5,955 research outputs found
The os penis of the frugivorous bat Eidolon helvum (Kerr)
The os penis reported in some species of the mammalian orders was observed in the juvenile and adult penes of the friguvorous African bat, Eidolon helvum. The morphology of the os penis in Eidolon helvum differs from those observed in bat species and other mammalian orders. In the adult form it is large, disc-shaped and located at the distal segment of the penile organ. The proximal segment of the penis does not contain any bone. In the juvenile bat the os penis is made of two separate bones located longitudinally close to each other at the distal third of the penile tissue. The distal location in both the juvenile and the adult poses a question about the true function of this tissue. The bone may function in Eidolon helvum to support erection of the penis more for micturition than for intromission
Influence of Smartphones and Software on Acoustic Voice Measures.
This study assessed the within-subject variability of voice measures captured using different recording devices (i.e., smartphones and head mounted microphone) and software programs (i.e., Analysis of Dysphonia in Speech and Voice (ADSV), Multi-dimensional Voice Program (MDVP), and Praat). Correlations between the software programs that calculated the voice measures were also analyzed. Results demonstrated no significant within-subject variability across devices and software and that some of the measures were highly correlated across software programs. The study suggests that certain smartphones may be appropriate to record daily voice measures representing the effects of vocal loading within individuals. In addition, even though different algorithms are used to compute voice measures across software programs, some of the programs and measures share a similar relationship.
CLASH-VLT: Strangulation of cluster galaxies in MACSJ0416.1-2403 as seen from their chemical enrichment
(abridged) We explore the Frontier Fields cluster MACS J0416.1-2403 at
z=0.3972 with VIMOS/VLT spectroscopy from the CLASH-VLT survey covering a
region which corresponds to almost three virial radii. We measure fluxes of 5
emission lines of 76 cluster members enabling us to unambiguously derive O/H
gas metallicities, and also SFRs from Halpha. For intermediate massses we find
a similar distribution of cluster and field galaxies in the MZR and mass vs.
sSFR diagrams. Bulge-dominated cluster galaxies have on average lower sSFRs and
higher O/Hs compared to their disk-dominated counterparts. We use the location
of galaxies in the projected velocity vs. position phase-space to separate our
cluster sample into a region of objects accreted longer time ago and a region
of recently accreted and infalling galaxies. We find a higher fraction of
accreted metal-rich galaxies (63%) compared to the fraction of 28% of
metal-rich galaxies in the infalling regions. Intermediate mass galaxies
falling into the cluster for the first time are found to be in agreement with
predictions of the fundamental metallicity relation. In contrast, for already
accreted star-forming galaxies of similar masses, we find on average
metallicities higher than predicted by the models. This trend is intensified
for accreted cluster galaxies of the lowest mass bin, that display
metallicities 2-3 times higher than predicted by models with primordial gas
inflow. Environmental effects therefore strongly influence gas regulations and
control gas metallicities of log(M/Msun)<10.2 (Salpeter IMF) cluster galaxies.
We also investigate chemical evolutionary paths of model galaxies with and
without inflow of gas showing that strangulation is needed to explain the
higher metallicities of accreted cluster galaxies. Our results favor a
strangulation scenario in which gas inflow stops for log(M/Msun)<10.2 galaxies
when accreted by the cluster.Comment: Version better matched to the published version, including table with
observed and derived quantities for the 76 cluster galaxie
The Kormendy relation of early-type galaxies as a function of wavelength in Abell S1063, MACS J0416.1-2403 and MACS J1149.5+2223
The wavelength dependence of the Kormendy relation (KR) is well characterised
at low-redshift, but poorly studied at intermediate redshifts. The KR provides
information on the evolution of the population of early-type galaxies (ETGs),
therefore, by studying it, we may shed light on the assembly processes of these
objects and their size evolution. Since studies at different redshifts are
generally conducted in different rest-frame wavebands, investigating whether
there is a wavelength dependence of the KR is fundamental to interpret the
conclusions we might draw from it. We analyse the KRs of the three Hubble
Frontier Fields clusters, Abell S1063 (z = 0.348), MACS J0416.1-2403 (z =
0.396), and MACS J1149.5+2223 (z = 0.542), as a function of wavelength. This is
the first time the KR of ETGs has been explored consistently in such a large
