[Fe/H] derived from the light curves of RR Lyrae stars
in the Galactic halo

Wu, Chao; Qiu, Y.; Deng, J. S.; Hu, Jingyao; Zhao, Yi

doi:10.1051/0004-6361:20054343

Cited by 6 publications

(12 citation statements)

References 29 publications

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“…Besides the V -band light curves, Smolec (2005) gives the relation based on I-band light curves. Wu et al (2006) and De Lee (2008) derived a similar relation as in Jurcsik & Kovács (1996) for unfiltered, or white light, CCD observations, and for the g-band SDSS (Sloan Digitized Sky Survey) data, respectively. Watkins et al (2009), Sesar et al (2010), and Oluseyi et al (2012) further developed the metallicity-light curve relation in the SDSS photometric system with additional terms in the relation.…”

Section: Introductionsupporting

confidence: 52%

“…Among these RRab stars, 26 of them have [F e/H] values, listed in the forth column of Table 3, based on highresolution spectroscopic observations taken from the 3.6m Canada-France-Hawaii Telescope and the 10m Keck I Telescope (Nemec et al 2013). To derive the R P T Fband metallicity-light curve relation, we adopted the well established regression function as in Jurcsik & Kovács (1996) and Wu et al (2006)…”

Section: The Metallicity-light Curve Relationmentioning

confidence: 99%

“…Alternatively, Deb & Singh (2010) and Skowron et al (2016) derived the Fourier interrelations to convert the φ 31 parameters in I band to V band and then applied the metallicity-light curve relations mentioned. The validity of such a metallicity-light curve relation has been tested and verified, for example, in Jurcsik (2003), Gratton et al (2004), Kovács (2005), Wu et al (2006), and Kunder & Chaboyer (2008).…”

Section: Introductionmentioning

confidence: 98%

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The Palomar Transient Factory and Rr Lyrae: The Metallicity–light Curve Relation Based on Ab-Type Rr Lyrae in the Kepler Field

Ngeow

Bellm

et al. 2016

ApJS

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The wide-field synoptic sky surveys, known as the Palomar Transient Factory (PTF) and the intermediate Palomar Transient Factory (iPTF), will accumulate a large number of known and new RR Lyrae. These RR Lyrae are good tracers to study the substructure of the Galactic halo if their distance, metallicity, and galactocentric velocity can be measured. Candidates of halo RR Lyrae can be identified from their distance and metallicity before requesting spectroscopic observations for confirmation. This is because both quantities can be obtained via their photometric light curves, because the absolute V -band magnitude for RR Lyrae is correlated with metallicity, and the metallicity can be estimated using a metallicity-light curve relation. To fully utilize the PTF and iPTF light-curve data in related future work, it is necessary to derive the metallicity-light curve relation in the native PTF/iPTF R-band photometric system. In this work, we derived such a relation using the known ab-type RR Lyrae located in the Kepler field, and it is found to be [F e/H] P T F = −4.089 − 7.346P + 1.280φ 31 (where P is pulsational period and φ 31 is one of the Fourier parameters describing the shape of the light curve), with a dispersion of 0.118 dex. We tested our metallicity-light curve relation with new spectroscopic observations of a few RR Lyrae in the Kepler field, as well as several data sets available in the literature. Our tests demonstrated that the derived metallicity-light curve relation could be used to estimate metallicities for the majority of the RR Lyrae, which are in agreement with the published values.

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Section: Introductionsupporting

confidence: 52%

Section: The Metallicity-light Curve Relationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

See 1 more Smart Citation

The Palomar Transient Factory and Rr Lyrae: The Metallicity–light Curve Relation Based on Ab-Type Rr Lyrae in the Kepler Field

Ngeow

Bellm

et al. 2016

ApJS

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“…Most of these photometric nights are moonless or crescent nights, with steady and cloudless sky. For a better comparison of these observations obtained at different time, we divided the photometric nights and the corresponding results into three epochs: Epoch 1 (2004-2005), Epoch 2 (2006( -2007( ), and Epoch 3 (2011. Table 3 lists part of the Landolt's standard stars that were observed during Epoch 3.…”

Section: Photometric Calibrationsmentioning

confidence: 99%

The photometric system of the Tsinghua-NAOC 80-cm telescope at NAOC Xinglong Observatory

Huang¹,

Li²,

Wang³

et al. 2012

Res. Astron. Astrophys.

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Tsinghua-NAOC (National Astronomical Observatories of China) Telescope (hereafter, TNT) is an 80-cm Cassegrain reflecting telescope located at Xinglong Observatory of NAOC, with main scientific goals of monitoring various transients in the universe such as supernovae, gamma-ray bursts, novae, variable stars, and active galactic nuclei. We present in this paper a systematic test and analysis of the photometric performance of this telescope. Based on the calibration observations on twelve photometric nights, spanning the period from year 2004 to year 2012, we derived an accurate transformation relationship between the instrumental ubvri magnitudes and standard Johnson U BV and Cousins RI magnitudes. In particular, the color terms and the extinction coefficients of different passbands are well determined. With these data, we also obtained the limiting magnitudes and the photometric precision of TNT. It is worthwhile to point out that the sky background at Xinglong Observatory may become gradually worse over the period from year 2005 to year 2012 (e.g., ∼21.4 mag vs. ∼20.1 mag in the V band).

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“…U Lep is a class RRab variable. Previous light curve measurements using Hipparcos data determined a period for U Lep of 0.581236 days (Wu, Qiu, Deng, Hu, & Zhao, 2006) to 0.581479 days (Feast, Laney, Kinman, Van Leeuwen, & Whitelock, 2008). Klein et al (2011) used this period and the preliminary data release of the Wide-field Infrared Survey Explorer (WISE) to determine a distance of 976.8 pc to U Lep.…”

Section: Introductionmentioning

confidence: 98%

Observations of U Leporis

Pavey¹,

Smith²,

Wyss³

et al. 2021

ATOM

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U Leporis (U Lep) is a pulsating variable that demonstrates periodic variation in apparent magnitude consistent with RR Lyrae variable stars. Images were acquired by the 0.4 meter telescopes of the Las Cumbres Observatory Global Telescope network in the visible (B, V) and near infrared (i and z) over a two week period in October 2019 and analyzed using Astrosource. Light curves were constructed for each of the four bandpasses, yielding a mean period of 0.581±0.011 days. The middle apparent magnitudes determined for the B, V, i, and z filters were 10.75, 10.55, 10.30, and 10.35 respectively. Color excess E(B-V) was determined by two methods (1) minimizing variance in the calculated distances for the V, i, and z bands (0.065) and (2) galactic dust (0.029), with the second method preferred. Distances in parsecs to U Lep were determined for the V (968±38), i (932±33), and z (951±38) filters. The average distance of 950±21 compares favorably to that obtained by Klein (977±8 pc) and less so to Gaia DR2 (1076±36 pc).

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[Fe/H] derived from the light curves of RR Lyrae stars in the Galactic halo

Abstract: Context. The iron abundance of halo RR Lyrae stars can provide important information about the formation history of the Galactic halo. Aims. We determine the [Fe/H]

Cited by 6 publications

References 29 publications

The Palomar Transient Factory and Rr Lyrae: The Metallicity–light Curve Relation Based on Ab-Type Rr Lyrae in the Kepler Field

The Palomar Transient Factory and Rr Lyrae: The Metallicity–light Curve Relation Based on Ab-Type Rr Lyrae in the Kepler Field

The photometric system of the Tsinghua-NAOC 80-cm telescope at NAOC Xinglong Observatory

Observations of U Leporis

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