257 research outputs found
Trends in Consumer Behavior Literature: A Content Analysis
While a comprehensive review and classification of consumer behavior literature has been called for periodically, none has been forthcoming. This paper attempts partially to rectify this situation. It classifies by several key variables 32 years of consumer behavior literature from selected journals and proceedings
The Young Stellar Population of the Nearby Late-Type Galaxy NGC 1311
We have extracted PSF-fitted stellar photometry from near-ultraviolet,
optical and near-infrared images, obtained with the Hubble Space Telescope, of
the nearby (D ~ 5.5 Mpc) SBm galaxy NGC 1311. The ultraviolet and optical data
reveal a population of hot main sequence stars with ages of 2-10 Myr. We also
find populations of blue supergiants with ages between 10 and 40 Myr and red
supergiants with ages between 10 and 100 Myr. Our near-infrared data shows
evidence of star formation going back ~1 Gyr, in agreement with previous work.
Fits to isochrones indicate a metallicity of Z ~ 0.004. The ratio of blue to
red supergiants is consistent with this metallicity. This indicates that NGC
1311 follows the well-known luminosity-metallicity relation for late-type dwarf
galaxies. About half of the hot main sequence stars and blue supergiants are
found in two regions in the inner part of NGC 1311. These two regions are each
about 200 pc across, and thus have crossing times roughly equal to the 10 Myr
age we find for the dominant young population. The Luminosity Functions of the
supergiants indicate a slowly rising star formation rate (of 0.001 Solar masses
per year) from ~100 Myr ago until ~15 Myr ago, followed by a strong enhancement
(to 0.01 Solar Masses per year) at ~10 Myr ago. We see no compelling evidence
for gaps in the star-forming history of NGC 1311 over the last 100 Myr, and,
with lower significance, none over the last Gyr. This argues against a bursting
mode, and in favor of a gasping or breathing mode for the recent star-formation
history.Comment: AASTex, 34 pages, 13 postscript figures. Accepted for publication by
The Astronomical Journa
Chronic Effects of Lead Exposure on Topsmelt Fish (Atherinops Affinis): Influence of Salinity, Organism Age, and Relative Sensitivity to Other Marine Fish
The aim of this study was to determine the influence of salinity and organism age on the chronic toxicity of waterborne lead (Pb) to Atherinops affinis and to compare the relative Pb sensitivity of A. affinis with other marine species. Chronic Pb exposure experiments were conducted in a water flow‐through testing system. Survival, standard length, dry weight, and tissue Pb concentration were measured and lethal concentrations (LC), effective concentrations (EC), and bioconcentration factor (BCF) were calculated. In general, increasing salinity and organism age decreased Pb toxicity. The LC50s for larval fish at 14 and 28 ppt salinity were 15.1 and 79.8 µg/L dissolved Pb, respectively; whereas, the LC50 for juvenile fish was 167.6 µg/L dissolved Pb at 28 ppt salinity. Using standard length data, the EC10 values for larval fish were 16.4 and 82.4 µg/L dissolved Pb at 14 and 28 ppt salinity, respectively. The dry weight EC25 for low and high salinity were 15.6 and 61.84 µg/L dissolved Pb, respectively. The BCF was higher with the lower salinity study (1,703) in comparison to the higher salinity study (654). Results of Pb speciation calculation showed higher fraction of Pb2+ in water with lower salinity, explaining the higher observed toxicity of Pb in lower salinity water than higher salinity water. Atherinops affinis is more sensitive to Pb than several other marine species. Evidences for abnormal swimming and skeletal deformities were observed in Pb exposure treatment. Results of the present study are useful for marine Biotic Ligand Modeling and support ecological risk assessment and deriving Pb environmental quality criteria for marine environment
The evolution of galaxies at constant number density: a less biased view of star formation, quenching, and structural formation
Due to significant galaxy contamination and impurity in stellar mass selected samples (up to 95 per cent from z = 0–3), we examine the star formation history, quenching time-scales, and structural evolution of galaxies using a constant number density selection with data from the United Kingdom Infra-Red Deep Sky Survey Ultra-Deep Survey field. Using this methodology, we investigate the evolution of galaxies at a variety of number densities from z= 0–3. We find that samples chosen at number densities ranging from 3 × 10−4 to 10−5 galaxies Mpc−3 (corresponding to z ∼ 0.5 stellar masses of M∗ = 1010.95−11.6 M0) have a star-forming blue fraction of ∼50 per cent at z ∼ 2.5, which evolves to a nearly 100 per cent quenched red and dead population by z ∼ 1. We also see evidence for number density downsizing, such that the galaxies selected at the lowest densities (highest masses) become a homogeneous