range of wavelength at intermediate redshifts. We exploit very deep HST
photometry, ranging from the observed B-band to the H-band, and VLT/MUSE
integral field spectroscopy. We improve the structural parameters estimation we
performed in a previous work (Tortorelli et al. 2018) by means of a newly
developed Python package called morphofit (Tortorelli&Mercurio 2023). With its
use on cluster ETGs, we find that the KR slopes smoothly increase with
wavelength from the optical to the near-infrared bands in all three clusters,
with the intercepts getting fainter at lower redshifts due to the passivisation
of the ETGs population. The slope trend is consistent with previous findings at
lower redshifts. The slope increase with wavelength implies that smaller size
ETGs are more centrally concentrated than larger size ETGs in the near-infrared
with respect to the optical regime. Since different bands probe different
stellar populations in galaxies, the slope increase also implies that smaller
ETGs have stronger internal gradients with respect to larger ETGs.Comment: Submitted to Astronomy and Astrophysics in the form of letter to the
Editor, 5 pages, 1 figure, 1 tabl
Cultural Expertise and Socio-legal Studies: Introduction
International audienceEmerald is a global publisher linking research and practice to the benefit of society. The company manages a portfolio of more than 290 journals and over 2,350 books and book series volumes, as well as providing an extensive range of online products and additional customer resources and services. Emerald is both COUNTER 4 and TRANSFER compliant. The organization is a partner of the Committee on Publication Ethics (COPE) and also works with Portico and the LOCKSS initiative for digital archive preservation
CLASH: z ~ 6 young galaxy candidate quintuply lensed by the frontier field cluster RXC J2248.7-4431
We present a quintuply lensed z ~ 6 candidate discovered in the field of the
galaxy cluster RXC J2248.7-4431 (z ~ 0.348) targeted within the Cluster Lensing
and Supernova survey with Hubble (CLASH) and selected in the deep HST Frontier
Fields survey. Thanks to the CLASH 16-band HST imaging, we identify the
quintuply lensed z ~ 6 candidate as an optical dropout in the inner region of
the cluster, the brightest image having magAB=24.81+-0.02 in the f105w filter.
We perform a detailed photometric analysis to verify its high-z and lensed
nature. We get as photometric redshift z_phot ~ 5.9, and given the extended
nature and NIR colours of the lensed images, we rule out low-z early type and
galactic star contaminants. We perform a strong lensing analysis of the
cluster, using 13 families of multiple lensed images identified in the HST
images. Our final best model predicts the high-z quintuply lensed system with a
position accuracy of 0.8''. The magnifications of the five images are between
2.2 and 8.3, which leads to a delensed UV luminosity of L_1600 ~ 0.5L*_1600 at
z=6. We also estimate the UV slope from the observed NIR colours, finding a
steep beta=-2.89+-0.38. We use singular and composite stellar population SEDs
to fit the photometry of the hiz candidate, and we conclude that it is a young
(age <300 Myr) galaxy with mass of M ~ 10^8Msol, subsolar metallicity
(Z<0.2Zsol) and low dust content (AV ~ 0.2-0.4).Comment: 21 pages, 13 figures, 6 tables, submitted to MNRAS on 11 Aug 2013,
accepted on 23 Nov 201
CLASH-VLT: The stellar mass function and stellar mass density profile of the z=0.44 cluster of galaxies MACS J1206.2-0847
Context. The study of the galaxy stellar mass function (SMF) in relation to
the galaxy environment and the stellar mass density profile, rho(r), is a
powerful tool to constrain models of galaxy evolution. Aims. We determine the
SMF of the z=0.44 cluster of galaxies MACS J1206.2-0847 separately for passive
and star-forming (SF) galaxies, in different regions of the cluster, from the
center out to approximately 2 virial radii. We also determine rho(r) to compare
it to the number density and total mass density profiles. Methods. We use the
dataset from the CLASH-VLT survey. Stellar masses are obtained by SED fitting
on 5-band photometric data obtained at the Subaru telescope. We identify 1363
cluster members down to a stellar mass of 10^9.5 Msolar. Results. The whole
cluster SMF is well fitted by a double Schechter function. The SMFs of cluster
SF and passive galaxies are statistically different. The SMF of the SF cluster
galaxies does not depend on the environment. The SMF of the passive population
has a significantly smaller slope (in absolute value) in the innermost (<0.50
Mpc), highest density cluster region, than in more external, lower density
regions. The number ratio of giant/subgiant galaxies is maximum in this
innermost region and minimum in the adjacent region, but then gently increases
again toward the cluster outskirts. This is also reflected in a decreasing
radial trend of the average stellar mass per cluster galaxy. On the other hand,
