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To cope with discontinuous change, recent research advocates to implement ambidexterity in which firms pursue exploitative innovation and exploratory innovation simultaneously. While previous studies on the determinants of organizational ambidexterity focused primarily on the organizational characteristics and the behavior of top management teams, a growing body of research calls attention to the role of the paradoxical cognitive frame of top managers in managing organizational ambidexterity. This article examines whether CEO ambivalence—a paradoxical cognitive frame that accepts and accommodates the presence of both threats and opportunities of a strategic issue such as a crisis—drives or hinders organizational ambidexterity. Moreover, although both exploitation and exploration require the deployment of technological capability, whether technological capability inhibits or facilitates managerial cognition to adapt to environmental change remains a puzzle to be solved. Based on the theory of paradoxical cognitive frame, this article predicts that CEO ambivalence follows a U-shaped effect on organizational ambidexterity while technological capability amplifies the curvilinear effect. A longitudinal survey among 260 CEOs of Chinese firms provides empirical support to the hypotheses. The research findings contain rich theoretical and managerial implications.

Many businesses have joined governments and nonprofit organizations to serve the social needs under the tremendous pressure of Covid-19. We propose that businesses that expanded into the social domain during the Covid-19 crisis differ significantly from each other and vary extensively in value creation. We extend the motivation and ability framework to derive a typology of businesses under this situation and conceptualize value creation behaviors in both a free market and a monopolistic market with the governments as the buyer.

Context. Classical Cepheids are primary distance indicators and a crucial stepping stone in determining the present-day value of the Hubble constant H0 to the precision and accuracy required to constrain apparent deviations from the ΛCDM Concordance Cosmological Model. Aims. We measured the iron and oxygen abundances of a statistically significant sample of 89 Cepheids in the Large Magellanic Cloud (LMC), one of the anchors of the local distance scale, quadrupling the prior sample and including 68 of the 70 Cepheids used to constrain H0 by the SH0ES program. The goal is to constrain the extent to which the luminosity of Cepheids is influenced by their chemical composition, which is an important contributor to the uncertainty on the determination of the Hubble constant itself and a critical factor in the internal consistency of the distance ladder. Methods. We derived stellar parameters and chemical abundances from a self-consistent spectroscopic analysis based on equivalent width of absorption lines. Results. The iron distribution of Cepheids in the LMC can be very accurately described by a single Gaussian with a mean [Fe/H] = −0.409 ± 0.003 dex and σ = 0.076 ± 0.003 dex. We estimate a systematic uncertainty on the absolute mean values of 0.1 dex. The width of the distribution is fully compatible with the measurement error and supports the low dispersion of 0.069 mag seen in the near-infrared Hubble Space Telescope LMC period–luminosity relation. The uniformity of the abundance has the important consequence that the LMC Cepheids alone cannot provide any meaningful constraint on the dependence of the Cepheid period–luminosity relation on chemical composition at any wavelength. This revises a prior claim based on a small sample of 22 LMC Cepheids that there was little dependence (or uncertainty) between composition and near-infrared luminosity, a conclusion which would produce an apparent conflict between anchors of the distance ladder with different mean abundance. The chemical homogeneity of the LMC Cepheid population makes it an ideal environment in which to calibrate the metallicity dependence between the more metal-poor Small Magellanic Cloud and metal-rich Milky Way and NGC 4258.

The three rung distance ladder, which calibrates Type Ia supernovae through stellar distances linked to geometric measurements, provides the highest precision direct measurement of the Hubble constant. In light of the Hubble tension, it is important to test the individual components of the distance ladder. For this purpose, we report a measurement of the Hubble constant from 35 extragalactic Cepheid hosts measured by the SH0ES team, using their distances and redshifts at cz < 3300 km /s , instead of any, more distant Type Ia supernovae, to measure the Hubble flow. The Cepheid distances are calibrated geometrically in the Milky Way, NGC 4258, and the Large Magellanic Cloud. Peculiar velocities are a significant source of systematic uncertainty at z $\sim$ 0.01, and we present a formalism for both mitigating and quantifying their effects, making use of external reconstructions of the density and velocity fields in the nearby universe. We identify a significant source of uncertainty originating from different assumptions about the selection criteria of this sample, whether distance or redshift limited, as it was assembled over three decades. Modeling these assumptions yields central values ranging from H0 = 71.8 to 77.0 km/s/Mpc. Combining the four best fitting selection models yields H0 = 73.1 (+2.6/-2.3) km/s/Mpc as a fiducial result, at $2.6\sigma$ tension with Planck. While Type Ia supernovae are essential for a precise measurement of H0, unknown systematics in these supernovae are unlikely to be the source of the Hubble tension, Comment: 26 Pages, 11 Figures, Submitted to ApJ

