The Araucaria project: A study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the large magellanic cloud

Wolfgang Gieren, Bogumił Pilecki, Grzegorz Pietrzyński, Dariusz Graczyk, Andrzej Udalski, Igor Soszyński, Ian B. Thompson, Pier Giorgio Prada Moroni, Radosław Smolec, Piotr Konorski, Marek Górski, Paulina Karczmarek, Ksenia Suchomska, Mónica Taormina, Alexandre Gallenne, Jesper Storm, Giuseppe Bono, Márcio Catelan, Michał Szymański, Szymon KozłowskiPaweł Pietrukowicz, Łukasz Wyrzykowski, Radosław Poleski, Jan Skowron, Dante Minniti, K. Ulaczyk, P. Mróz, M. Pawlak, Nicolas Nardetto

Resultado de la investigación: Article

22 Citas (Scopus)

Resumen

We present a detailed study of the classical Cepheid in the double-lined, highly eccentric eclipsing binary system OGLE-LMC562.05.9009. The Cepheid is a fundamental mode pulsator with a period of 2.988 days. The orbital period of the system is 1550 days. Using spectroscopic data from three 4-8-m telescopes and photometry spanning 22 years, we were able to derive the dynamical masses and radii of both stars with exquisite accuracy. Both stars in the system are very similar in mass, radius, and color, but the companion is a stable, non-pulsating star. The Cepheid is slightly more massive and bigger (M1 = 3.70 ± 0.03 Mo, R1 = 28.6 ± 0.2 Ro) than its companion (M2 = 3.60 ± 0.03 Mo, R2 = 26.6 ± 0.2 Ro). Within the observational uncertainties both stars have the same effective temperature of 6030 ± 150 K. Evolutionary tracks place both stars inside the classical Cepheid instability strip, but it is likely that future improved temperature estimates will move the stable giant companion just beyond the red edge of the instability strip. Within current observational and theoretical uncertainties, both stars fit on a 205 Myr isochrone arguing for their common age. From our model, we determine a value of the projection factor of p = 1.37 ± 0.07 for the Cepheid in the OGLE-LMC562.05.9009 system. This is the second Cepheid for which we could measure its p-factor with high precision directly from the analysis of an eclipsing binary system, which represents an important contribution toward a better calibration of Baade-Wesselink methods of distance determination for Cepheids.

Idioma originalEnglish
Número de artículo28
PublicaciónAstrophysical Journal
Volumen815
N.º1
DOI
EstadoPublished - 10 dic 2015

Huella dactilar

Magellanic clouds
stars
temperature
calibration
strip
radii
eccentrics
photometry
project
projection
telescopes
color
orbitals
estimates
analysis
method

