Period—colour and amplitude-colour relations for MACHO project Large Magellanic Cloud RR Lyrae stars

Kanbur, S. M.; Fernando, I.

doi:10.1111/j.1745-3933.2005.00025.x

Cited by 12 publications

(21 citation statements)

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“…In summary, our study reveals that the structural form of PC and AC relations at maximum and minimum lights for RR Lyraes are much more complicated than previously thought (Kanbur & Fernando 2005;Bhardwaj et al 2014). They can be expressed as either a flat, a linear, or a quadratic relation in different colors.…”

Section: Discussionmentioning

confidence: 60%

“…The observed PC relations were also compared to the synthetic colors in Figure 5. 3.1. The PC Relations at Maximum Light Kanbur & Fernando (2005) and Bhardwaj et al (2014) found a significant non-zero and positive slope for the PC relation at maximum light in the (V − R) MACHO and (V − I) colors, respectively. In the left panel of Figure 3 we plotted the PC relations at maximum light for RRab and RRc stars: these display a variety of behavior.…”

Section: Methodsmentioning

confidence: 95%

“…In the case of Cepheids, the PC and AC relations have been extensively studied in a series of papers ; Kanbur & Ngeow 2006;Kanbur et al 2007Kanbur et al , 2010, as well as in Bhardwaj et al (2014). For RR Lyraes, Kanbur & Fernando (2005) investigated the PC and AC relations based on 4829 RR Lyraes in Large Magellanic Cloud obtained from the MACHO project, and found that the PC and AC relations at minimum light have a slope close to zero for this set of RR Lyraes. A similar result was also found with the fundamental mode RR Lyraes in the Large and Small Magellanic Cloud using the Optical Gravitational Lensing Experiment III (OGLE-III) data (Bhardwaj et al 2014).…”

Section: Introductionmentioning

confidence: 99%

“…Kanbur & Fernando (2005) and Bhardwaj et al (2014) studied the PC and AC relations based on the (V − R) MACHO color and the (V −I) color respectively. In contrast, the SDSS data enables our investigation of PC and AC relations in multicolors.…”

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confidence: 99%

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Period–color and Amplitude–color Relations at Maximum and Minimum Light for Rr Lyrae Stars in The sdss Stripe 82 Region

Ngeow

Bhardwaj

Schrecengost

et al. 2017

ApJ

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Investigation of period-color (PC) and amplitude-color (AC) relations at the maximum and minimum light can be used to probe the interaction of the hydrogen ionization front (HIF) with photosphere and the radiation hydrodynamics of the outer envelopes of Cepheids and RR Lyraes. For example, theoretical calculations indicated that such interactions would occur at minimum light for RR Lyrae and result in a flatter PC relation. In the past, the PC and AC relations have been investigated by using either the (V − R) MACHO or (V − I) colors. In this work, we extend previous work to other bands by analyzing the RR Lyraes in the Sloan Digital Sky Survey Stripe 82 Region. Multi-epoch data is available for RR Lyraes located within the footprint of the Stripe 82 Region in five (ugriz) bands. We present the PC and AC relations at maximum and minimum light in four colors: (u − g) 0 , (g − r) 0 , (r − i) 0 and (i − z) 0 , after they are corrected for extinction. We found that the PC and AC relations for this sample of RR Lyraes show a complex nature in the form of flat, linear or quadratic relations. Furthermore, the PC relations at minimum light for fundamental mode RR Lyrae stars are separated according to the Oosterhoff type, especially in the (g − r) 0 and (r − i) 0 colors. If only considering the results from linear regressions, our results are quantitatively consistent with the theory of HIF-photosphere interaction for both fundamental and first overtone RR Lyraes.

