Ball, Warrick Heinz

[["dc.bibliographiccitation.artnumber","A25"],["dc.bibliographiccitation.journal","Astronomy & Astrophysics"],["dc.bibliographiccitation.volume","582"],["dc.contributor.author","Appourchaux, Thierry"],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Lebreton, Y."],["dc.contributor.author","Verma, K."],["dc.contributor.author","Vorontsov, S."],["dc.contributor.author","Campante, T. L."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Régulo, C."],["dc.contributor.author","Horch, E."],["dc.contributor.author","Howell, S. B."],["dc.contributor.author","Everett, M."],["dc.contributor.author","Ciardi, D."],["dc.contributor.author","Fossati, L."],["dc.contributor.author","Miglio, A."],["dc.contributor.author","Montalbán, J."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","García, R. A."],["dc.contributor.author","Gizon, Laurent"],["dc.date.accessioned","2017-09-07T11:48:37Z"],["dc.date.available","2017-09-07T11:48:37Z"],["dc.date.issued","2015"],["dc.description.abstract","Context. Solar-like oscillations have been observed by Kepler and CoRoT in many solar-type stars, thereby providing a way to probe stars using asteroseismology.Aims. The derivation of stellar parameters has usually been done with single stars. The aim of the paper is to derive the stellar parameters of a double-star system (HIP 93511), for which an interferometric orbit has been observed along with asteroseismic measurements.Methods. We used a time series of nearly two years of data for the double star to detect the two oscillation-mode envelopes that appear in the power spectrum. Using a new scaling relation based on luminosity, we derived the radius and mass of each star. We derived the age of each star using two proxies: one based upon the large frequency separation and a new one based upon the small frequency separation. Using stellar modelling, the mode frequencies allowed us to derive the radius, the mass, and the age of each component. In addition, speckle interferometry performed since 2006 has enabled us to recover the orbit of the system and the total mass of the system.Results. From the determination of the orbit, the total mass of the system is 2.34-0.33+0.45 M⊙. The total seismic mass using scaling relations is 2.47 ± 0.07 M⊙. The seismic age derived using the new proxy based upon the small frequency separation is 3.5 ± 0.3 Gyr. Based on stellar modelling, the mean common age of the system is 2.7–3.9 Gyr. The mean total seismic mass of the system is 2.34–2.53 M⊙  consistent with what we determined independently with the orbit. The stellar models provide the mean radius, mass, and age of the stars as RA = 1.82−1.87R⊙, MA = 1.25−1.39 M⊙, AgeA = 2.6–3.5 Gyr; RB = 1.22−1.25 R⊙, MB = 1.08−1.14 M⊙, AgeB = 3.35–4.21 Gyr. The models provide two sets of values for Star A: [1.25–1.27] M⊙ and [1.34–1.39] M⊙. We detect a convective core in Star A, while Star B does not have any. For the metallicity of the binary system of Z ≈ 0.02, we set the limit between stars having a convective core in the range [1.14–1.25] M⊙."],["dc.identifier.doi","10.1051/0004-6361/201526610"],["dc.identifier.gro","3146954"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/12450"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4724"],["dc.language.iso","en"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","public"],["dc.notes.submitter","chake"],["dc.relation.issn","0004-6361"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","A seismic and gravitationally bound double star observed by Kepler"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","no"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A82"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","601"],["dc.contributor.author","White, Timothy R."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Aguirre, Victor Silva"],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Bedding, Timothy R."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Christensen-Dalsgaard, Joergen"],["dc.contributor.author","Garcia, R. A."],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Stello, Dennis"],["dc.contributor.author","Aigrain, S."],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Appourchaux, T."],["dc.contributor.author","Bazot, M."],["dc.contributor.author","Campante, Tiago L."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Elsworth, Yvonne P."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Handberg, Rasmus"],["dc.contributor.author","Hekker, Saskia"],["dc.contributor.author","Houdek, Gunter"],["dc.contributor.author","Howe, R."],["dc.contributor.author","Huber, D."],["dc.contributor.author","Karoff, Christoffer"],["dc.contributor.author","Marques, J. P."],["dc.contributor.author","Mathur, S."],["dc.contributor.author","McQuillan, A."],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Nielsen, M. B."],["dc.contributor.author","Regulo, C."