red population before those at higher number densities. Examining the evolution of the colours for these systems furthermore shows that the formation redshift of galaxies selected at these number densities is zform > 3. The structural evolution through size and S´ersic index fits reveal that while there remains evolution in terms of galaxies becoming larger and more concentrated in stellar mass at lower redshifts, the magnitude of the change is significantly smaller than for a mass-selected sample. We also find that changes in size and structure continues at z < 1, and is coupled strongly to passivity evolution.We conclude that galaxy structure is driving the quenching of galaxies, such that galaxies become concentrated before they become passive
Size evolution of the most massive galaxies at 1.7<z<3 from GOODS NICMOS survey imaging
We measure the sizes of 82 massive (M>10^11 M_sun) galaxies at 1.7<z<3
utilizing deep HST NICMOS data taken in the GOODS North and South fields. Our
sample is almost an order of magnitude larger than previous studies at these
redshifts, providing the first statistical study of massive galaxy sizes at
z>2, confirming the extreme compactness of these galaxies. We split our sample
into disk-like (n2) galaxies based on their Sersic
indices, and find that at a given stellar mass disk-like galaxies at z~2.3 are
a factor of 2.6+/-0.3 smaller than present day equal mass systems, and
spheroid-like galaxies at the same redshifts are 4.3+/-0.7 smaller than
comparatively massive elliptical galaxies today. At z>2 our results are
compatible with both a leveling off, or a mild evolution in size. Furthermore,
the high density (~2x10^10 M_sun kpc^-3) of massive galaxies at these
redshifts, which are similar to present day globular clusters, possibly makes
any further evolution in sizes beyond z=3 unlikely.Comment: 5 pages, 2 figures, 2 tables, accepted by ApJ Letters, minor changes
added to match the accepted versio
Recovering Residual Forensic Data from Smartphone Interactions with Cloud Storage Providers
There is a growing demand for cloud storage services such as Dropbox, Box,
Syncplicity and SugarSync. These public cloud storage services can store
gigabytes of corporate and personal data in remote data centres around the
world, which can then be synchronized to multiple devices. This creates an
environment which is potentially conducive to security incidents, data breaches
and other malicious activities. The forensic investigation of public cloud
environments presents a number of new challenges for the digital forensics
community. However, it is anticipated that end-devices such as smartphones,
will retain data from these cloud storage services. This research investigates
how forensic tools that are currently available to practitioners can be used to
provide a practical solution for the problems related to investigating cloud
storage environments. The research contribution is threefold. First, the
findings from this research support the idea that end-devices which have been
used to access cloud storage services can be used to provide a partial view of
the evidence stored in the cloud service. Second, the research provides a
comparison of the number of files which can be recovered from different
versions of cloud storage applications. In doing so, it also supports the idea
that amalgamating the files recovered from more than one device can result in
the recovery of a more complete dataset. Third, the chapter contributes to the
documentation and evidentiary discussion of the artefacts created from specific
cloud storage applications and different versions of these applications on iOS
and Android smartphones
The Structures of Distant Galaxies V: The Evolution of Galaxy Structure in Stellar Mass at z < 1
Galaxy structure and morphology is nearly always studied using the light
originating from stars, however ideally one is interested in measuring
structure using the stellar mass distribution. Not only does stellar mass trace
out the underlying distribution of matter, it also minimises the effects of
star formation and dust on the appearance and structure of a galaxy. We present
in this paper a study of the stellar mass distributions and structures of
galaxies at z<1 as found within the GOODS fields. We use pixel by pixel
K-corrections to construct stellar mass and mass-to-light ratio maps of 560
galaxies of known morphology at magnitudes z_{850}<24. We measure structural
and size parameters using these stellar mass maps, as well as on ACS BViz band
imaging. This includes investigating the structural CAS-Gini-M_{20} parameters
and half-light radius for each galaxy. We compare structural parameters and
half-light radii in the ACS z_{850}-band and stellar mass maps, finding no
systematic bias introduced by measuring galaxy sizes in z_{850}. We furthermore
investigate relations between structural parameters in the ACS BViz bands and
stellar mass maps, and compare our result to previous morphological studies.