NGC 4258 is one of the most important anchors for calibrating the Cepheid period--luminosity relations (PLRs) owing to its accurate distance measured from water maser motions. We expand on previous efforts and carry out a new Cepheid search in this system using the Hubble Space Telescope (HST). We discover and measure a sample of 669 Cepheids in four new and two archival NGC 4258 fields, doubling the number of known Cepheids in this galaxy and obtaining an absolute calibration of their optical PLRs. We determine a Wesenheit PLR of $-2.574(\pm0.034) -3.294(\pm0.042) \log P$, consistent with an independent Large Magellanic Cloud (LMC) calibration at the level of $0.032\pm0.044$~mag in its zeropoint, after accounting for a metallicity dependence of $-0.20\pm0.05$~mag\,dex$^{-1}$ (Riess et al. 2006). Our determination of the PLR slope also agrees with the LMC-based value within their uncertainties. We attempt to characterize the metallicity effect of Cepheid PLRs using only the NGC 4258 sample, but a relatively narrow span of abundances limits our sensitivity and yields a Wesenheit zero-point dependence of $-0.07 \pm 0.21$ mag\,dex$^{-1}$. The Cepheid measurements presented in this study have been used as part of the data to derive the Hubble constant in a companion paper by the SH0ES team., Accepted to ApJ. 13 pages, 8 figures

We present HST photometry of 17 Cepheids in open clusters and their mean parallaxes from Gaia EDR3. These parallaxes are more precise than those from individual Cepheids (G300 stars per cluster. Cluster parallaxes also have smaller systematic uncertainty because their stars lie in the range (G>13 mag) where the Gaia parallax calibration is most comprehensive. Cepheid photometry employed in the period--luminosity relation was measured using the same instrument(WFC3) and filters(F555W,F814W,F160W) as extragalactic Cepheids in SNIa hosts. We find no evidence of residual parallax offset in this magnitude range, zp=-3+/-4 muas, consistent with Lindegren:2021b and most studies. The Cepheid luminosity (P=10d, solar-metallicity) in the HST near-infrared, Wesenheit system derived from the cluster sample is M_{H,1}^W=-5.902+/-0.025 and -5.890+/-0.018 mag with or without simultaneous determination of a parallax offset, respectively. These results are similar to measurements from field Cepheids, confirming the accuracy of the Gaia parallaxes over a broad range of magnitudes. The SH0ES distance ladder calibrated solely from this sample gives H_0=72.8+/-1.3 and H_0=73.2+/-1.1 km/s/Mpc with or without offset marginalization; combined with all anchors we find H_0=73.01+/-0.99 and 73.15+/-0.97, respectively, a 5% or 7% reduction in the uncertainty and a 5.3 sigma Hubble Tension relative to Planck+LambdaCDM. It appears increasingly difficult to reconcile two of the best measured cosmic scales, parallaxes from Gaia and the angular size of the acoustic scale of the CMB, using the simplest form of LambdaCDM to join the two., 12 pages, submitted to ApJ, comments welcome

