56 research outputs found
How does home country bribery affect firmsâ foreign market focus?:The case of firms in transition economies
Purpose: Drawing on the bribery literature, this paper aims to examine the effect of bribes paid in the home country on firmsâ decision to internationalize through exports from transition economies. It also investigates whether the effect of home country bribery may vary from new ventures to established firms, and from those firms that operate in an environment with high to low informal competition. Design/methodology/approach: This paper tests several hypotheses using a panel data with fixed effects based on a sample of firms in transition economies from the Business Environment and Enterprise Performance Survey. Findings: First, home country bribery in transition economies can make domestic markets more lenient and dampen firmsâ motivation to seek opportunities abroad. Second, new ventures have a higher motivation to focus on their domestic markets after paying bribes. Finally, despite the benefits accrued in the home country through bribery, firms that face a higher level of informal competition in the home country are more likely to seek opportunities abroad. Practical implications: Managers in transition economies should consider their home country bribery activities in their evaluation of foreign market opportunities. Firms that use money to influence home country government officials, especially new ventures, are advised to have a more holistic view in evaluating foreign market opportunities so they will not miss out on new opportunities. Originality/value: This paper advances literature on home country institutions and the research on firm global strategies. Moreover, it also highlights several contingencies that shape the effect of home country bribery on firmsâ foreign market focus
KMT-2018-BLG-0029Lb: A Very Low Mass-Ratio Spitzer Microlens Planet
At q = 1.81 ± 0.20 Ă 10â»â”, KMT-2018-BLG-0029Lb has the lowest planet-host mass ratio q of any microlensing planet to date by more than a factor of two. Hence, it is the first planet that probes below the apparent âpile-upâ at q = 5â10 Ă10â»â”. The event was observed by Spitzer, yielding a microlens-parallax Ï_E measurement. Combined with a measurement of the Einstein radius Ξ_E from finite-source effects during the caustic crossings, these measurements imply masses of the host M_(host) = 1.14^(+0.10)_(â0.12)Mâ and planet M_(planet) = 7.59^(+0.75)_(â0.69)Mâ, system distance D_L = 3.38^(+0.22)_(â0.26) 3.38^(+0.22)_(â0.26) kpc and projected separation aâ„ = 4.27^(+0.21)_(â0.23) 4.27^(+0.21)_(â0.23) AU. The blended light, which is substantially brighter than the microlensed source, is plausibly due to the lens and could be observed at high resolution immediately
OGLE-2018-BLG-0022: First Prediction of an Astrometric Microlensing Signal from a Photometric Microlensing Event
In this work, we present the analysis of the binary microlensing event
OGLE-2018-BLG-0022 that is detected toward the Galactic bulge field. The dense
and continuous coverage with the high-quality photometry data from ground-based
observations combined with the space-based {\it Spitzer} observations of this
long time-scale event enables us to uniquely determine the masses and of the individual lens components.
