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Normative and systems integration in human resource management in Japanese multinational companies
Purpose
This paper aims to conceptualise a framework of “transnational human resource management” (HRM) and to demonstrate the validity of the model.
Design/methodology/approach
Evidence is drawn from survey of 93 large Japanese multinational companies (MNCs). Data are analysed through descriptive statistics, hierarchical multiple regression analyses and mediation effect analyses.
Findings
The analysis reveals that the practices for normative and systems integration are associated with increasing levels of social capital and geocentric staffing, respectively, and the social capital and geocentric staffing fully mediate the relationship between normative and systems integration and transnationality.
Originality/value
The research extends the integration theory in international HRM and demonstrates the validity of our framework for transnational HRM. The authors also shed light on the reality of the integration aspects of international HRM in Japanese MNCs
A Systematic Survey of Protoclusters at in the CFHTLS Deep Fields
We present the discovery of three protoclusters at with
spectroscopic confirmation in the Canada-France-Hawaii Telescope (CFHT) Legacy
Survey Deep Fields. In these fields, we investigate the large-scale projected
sky distribution of Lyman break galaxies and identify 21
protocluster candidates from regions that are overdense at more than
overdensity significance. Based on cosmological simulations, it is expected
that more than of these candidates will evolve into a galaxy cluster of
at least a halo mass of at . We perform
follow-up spectroscopy for eight of the candidates using Subaru/FOCAS,
KeckII/DEIMOS, and Gemini-N/GMOS. In total we target 462 dropout candidates and
obtain 138 spectroscopic redshifts. We confirm three real protoclusters at
with more than five members spectroscopically identified, and
find one to be an incidental overdense region by mere chance alignment. The
other four candidate regions at require more spectroscopic
follow-up in order to be conclusive. A protocluster, which has eleven
spectroscopically confirmed members, shows a remarkable core-like structure
composed of a central small region (Mpc}) and an
outskirts region (). The Ly equivalent
widths of members of the protocluster are significantly smaller than those of
field galaxies at the same redshift while there is no difference in the UV
luminosity distributions. These results imply that some environmental effects
start operating as early as at along with the growth of the
protocluster structure.Comment: 25 pages, 6 tables, 25 figures, accepted for publication in Ap
A New Milky Way Satellite Discovered In The Subaru/Hyper Suprime-Cam Survey
We report the discovery of a new ultra-faint dwarf satellite companion of the
Milky Way based on the early survey data from the Hyper Suprime-Cam Subaru
Strategic Program. This new satellite, Virgo I, which is located in the
constellation of Virgo, has been identified as a statistically significant (5.5
sigma) spatial overdensity of star-like objects with a well-defined main
sequence and red giant branch in their color-magnitude diagram. The
significance of this overdensity increases to 10.8 sigma when the relevant
isochrone filter is adopted for the search. Based on the distribution of the
stars around the likely main sequence turn-off at r ~ 24 mag, the distance to
Virgo I is estimated as 87 kpc, and its most likely absolute magnitude
calculated from a Monte Carlo analysis is M_V = -0.8 +/- 0.9 mag. This stellar
system has an extended spatial distribution with a half-light radius of 38
+12/-11 pc, which clearly distinguishes it from a globular cluster with
comparable luminosity. Thus, Virgo I is one of the faintest dwarf satellites
known and is located beyond the reach of the Sloan Digital Sky Survey. This
demonstrates the power of this survey program to identify very faint dwarf
satellites. This discovery of VirgoI is based only on about 100 square degrees
of data, thus a large number of faint dwarf satellites are likely to exist in
the outer halo of the Milky Way.Comment: typos are corrected, 6 pages, 4 figures, accepted for publication in
Ap
Minor Contribution of Quasars to Ionizing Photon Budget at z~6: Update on Quasar Luminosity Function at the Faint-end with Subaru/Suprime-Cam
We constrain the quasar contribution to cosmic reionization based on our deep
optical survey of z~6 quasars down to z_R=24.15 using Subaru/Suprime-Cam in
three UKIDSS-DXS fields covering 6.5 deg^2. In Kashikawa et al. (2015), we
select 17 quasar candidates and report our initial discovery of two
low-luminosity quasars (M_1450~ -23) from seven targets, one of which might be
a Lyman alpha emitting galaxy. From an additional optical spectroscopy, none of
the four candidates out of the remaining ten turn out to be genuine quasars.
Moreover, the deeper optical photometry provided by the Hyper Suprime-Cam
Subaru Strategic Program (HSC-SSP) shows that, unlike the two already-known
quasars, the i-z and z-y colors of the last six candidates are consistent with
M- or L-type brown dwarfs. Therefore, the quasar luminosity function (QLF) in
the previous paper is confirmed. Compiling QLF measurements from the literature
over a wide magnitude range, including an extremely faint AGN candidate from
Parsa et al. (2017}, to fit them with a double power-law, we find that the
best-fit faint-end slope is alpha=-2.04^+0.33_-0.18 (-1.98^+0.48_-0.21) and
characteristic magnitude is M_1450^*=-25.8^+1.1_-1.9 (-25.7^+1.0_-1.8) in the
case of two (one) quasar detection. Our result suggests that, if the QLF is
integrated down to M_1450=-18, quasars produce ~1-12% of the ionizing photons
required to ionize the whole universe at z~6 with 2sigma confidence level,
assuming that the escape fraction is f_esc=1 and the IGM clumpy factor is C=3.
Even when the systematic uncertainties are taken into account, our result
supports the scenario that quasars are the minor contributors of reionization.Comment: 8 pages, 3 figures, ApJL accepte
Comoving Space Density and Obscured Fraction of High-Redshift Active Galactic Nuclei in the Subaru/{\it XMM-Newton} Deep Survey
We study the comoving space density of X-ray-selected luminous active
galactic nuclei (AGNs) and the obscured AGN fraction at high redshifts () in the Subaru/{\it XMM-Newton} Deep Survey (SXDS) field. From an X-ray
source catalog with high completeness of optical identification thanks to deep
optical images, we select a sample of 30 AGNs at with intrinsic
(de-absorbed and rest-frame 2--10 keV) luminosities of
erg s detected in the 0.5--2 keV band, consisting of 20 and 10 objects
with spectroscopic and photometric redshifts, respectively. Utilizing the
method, we confirm that the comoving space density of luminous
AGNs decreases with redshift above . When combined with the {\it
Chandra}-COSMOS result of Civano et al.\ (2011), the density decline of AGNs
with erg s is well represented by a power law
of . We also determine the fraction of X-ray obscured
AGNs with cm in the Compton-thin population to be
0.54, by carefully taking into account observational biases
including the effects of photon statistics for each source. This result is
consistent with an independent determination of the type-2 AGN fraction based
on optical properties, for which the fraction is found to be 0.590.09.
Comparing our result with that obtained in the local Universe, we conclude that
the obscured fraction of luminous AGNs increases significantly from to
by a factor of 2.51.1.Comment: 12 pages, 12 figures, 1 table. Accepted for publication in Ap
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