The tip of the red giant branch has been used to measure distances to 500 nearby galaxies with the Hubble Space Telescope (HST) which are available in the Color-Magnitude Diagrams and Tip of the Red Giant Branch (CMDs/TRGB) catalog on the Extragalactic Distance Database (EDD). Our established methods are employed to perform an independent reduction of the targets presented by the Carnegie-Chicago Hubble Program (CCHP) in the series of papers culminating in Freedman (2021). Our distinct methodology involves modeling the observed luminosity function of red giant branch and asymptotic giant branch stars, which differs from the edge-detection algorithms employed by the CCHP. We find excellent agreement between distances for 11 hosts with new imaging, all at D < 20 Mpc. However, we are unable to measure the TRGB for 4 of the 5 hosts that use archival data designed to measure distances with Cepheids, all at D > 23 Mpc. With two new HST observations taken in the halo of the megamaser host NGC 4258, the first with the same ACS F606W and F814W filters and the post-servicing electronics used for SN Ia hosts, we then calibrate our TRGB distance scale to the geometric megamaser distance. Using our TRGB distances, we find a value of the Hubble Constant of $H_{0}$ = 71.5 $\pm$ 1.8 km/s/Mpc when using either the Pantheon or Carnegie Supernova Project (CSP) samples of supernovae. In the future, the James Webb Space Telescope will extend measurements of the TRGB to additional hosts of SN Ia and surface brightness fluctuation measurements for separate paths to $H_{0}$., Accepted to ApJ

We present Period-Luminosity Relations (PLRs) for 55 Cepheids in M31 with periods ranging from 4 to 78 days observed with the Hubble Space Telescope (HST) using the same three-band photometric system recently used to calibrate their luminosities. Images were taken with the Wide Field Camera 3 in two optical filters (F555W and F814W) and one near-infrared filter (F160W) using the Drift And SHift (DASH) mode of operation to significantly reduce overheads and observe widely-separated Cepheids in a single orbit. We include additional F160W epochs for each Cepheid from the Panchromatic Hubble Andromeda Treasury (PHAT) and use light curves from the Panoramic Survey Telescope and Rapid Response System of the Andromeda galaxy (PAndromeda) project to determine mean magnitudes. Combined with a 1.28$\%$ absolute calibration of Cepheid PLRs in the Large Magellanic Cloud from Riess et al. (2019a) in the same three filters, we find a distance modulus to M31 of $\mu_0$ = 24.407 $\pm$ 0.032, corresponding to 761 $\pm$ 11 kpc and 1.49$\%$ uncertainty including all error sources, the most precise determination of its distance to date. We compare our results to past measurements using Cepheids and the Tip of the Red Giant Branch (TRGB). This study also provides the groundwork for turning M31 into a precision anchor galaxy in the cosmic distance ladder to measure the Hubble constant together with efforts to measure a fully geometric distance to M31., Comment: Accepted by ApJ, 19 pages, 5 figures, 6 tables

Differentiation strategy represents the shared belief about the market and provides the lens through which executives filter external information. Based on the relevant information peculiar to the strategy and resource configurations in the firm, executives develop opportunity or threat interpretations and take responsive actions. Using the two-wave survey data from 294 CEOs in China during the 2008 macro crisis, we find that the configuration of differentiation, financial slack, and technological capabilities affects corporate entrepreneurship through opportunity interpretations.

Recent analysis of family firm internationalization has shown that international performance can suffer when family owners or managers engage in an unwarranted, strict separation between two ‘generic categories’ of resources in their strategic decision-making. On the one hand, there are resources perceived as ‘being part of the family in the long run’, and therefore unique and worthy of nurturing. On the other hand, there are resources perceived as ‘with the family only for the short run’, and therefore having commodity-type status and being fungible. The concept of bifurcation bias describes this frequently observed, affect-based phenomenon of separating all resources utilized by the firm into two categories. Bifurcation bias has been argued to be particularly damaging in the context of internationalization, whereby accurate assessment and complex recombination of resources is critical. In this paper, we extend the analysis of bifurcation bias in family firms. We examine how the personal values of family firm owners and non-family members, as well as the dominant cultural values in the relevant, surrounding societies (both home and host), can influence the magnitude and dysfunctional effects of this phenomenon. Infusing values-based analysis into assessing how bifurcation bias plays out in family firms, can improve our understanding of family firm heterogeneity, has implications for empirical research, and may help invalidate some overgeneralized narratives in research on family-firm international behaviour.

This study explores whether firms strategically utilize symbolic and substantive CSR as means to repair reputational damage following a corporate controversy. Further, we shed light on market reaction towards firms’ engagement in symbolic and substantive CSR and how such reaction varies across countries when differing levels of trust are evident. Using a sample of 9117 firm-year observations in an international setting, we find that firms are more likely to engage in symbolic CSR than substantive CSR and the relationship between the level of controversy and the firm’s engagement in symbolic CSR is an inverted U. In addition, our two-way interaction analysis illustrates that the market positively views the symbolic CSR engagement following a corporate controversy, and this positive effect is only pronounced in countries with higher levels of mutual trust.

