Spectroscopic and photometric study of Kepler asteroseismic targets

Molenda-Żakowicz, J.; Frasca, A.; Latham, David W.; Jerzykiewicz, M.

doi:10.1088/1742-6596/118/1/012065

Cited by 27 publications

(47 citation statements)

References 6 publications

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“…The spectroscopic investigation of the Kepler asteroseismic targets aims at deriving the atmospheric parameters of the stars and the value of the microturbulence in their atmospheres, as well as the projected rotational velocity and the radial velocity (see Molenda-Żakowicz et al 2007Molenda-Żakowicz et al , 2008Molenda-Żakowicz et al , 2010Catanzaro et al 2010;Frasca et al 2010. )…”

Section: Spectroscopymentioning

confidence: 99%

“…These data, when combined with 2MASS JHK magnitudes (Cutri et al 2003), can be used for computing the spectral energy distribution of the stars and deriving their atmospheric parameters. Additionally, photometric observations allow to measure the reddening of the stars and their absolute magnitude (see Molenda-Żakowicz, Jerzykiewicz & Frasca 2009;Frasca et al 2009;Kupka & Bruntt 2001. ) …”

Section: Photometrymentioning

confidence: 99%

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Asteroseismology of solar‐type stars with Kepler: III. Ground‐based data

Molenda‐Żakowicz¹,

Bruntt²,

Sousa³

et al. 2010

Astron Nachr

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We report on the ground-based follow-up program of spectroscopic and photometric observations of solar-like asteroseismic targets for the Kepler space mission. These stars constitute a large group of more than a thousand objects which are the subject of an intensive study by the Kepler Asteroseismic Science Consortium Working Group 1 (KASC WG-1). In the current work we will discuss the methods we use to determine the fundamental stellar atmospheric parameters using high-quality stellar spectra. These provide essential constraints for the asteroseismic modelling and make it possible to verify the parameters in the Kepler Input Catalogue (KIC).

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Section: Spectroscopymentioning

confidence: 99%

Section: Photometrymentioning

confidence: 99%

Asteroseismology of solar‐type stars with Kepler: III. Ground‐based data

Molenda‐Żakowicz¹,

Bruntt²,

Sousa³

et al. 2010

Astron Nachr

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“…These are available in the Kepler Input Catalog (KIC; Brown et al 2011). Unfortunately, KIC stellar parameters are not available for all of the stars of interest and the precision of T eff and g log in the KIC is generally too low for asteroseismic modeling, especially for hot and peculiar stars (Molenda-Żakowicz et al 2010b;McNamara et al 2012). Also, detailed information on the stellar chemical composition and rotation rate is lacking.…”

Section: Introductionmentioning

confidence: 99%

LAMOST OBSERVATIONS IN THE KEPLER FIELD. I. DATABASE OF LOW-RESOLUTION SPECTRA

Cat

Ren

et al. 2015

ApJS

135

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The nearly continuous light curves with micromagnitude precision provided by the space mission Kepler are revolutionizing our view of pulsating stars. They have revealed a vast sea of low-amplitude pulsation modes that were undetectable from Earth. The long time base of Kepler light curves allows for the accurate determination of the frequencies and amplitudes of pulsation modes needed for in-depth asteroseismic modeling. However, for an asteroseismic study to be successful, the first estimates of stellar parameters need to be known and they cannot be derived from the Kepler photometry itself. The Kepler Input Catalog provides values for the effective temperature, surface gravity, and metallicity, but not always with sufficient accuracy. Moreover, information on the chemical composition and rotation rate is lacking. We are collecting low-resolution spectra for objects in the Kepler field of view with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST, Xinglong observatory, China). All of the requested fields have now been observed at least once. In this paper, we describe those observations and provide a useful database for the whole astronomical community.

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“…Finally, dispersion corrections were applied to the science spectra observed nearest in time to each standard, based on the cubic polynomial and individual pixel shifts determined from the comparison lamp spectra. For KIC 5738698 we include one spectrum taken at Lowell Observatory in 2010 July for which we used the velocity standard HD 187691 (T eff = 6107 K, log g = 4.30, Cenarro et al 2007; V r = −0.15 ± 0.40 km s −1 , Molenda-Zakowicz et al 2007). …”

Section: Ground-based Spectroscopymentioning

confidence: 99%

Fundamental Parameters of Kepler Eclipsing Binaries. I. Kic 5738698

Matson

Gies

Guo

et al. 2016

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Eclipsing binaries serve as a valuable source of stellar masses and radii that inform stellar evolutionary models and provide insight into additional astrophysical processes. The exquisite light curves generated by space-based missions such as Kepler offer the most stringent tests to date. We use the Kepler light curve of the 4.8 day eclipsing binary KIC 5739896 with ground based optical spectra to derive fundamental parameters for the system. We reconstruct the component spectra to determine the individual atmospheric parameters, and model the Kepler photometry with the binary synthesis code ELC to obtain accurate masses and radii. The two components of KIC 5738698 are F-type stars with M 1 = 1.39 ± 0.04M , M 2 = 1.34 ± 0.06M , and R 1 = 1.84 ± 0.03R , R 2 = 1.72 ± 0.03R . We also report a small eccentricity (e 0.0017) and unusual albedo values that are required to match the detailed shape of the Kepler light curve. Comparison with evolutionary models indicate an approximate age of 2.3 Gyr for the system.

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Spectroscopic and photometric study of Kepler asteroseismic targets

Cited by 27 publications

References 6 publications

Asteroseismology of solar‐type stars with Kepler: III. Ground‐based data

Asteroseismology of solar‐type stars with Kepler: III. Ground‐based data

LAMOST OBSERVATIONS IN THE KEPLER FIELD. I. DATABASE OF LOW-RESOLUTION SPECTRA

Fundamental Parameters of Kepler Eclipsing Binaries. I. Kic 5738698

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