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Pinsonneault, Marc H.,Elsworth, Yvonne,Epstein, Courtney,Hekker, Saskia,Mé,szá,ros, Sz.,Chaplin, William J.,Johnson, Jennifer A.,Garcí,a, Rafael A.,Holtzman, Jon,Mathur, Savita,Garc& IOP Publishing 2014 The Astrophysical journal Supplement series Vol.215 No.2
<P>We present the first APOKASC catalog of spectroscopic and asteroseismic properties of 1916 red giants observed in the Kepler fields. The spectroscopic parameters provided from the Apache Point Observatory Galactic Evolution Experiment project are complemented with asteroseismic surface gravities, masses, radii, and mean densities determined by members of the Kepler Asteroseismology Science Consortium. We assess both random and systematic sources of error and include a discussion of sample selection for giants in the Kepler fields. Total uncertainties in the main catalog properties are of the order of 80 K in Teff, 0.06 dex in [M/ H], 0.014 dex in log g, and 12% and 5% in mass and radius, respectively; these reflect a combination of systematic and random errors. Asteroseismic surface gravities are substantially more precise and accurate than spectroscopic ones, and we find good agreement between their mean values and the calibrated spectroscopic surface gravities. There are, however, systematic underlying trends with Teff and log g. Our effective temperature scale is between 0 and 200 K cooler than that expected from the infrared flux method, depending on the adopted extinction map, which provides evidence for a lower value on average than that inferred for the Kepler Input Catalog (KIC). We find a reasonable correspondence between the photometric KIC and spectroscopic APOKASC metallicity scales, with increased dispersion in KIC metallicities as the absolute metal abundance decreases, and offsets in T-eff and log g consistent with those derived in the literature. We present mean fitting relations between APOKASC and KIC observables and discuss future prospects, strengths, and limitations of the catalog data.</P>
Hyelim Oh,Animesh Animesh,Alain Pinsonneault 한국경영정보학회 2019 한국경영정보학회 학술대회논문집 Vol.2019 No.11
This paper examines how the wisdom of crowds can be leveraged in crowdsourced ideation-based product innovation where individual consumers co-create value together with firms. Specifically, we examine how the distribution of contribution equality (DCI) mediates the effect of interdependence on ideation project success. To address the research question we collected data from Quirky platform, which leverages the crowd in the ideation phase of new product development. The analysis of Quirky’s product co-development project affiliation networks (i.e., a two-mode network constructed from inventor and co-inventor collaborations) shows that the mechanism through which interdependence affects the outcome and find that (long-tail) distributional pattern of contribution inequality mediates the relationship between interdependence and crowdsourcing performance, such that higher is DCI, lower is project success. This study provides practical implications for crowdsourcing platform designers by demonstrating the importance of guiding and managing project team composition in crowdsourced ideation projects.
An, Deokkeun,Terndrup, Donald M.,Pinsonneault, Marc H.,Lee, Jae-Woo IOP Publishing 2015 The Astrophysical journal Vol.811 No.1
<P>We extend our effort to calibrate stellar isochrones in the Johnson-Cousins (BVIC) and the 2MASS (JHK(s)) filter systems based on observations of well-studied open clusters. Using cool main-sequence (MS) stars in Praesepe, we define empirical corrections to the Lejeune et al. color-effective temperature (T-eff) relations down to T-eff similar to 3600 K, complementing our previous work based on the Hyades and the Pleiades. We apply empirically corrected isochrones to existing optical and near-infrared photometry of cool (T-eff less than or similar to 5500 K) and metal-rich ([Fe/H] = +0.37) MS stars in NGC 6791. The current methodology relies on an assumption that color-T-eff corrections are independent of metallicity, but we find that estimates of color excess and distance from color-magnitude diagrams with different color indices converge on each other at the precisely known metallicity of the cluster. Along with a satisfactory agreement with eclipsing binary data in the cluster, we view the improved internal consistency as a validation of our calibrated isochrones at super-solar metallicities. For very cool stars (T-eff less than or similar to 4800 K), however, we find that B - V colors of our models are systematically redder than the cluster photometry by similar to 0.02 mag. We use color-T-eff transformations from the infrared flux method and alternative photometry to examine a potential color-scale error in the input cluster photometry. After excluding B - V photometry of these cool MS stars, we derive E(B - V) = 0.105 +/- 0.014, [M/H] = +0.42 +/- 0.07, (m - M)(0) = 13.04 +/- 0.08, and the age of 9.5 +/- 0.3 Gyr for NGC 6791.</P>