We report observations from the Hubble Space Telescope (HST) of Cepheid variables in the host galaxies of 42 Type Ia supernovae (SNe Ia) used to calibrate the Hubble constant (H 0). These include the complete sample of all suitable SNe Ia discovered in the last four decades at redshift z ≤ 0.01, collected and calibrated from ≥1000 HST orbits, more than doubling the sample whose size limits the precision of the direct determination of H 0. The Cepheids are calibrated geometrically from Gaia EDR3 parallaxes, masers in NGC 4258 (here tripling that sample of Cepheids), and detached eclipsing binaries in the Large Magellanic Cloud. All Cepheids in these anchors and SN Ia hosts were measured with the same instrument (WFC3) and filters (F555W, F814W, F160W) to negate zero-point errors. We present multiple verifications of Cepheid photometry and six tests of background determinations that show Cepheid measurements are accurate in the presence of crowded backgrounds. The SNe Ia in these hosts calibrate the magnitude–redshift relation from the revised Pantheon+ compilation, accounting here for covariance between all SN data and with host properties and SN surveys matched throughout to negate systematics. We decrease the uncertainty in the local determination of H 0 to 1 km s−1 Mpc−1 including systematics. We present results for a comprehensive set of nearly 70 analysis variants to explore the sensitivity of H 0 to selections of anchors, SN surveys, redshift ranges, the treatment of Cepheid dust, metallicity, form of the period–luminosity relation, SN color, peculiar-velocity corrections, sample bifurcations, and simultaneous measurement of the expansion history. Our baseline result from the Cepheid–SN Ia sample is H 0 = 73.04 ± 1.04 km s−1 Mpc−1, which includes systematic uncertainties and lies near the median of all analysis variants. We demonstrate consistency with measures from HST of the TRGB between SN Ia hosts and NGC 4258, and include them simultaneously to yield 72.53 ± 0.99 km s−1 Mpc−1. The inclusion of high-redshift SNe Ia yields H 0 = 73.30 ± 1.04 km s−1 Mpc−1 and q 0 = −0.51 ± 0.024. We find a 5σ difference with the prediction of H 0 from Planck cosmic microwave background observations under ΛCDM, with no indication that the discrepancy arises from measurement uncertainties or analysis variations considered to date. The source of this now long-standing discrepancy between direct and cosmological routes to determining H 0 remains unknown.

We derive a distance of $D = 16.6 \pm 0.3$~Mpc ($\mu=31.10\pm0.04$~mag) to the archetypal narrow-line Seyfert 1 galaxy NGC 4051 based on Cepheid Period--Luminosity relations and new Hubble Space Telescope multiband imaging. We identify 419 Cepheid candidates and estimate the distance at both optical and near-infrared wavelengths using subsamples of precisely-photometered variables (123 and 47 in the optical and near-infrared subsamples, respectively). We compare our independent photometric procedures and distance-estimation methods to those used by the SH0ES team and find agreement to 0.01~mag. The distance we obtain suggests an Eddington ratio $\dot{m} \approx 0.2$ for NGC 4051, typical of narrow-line Seyfert 1 galaxies, unlike the seemingly-odd value implied by previous distance estimates. We derive a peculiar velocity of $-490\pm34$~km~s$^{-1}$ for NGC 4051, consistent with the overall motion of the Ursa Major Cluster in which it resides. We also revisit the energetics of the NGC 4051 nucleus, including its outflow and mass accretion rates., Comment: 15 pages, 12 figures, 6 tables, accepted for publication in ApJ

A chief executive officer (CEO) acting as the firm's transformational leader is typically viewed as instrumental to corporate entrepreneurship in established firms, but how exactly does a higher level of corporate entrepreneurship come about, given a transformational CEO's actions? We suggest that organizational ambidexterity can function as a core mediating mechanism between transformational CEOs and the observed level of corporate entrepreneurship and that the effectiveness of this mediating process varies as a function of critical contingencies related to characteristics of the top management team (TMT), the environment and the organization's design. Our empirical evidence, based on a sample of 145 Chinese private sector firms, and using three primary sources of data (145 CEOs, 506 TMT members, and 1,981 middle managers), provides support for a moderated mediation process. We find that the mediating pathway from transformational leadership to corporate entrepreneurship through organizational ambidexterity is not significant when boundary conditions are ignored. However, when environmental dynamism, TMT collectivism, and structural differentiation are included as moderators, CEO transformational leadership does affect corporate entrepreneurship via the creation and effective functioning of organizational ambidexterity.

