2015ApJ...815...28G


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.23CEST12:50:52

2015ApJ...815...28G - Astrophys. J., 815, 28 (2015/December-2)

The araucaria project: a study of the classical cepheid in the eclipsing binary system OGLE LMC562.05.9009 in the Large Magellanic Cloud.

GIEREN W., PILECKI B., PIETRZYNSKI G., GRACZYK D., UDALSKI A., SOSZYNSKI I., THOMPSON I.B., PRADA MORONI P.G., SMOLEC R., KONORSKI P., GORSKI M., KARCZMAREK P., SUCHOMSKA K., TAORMINA M., GALLENNE A., STORM J., BONO G., CATELAN M., SZYMANSKI M., KOZLOWSKI S., PIETRUKOWICZ P., WYRZYKOWSKI L., POLESKI R., SKOWRON J., MINNITI D., ULACZYK K., MROZ P., PAWLAK M. and NARDETTO N.

Abstract (from CDS):

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 M, R1= 28.6±0.2 R) than its companion (M2= 3.60±0.03 M, R2= 26.6±0.2 R). 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.

Abstract Copyright:

Journal keyword(s): binaries: eclipsing - galaxies: individual: LMC - stars: oscillations - stars: variables: Cepheids

Simbad objects: 6

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Number of rows : 6

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 OGLE LMC-CEP-227 cC* 04 52 15.6982549282 -70 14 31.242341027     15.317   14.438 ~ 46 0
2 OGLE LMC-SC6 330185 cC* 05 21 54.92 -69 21 50.1   15.706 15.190   14.511 ~ 18 0
3 SV* HV 12024 cC* 05 23 07.71 -69 33 49.9   17.360 16.707   16.054 ~ 24 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14325 1
5 OGLE LMC-SC16 119952 cC* 05 36 04.456 -70 01 55.66     16.88 16.23 15.743 F4II+K1III-II 21 1
6 OGLE LMC-CEP-4506 cC* 05 53 29.3579743272 -67 53 59.360079055     15.459   14.778 ~ 15 0

    Equat.    Gal    SGal    Ecl

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2019.10.23-12:50:52

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