An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent

Pietrzyński, G.; Graczyk, D.; Gieren, W.; Thompson, I. B.; Pilecki, B.; Udalski, A.; Soszyński, I.; Kozłowski, S.; Konorski, P.; Suchomska, K.; Bono, G.; Moroni, Pier Giorgio Prada; Villanova, S.; Nardetto, N.; Bresolin, Fabio; Kudritzki, Rolf‐Peter; Storm, J.; Gallenne, A.; Smolec, R.; Minniti, D.; Kubiak, M.; Szymański, M. K.; Poleski, R.; Wyrzykowski, Ł.; Ulaczyk, K.; Pietrukowicz, P.; Górski, Marek; Karczmarek, P.

doi:10.1038/nature11878

Cited by 634 publications

(638 citation statements)

References 38 publications

(53 reference statements)

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“…The flux corrected for vignetting was 0.0112 counts/sec which is ∼140 times less than the flux of AG Dra observed at quiescence on Nov 27-Dec 7 (Bickert et al 1993), at orbital phase φ ∼ 0.7 and L h ∼ 1000 (d/2.5 kpc) 2 (Mikołajewska et al 1995). After scaling the AG Dra flux to the distance of the LMC (Pietrzyński et al 2013) its flux should be equal to ∼0.00385 counts/sec, ∼3 times fainter than LMC S63. We recall here that the LMC S63 hot component luminosity was ∼ 5× higher in 1994 than that for AG Dra.…”

Section: The Hot Componentmentioning

confidence: 99%

“…7). The scaling factor, (R g /d) −2 = 7.48 × 10 −21 , corresponds to the red giant radius R g = 190 R ⊙ at the distance to the LMC, d = 49.97 kpc (Pietrzyński et al 2013).…”

Section: The Cool Giantmentioning

confidence: 99%

“…Using VOSA (Bayo et al 2008) we performed a Bayesian analysis of the data. We assumed the distance of LMC d = 49.97 kpc (Pietrzyński et al 2013) and E(B-V)=0.05 (Muerset et al 1991). As a result, apart from parameters of the red giant, we estimated such parameters as the dust mass-loss rateṀ dust , inner radius of the dust shell R in and optical depth at 11.3 microns τ 11.3 (see Table 2).…”

Section: The Cool Giantmentioning

confidence: 99%

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LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

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We present an analysis of multi-epoch low-resolution spectrophotometry, complemented by the light curves provided by massive photometric surveys spanning over 100 years, of the symbiotic binary LMC S63. We showed that it is an eclipsing binary with the orbital period of 1050 d . We also found evidence of outbursts in history of the white dwarf. If it was a Z-And type outburst, as is most likely, it would be a second such outburst recorded in the Magellanic Cloud symbiotic system. We confirmed that the red giant is enhanced in carbon, and estimated C/O ≃ 1.2 by fitting a model atmosphere to the SALT spectrum. We also found bi-periodic pulsations of the red giant, and demonstrated that it is similar to other carbon variables with confirmed bi-periodicity.

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Section: The Hot Componentmentioning

confidence: 99%

“…7). The scaling factor, (R g /d) −2 = 7.48 × 10 −21 , corresponds to the red giant radius R g = 190 R ⊙ at the distance to the LMC, d = 49.97 kpc (Pietrzyński et al 2013).…”

Section: The Cool Giantmentioning

confidence: 99%

Section: The Cool Giantmentioning

confidence: 99%

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LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

Iłkiewicz

Mikołajewska

Miszalski

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Well-constrained systems can also be used to accurately measure distances (e.g. Pietrzynski et al 2013).…”

Section: Eclipsing Binariesmentioning

confidence: 99%

The Catalina Surveys Southern periodic variable star catalogue

Drake

Djorgovski

Catelan

et al. 2017

Monthly Notices of the Royal Astronomical Society

166

133

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Here, we present the results from our analysis of 6 yr of optical photometry taken by the Siding Spring Survey (SSS). This completes a search for periodic variable stars within the 30 000 deg 2 of the sky covered by the Catalina Surveys. The current analysis covers 81 million sources with declinations between −20 • and −75 • with median magnitudes in the range 11 < V < 19.5. We find approximately 34 000 new periodic variable stars in addition to the ∼9000 RR Lyrae that we previously discovered in SSS data. This brings the total number of periodic variables identified in Catalina data to ∼110 000. The new SSS periodic variable stars mainly consist of eclipsing binaries, RR Lyrae, LPVs, RS CVn stars, δ Scutis, and Anomalous Cepheids. By cross-matching these variable stars with those from prior surveys, we find that ∼90 per cent of the sources are new discoveries and recover ∼95 per cent of the known periodic variables in the survey region. For the known sources, we find excellent agreement between our catalogue and prior values of luminosity, period, and amplitude. However, we find many variable stars that had previously been misclassified. Examining the distribution of RR Lyrae, we find a population associated with the Large Magellanic Cloud (LMC) that extends more than 20 • from its centre confirming recent evidence for the existence of a very extended stellar halo in the LMC. By combining SSS photometry with Dark Energy Survey data, we identify additional LMC halo RR Lyrae, thus confirming the significance of the population.

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“…We focus on the more numerous LMC sample of anomalous RRd stars. For a given model, mean colours and Wesenheit index were computed through interpolation in the Kurucz (2005) 1 atmosphere models and adopting a 18.5 mag distance modulus to the LMC (Pietrzyński et al 2013). The model lines presented in Fig.…”

Section: Nature and Cause Of The Anomalous Rrd Pulsationmentioning

confidence: 99%

Anomalous double-mode RR Lyrae stars in the Magellanic Clouds

Soszyński

Smolec

Dziembowski

et al. 2016

Mon. Not. R. Astron. Soc.

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172

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We report the discovery of a new subclass of double-mode RR Lyrae stars in the Large and Small Magellanic Clouds. The sample of 22 pulsating stars have been extracted from the latest edition of the OGLE collection of RR Lyrae variables in the Magellanic System. The stars pulsating simultaneously in the fundamental (F) and first-overtone (1O) modes have distinctly different properties than regular double-mode RR Lyrae variables (RRd stars). The P 1O /P F period ratios of our anomalous RRd stars are within a range 0.725-0.738, while "classical" double-mode RR Lyrae variables have period ratios in the range 0.742-0.748. In contrast to the typical RRd stars, in the majority of the anomalous pulsators the F-mode amplitudes are higher than the 1O-mode amplitudes. The light curves associated with the F-mode in the anomalous RRd stars show different morphology than the light curves of, both, regular RRd stars and single-mode RRab stars. Most of the anomalous double-mode stars show long-term modulations of the amplitudes (Blazhko-like effect). Translating the period ratios into the abundance parameter, Z, we find for our stars Z ∈ (0.002, 0.005) -an order of magnitude higher values than typical for RR Lyrae stars. The mass range of the RRd stars inferred from the W I vs. P F diagram is (0.55 − 0.75) M ⊙ . These parameters cannot be accounted for with single star evolution assuming a Reimers-like mass loss. Much greater mass loss caused by interaction with other stars is postulated. We blame the peculiar pulsation properties of our stars to the parametric resonance instability of the 1O-mode to excitation of the F-and 2O-modes as with the inferred parameters of the stars 2ω 1O ≈ ω F + ω 2O .

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An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent

Cited by 634 publications

References 38 publications

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star

The Catalina Surveys Southern periodic variable star catalogue

Anomalous double-mode RR Lyrae stars in the Magellanic Clouds

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