42 research outputs found
Pengaruh Citra Merek dan Harga Terhadap Keputusan Pembelian Konsumen Produk Pakaian Dalam Pria PT. Colorindo Internusa di Carrefour Tangcity Mall
Nowadays, with the help of the internet, all information can be obtained quickly and easily including information about all products, this makes consumers smarter and more critical in choosing a product. Sales of men's underwear with the Mario Marcello brand are still not satisfactory from the target set by the company, which is likely due to the increasing competition among similar product providers, which requires the company to be able to compete for new customers and be more vigilant in retaining its customers.
This study aims to determine how much the effect of the brand image and price have on purchasing decisions for men's underwear, Mario Marcello brand at Carrefour Tangcity Mall.
This type of research uses quantitative descriptive methods. The population that used is the male consumer of Mario Marcelloâs product at Carrefour Tangcity Mall and the sample taken is 100 respondents.
From the results of data analysis with the correlation coefficient test, it shows that Brand Image and Price have a positive and strong relationship with Purchasing Decisions. From the results of data analysis with the T hypothesis test shows that brand image and price have a significant effect on purchasing decisions. Hypothesis F test shows that there is a linear effect between the Brand Image and Price variables on Purchasing Decisions, so the regression model is appropriate and feasible.Disaat sekarang dimana dengan bantuan internet semua informasi bisa didapatkan dengan cepat dan mudah termasuk informasi mengenai semua produk, hal ini membuat konsumen semakin cerdas dan kritis dalam memilih suatu produk. Penjualan produk pakaian dalam pria bermerek Mario Marcello yang masih belum memuaskan dari target yang di tentukan perusahaan yang kemungkinan besar disebabkan dengan semakin ketatnya persaingan antar penyedia produk sejenis mengharuskan perusahaan untuk mampu bersaing mendapatkan pelanggan baru dan semakin waspada dalam mempertahankan pelanggannya.
Penelitian ini bertujuan untuk mengetahui seberapa besar pengaruh citra merek dan harga terhadap keputusan pembelian produk pakaian dalam pria merek Mario Marcello di Carrefour Tangcity Mall.
Jenis penelitian ini menggunakan metode deskriptif kuantitatif. Populasi yang digunakan merupakan konsumen produk pakai dalam pria Mario Marcello di Carrefour Tangcity Mall dan sampel yang diambil berjumlah 100 orang responden.
Dari hasil analisis data dengan uji koefisien korelasi menunjukkan bahwa Citra Merek dan Harga mempunyai hubungan yang positif dan kuat terhadap Keputusan Pembelian. Dari hasil analisis data dengan uji hipotesis T menunjukkan bahwa Citra Merek dan Harga benar berpengaruh signifikan terhadap Keputusan Pembelian. Uji hipotesis F menunjukkan bahwa terdapat pengaruh linier antara variabel Citra Merek dan Harga terhadap Keputusan Pembelian, maka model regresi tersebut sudah tepat dan layak
High-Resolution Spectroscopy of the Lunar Sodium Exosphere
We have applied high-resolution Fabry-Perot spectroscopy to the study of the lunar sodium exosphere for the study of exospheric effective temperature and velocity variations. Observing from the National Solar Observatory McMath-Pierce Telescope, we used a dual-etalon Fabry-Perot spectrometer with a resolving power of 180,000 to measure line widths and Doppler shifts of the sodium D2 (5889.95 ) emission line. Our field of view was 360 km, and measurements were made in equatorial and polar regions from 500 km to 3500 km off the limb. Data were obtained from full moon to 3 days following full moon (waning phase) in March 2009. Measured Doppler line widths within 1100 km of the sunlit east and south lunar limbs for observations between 5 and 40 deg lunar phase imply effective temperatures ranging between 3260 +/- 190 and 1000 +/- 135 K. Preliminary line center analysis indicates velocity displacements between different locations off the lunar limb ranging between 100 and 600 m/s from the lunar rest velocity with a precision of +/-20 to +/-50 m/s depending on brightness. Based on the success of these exploratory observations, an extensive program has been initiated that is expected to constrain lunar atmospheric and surface-process modeling and help quantify source and escape mechanisms
A Search for Intrinsic Polarization in O Stars with Variable Winds
New observations of 9 of the brightest northern O stars have been made with
the Breger polarimeter on the 0.9~m telescope at McDonald Observatory and the
AnyPol polarimeter on the 0.4~m telescope at Limber Observatory, using the
Johnson-Cousins UBVRI broadband filter system. Comparison with earlier
measurements shows no clearly defined long-term polarization variability. For
all 9 stars the wavelength dependence of the degree of polarization in the
optical range can be fit by a normal interstellar polarization law. The
polarization position angles are practically constant with wavelength and are
consistent with those of neighboring stars. Thus the simplest conclusion is
that the polarization of all the program stars is primarily interstellar.