VALUE CO-CREATION AND WEALTH SPILLOVER IN OPEN INNOVATION ALLIANCES
Kunsoo Han,Wonseok Oh,Kun Shin Im,Ray Chang,Hyelim Oh,Alain Pinsonneault 한국경영정보학회 2010 한국경영정보학회 학술대회논문집 Vol.2010 No.1
Based on an event study approach, we investigate the economic and strategic value of open innovation alliances (OIAs), in which collaborators and competitors join together in the pursuit of the co-development of technological innovations. Unlike previous event studies in the IS field, this study not only assesses the wealth impact on the OIA-participating focal firm but also on the firm’s rivals. To gain additional insights into the factors that moderate the market valuation of OIA participation, several contextual factors, including the degree of partner heterogeneity, innovation type, and the degree of openness of the OIAs are used to account for variability in abnormal returns. We found that allying firms realize significant positive abnormal returns when their entry into an OIA is made public. The results also suggest that substantial excessive returns accrued to the allying firms with the belated entry of a large, established firm. A firm’s entry into an OIA increases, rather than decreases, the market valuation of its rival. Innovation type and openness were significantly associated with the amount of abnormal returns accruing to allying firms, while no significance was found for partner heterogeneity.
THE STELLAR METALLICITY DISTRIBUTION FUNCTION OF THE GALACTIC HALO FROM SDSS PHOTOMETRY
An, Deokkeun,Beers, Timothy C.,Johnson, Jennifer A.,Pinsonneault, Marc H.,Lee, Young Sun,Bovy, Jo,Ivezić,, Ž,eljko,Carollo, Daniela,Newby, Matthew IOP Publishing 2013 The Astrophysical journal Vol.763 No.1
<P>We explore the stellar metallicity distribution function of the Galactic halo based on SDSS ugriz photometry. A set of stellar isochrones is calibrated using observations of several star clusters and validated by comparisons with medium-resolution spectroscopic values over a wide range of metal abundance. We estimate distances and metallicities for individual main-sequence stars in the multiply scanned SDSS Stripe 82, at heliocentric distances in the range 5-8 kpc and |b| > 35 degrees, and find that the in situ photometric metallicity distribution has a shape that matches that of the kinematically selected local halo stars from Ryan & Norris. We also examine independent kinematic information from proper-motion measurements for high Galactic latitude stars in our sample. We find that stars with retrograde rotation in the rest frame of the Galaxy are generally more metal poor than those exhibiting prograde rotation, which is consistent with earlier arguments by Carollo et al. that the halo system comprises at least two spatially overlapping components with differing metallicity, kinematics, and spatial distributions. The observed photometric metallicity distribution and that of Ryan & Norris can be described by a simple chemical evolution model by Hartwick (or by a single Gaussian distribution); however, the suggestive metallicity-kinematic correlation contradicts the basic assumption in this model that the Milky Way halo consists primarily of a single stellar population. When the observed metallicity distribution is deconvolved using two Gaussian components with peaks at [Fe/H] approximate to -1.7 and -2.3, the metal-poor component accounts for approximate to 20%-35% of the entire halo population in this distance range.</P>
MOA-2010-BLG-523: “FAILED PLANET” = RS CVn STAR
Gould, A.,Yee, J. C.,Bond, I. A.,Udalski, A.,Han, C.,Jørgensen, U. G.,Greenhill, J.,Tsapras, Y.,Pinsonneault, M. H.,Bensby, T.,Allen, W.,Almeida, L. A.,Bos, M.,Christie, G. W.,DePoy, D. L.,Dong, Subo IOP Publishing 2013 The Astrophysical journal Vol.763 No.2
<P>The Galactic bulge source MOA-2010-BLG-523S exhibited short-term deviations from a standard microlensing light curve near the peak of an A(max) similar to 265 high-magnification microlensing event. The deviations originally seemed consistent with expectations for a planetary companion to the principal lens. We combine long-term photometric monitoring with a previously published high-resolution spectrum taken near peak to demonstrate that this is an RS CVn variable, so that planetary microlensing is not required to explain the light-curve deviations. This is the first spectroscopically confirmed RS CVn star discovered in the Galactic bulge.</P>