Because the lens-source relative parallax and the vector lens-source relative
proper motion are unambiguously determined, we can likewise unambiguously
predict the astrometric offset between the light centroid of the magnified
images (as observed by the {\it Gaia} satellite) and the true position of the
source. This prediction can be tested when the individual-epoch {\it Gaia}
astrometric measurements are released.Comment: 10 pages, 10 figures, 4 table
Parallax of OGLE-2018-BLG-0596: A Low-mass-ratio Planet around an M-dwarf
We report the discovery of a microlensing planet
OGLE-2018-BLG-0596Lb, with preferred planet-host mass ratio . The planetary signal, which is characterized by a short "bump" on the rising side of the lensing light curve, was densely
covered by ground-based surveys. We find that the signal can be explained by a
bright source that fully envelops the planetary caustic, i.e., a "Hollywood"
geometry. Combined with the source proper motion measured from , the
satellite parallax measurement makes it possible to precisely
constrain the lens physical parameters. The preferred solution, in which the
planet perturbs the minor image due to lensing by the host, yields a
Uranus-mass planet with a mass of orbiting
a mid M-dwarf with a mass of . There is also
a second possible solution that is substantially disfavored but cannot be ruled
out, for which the planet perturbs the major image. The latter solution yields
and . By
combining the microlensing and data together with a Galactic model, we
find in either case that the lens lies on the near side of the Galactic bulge
at a distance . Future adaptive optics
observations may decisively resolve the major image/minor image degeneracy.Comment: 34 pages, 8 figures, Submitted to AAS journa
Systematic KMTNet Planetary Anomaly Search. X. Complete Sample of 2017 Prime-Field Planets
We complete the analysis of planetary candidates found by the KMT
AnomalyFinder for the 2017 prime fields that cover . We
report 3 unambiguous planets: OGLE-2017-BLG-0640, OGLE-2017-BLG-1275, and
OGLE-2017-BLG-1237. The first two of these were not previously identified,
while the last was not previously published due to technical complications
induced by a nearby variable. We further report that a fourth anomalous event,
the previously recognized OGLE-2017-BLG-1777, is very likely to be planetary,
although its light curve requires unusually complex modeling because the lens
and source both have orbiting companions. One of the 3 unambiguous planets,
OGLE-2017-BLG-1275 is the first AnomalyFinder discovery that has a {\it
Spitzer} microlens parallax measurement, , implying
that this planetary system almost certainly lies in the Galactic bulge. In the
order listed, the four planetary events have planet-host mass ratios , and
normalized projected separations , of = ,
, , and . Combined with
previously published events, the 2017 AnomalyFinder prime fields contain 11
unambiguous planets with well-measured and one very likely candidate, of
which 3 are AnomalyFinder discoveries. In addition to these 12, there are three
other unambiguous planets with large uncertainties in .Comment: 67 pages, 13 figures, 16 table
OGLE-2017-BLG-1038: A Possible Brown-dwarf Binary Revealed by Spitzer Microlensing Parallax
We report the analysis of microlensing event OGLE-2017-BLG-1038, observed by
the Optical Gravitational Lensing Experiment, Korean Microlensing Telescope
Network, and Spitzer telescopes. The event is caused by a giant source star in
the Galactic Bulge passing over a large resonant binary lens caustic. The
availability of space-based data allows the full set of physical parameters to
be calculated. However, there exists an eightfold degeneracy in the parallax
measurement. The four best solutions correspond to very-low-mass binaries near
( and ), or well below
( and ) the
boundary between stars and brown dwarfs. A conventional analysis, with scaled
uncertainties for Spitzer data, implies a very-low-mass brown dwarf binary lens
at a distance of 2 kpc. Compensating for systematic Spitzer errors using a
Gaussian process model suggests that a higher mass M-dwarf binary at 6 kpc is
equally likely. A Bayesian comparison based on a galactic model favors the
larger-mass solutions. We demonstrate how this degeneracy can be resolved
within the next ten years through infrared adaptive-optics imaging with a 40 m
class telescope.Comment: 20 pages, 11 figures, 4 table
Systematic KMTNet Planetary Anomaly Search, Paper I: OGLE-2019-BLG-1053Lb, A Buried Terrestrial Planet
In order to exhume the buried signatures of "missing planetary caustics" in
the KMTNet data, we conducted a systematic anomaly search to the residuals from
point-source point-lens fits, based on a modified version of the KMTNet
EventFinder algorithm. This search reveals the lowest mass-ratio planetary
caustic to date in the microlensing event OGLE-2019-BLG-1053, for which the
planetary signal had not been noticed before. The planetary system has a
planet-host mass ratio of . A Bayesian
analysis yields estimates of the mass of the host star, , the mass of its planet, , the projected planet-host separation,
au, and the lens distance of kpc. The discovery of this very low mass-ratio planet
illustrates the utility of our method and opens a new window for a large and
homogeneous sample to study the microlensing planet-host mass-ratio function
down to .Comment: published by A
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