the stellar mass fraction, i.e., the ratio of stellar to total cluster mass,
does not show any significant radial trend. Conclusions. Our results appear
consistent with a scenario in which SF galaxies evolve into passive galaxies
due to density-dependent environmental processes, and eventually get destroyed
very near the cluster center to become part of a diffuse intracluster medium.Comment: A&A accepted, 15 pages, 13 figure
Boundary lubrication properties of materials with expansive freezing
We have performed molecular dynamics simulations of solid-solid contacts
lubricated by a model fluid displaying many of the properties of water,
particularly its expansive freezing. Near the region where expansive freezing
occurs, the lubricating film remains fluid, and the friction force decreases
linearly as the shear velocity is reduced. No sign of stick-slip motion is
observed even at the lowest velocities. We give a simple interpretation of
these results, and suggest that in general good boundary lubrication properties
will be found in the family of materials with expansive freezing.Comment: Version to appear in Phys. Rev. Let
CLASH-VLT: spectroscopic confirmation of a z=6.11 quintuply lensed galaxy in the Frontier Fields Cluster RXC J2248.7-4431
We present VIsible Multi-Object Spectrograph (VIMOS) observations of a z 6
galaxy quintuply imaged by the Frontier Fields galaxy cluster RXC J2248.7-4431
(z=0.348). This sub-L^*, high-z galaxy has been recently discovered by Monna et
al. (2013) using dropout techniques with the 16-band HST photometry acquired as
part of the Cluster Lensing And Supernova survey with Hubble (CLASH). Obtained
as part of the CLASH-VLT survey, the VIMOS medium-resolution spectra of this
source show a very faint continuum between ~8700A and ~9300A and a prominent
emission line at 8643A, which can be readily identified with Lyman-alpha at
z=6.110. The emission line exhibits an asymmetric profile, with a more
pronounced red wing. The rest-frame equivalent width of the line is EW=79+-10A.
After correcting for magnification, the star-formation rate (SFR) estimated
from the Lya line is SFR(Lya)=11 M_{sol}/yr and that estimated from the UV data
is SFR(UV)=3 M_{sol}/yr. We estimate that the effective radius of the source is
R_e6
M_{sol}/yr/kpc^2 and, using the Kennicutt-Schmidt relation, a gas surface mass
density Sigma_{gas}>10^3 M_{sol}/pc^2. Our results support the idea that this
magnified, distant galaxy is a young and compact object with 0.4 L^* at z=6,
with comparable amount of mass in gas and stars. Future follow-up observations
with ALMA will provide valuable insight into the SFR and molecular gas content
of this source. In the spirit of the Frontier Fields initiative, we also
publish the redshifts of several multiply imaged sources and other background
objects which will help improving the strong lensing model of this galaxy
cluster.Comment: 4 pages, 3 figures, 1 table, Accepted for publication in A&A (minor
changes, published version
CLASH-VLT: The mass, velocity-anisotropy, and pseudo-phase-space density profiles of the z=0.44 galaxy cluster MACS 1206.2-0847
We use an unprecedented data-set of about 600 redshifts for cluster members,
obtained as part of a VLT/VIMOS large programme, to constrain the mass profile
of the z=0.44 cluster MACS J1206.2-0847 over the radial range 0-5 Mpc (0-2.5
virial radii) using the MAMPOSSt and Caustic methods. We then add external
constraints from our previous gravitational lensing analysis. We invert the
Jeans equation to obtain the velocity-anisotropy profiles of cluster members.
With the mass-density and velocity-anisotropy profiles we then obtain the first
determination of a cluster pseudo-phase-space density profile. The kinematics
and lensing determinations of the cluster mass profile are in excellent
agreement. This is very well fitted by a NFW model with mass M200=(1.4 +- 0.2)
10^15 Msun and concentration c200=6 +- 1, only slightly higher than theoretical
expectations. Other mass profile models also provide acceptable fits to our
data, of (slightly) lower (Burkert, Hernquist, and Softened Isothermal Sphere)
or comparable (Einasto) quality than NFW. The velocity anisotropy profiles of
the passive and star-forming cluster members are similar, close to isotropic
near the center and increasingly radial outside. Passive cluster members follow
extremely well the theoretical expectations for the pseudo-phase-space density
profile and the relation between the slope of the mass-density profile and the
velocity anisotropy. Star-forming cluster members show marginal deviations from
theoretical expectations. This is the most accurate determination of a cluster
mass profile out to a radius of 5 Mpc, and the only determination of the
velocity-anisotropy and pseudo-phase-space density profiles of both passive and
star-forming galaxies for an individual cluster [abridged]Comment: A&A in press; 22 pages, 19 figure
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