The O stars chosen for this study are generally known from ultraviolet and
optical spectroscopy to have substantial mass loss rates and variable winds, as
well as occasional circumstellar emission. Their lack of intrinsic polarization
in comparison with the similar Be stars may be explained by the dominance of
radiation as a wind driving force due to higher luminosity, which results in
lower density and less rotational flattening in the electron scattering inner
envelopes where the polarization is produced. However, time series of
polarization measurements taken simultaneously with H-alpha and UV spectroscopy
during several coordinated multiwavelength campaigns suggest two cases of
possible small-amplitude, periodic short-term polarization variability, and
therefore intrinsic polarization, which may be correlated with the more widely
recognized spectroscopic variations.Comment: LaTeX2e, 22 pages including 11 tables; 12 separate gif figures; uses
aastex.cls preprint package; accepted by The Astronomical Journa
Blobs in Wolf-Rayet Winds: Random Photometric and Polarimetric Variability
Some isolated Wolf-Rayet stars present random variability in their optical
flux and polarization. We make the assumption that such variability is caused
by the presence of regions of enhanced density, i.e. blobs, in their envelopes.
In order to find the physical characteristics of such regions we have modeled
the stellar emission using a Monte Carlo code to treat the radiative transfer
in an inhomogeneous electron scattering envelope. We are able to treat multiple
scattering in the regions of enhanced density as well as in the envelope
itself. The finite sizes of the source and structures in the wind are also
taken into account. Most of the results presented here are based on a parameter
study of models with a single blob. The effects due to multiple blobs in the
envelope are considered to a more limited extent. Our simulations indicate that
the density enhancements must have a large geometric cross section in order to
produce the observed photopolarimetric variability. The sizes must be of the
order of one stellar radius and the blobs must be located near the base of the
envelope. These sizes are the same inferred from the widths of the sub-peaks in
optical emission lines of Wolf-Rayet stars. Other early-type stars show random
polarimetric fluctuations with characteristics similar to those observed in
Wolf-Rayet stars, which may also be interpreted in terms of a clumpy wind.
Although the origin of such structures is still unclear, the same mechanism may
be working in different types of hot stars envelopes to produce such
inhomogeneities.Comment: Accepted to ApJ. 17 pages + 6 figure
Hubble Space Telescope Observations of the Gravitationally Lensed Cloverleaf Broad Absorption Line QSO H1413+1143: Imaging Polarimetry and Evidence for Microlensing of a Scattering Region
We report the results of HST WFPC2 broadband F555W and F702W photometric and
F555W polarimetric observations of the "Cloverleaf" QSO H1413+1143. This is a
four-component gravitationally-lensed broad absorption line (BAL) QSO.
Observations were obtained at two epochs in March 1999 and June 1999 separated
by about 100 days. The goal of our program was to detect any relative changes
among the components and between the two epochs. Over this time baseline we
detected an approximately 0.07 mag dimming in component D of the lensed image,
which we interpret as evidence for microlensing. In March 1999 we find
significant evidence for a difference in the relative linear polarization of
component D in comparison to the other three components; in June 1999 the
combined polarization of the Cloverleaf components was lower. In March 1999 the
apparently microlensed component D has a rotated polarization position angle
and a somewhat higher degree of polarization than the other three components.
We suggest that this difference in polarization is due to microlensing
magnification of part of a scattered-light (i.e. polarized) continuum-producing
region. The results indicate that in the Cloverleaf the size-scale of the
polarized scattered-light region exceeds about 10^{16} cm but lies interior to
the region producing the broad emission lines (< 10^{18} cm).Comment: 21 pages, accepted for publication in Ap
Modelling the clumping-induced polarimetric variability of hot star winds
Clumping in the winds of massive stars may significantly reduce empirical
mass-loss rates, and which in turn may have a large impact on our understanding
of massive star evolution. Here, we investigate wind-clumping through the
linear polarization induced by light scattering off the clumps. Through the use
of an analytic wind clumping model, we predict the time evolution of the linear
polarimetry over a large parameter space. We concentrate on the Luminous Blue
Variables, which display the greatest amount of polarimetric variability and
for which we recently conducted a spectropolarimetric survey. Our model results
indicate that the observed level of polarimetric variability can be reproduced
for two regimes of parameter space: one of a small number of massive,
optically-thick clumps; and one of a very large number of low-mass clumps.