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Stahn, Thorsten"],["dc.date.accessioned","2018-11-07T10:24:05Z"],["dc.date.available","2018-11-07T10:24:05Z"],["dc.date.issued","2017"],["dc.description.abstract","Binary star systems are important for understanding stellar structure and evolution, and are especially useful when oscillations can be detected and analysed with asteroseismology. However, only four systems are known in which solar-like oscillations are detected in both components. Here, we analyse the fifth such system, HD 176465, which was observed by Kepler. We carefully analysed the system's power spectrum to measure individual mode frequencies, adapting our methods where necessary to accommodate the fact that both stars oscillate in a similar frequency range. We also modelled the two stars independently by fitting stellar models to the frequencies and complementary parameters. We are able to cleanly separate the oscillation modes in both systems. The stellar models produce compatible ages and initial compositions for the stars, as is expected from their common and contemporaneous origin. Combining the individual ages, the system is about 3.0 +/- 0.5 Gyr old. The two components of HD 176465 are young physically-similar oscillating solar analogues, the first such system to be found, and provide important constraints for stellar evolution and asteroseismology."],["dc.identifier.doi","10.1051/0004-6361/201628706"],["dc.identifier.isi","000402313500082"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/15004"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/42591"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Edp Sciences S A"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/338251/EU//STELLARAGES"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","Kepler observations of the asteroseismic binary HD 176465"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","A14"],["dc.bibliographiccitation.journal","Astronomy and Astrophysics"],["dc.bibliographiccitation.volume","592"],["dc.contributor.author","Reese, Daniel R."],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Miglio, Andrea"],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Basu, S."],["dc.contributor.author","Buldgen, G."],["dc.contributor.author","Christensen-Dalsgaard, Joergen"],["dc.contributor.author","Coelho, Hugo R."],["dc.contributor.author","Hekker, Saskia"],["dc.contributor.author","Houdek, Gunter"],["dc.contributor.author","Lebreton, Yveline"],["dc.contributor.author","Mazumdar, Anupam"],["dc.contributor.author","Metcalfe, T. S."],["dc.contributor.author","Aguirre, Victor Silva"],["dc.contributor.author","Stello, Dennis"],["dc.contributor.author","Verma, Kuldeep"],["dc.date.accessioned","2018-11-07T10:10:38Z"],["dc.date.available","2018-11-07T10:10:38Z"],["dc.date.issued","2016"],["dc.description.abstract","Context. Detailed oscillation spectra comprising individual frequencies for numerous solar-type stars and red giants are either currently available, e.g. courtesy of the CoRoT, Kepler, and K2 missions, or will become available with the upcoming NASA TESS and ESA PLATO 2.0 missions. The data can lead to a precise characterisation of these stars thereby improving our understanding of stellar evolution, exoplanetary systems, and the history of our galaxy. Aims. Our goal is to test and compare different methods for obtaining stellar properties from oscillation frequencies and spectroscopic constraints. Specifically, we would like to evaluate the accuracy of the results and reliability of the associated error bars, and to see where there is room for improvement. Methods. In the context of the SpaceInn network, we carried out a hare-and-hounds exercise in which one group, the hares, simulated observations of oscillation spectra for a set of ten artificial solar-type stars, and a number of hounds applied various methods for characterising these stars based on the data produced by the hares. Most of the hounds fell into two main groups. The first group used forward modelling (i.e. applied various search/optimisation algorithms in a stellar parameter space) whereas the second group relied on acoustic glitch signatures. Results. Results based on the forward modelling approach were accurate to 1:5% (radius), 3.9% (mass), 23% (age), 1.5% (surface gravity), and 1.8% (mean density), as based on the root mean square difference. Individual hounds reached