The Period--Luminosity relation (PLR) of Mira variable stars is an important tool to determine astronomical distances. The common approach of estimating the PLR is a two-step procedure that first estimates the Mira periods and then runs a linear regression of magnitude on log period. When the light curves are sparse and noisy, the accuracy of period estimation decreases and can suffer from aliasing effects. Some methods improve accuracy by incorporating complex model structures at the expense of significant computational costs. Another drawback of existing methods is that they only provide point estimation without proper estimation of uncertainty. To overcome these challenges, we develop a hierarchical Bayesian model that simultaneously models the quasi-periodic variations for a collection of Mira light curves while estimating their common PLR. By borrowing strengths through the PLR, our method automatically reduces the aliasing effect, improves the accuracy of period estimation, and is capable of characterizing the estimation uncertainty. We develop a scalable stochastic variational inference algorithm for computation that can effectively deal with the multimodal posterior of period. The effectiveness of the proposed method is demonstrated through simulations, and an application to observations of Miras in the Local Group galaxy M33. Without using ad-hoc period correction tricks, our method achieves a distance estimate of M33 that is consistent with published work. Our method also shows superior robustness to downsampling of the light curves.

The accuracy of the Hubble constant measured with extragalactic Cepheids depends on robust photometry and background estimation in the presence of stellar crowding. The conventional approach accounts for crowding by sampling backgrounds near Cepheids and assuming they match those at their positions. We show a direct consequence of crowding by unresolved sources at Cepheid sites is a reduction in the fractional amplitudes of their light curves. We use a simple analytical expression to infer crowding directly from the light curve amplitudes of >200 Cepheids in 3 SNe~Ia hosts and NGC 4258 as observed by HST -- the first near-infrared amplitudes measured beyond the Magellanic Clouds. Where local crowding is minimal, we find near-infrared amplitudes match Milky Way Cepheids at the same periods. At greater stellar densities we find that the empirically measured amplitudes match the values predicted (with no free parameters) from crowding assessed in the conventional way from local regions, confirming their accuracy for estimating the background at the Cepheid locations. Extragalactic Cepheid amplitudes would need to be ~20% smaller than measured to indicate additional, unrecognized crowding as a primary source of the present discrepancy in H_0. Rather we find the amplitude data constrains a systematic mis-estimate of Cepheid backgrounds to be 0.029 +/- 0.037 mag, more than 5x smaller than the size of the present ~0.2 mag tension in H_0. We conclude that systematic errors in Cepheid backgrounds do not provide a plausible resolution to the Hubble tension., submitted to ApJ, comments welcome, 25 pages, 7 figures

The zero point of the reddening toward the Large Magellanic Cloud (LMC) has been the subject of some dispute. Its uncertainty propagates as a systematic error for methods which measure the extragalactic distance scale through knowledge of the absolute extinction of LMC stars. In an effort to resolve this issue, we used three different methods to calibrate the most widely-used metric to predict LMC extinction, the intrinsic color of the red clump, $(V-I)_{RC,0}$, for the inner $\sim$3 degrees of that galaxy. The first approach was to empirically calibrate the color zeropoints of the BaSTI isochrones over a wide metallicity range of ${\Delta}\rm{[Fe/H]} \approx 1.10$ using measurements of red clump stars in 47 Tuc, the Solar Neighborhood, and NGC 6791. From these efforts we also measure these properties of the Solar Neighborhood red clump, ($V-I$, $G_{BP}-K_{s}$, $G-K_{s}$, $G_{RP}-K_{s}$, $J-K_{s}$, $H-K_{s}$, $M_{I}$, $M_{Ks}$)$_{RC,0} =$ (1.02, 2.75, 2.18, 1.52, 0.64, 0.15, $-$0.23, $-$1.63). The second and third methods were to compare the observed colors of the red clump to those of Cepheids and RR Lyrae in the LMC. With these three methods, we estimated the intrinsic color of the red clump of the LMC to be $(V-I)_{RC,0,\rm{LMC}} = \{ \approx 0.93,0.91 \pm 0.02,0.89 \pm 0.02\}$ respectively, and similarly using the first and third method we estimated $ (V-I)_{RC,0,\rm{SMC}} = \{\approx 0.85,0.84 \pm 0.02 \}$ respectively for the Small Magellanic Cloud. We estimate the luminosities to be $M_{I,RC,\rm{LMC}}=-0.26$ and $M_{I,RC,\rm{SMC}}=-0.37$. We show that this has important implications for recent calibrations of the tip of the red giant branch in the Magellanic Clouds used to measure $H_0$., Comment: 20 pages, 5 figures, 4 tables. Accepted for Publication in The Astrophysical Journal as of February 9th, 2021