Although a systematic time-resolved monitoring campaign is required to
distinguish between the two scenarios, we currently favour the latter, given
the short timescale of the observed polarization variability. As the
polarization is predicted to scale linearly with mass-loss rate, we anticipate
that all hot stars with very large mass-loss rates should display polarimetric
variability. This is consistent with recent findings that intrinsic
polarization is more common in stars with strong H emission.Comment: 12 pages, 11 figures, accepted to A&
Hubble Space Telescope Observations of Field Ultracool Dwarfs at High Galactic Latitude
We present a sample of 17 newly discovered ultracool dwarf candidates later
than ~M8, drawn from 231.90 arcmin2 of {\it Hubble Space Telescope} Wide Field
Camera 3 infrared imaging. By comparing the observed number counts for
17.5<J_125<25.5 AB mag to an exponential disk model, we estimate a vertical
scale height of z_scl=290 +- 25 (random) +- 30 (systematic) pc for a binarity
fraction of f_b=0. While our estimate is roughly consistent with published
results, we suggest that the differences can be attributed to sample
properties, with the present sample containing far more substellar objects than
previous work. We predict the object counts should peak at J_{125}~24 AB mag
due to the exponentially-declining number density at the edge of the disc. We
conclude by arguing that trend in scale height with spectral type may breakdown
for brown dwarfs since they do not settle onto the main sequence.Comment: 9 pages, 6 figures, 3 tables, accepted to ApJ (v2 is consistent with
Referee changes
Polarimetric Evidence of Non-Spherical Winds
Polarization observations yield otherwise unobtainable information about the
geometrical structure of unresolved objects. In this talk we review the
evidences for non-spherically symmetric structures around Luminous Hot Stars
from polarimetry and what we can learn with this technique. Polarimetry has
added a new dimension to the study of the envelopes of Luminous Blue Variables,
Wolf-Rayet stars and B[e] stars, all of which are discussed in some detail.Comment: 8 pages, 2 encapsulated Postscript figures, uses lamuphys.sty.
Invited review to appear in IAU Coll. 169, Variable and Non-Spherical Stellar
Winds in Luminous Hot Stars, eds. B. Wolf, A.Fullerton and O. Stahl
(Springer
On the presence and absence of disks around O-type stars
(abridged) As the favoured progenitors of long-duration gamma-ray bursts,
massive stars may represent our best signposts of individual objects in the
early Universe, but special conditions seem required to make these bursters,
which might originate from the progenitor's rapid rotation and associated
asymmetry. To obtain empirical constraints on the interplay between stellar
rotation and wind asymmetry, we perform linear Halpha spectropolarimetry on a
sample of 18 spectroscopically peculiar massive O stars, including OVz, Of?p,
Oe, and Onfp stars, supplemented by an earlier sample of 20 O supergiants.
Despite their rapid rotation (with vsin(i) up to 400 km/s) most O-type stars
are found to be spherically symmetric, but with notable exceptions amongst
specific object classes. We divide the peculiar O stars into four distinct
categories: Groups III and IV include the Oe stars and Onfp stars, which are on
the high-end tail of the O star rotation distribution and have in the past been
claimed to be embedded in disks. Here we report the detection of a classical
depolarization ``line effect'' in the Oe star HD 45314, but the overall
incidence of line effects amongst Oe stars is significantly lower (1 out of 6)
than amongst Be stars. The chance that the Oe and Be datasets are drawn from
the same parent population is negligible (with 95% confidence). This implies
there is as yet no evidence for a disk hypothesis in Oe stars, providing
relevant constraints on the physical mechanism that is responsible for the Be
phenomenon. Finally, we find that 3 out of 4 of the group IV Onfp stars show
evidence for complex polarization effects, which are likely related to rapid
rotation, and we speculate on the evolutionary links to B[e] stars.Comment: Astronomy & Astrophyics (in press) 12 page