Combinations of various parameters in stellar mass generally reveal clear
separations between early and late type morphologies, but cannot easily
distinguish between star formation and dynamically disturbed systems. We also
show that while ellipticals and early-type spirals have fairly constant CAS
values at z<1 we find a tendency for late-type spiral and peculiar
morphological types to have a higher A(M_{*}) at higher redshift. We argue that
this, and the large fraction of peculiars that appear spiral-like in stellar
mass maps, are possible evidence for either an active bulge formation in some
late-type disks at z<1 or the presence of minor merger events.Comment: 27 pages, MNRAS in pres
Galaxy evolution by color-log(n) type since redshift unity in the Hubble Ultra Deep Field
We explore the use of the color-log(n) plane (where n is the global Sersic
index) as a tool for subdividing the high redshift galaxy population in a
physically-motivated manner. Using a series of volume-limited samples out to
z=1.5 in the Hubble Ultra Deep Field (UDF) we confirm the correlation between
color-log(n) plane position and visual morphology observed locally and in other
high redshift studies in the color and/or structure domain. Via comparison to a
low redshift sample from the Millennium Galaxy Catalogue we quantify evolution
by color-log(n) type, accounting separately for the specific selection and
measurement biases against each. Specifically, we measure decreases in B-band
surface brightness of 1.57 +/- 0.22 mag/sq.arcsec and 1.65 +/- 0.22
mag/sq.arcsec for `blue, diffuse' and `red, compact' galaxies respectively
between redshift unity and the present day.Comment: 12 pages, 6 figures, to be published in A&A (accepted 29/10/08
Emission-Line Galaxies from the Hubble Space Telescope Probing Evolution and Reionization Spectroscopically (PEARS) Grism Survey. II: The Complete Sample
We present a full analysis of the Probing Evolution And Reionization
Spectroscopically (PEARS) slitess grism spectroscopic data obtained with the
Advanced Camera for Surveys on HST. PEARS covers fields within both the Great
Observatories Origins Deep Survey (GOODS) North and South fields, making it
ideal as a random survey of galaxies, as well as the availability of a wide
variety of ancillary observations to support the spectroscopic results. Using
the PEARS data we are able to identify star forming galaxies within the
redshift volume 0< z<1.5. Star forming regions in the PEARS survey are
pinpointed independently of the host galaxy. This method allows us to detect
the presence of multiple emission line regions (ELRs) within a single galaxy.
1162 Ha, [OIII] and/or [OII] emission lines have been identified in the PEARS
sample of ~906 galaxies down to a limiting flux of ~1e-18 erg/s/cm^2. The ELRs
have also been compared to the properties of the host galaxy, including
morphology, luminosity, and mass. From this analysis we find three key results:
1) The computed line luminosities show evidence of a flattening in the
luminosity function with increasing redshift; 2) The star forming systems show
evidence of disturbed morphologies, with star formation occurring predominantly
within one effective (half-light) radius. However, the morphologies show no
correlation with host stellar mass; and 3) The number density of star forming
galaxies with M_* > 1e9} M_sun decreases by an order of magnitude at z<0.5
relative to the number at 0.5<z<0.9 in support of the argument for galaxy
downsizing.Comment: Submitted. 48 pages. 19 figures. Accepted to Ap
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