We present H-band light curves of Milky Way Classical Cepheids observed as part of the DEHVILS survey with the Wide-Field Infrared Camera on the United Kingdom InfraRed Telescope. Due to the crowded nature of these fields caused by defocusing the Camera, we performed difference-imaging photometry by modifying a pipeline originally developed to analyze images from the Transiting Exoplanet Survey Satellite. We achieved a photometric precision in line with expectations from photon statistics, reaching 0.01 mag for 8, Accepted for publication in the Astrophysical Journal Supplement Series. 14 pages, 6 figures

This commentary extends Hillier, Martínez, Patel, Pindado, and Requejo (2018) by placing their insights within a wider context of the debate between the agency theory and stewardship theory. To reconcile the conflicts between the two theories, we propose a family-value perspective to incorporate the intrinsic heterogeneity of family firms. We highlight how different family values may lead to different strategic behavior and how various theoretical perspectives may be best used to describe the behavior of family firms with certain specific values.

Developing predictions by drawing upon the limited attention perspective, we investigate if small firms may use advertising as an attention grabber to increase their opportunities to access debt financing. Using a sample of over a million observations, we find that small firms with higher advertising expenditure are more likely to gain access to debt financing, thus increasing their financial leverage. Our tests show that lenders constrained by a limited attentional capacity are more likely to be attracted by small firms with higher advertising expenditure, and that small firms with financial constraints are not found to use advertisement intentionally to acquire resource.

We present a calibration of the Tip of the Red Giant Branch (TRGB) in the Large Magellanic Cloud (LMC) on the HST/ACS F814W system. We use archival HST observations to derive blending corrections and photometric transformations for two ground-based wide-area imaging surveys of the Magellanic Clouds. We show that these surveys are biased bright by up to ~0.1 mag in the optical due to blending, and that the bias is a function of local stellar density. We correct the LMC TRGB magnitudes from Jang & Lee (2017) and use the geometric distance from Pietrzynski et al. (2019) to obtain an absolute TRGB magnitude of M_F814W=-3.97+/-0.046 mag. Applying this calibration to the TRGB magnitudes from Freedman et al. (2019) in SN Ia hosts yields a value for the Hubble constant of H_0=72.4+/-2.0 km/s/Mpc for their TRGB+SNe Ia distance ladder. The difference in the TRGB calibration and the value of H_0 derived here and by Freedman et al. (2019) primarily results from their overestimate of the LMC extinction, caused by inconsistencies in their different sources of TRGB photometry for the Magellanic Clouds. Using the same source of photometry (OGLE) for both Clouds and applying the aforementioned corrections yields a value for the LMC I-band TRGB extinction that is lower by 0.06 mag, consistent with independent OGLE reddening maps used by us and by Jang & Lee (2017) to calibrate TRGB and determine H_0., Accepted for publication in ApJ. This version incorporates all changes introduced during the refereeing process