different degrees of accuracy, some of which were substantially better than the above average values. For the two 1 M-circle dot stellar targets, the accuracy on the age is better than 10% thereby satisfying the requirements for the PLATO 2.0 mission. High stellar masses and atomic diffusion (which in our models does not include the effects of radiative accelerations) proved to be sources of difficulty. The average accuracies for the acoustic radii of the base of the convection zone, the He II ionisation, and the Gamma(1) peak located between the two He ionisation zones were 17%, 2.4%, and 1.9%, respectively. The results from the forward modelling were on average more accurate than those from the glitch fitting analysis as the latter seemed to be affected by aliasing problems for some of the targets. Conclusions. Our study indicates that forward modelling is the most accurate way of interpreting the pulsation spectra of solar-type stars. However, given its model-dependent nature, this method needs to be complemented by model-independent results from, e.g. glitch analysis. Furthermore, our results indicate that global rather than local optimisation algorithms should be used in order to obtain robust error bars."],["dc.identifier.doi","10.1051/0004-6361/201527987"],["dc.identifier.isi","000384722600072"],["dc.identifier.purl","https://resolver.sub.uni-goettingen.de/purl?gs-1/14281"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/39895"],["dc.notes.intern","Merged from goescholar"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","Najko"],["dc.publisher","Edp Sciences S A"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/312844/EU/Exploitation of Space Data for Innovative Helio- and Asteroseismology/SPACEINN"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/267864/EU/ASTERoseismic Investigations with SONG and Kepler/ASTERISK"],["dc.relation","info:eu-repo/grantAgreement/EC/FP7/338251/EU/Accurate ages of stars/StellarAges"],["dc.relation.issn","1432-0746"],["dc.relation.orgunit","Fakultät für Physik"],["dc.title","SpaceInn hare-and-hounds exercise: Estimation of stellar properties using space-based asteroseismic data"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dc.type.version","published_version"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","173"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","835"],["dc.contributor.author","Aguirre, Victor Silva"],["dc.contributor.author","Lund, Mikkel N."],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Basu, Sarbani"],["dc.contributor.author","Christensen-Dalsgaard, Jorgen"],["dc.contributor.author","Lebreton, Yveline"],["dc.contributor.author","Reese, Daniel R."],["dc.contributor.author","Verma, Kuldeep"],["dc.contributor.author","Casagrande, Luca"],["dc.contributor.author","Justesen, Anders B."],["dc.contributor.author","Mosumgaard, Jakob R."],["dc.contributor.author","Chaplin, William J."],["dc.contributor.author","Bedding, Timothy R."],["dc.contributor.author","Davies, Guy R."],["dc.contributor.author","Handberg, Rasmus"],["dc.contributor.author","Houdek, Gunter"],["dc.contributor.author","Huber, Daniel"],["dc.contributor.author","Kjeldsen, Hans"],["dc.contributor.author","Latham, David W."],["dc.contributor.author","White, Timothy R."],["dc.contributor.author","Coelho, Hugo R."],["dc.contributor.author","Miglio, Andrea"],["dc.contributor.author","Rendle, Ben"],["dc.date.accessioned","2018-11-07T10:27:36Z"],["dc.date.available","2018-11-07T10:27:36Z"],["dc.date.issued","2017"],["dc.description.abstract","We use asteroseismic data from the Kepler satellite to determine fundamental stellar properties of the 66 main-sequence targets observed for at least one full year by the mission. We distributed tens of individual oscillation frequencies extracted from the time series of each star among seven modeling teams who applied different methods to determine radii, masses, and ages for all stars in the sample. Comparisons among the different results reveal a good level of agreement in all stellar properties, which is remarkable considering the variety of codes, input physics, and analysis methods employed by the different teams. Average uncertainties are of the order of similar to 2% in radius, similar to 4% in mass, and similar to 10% in age, making this the best-characterized sample of main-sequence stars available to date. Our predicted initial abundances and mixing-length parameters are checked against inferences from chemical enrichment laws Delta Y/Delta Zand predictions from 3D atmospheric simulations. We test the accuracy of the determined stellar properties by comparing them to the Sun, angular