1,795 research outputs found
The evolution of quiescent galaxies at high redshifts (z ≥ 1.4)
The goal of this work is to study the evolution of high-redshift (z ≥ 1.4) quiescent galaxies over an effective area of ~ 1.7 deg^2 in the COSMOS field. Galaxies have been divided according to their star formation activity and the evolution of the different populations, in particular of the quiescent galaxies, has been investigated in detail. We have studied an IRAC (ma_( 3.6 μm) 2.5 (log_ρ[M_⊙ Mpc^(−3)]~ 6), meaning that efficient star formation had to take place before that time
Hidden AGN in dwarf galaxies revealed by MaNGA: light echoes, off-nuclear wanderers, and a new broad-line AGN
Active galactic nuclei (AGN) in dwarf galaxies could possibly host the relics
of those early Universe seed black holes that did not grow into supermassive
black holes. Using MaNGA integral field unit (IFU) spectroscopy we have found a
sample of 37 dwarf galaxies that show AGN ionisation signatures in
spatially-resolved emission line diagnostic diagrams. The AGN signatures are
largely missed by integrated emission line diagnostics for 23 of them. The
bolometric luminosity of these 23 new AGN candidates is erg
s, fainter than that of single-fiber SDSS AGN, X-ray AGN, and radio AGN
in dwarf galaxies, which stands IFU spectroscopy as a powerful tool for
identifying hidden and faint AGN in dwarf galaxies. The AGN emission is in most
cases offset from the optical center of the dwarf galaxy and shows a symmetric
morphology, which indicates that either the AGN are off-nuclear, that the
central emission of the galaxy is dominated by star formation, or that the AGN
are turned-off and we are observing a past ionisation burst. One of the new AGN
shows a broad H emission line component, from which we derive a black
hole mass in the realm of intermediate-mass black holes. This constitutes the
first hidden type 1 AGN discovered in a dwarf galaxy based on IFU spectroscopy.
The finding of this sample of hidden and faint AGN has important implications
for population studies of AGN in dwarf galaxies and for seed black hole
formation models.Comment: 13 pages, 5 figures, accepted for publication in ApJ Letter
Frenkel Excitons in Random Systems With Correlated Gaussian Disorder
Optical absorption spectra of Frenkel excitons in random one-dimensional
systems are presented. Two models of inhomogeneous broadening, arising from a
Gaussian distribution of on-site energies, are considered. In one case the
on-site energies are uncorrelated variables whereas in the second model the
on-site energies are pairwise correlated (dimers). We observe a red shift and a
broadening of the absorption line on increasing the width of the Gaussian
distribution. In the two cases we find that the shift is the same, within our
numerical accuracy, whereas the broadening is larger when dimers are
introduced. The increase of the width of the Gaussian distribution leads to
larger differences between uncorrelated and correlated disordered models. We
suggest that this higher broadening is due to stronger scattering effects from
dimers.Comment: 9 pages, REVTeX 3.0, 3 ps figures. To appear in Physical Review
Three-dimensional effects on extended states in disordered models of polymers
We study electronic transport properties of disordered polymers in the
presence of both uncorrelated and short-range correlated impurities. In our
procedure, the actual physical potential acting upon the electrons is replaced
by a set of nonlocal separable potentials, leading to a Schr\"odinger equation
that is exactly solvable in the momentum representation. We then show that the
reflection coefficient of a pair of impurities placed at neighboring sites
(dimer defect) vanishes for a particular resonant energy. When there is a
finite number of such defects randomly distributed over the whole lattice, we
find that the transmission coefficient is almost unity for states close to the
resonant energy, and that those states present a very large localization
length. Multifractal analysis techniques applied to very long systems
demonstrate that these states are truly extended in the thermodynamic limit.
These results reinforce the possibility to verify experimentally theoretical
predictions about absence of localization in quasi-one-dimensional disordered
systems.Comment: 16 pages, REVTeX 3.0, 5 figures on request from FDA
([email protected]). Submitted to Phys. Rev. B. MA/UC3M/09/9
Bridging the gap in the mass-size relation of compact galaxies with MaNGA
We present the analysis of the full MaNGA DR17 sample to characterize its
population of compact galaxies. We focus on galaxies that fill the stellar mass
(M) gap between compact elliptical galaxies (cEs; ) and compact massive galaxies
(CMGs; ). We study their
stellar populations and kinematics to reveal how their properties depend on
stellar mass. We select compact galaxies in the MaNGA DR17 sample according to
their effective radius () and stellar mass. 37 galaxies fulfill our
selection criteria in the bridging region between cEs and CMGs. We derive their
kinematics and stellar population parameters from the stacked spectra at
1~ using a full spectral fitting routine. We then classify the selected
compact galaxies in three main groups based on their stellar population
properties. One of the groups shows characteristics compatible with relic
galaxies, i.e. galaxies that have remained mostly unchanged since their early
formation epoch (). Another group shows more extended and continuous
star formation histories (SFHs). The third group shows a low star-forming rate
at initial times, which increases at around Gyr. We compare the derived
properties of the selected galaxies with those of previously studied compact
galaxies at different mass ranges. The selected galaxies successfully fill the
mass gap between cEs and CMGs. Their properties are compatible with the
assumption that the scaling relations of compact galaxies at different mass
ranges are related, although galaxies in the first group are clear outliers in
the fundamental plane, suggesting different formation mechanisms for this relic
population.Comment: 16 pages, 14 figures, 2 table
Link between the chromospheric network and magnetic structures of the corona
Recent work suggested that the traditional picture of the corona above the
quiet Sun being rooted in the magnetic concentrations of the chromospheric
network alone is strongly questionable. Building on that previous study we
explore the impact of magnetic configurations in the photosphere and the low
corona on the magnetic connectivity from the network to the corona.
Observational studies of this connectivity are often utilizing magnetic field
extrapolations. However, it is open to which extent such extrapolations really
represent the connectivity found on the Sun, as observations are not able to
resolve all fine scale magnetic structures. The present numerical experiments
aim at contributing to this question. We investigated random
salt-and-pepper-type distributions of kilo-Gauss internetwork flux elements
carrying some to Mx, which are hardly distinguishable by
current observational techniques. These photospheric distributions are then
extrapolated into the corona using different sets of boundary conditions at the
bottom and the top. This allows us to investigate the fraction of network flux
which is connected to the corona, as well as the locations of those coronal
regions which are connected to the network patches. We find that with current
instrumentation one cannot really determine from observations, which regions on
the quiet Sun surface, i.e. in the network and internetwork, are connected to
which parts of the corona through extrapolation techniques. Future
spectro-polarimetric instruments, such as with Solar B or GREGOR, will provide
a higher sensitivity, and studies like the present one could help to estimate
to which extent one can then pinpoint the connection from the chromosphere to
the corona.Comment: 8 pages, 5 figures, acceped for publication in A&
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