We present an expanded sample of 75 Milky Way Cepheids with Hubble Space Telescope (HST) photometry and Gaia EDR3 parallaxes which we use to recalibrate the extragalactic distance ladder and refine the determination of the Hubble constant. All HST observations were obtained with the same instrument (WFC3) and filters (F555W, F814W, F160W) used for imaging of extragalactic Cepheids in Type Ia supernova (SN Ia) hosts. The HST observations used the WFC3 spatial scanning mode to mitigate saturation and reduce pixel-to-pixel calibration errors, reaching a mean photometric error of 5 millimags per observation. We use new Gaia EDR3 parallaxes, vastly improved since DR2, and the Period-Luminosity (PL) relation of these Cepheids to simultaneously calibrate the extragalactic distance ladder and to refine the determination of the Gaia EDR3 parallax offset. The resulting geometric calibration of Cepheid luminosities has 1.0% precision, better than any alternative geometric anchor. Applied to the calibration of SNe~Ia, it results in a measurement of the Hubble constant of 73.0 +/- 1.4 km/sec/Mpc, in good agreement with conclusions based on earlier Gaia data releases. We also find the slope of the Cepheid PL relation in the Milky Way, and the metallicity dependence of its zeropoint, to be in good agreement with the mean values derived from other galaxies. In combination with the best complementary sources of Cepheid calibration, we reach 1.8% precision and find H_0=73.2 +/- 1.3 km/sec/Mpc, a 4.2 sigma difference with the prediction from Planck CMB observations under LambdaCDM. We expect to reach ~1.3% precision in the near term from an expanded sample of ~40 SNe Ia in Cepheid hosts., submitted to ApJ, 21 pages, 5 figures, data table included

To optimise the performance of distributed compute, smaller lightweight storage caches are needed which integrate with existing grid computing workflows. A good solution to provide lightweight storage caches is to use an XRootD-proxy cache. To support distributed lightweight XRootD proxy services across GridPP we have developed a centralised monitoring framework. With the v5 release of XRootD it is possible to build a monitoring framework which collects distributed caching metadata broadcast from multiple sites. To provide the best support for these distributed caches we have built a centralised monitoring service for XRootD storage instances within GridPP. This monitoring solution is built upon experiences presented by CMS in setting up a similar service as part of their AAA system. This new framework is designed to provide remote monitoring of the behaviour, performance, and reliability of distributed XRootD services across the UK. Effort has been made to simplify ease of deployment by remote site administrators. The result of this work is an interactive dashboard system which enables administrators to access real-time metrics on the performance of their lightweight storage systems. This monitoring framework is intended to supplement existing functionality and availability testing metrics by providing detailed information and logging from a site perspective.

Purpose The aim of this paper is to investigate how multinational enterprise (MNE) subsidiary capabilities are influenced by the firm-specific advantages (FSAs) of the parent company, as well as by cultural and geographic distance between the home and host country. Design/methodology/approach This paper assesses how the effects of the parent FSAs, cultural distance and geographic distance on subsidiary capabilities vary for different value-chain activities, with an empirical application to 60 foreign subsidiaries operating in Canada. Findings This paper uncovers distinct, three-way interaction effects among parent-level FSAs, cultural distance and geographic distance for upstream versus downstream activities in the value chain. Originality/value We find that in special cases, high levels of distance can be positive for MNEs, in terms of driving the creation of stronger subsidiary capabilities.

We discuss the strategic significance of ‘regional multinationals’, and highlight a number of conceptual and empirical challenges that a regional multinationals research agenda should address. In line with the intellectual legacy of the late Alan Rugman, we argue that to deepen our understanding of regional strategy and organization, we cannot limit ourselves to studying the multinational enterprise’s (MNE’s) geographic footprint, but we must also explore the entire spectrum of regional elements in the firm’s organizational functioning, including the impact of the regional effect on subsidiary capabilities across the value chain. More specifically, we argue that operating in a host region can affect a foreign subsidiary’s capabilities: subsidiaries of outsider MNEs (meaning headquartered outside of the region) are disadvantaged as compared to insider MNE subsidiaries. This regional effect, however, is predicted to vary according to the value chain activity considered. Further, the regional effect will tend to diminish over time, though at a different pace for the various value chain activities.

We derive a distance of $15.8\pm0.4$ Mpc to the archetypical Seyfert 1 galaxy NGC 4151 based on the near-infrared Cepheid Period-Luminosity relation and new Hubble Space Telescope multiband imaging. This distance determination, based on measurements of 35 long-period ($P > 25$d) Cepheids, will support the absolute calibration of the supermassive black hole mass in this system, as well as studies of the dynamics of the feedback or feeding of its active galactic nucleus., 18 pages. 11 figures. 7 tables. Accepted for publication in ApJ