3,312 research outputs found
Spitzer bright, UltraVISTA faint sources in COSMOS: the contribution to the overall population of massive galaxies at z=3-7
We have analysed a sample of 574 Spitzer 4.5 micron-selected galaxies with
[4.5]24 (AB) over the UltraVISTA ultra-deep COSMOS field. Our
aim is to investigate whether these mid-IR bright, near-IR faint sources
contribute significantly to the overall population of massive galaxies at
redshifts z>=3. By performing a spectral energy distribution (SED) analysis
using up to 30 photometric bands, we have determined that the redshift
distribution of our sample peaks at redshifts z~2.5-3.0, and ~32% of the
galaxies lie at z>=3. We have studied the contribution of these sources to the
galaxy stellar mass function (GSMF) at high redshifts. We found that the
[4.5]24 galaxies produce a negligible change to the GSMF
previously determined for Ks_auto<24 sources at 3=<z<4, but their contribution
is more important at 4=~50% of the galaxies with stellar
masses Mst>~6 x 10^10 Msun. We also constrained the GSMF at the highest-mass
end (Mst>~2 x 10^11 Msun) at z>=5. From their presence at 5=<z<6, and virtual
absence at higher redshifts, we can pinpoint quite precisely the moment of
appearance of the first most massive galaxies as taking place in the ~0.2 Gyr
of elapsed time between z~6 and z~5. Alternatively, if very massive galaxies
existed earlier in cosmic time, they should have been significantly
dust-obscured to lie beyond the detection limits of current, large-area, deep
near-IR surveys.Comment: 18 pages, 15 figures, 4 tables. Updated to match version in press at
the Ap
Sub-parsec-scale Accleration of the Radio Jet in the Powerful Radio Galaxy NGC 6251
In order to investigate the genesis of powerful radio jet, we have mapped the
central 10 pc region of the nearby radio galaxy NGC 6251 with a 0.2 pc
resolution using Very Long Baseline Interferometer (VLBI) at two radio
frequencies, 5 GHz and 15 GHz, we have found the sub-parsec-scale counterjet
for the first time in this radio galaxy. This discovery allows us to
investigate the jet acceleration based on the relativistic beaming model.Comment: 7 pages with 7 figures. To appear in PASJ, 52, No. 5, Oct. 25, 200
Stochastic Interactions of Two Brownian Hard Spheres in the Presence of Depletants
A quantitative analysis is presented for the stochastic interactions of a
pair of Brownian hard spheres in non-adsorbing polymer solutions. The hard
spheres are hypothetically trapped by optical tweezers and allowed for random
motion near the trapped positions. The investigation focuses on the long-time
correlated Brownian motion. The mobility tensor altered by the polymer
depletion effect is computed by the boundary integral method, and the
corresponding random displacement is determined by the fluctuation-dissipation
theorem. From our computations it follows that the presence of depletion layers
around the hard spheres has a significant effect on the hydrodynamic
interactions and particle dynamics as compared to pure solvent and pure polymer
solution (no depletion) cases. The probability distribution functions of random
walks of the two interacting hard spheres that are trapped clearly shifts due
to the polymer depletion effect. The results show that the reduction of the
viscosity in the depletion layers around the spheres and the entropic force due
to the overlapping of depletion zones have a significant influence on the
correlated Brownian interactions.Comment: 30 pages, 9 figures, 1 appendix, 40 formulas inside the text, 5
formulas in appendi
Orbital Magnetism of 2D Chaotic Lattices
We study the orbital magnetism of 2D lattices with chaotic motion of
electrons withing a primitive cell. Using the temperature diagrammatic
technique we evaluate the averaged value and rms fluctuation of magnetic
response in the diffusive regime withing the model of non-interacting
electrons. The fluctuations of magnetic susceptibility turn out to be large and
at low temperature can be of the order of , where
is the Fermi wavevector, is the mean free path, and is
the Landau susceptibility. In the certain region of magnetic fields the
paramagnetic contribution to the averaged response is field independent and
larger than the absolute value of Landau response.Comment: 6 pages, Latex file, figures available upon reques