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Citar esto

Gieren, Wolfgang ; Pilecki, Bogumił ; Pietrzyński, Grzegorz ; Graczyk, Dariusz ; Udalski, Andrzej ; Soszyński, Igor ; Thompson, Ian B. ; Moroni, Pier Giorgio Prada ; Smolec, Radosław ; Konorski, Piotr ; Górski, Marek ; Karczmarek, Paulina ; Suchomska, Ksenia ; Taormina, Mónica ; Gallenne, Alexandre ; Storm, Jesper ; Bono, Giuseppe ; Catelan, Márcio ; Szymański, Michał ; Kozłowski, Szymon ; Pietrukowicz, Paweł ; Wyrzykowski, Łukasz ; Poleski, Radosław ; Skowron, Jan ; Minniti, Dante ; Ulaczyk, K. ; Mróz, P. ; Pawlak, M. ; Nardetto, Nicolas. / The Araucaria project : A study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the large magellanic cloud. En: Astrophysical Journal. 2015 ; Vol. 815, N.º 1.
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abstract = "We present a detailed study of the classical Cepheid in the double-lined, highly eccentric eclipsing binary system OGLE-LMC562.05.9009. The Cepheid is a fundamental mode pulsator with a period of 2.988 days. The orbital period of the system is 1550 days. Using spectroscopic data from three 4-8-m telescopes and photometry spanning 22 years, we were able to derive the dynamical masses and radii of both stars with exquisite accuracy. Both stars in the system are very similar in mass, radius, and color, but the companion is a stable, non-pulsating star. The Cepheid is slightly more massive and bigger (M1 = 3.70 ± 0.03 Mo, R1 = 28.6 ± 0.2 Ro) than its companion (M2 = 3.60 ± 0.03 Mo, R2 = 26.6 ± 0.2 Ro). Within the observational uncertainties both stars have the same effective temperature of 6030 ± 150 K. Evolutionary tracks place both stars inside the classical Cepheid instability strip, but it is likely that future improved temperature estimates will move the stable giant companion just beyond the red edge of the instability strip. Within current observational and theoretical uncertainties, both stars fit on a 205 Myr isochrone arguing for their common age. From our model, we determine a value of the projection factor of p = 1.37 ± 0.07 for the Cepheid in the OGLE-LMC562.05.9009 system. This is the second Cepheid for which we could measure its p-factor with high precision directly from the analysis of an eclipsing binary system, which represents an important contribution toward a better calibration of Baade-Wesselink methods of distance determination for Cepheids.",
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author = "Wolfgang Gieren and Bogumił Pilecki and Grzegorz Pietrzyński and Dariusz Graczyk and Andrzej Udalski and Igor Soszyński and Thompson, {Ian B.} and Moroni, {Pier Giorgio Prada} and Radosław Smolec and Piotr Konorski and Marek G{\'o}rski and Paulina Karczmarek and Ksenia Suchomska and M{\'o}nica Taormina and Alexandre Gallenne and Jesper Storm and Giuseppe Bono and M{\'a}rcio Catelan and Michał Szymański and Szymon Kozłowski and Paweł Pietrukowicz and Łukasz Wyrzykowski and Radosław Poleski and Jan Skowron and Dante Minniti and K. Ulaczyk and P. Mr{\'o}z and M. Pawlak and Nicolas Nardetto",
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Gieren, W, Pilecki, B, Pietrzyński, G, Graczyk, D, Udalski, A, Soszyński, I, Thompson, IB, Moroni, PGP, Smolec, R, Konorski, P, Górski, M, Karczmarek, P, Suchomska, K, Taormina, M, Gallenne, A, Storm, J, Bono, G, Catelan, M, Szymański, M, Kozłowski, S, Pietrukowicz, P, Wyrzykowski, Ł, Poleski, R, Skowron, J, Minniti, D, Ulaczyk, K, Mróz, P, Pawlak, M & Nardetto, N 2015, 'The Araucaria project: A study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the large magellanic cloud', Astrophysical Journal, vol. 815, n.º 1, 28. https://doi.org/10.1088/0004-637X/815/1/28

The Araucaria project : A study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the large magellanic cloud. / Gieren, Wolfgang; Pilecki, Bogumił; Pietrzyński, Grzegorz; Graczyk, Dariusz; Udalski, Andrzej; Soszyński, Igor; Thompson, Ian B.; Moroni, Pier Giorgio Prada; Smolec, Radosław; Konorski, Piotr; Górski, Marek; Karczmarek, Paulina; Suchomska, Ksenia; Taormina, Mónica; Gallenne, Alexandre; Storm, Jesper; Bono, Giuseppe; Catelan, Márcio; Szymański, Michał; Kozłowski, Szymon; Pietrukowicz, Paweł; Wyrzykowski, Łukasz; Poleski, Radosław; Skowron, Jan; Minniti, Dante; Ulaczyk, K.; Mróz, P.; Pawlak, M.; Nardetto, Nicolas.

En: Astrophysical Journal, Vol. 815, N.º 1, 28, 10.12.2015.

Resultado de la investigación: Article

TY - JOUR

T1 - The Araucaria project

T2 - A study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the large magellanic cloud

AU - Gieren, Wolfgang

AU - Pilecki, Bogumił

AU - Pietrzyński, Grzegorz

AU - Graczyk, Dariusz

AU - Udalski, Andrzej

AU - Soszyński, Igor

AU - Thompson, Ian B.

