The variable stars of the Large Magellanic Cloud

Gaposchkin, Cecilia Helena Payne

doi:10.5479/si.00810231.13.1

Cited by 43 publications

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“…It is now known from the work of Gaposhkin (1972) and Payne-Gaposchkin (1971) that the Large Cloud does contain some Type II Cepheids about 2 magnitudes below the period-luminosity relation. In addition to 16 such stars in the Large Cloud, there are 3 in the Small Cloud.…”

Section: Square Degreementioning

confidence: 99%

Distribution and ages of Magellanic Cepheids

Gaposchkin¹

1974

Smithsonian Contributions to Astrophysics

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Section: Square Degreementioning

confidence: 99%

Distribution and ages of Magellanic Cepheids

Gaposchkin¹

1974

Smithsonian Contributions to Astrophysics

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“…They are population I, relatively massive (M > 4 M ) giant stars obeying the famous period-luminosity (PL) relationship discovered in the Magellanic Clouds by Henrietta Leavitt in 1908 ([18]). Figure 1 shows how many classical Cepheids in the Magellanic Clouds have been known from the beginning of the twentieth century, starting from 16 Cepheids 1 discovered by Leavitt ([18]), through several review and catalog papers summarizing the number of Cepheids known in those days ( [25,26,36,37]), the first catalogs of Cepheids in the Magellanic Clouds released by the MACHO and OGLE-II projects in 1999 ( [5,60,61]), ending with a real breakthrough that was made in recent years by OGLE-III ( [40,44]) and OGLE-IV projects ( [53]). Currently, we almost reached the maximum value of this distribution.…”

Section: Classical Cepheidsmentioning

confidence: 99%

“…In the next sections we present respectively classical Cepheids, RR Lyrae stars, type II Cepheids, anomalous Cepheids, long-period variables, and other pulsating stars. [18], [19], [36], [37], [25], [26], [5], [60], [61], [40], [44], [53].…”

Section: Introductionmentioning

confidence: 99%

The impact of large-scale, long-term optical surveys on pulsating star research

Soszyński

2017

EPJ Web Conf.

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Abstract. The era of large-scale photometric variability surveys began a quarter of a century ago, when three microlensing projects -EROS, MACHO, and OGLE -started their operation. These surveys initiated a revolution in the field of variable stars and in the next years they inspired many new observational projects. Large-scale optical surveys multiplied the number of variable stars known in the Universe. The huge, homogeneous and complete catalogs of pulsating stars, such as Cepheids, RR Lyrae stars, or long-period variables, offer an unprecedented opportunity to calibrate and test the accuracy of various distance indicators, to trace the three-dimensional structure of the Milky Way and other galaxies, to discover exotic types of intrinsically variable stars, or to study previously unknown features and behaviors of pulsators. We present historical and recent findings on various types of pulsating stars obtained from the optical large-scale surveys, with particular emphasis on the OGLE project which currently offers the largest photometric database among surveys for stellar variability.

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“…One of the first attempts to survey eclipsing binaries in the LMC goes back to Payne-Gaposchkin (1971), who visually examined about 2000 photographic plates, and classified and listed the main characteristics of 78 eclipsing binaries. At that time computers only started infiltrating modern astronomy and automatic handling was not possible.…”

Section: First Bites On Large Databasesmentioning

confidence: 99%

Pipeline Reduction of Binary Light Curves from Large–Scale Surveys

Prša

Zwitter

2006

Proc. IAU

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Abstract.One of the most important changes in observational astronomy of the 21 st Century is a rapid shift from classical object-by-object observations to extensive automatic surveys. As CCD detectors are getting better and their prices are getting lower, more and more small and medium-size observatories are refocusing their attention to detection of stellar variability through systematic sky-scanning missions. This trend is aditionally powered by the success of pioneering surveys such as ASAS, DENIS, OGLE, TASS, their space counterpart Hipparcos and others. Such surveys produce massive amounts of data and it is not at all clear how these data are to be reduced and analysed. This is especially striking in the eclipsing binary (EB) field, where most frequently used tools are optimized for object-by-object analysis. A clear need for thorough, reliable and fully automated approaches to modeling and analysis of EB data is thus obvious. This task is very difficult because of limited data quality, non-uniform phase coverage and solution degeneracy. This paper reviews recent advancements in putting together semi-automatic and fully automatic pipelines for EB data processing. Automatic procedures have already been used to process Hipparcos data, LMC/SMC observations, OGLE and ASAS catalogs etc. We discuss the advantages and shortcomings of these procedures.

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The variable stars of the Large Magellanic Cloud

Cited by 43 publications

References 0 publications

Distribution and ages of Magellanic Cepheids

Distribution and ages of Magellanic Cepheids

The impact of large-scale, long-term optical surveys on pulsating star research

Pipeline Reduction of Binary Light Curves from Large–Scale Surveys

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