Competing Fractional Quantum Hall and Electron Solid Phases in Graphene
We report experimental observation of the reentrant integer quantum Hall
effect in graphene, appearing in the N2 Landau level. Similar to
high-mobility GaAs/AlGaAs heterostructures, the effect is due to a competition
between incompressible fractional quantum Hall states, and electron solid
phases. The tunability of graphene allows us to measure the - phase
diagram of the electron-solid phase. The hierarchy of reentrant states suggest
spin and valley degrees of freedom play a role in determining the ground state
energy. We find that the melting temperature scales with magnetic field, and
construct a phase diagram of the electron liquid-solid transition
Goldstone modes in Lyapunov spectra of hard sphere systems
In this paper, we demonstrate how the Lyapunov exponents close to zero of a
system of many hard spheres can be described as Goldstone modes, by using a
Boltzmann type of approach. At low densities, the correct form is found for the
wave number dependence of the exponents as well as for the corresponding
eigenvectors in tangent-space. The predicted values for the Lyapunov exponents
belonging to the transverse mode are within a few percent of the values found
in recent simulations, the propagation velocity for the longitudinal mode is
within 1%, but the value for the Lyapunov exponent belonging to the
longitudinal mode deviates from the simulations by 30%. For higher densities,
the predicted values deviate more from the values calculated in the
simulations. These deviations may be due to contributions from ring collisions
and similar terms, which, even at low densities, can contribute to the leading
order.Comment: 12 pages revtex, 5 figures, accepted by Physical Review
Fine structure of -excitons in multilayers of transition metal dichalcogenides
Reflectance and magneto-reflectance experiments together with theoretical
modelling based on the approach have been employed to study
the evolution of direct bandgap excitons in MoS layers with a thickness
ranging from mono- to trilayer. The extra excitonic resonances observed in
MoS multilayers emerge as a result of the hybridization of Bloch states of
each sub-layer due to the interlayer coupling. The properties of such excitons
in bi- and trilayers are classified by the symmetry of corresponding crystals.
The inter- and intralayer character of the reported excitonic resonances is
fingerprinted with the magneto-optical measurements: the excitonic -factors
of opposite sign and of different amplitude are revealed for these two types of
resonances. The parameters describing the strength of the spin-orbit
interaction are estimated for bi- and trilayer MoS.Comment: 14 pages, 10 figure
Evolution of the Fraction of Clumpy Galaxies at 0.2<z<1.0 in the COSMOS field
Using the Hubble Space Telescope/Advanced Camera for Surveys data in the
COSMOS field, we systematically searched clumpy galaxies at 0.2<z<1.0 and
investigated the fraction of clumpy galaxies and its evolution as a function of
stellar mass, star formation rate (SFR), and specific SFR (SSFR). The fraction
of clumpy galaxies in star-forming galaxies with Mstar > 10^9.5 Msun decreases
with time from ~0.35 at 0.8<z<1.0 to ~0.05 at 0.2<z<0.4 irrespective of the
stellar mass, although the fraction tends to be slightly lower for massive
galaxies with Mstar > 10^10.5 Msun at each redshift. On the other hand, the
fraction of clumpy galaxies increases with increasing both SFR and SSFR in all
the redshift ranges we investigated. In particular, we found that the SSFR
dependences of the fractions are similar among galaxies with different stellar
masses, and the fraction at a given SSFR does not depend on the stellar mass in
each redshift bin. The evolution of the fraction of clumpy galaxies from z~0.9
to z~0.3 seems to be explained by such SSFR dependence of the fraction and the
evolution of SSFRs of star-forming galaxies. The fraction at a given SSFR also
appears to decrease with time, but this can be due to the effect of the
morphological K-correction. We suggest that these results are understood by the
gravitational fragmentation model for the formation of giant clumps in disk
galaxies, where the gas mass fraction is a crucial parameter.Comment: 14 Pages, 13 Figures, 1 Table, Accepted for publication in Ap
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