AU - Moroni, Pier Giorgio Prada

AU - Smolec, Radosław

AU - Konorski, Piotr

AU - Górski, Marek

AU - Karczmarek, Paulina

AU - Suchomska, Ksenia

AU - Taormina, Mónica

AU - Gallenne, Alexandre

AU - Storm, Jesper

AU - Bono, Giuseppe

AU - Catelan, Márcio

AU - Szymański, Michał

AU - Kozłowski, Szymon

AU - Pietrukowicz, Paweł

AU - Wyrzykowski, Łukasz

AU - Poleski, Radosław

AU - Skowron, Jan

AU - Minniti, Dante

AU - Ulaczyk, K.

AU - Mróz, P.

AU - Pawlak, M.

AU - Nardetto, Nicolas

PY - 2015/12/10

Y1 - 2015/12/10

N2 - We present a detailed study of the classical Cepheid in the double-lined, highly eccentric eclipsing binary system OGLE-LMC562.05.9009. The Cepheid is a fundamental mode pulsator with a period of 2.988 days. The orbital period of the system is 1550 days. Using spectroscopic data from three 4-8-m telescopes and photometry spanning 22 years, we were able to derive the dynamical masses and radii of both stars with exquisite accuracy. Both stars in the system are very similar in mass, radius, and color, but the companion is a stable, non-pulsating star. The Cepheid is slightly more massive and bigger (M1 = 3.70 ± 0.03 Mo, R1 = 28.6 ± 0.2 Ro) than its companion (M2 = 3.60 ± 0.03 Mo, R2 = 26.6 ± 0.2 Ro). Within the observational uncertainties both stars have the same effective temperature of 6030 ± 150 K. Evolutionary tracks place both stars inside the classical Cepheid instability strip, but it is likely that future improved temperature estimates will move the stable giant companion just beyond the red edge of the instability strip. Within current observational and theoretical uncertainties, both stars fit on a 205 Myr isochrone arguing for their common age. From our model, we determine a value of the projection factor of p = 1.37 ± 0.07 for the Cepheid in the OGLE-LMC562.05.9009 system. This is the second Cepheid for which we could measure its p-factor with high precision directly from the analysis of an eclipsing binary system, which represents an important contribution toward a better calibration of Baade-Wesselink methods of distance determination for Cepheids.

AB - We present a detailed study of the classical Cepheid in the double-lined, highly eccentric eclipsing binary system OGLE-LMC562.05.9009. The Cepheid is a fundamental mode pulsator with a period of 2.988 days. The orbital period of the system is 1550 days. Using spectroscopic data from three 4-8-m telescopes and photometry spanning 22 years, we were able to derive the dynamical masses and radii of both stars with exquisite accuracy. Both stars in the system are very similar in mass, radius, and color, but the companion is a stable, non-pulsating star. The Cepheid is slightly more massive and bigger (M1 = 3.70 ± 0.03 Mo, R1 = 28.6 ± 0.2 Ro) than its companion (M2 = 3.60 ± 0.03 Mo, R2 = 26.6 ± 0.2 Ro). Within the observational uncertainties both stars have the same effective temperature of 6030 ± 150 K. Evolutionary tracks place both stars inside the classical Cepheid instability strip, but it is likely that future improved temperature estimates will move the stable giant companion just beyond the red edge of the instability strip. Within current observational and theoretical uncertainties, both stars fit on a 205 Myr isochrone arguing for their common age. From our model, we determine a value of the projection factor of p = 1.37 ± 0.07 for the Cepheid in the OGLE-LMC562.05.9009 system. This is the second Cepheid for which we could measure its p-factor with high precision directly from the analysis of an eclipsing binary system, which represents an important contribution toward a better calibration of Baade-Wesselink methods of distance determination for Cepheids.

KW - binaries: eclipsing

KW - galaxies: individual (LMC)

KW - stars: oscillations

KW - stars: variables: Cepheids

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DO - 10.1088/0004-637X/815/1/28

M3 - Article

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JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

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