diameter measurements, Gaia parallaxes, and binary evolution, finding excellent agreement in all cases and further confirming the robustness of asteroseismically determined physical parameters of stars when individual frequencies of oscillation are available. Baptised as the Kepler dwarfs LEGACY sample, these stars are the solar-like oscillators with the best asteroseismic properties available for at least another decade. All data used in this analysis and the resulting stellar parameters are made publicly available for the community."],["dc.identifier.doi","10.3847/1538-4357/835/2/173"],["dc.identifier.isi","000401145500002"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43266"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.issn","1538-4357"],["dc.relation.issn","0004-637X"],["dc.title","Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. II. Radii, Masses, and Ages"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.artnumber","172"],["dc.bibliographiccitation.issue","2"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","835"],["dc.contributor.author","Lund, Mikkel N."],["dc.contributor.author","Aguirre, Victor Silva"],["dc.contributor.author","Davies, Guy R."],["dc.contributor.author","Chaplin, William J."],["dc.contributor.author","Christensen-Dalsgaard, Jorgen"],["dc.contributor.author","Houdek, Gunter"],["dc.contributor.author","White, Timothy R."],["dc.contributor.author","Bedding, Timothy R."],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Huber, Daniel"],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Lebreton, Yveline"],["dc.contributor.author","Latham, David W."],["dc.contributor.author","Handberg, Rasmus"],["dc.contributor.author","Verma, Kuldeep"],["dc.contributor.author","Basu, Sarbani"],["dc.contributor.author","Casagrande, Luca"],["dc.contributor.author","Justesen, Anders B."],["dc.contributor.author","Kjeldsen, Hans"],["dc.contributor.author","Mosumgaard, Jakob R."],["dc.date.accessioned","2018-11-07T10:27:37Z"],["dc.date.available","2018-11-07T10:27:37Z"],["dc.date.issued","2017"],["dc.description.abstract","The advent of space-based missions like Kepler has revolutionized the study of solar-type stars, particularly through the measurement and modeling of their resonant modes of oscillation. Here we analyze a sample of 66 Kepler main-sequence stars showing solar-like oscillations as part of the Kepler seismic LEGACY project. We use Kepler short-cadence data, of which each star has at least 12 months, to create frequency-power spectra optimized for asteroseismology. For each star, we identify its modes of oscillation and extract parameters such as frequency, amplitude, and line width using a Bayesian Markov chain Monte Carlo \"peak-bagging\" approach. We report the extracted mode parameters for all 66 stars, as well as derived quantities such as frequency difference ratios, the large and small separations Delta v and delta v(02); the behavior of line widths with frequency and line widths at v(max) with T-eff, for which we derive parametrizations; and behavior of mode visibilities. These average properties can be applied in future peak-bagging exercises to better constrain the parameters of the stellar oscillation spectra. The frequencies and frequency ratios can tightly constrain the fundamental parameters of these solar-type stars, and mode line widths and amplitudes can test models of mode damping and excitation."],["dc.identifier.doi","10.3847/1538-4357/835/2/172"],["dc.identifier.isi","000401145500001"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/43267"],["dc.notes.status","zu prüfen"],["dc.notes.submitter","PUB_WoS_Import"],["dc.publisher","Iop Publishing Ltd"],["dc.relation.haserratum","/handle/2/78805"],["dc.relation.issn","1538-4357"],["dc.relation.issn","0004-637X"],["dc.title","Standing on the Shoulders of Dwarfs: the Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.peerReviewed","yes"],["dc.type.status","published"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","1038"],["dc.bibliographiccitation.issue","956"],["dc.bibliographiccitation.journal","Publications of the Astronomical Society of the