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Section: Discussionmentioning

confidence: 60%

Section: Methodsmentioning

confidence: 95%

Section: Introductionmentioning

confidence: 99%

mentioning

confidence: 99%

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Period–color and Amplitude–color Relations at Maximum and Minimum Light for Rr Lyrae Stars in The sdss Stripe 82 Region

Ngeow

Bhardwaj

Schrecengost

et al. 2017

ApJ

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“…Yet another explanation proposes that the Oosterhoff gap is based on the structure of the envelope in these pulsating stars. Kanbur & Fernando (2005) have suggested that understanding the physics behind the Oosterhoff Effect requires a detailed investigation of the interplay between the photosphere and the hydrogen ionization front in an RR Lyrae variable. Because these features are not co-moving in a pulsating atmosphere, their interaction with each other can affect the period-color relation of RR Lyraes, possibly accounting for the behavior of their mean periods as a function of metallicity and, therefore, helping to explain the Oosterhoff Effect.…”

Section: Rr Lyrae Starsmentioning

confidence: 99%

LSST Science Book, Version 2.0

Abell¹,

Burke²,

Hamuy³

et al. 2009

553

653

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Prepared by the LSST Science Collaborations, with contributions from the LSST Project. PrefaceMajor advances in our understanding of the Universe over the history of astronomy have often arisen from dramatic improvements in our ability to observe the sky to greater depth, in previously unexplored wavebands, with higher precision, or with improved spatial, spectral, or temporal resolution. Aided by rapid progress in information technology, current sky surveys are again changing the way we view and study the Universe, and the next-generation instruments, and the surveys that will be made with them, will maintain this revolutionary progress. Substantial progress in the important scientific problems of the next decade (determining the nature of dark energy and dark matter, studying the evolution of galaxies and the structure of our own Milky Way, opening up the time domain to discover faint variable objects, and mapping both the inner and outer Solar System) all require wide-field repeated deep imaging of the sky in optical bands.The wide-fast-deep science requirement leads to a single wide-field telescope and camera which can repeatedly survey the sky with deep short exposures. The Large Synoptic Survey Telescope (LSST), a dedicated telecope with an effective aperture of 6.7 meters and a field of view of 9.6 deg 2 , will make major contributions to all these scientific areas and more. It will carry out a survey of 20,000 deg 2 of the sky in six broad photometric bands, imaging each region of sky roughly 2000 times (1000 pairs of back-to-back 15-sec exposures) over a ten-year survey lifetime.The LSST project will deliver fully calibrated survey data to the United States scientific community and the public with no proprietary period. Near real-time alerts for transients will also be provided worldwide. A goal is worldwide participation in all data products. The survey will enable comprehensive exploration of the Solar System beyond the Kuiper Belt, new understanding of the structure of our Galaxy and that of the Local Group, and vast opportunities in cosmology and galaxy evolution using data for billions of distant galaxies. Since many of these science programs will involve the use of the world's largest non-proprietary database, a key goal is maximizing the usability of the data. Experience with previous surveys is that often their most exciting scientific results were unanticipated at the time that the survey was designed; we fully expect this to be the case for the LSST as well.The purpose of this Science Book is to examine and document in detail science goals, opportunities, and capabilities that will be provided by the LSST. The book addresses key questions that will be confronted by the LSST survey, and it poses new questions to be addressed by future study. It contains previously available material (including a number of White Papers submitted to the ASTRO2010 Decadal Survey) as well as new results from a year-long campaign of study and evaluation. This book does not attempt to be complete; there are many ...

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The Extinction Toward the Galactic Bulge From Rr Lyrae Stars

Kunder

Popowski

Cook

et al. 2008

The Astronomical Journal

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We present mean reddenings toward 3525 RR0 Lyrae stars from the Galactic bulge fields of the MACHO Survey. These reddenings are determined using the color at minimum V -band light of the RR0 Lyrae stars themselves and are found to be in general agreement with extinction estimates at the same location obtained from other methods. Using 3256 stars located in the Galactic Bulge, we derive the selective extinction coefficientThis value is what is expected for a standard extinction law with R V,BV = 3.1 ± 0.3.

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Period—colour and amplitude-colour relations for MACHO project Large Magellanic Cloud RR Lyrae stars

Cited by 12 publications

References 12 publications

Period–color and Amplitude–color Relations at Maximum and Minimum Light for Rr Lyrae Stars in The sdss Stripe 82 Region

Period–color and Amplitude–color Relations at Maximum and Minimum Light for Rr Lyrae Stars in The sdss Stripe 82 Region

LSST Science Book, Version 2.0

The Extinction Toward the Galactic Bulge From Rr Lyrae Stars

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