also presented.

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“…were computed by averaging the extinction estimates in the literature (Dutra et al 2001;Oestreicher & Schmidt-Kaler 1996;Oestreicher et al 1995;Massey et al 1995;Schwering & Israel 1991;Bessel 1991;and Capaccioli et al 1990). Extinction values derived from extinction maps of the Magellanic Clouds were weighted twice in our computation.…”

Section: ) the Values For E(b − V)mentioning

confidence: 99%

Early decline spectra of nova SMC 2001 and nova LMC 2002

Mason¹,

Valle

Gilmozzi³

et al. 2005

A&A

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Abstract.We report results on the spectroscopic follow-up of Nova SMC 2001 and Nova LMC 2002 carried out at La Silla. The analysis of the spectroscopic evolution shows that these objects belong to the Fe II class, according to the Cerro Tololo scheme. From the line fluxes and the expansion velocities, we have derived an approximate mass for the ejected shells of 2÷3×10 −4 M . The filling factor measurements (ε ∼ 10 −4 ÷ 10 −1 ) suggest a clumpy structure for the ejecta.

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Background galaxies as reddening probes throughout the Magellanic Clouds

Cited by 40 publications

References 36 publications

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Properties of RR Lyrae stars in the inner regions of the Large Magellanic Cloud

Integrated spectral analysis of 18 concentrated star clusters in the Small Magellanic Cloud

Early decline spectra of nova SMC 2001 and nova LMC 2002

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