Pacific"],["dc.bibliographiccitation.lastpage","1044"],["dc.bibliographiccitation.volume","127"],["dc.contributor.author","Chaplin, W. J."],["dc.contributor.author","Lund, M. N."],["dc.contributor.author","Handberg, R."],["dc.contributor.author","Basu, S."],["dc.contributor.author","Buchhave, L. A."],["dc.contributor.author","Campante, T. L."],["dc.contributor.author","Davies, G. R."],["dc.contributor.author","Huber, D."],["dc.contributor.author","Latham, D. W."],["dc.contributor.author","Latham, C. A."],["dc.contributor.author","Serenelli, A."],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Appourchaux, Thierry"],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Benomar, O."],["dc.contributor.author","Casagrande, L."],["dc.contributor.author","Christensen-Dalsgaard, J."],["dc.contributor.author","Coelho, H. R."],["dc.contributor.author","Creevey, O. L."],["dc.contributor.author","Elsworth, Y."],["dc.contributor.author","García, R. A."],["dc.contributor.author","Gaulme, P."],["dc.contributor.author","Hekker, S."],["dc.contributor.author","Kallinger, T."],["dc.contributor.author","Karoff, C."],["dc.contributor.author","Kawaler, S. D."],["dc.contributor.author","Kjeldsen, H."],["dc.contributor.author","Lundkvist, M. S."],["dc.contributor.author","Marcadon, F."],["dc.contributor.author","Mathur, Saurabh"],["dc.contributor.author","Miglio, A."],["dc.contributor.author","Mosser, B."],["dc.contributor.author","Régulo, C."],["dc.contributor.author","Roxburgh, I. W."],["dc.contributor.author","Silva Aguirre, V."],["dc.contributor.author","Stello, D."],["dc.contributor.author","Verma, K."],["dc.contributor.author","White, T. R."],["dc.contributor.author","Bedding, T. R."],["dc.contributor.author","Barclay, T."],["dc.contributor.author","Buzasi, D. L."],["dc.contributor.author","Dehuevels, S."],["dc.contributor.author","Gizon, Laurent"],["dc.contributor.author","Houdek, G."],["dc.contributor.author","Howell, S. B."],["dc.contributor.author","Salabert, D."],["dc.contributor.author","Soderblom, D. R."],["dc.date.accessioned","2017-09-07T11:49:45Z"],["dc.date.available","2017-09-07T11:49:45Z"],["dc.date.issued","2015"],["dc.description.abstract","We present the first detections by the NASA K2 mission of oscillations in solar-type stars, using short-cadence data collected during K2 Campaign 1 (C1). We understand the asteroseismic detection thresholds for C1-like levels of photometric performance, and we can detect oscillations in subgiants having dominant oscillation frequencies around 1000 μHz. Changes to the operation of the fine-guidance sensors are expected to give significant improvements in the high-frequency performance from C3 onwards. A reduction in the excess high-frequency noise by a factor of 2.5 in amplitude would bring main-sequence stars with dominant oscillation frequencies as high as sime2500 μHz into play as potential asteroseismic targets for K2."],["dc.identifier.doi","10.1086/683103"],["dc.identifier.gro","3147413"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/4998"],["dc.language.iso","en"],["dc.notes.status","public"],["dc.notes.submitter","chake"],["dc.relation.issn","0004-6280"],["dc.title","Asteroseismology of Solar-Type Stars with K2: Detection of Oscillations in C1 Data"],["dc.type","journal_article"],["dc.type.internalPublication","unknown"],["dc.type.peerReviewed","no"],["dspace.entity.type","Publication"]]

[["dc.bibliographiccitation.firstpage","110"],["dc.bibliographiccitation.issue","1"],["dc.bibliographiccitation.journal","The Astrophysical Journal"],["dc.bibliographiccitation.volume","850"],["dc.contributor.author","Lund, Mikkel N."],["dc.contributor.author","Silva Aguirre, Víctor"],["dc.contributor.author","Davies, Guy R."],["dc.contributor.author","Chaplin, William J."],["dc.contributor.author","Christensen-Dalsgaard, Jørgen"],["dc.contributor.author","Houdek, Günter"],["dc.contributor.author","White, Timothy R."],["dc.contributor.author","Bedding, Timothy R."],["dc.contributor.author","Ball, Warrick H."],["dc.contributor.author","Huber, Daniel"],["dc.contributor.author","Antia, H. M."],["dc.contributor.author","Lebreton, Yveline"],["dc.contributor.author","Latham, David W."],["dc.contributor.author","Handberg, Rasmus"],["dc.contributor.author","Verma, Kuldeep"],["dc.contributor.author","Basu, Sarbani"],["dc.contributor.author","Casagrande, Luca"],["dc.contributor.author","Justesen, Anders B."],["dc.contributor.author","Kjeldsen, Hans"],["dc.contributor.author","Mosumgaard, Jakob R."],["dc.date.accessioned","2020-12-10T18:47:34Z"],["dc.date.available","2020-12-10T18:47:34Z"],["dc.date.issued","2017"],["dc.identifier.doi","10.3847/1538-4357/aa9658"],["dc.identifier.eissn","1538-4357"],["dc.identifier.uri","https://resolver.sub.uni-goettingen.de/purl?gro-2/78805"],["dc.notes.intern","DOI Import GROB-354"],["dc.relation.iserratumof","/handle/2/43267"],["dc.title","Erratum: “Standing on the Shoulders of Dwarfs: The Kepler Asteroseismic LEGACY Sample. I. Oscillation Mode Parameters” (2017, ApJ, 835, 172)"],["dc.type","journal_article"],["dc.type.internalPublication","yes"],["dc.type.subtype","erratum_ja"],["dspace.entity.type","Publication"]]