364 research outputs found
The role of E+A and post-starburst galaxies â I. Models and model results
âThe definitive version is available at www3.interscience.wiley.com '. Copyright Royal Astronomical Society. DOI: 10.1111/j.1365-2966.2009.14416.xDifferent compositions of galaxy types in the field in comparison to galaxy clusters as described by the morphologyâdensity relation in the local universe are interpreted as a result of transformation processes from late- to early-type galaxies. This interpretation is supported by the ButcherâOemler effect. We investigate E+A galaxies as an intermediate state between late-type galaxies in low-density environments and early-type galaxies in high-density environment to constrain the possible transformation processes. For this purpose, we model a grid of post-starburst galaxies by inducing a burst and/or a halting of star formation on the normal evolution of spiral galaxies with our galaxy evolution code galev. From our models, we find that the common E+A criteria exclude a significant number of post-starburst galaxies, and propose that comparing their spectral energy distributions leads to a more sufficient method to investigate post-starburst galaxies. We predict that a higher number of E+A galaxies in the early universe cannot be ascribed solely to a higher number of starburst, but is a result of a lower metallicity and a higher burst strength due to more gas content of the galaxies in the early universe. We find that even galaxies with a normal evolution without a starburst have an HÎŽ-strong phase at early galaxy ages.Peer reviewe
Double Photoproduction off the Proton at Threshold
The reaction has been measured using the TAPS
BaF calorimeter at the tagged photon facility of the Mainz Microtron
accelerator. Chiral perturbation theory (ChPT) predicts that close to threshold
this channel is significantly enhanced compared to double pion final states
with charged pions. In contrast to other reaction channels, the lower order
tree terms are strongly suppressed in 2 photoproduction. The consequence
is the dominance of pion loops in the 2 channel close to threshold - a
result that opens new prospects for the test of ChPT and in particular its
inherent loop terms. The present measurement is the first which is sensitive
enough for a conclusive comparison with the ChPT calculation and is in
agreement with its prediction. The data also show good agreement with a
calculation in the unitary chiral approach.Comment: Submitted to PL
Baryon magnetic moments in the external field method
We present a calculation of the magnetic moments of the baryon octet and
decuplet using the external field method and standard Wilson gauge and fermion
actions in the quenched approximation. Progressively smaller static magnetic
fields are introduced on a latticeat beta=6.0 and the pion mass is
probed down to about 500 MeV. Magnetic moments are extracted from the linear
response of the masses to the external field.Comment: Lattice2004 (weak matrix elements), 3 pages, 8 figure
Static observables of relativistic three-fermion systems with instantaneous interactions
We show that static properties like the charge radius and the magnetic moment
of relativistic three-fermion bound states with instantaneous interactions can
be formulated as expectation values with respect to intrinsically defined
wavefunctions. The resulting operators can be given a natural physical
interpretation in accordance with relativistic covariance. We also indicate how
the formalism may be generalized to arbitrary moments. The method is applied to
the computation of static baryon properties with numerical results for the
nucleon charge radii and the baryon octet magnetic moments. In addition we make
predictions for the magnetic moments of some selected nucleon resonances and
discuss the decomposition of the nucleon magnetic moments in contributions of
spin and angular momentum, as well as the evolution of these contributions with
decreasing quark mass.Comment: 13 pages, including 2 figures and 3 tables, submitted to Eur.Phys.J.
Filamentary Star Formation in NGC 1275
We examine the star formation in the outer halo of NGC~1275, the central
galaxy in the Perseus cluster (Abell 426), using far ultraviolet and optical
images obtained with the Hubble Space Telescope. We have identified a
population of very young, compact star clusters with typical ages of a few Myr.
The star clusters are organised on multiple-kiloparsec scales. Many of these
star clusters are associated with "streaks" of young stars, the combination of
which has a cometary appearance. We perform photometry on the star clusters and
diffuse stellar streaks, and fit their spectral energy distributions to obtain
ages and masses. These young stellar populations appear to be normal in terms
of their masses, luminosities and cluster formation efficiency; <10% of the
young stellar mass is located in star clusters. Our data suggest star formation
is associated with the evolution of some of the giant gas filaments in NGC~1275
that become gravitationally unstable on reaching and possibly stalling in the
outer galaxy. The stellar streaks then could represent stars moving on
ballistic orbits in the potential well of the galaxy cluster. We propose a
model where star-forming filaments, switched on ~50~Myr ago and are currently
feeding the growth of the NGC~1275 stellar halo at a rate of ~2-3 solar masses
per year. This type of process may also build stellar halos and form isolated
star clusters in the outskirts of youthful galaxies.Comment: 15 pages, 10 figures, accepted for publication in MNRA
The reaction and the magnetic dipole moment of the resonance
The reaction has been measured with
the TAPS calorimeter at the Mainz Microtron accelerator facility MAMI for
energies between = 1221--1331 MeV. Cross sections differential in
angle and energy have been determined for all particles in the final state in
three bins of the excitation energy. This reaction channel provides access to
the magnetic dipole moment of the resonance and, for the
first time, a value of has been extracted
Photoproduction of eta-mesic 3He
The photoproduction of eta-mesic 3He has been investigated using the TAPS
calorimeter at the Mainz Microtron accelerator facility MAMI. The total
inclusive cross section for the reaction gamma+3He->eta+X has been measured for
photon energies from threshold to 820 MeV. The total and angular differential
coherent eta cross sections have been extracted up to energies of 745 MeV. A
resonance-like structure just above the eta production threshold with an
isotropic angular distribution suggests the existence of a resonant quasi-bound
state. This is supported by studies of a competing decay channel of such a
quasi-bound eta-mesic nucleus into pi^0+p+X. A binding energy of (-4.4+-4.2)
MeV and a width of (25.6+-6.1) MeV is deduced for the quasi-bound eta-mesic
state in 3He.Comment: v1: 4 pages, 4 figures, submitted to PRL; v2: minor revisions and
corrections, new figure added, 4 pages, 5 figs; v3: minor change
Supersoft X-ray sources identified with Be binaries in the Magellanic Clouds
We investigated four luminous supersoft X-ray sources (SSS) in the Magellanic
Clouds suspected to have optical counterparts of Be spectral type. If the
origin of the X-rays is in a very hot atmosphere heated by hydrogen burning in
accreted envelopes of white dwarfs (WDs), like in the majority of SSS, these
objects are close binaries, with very massive WD primaries. Using the South
African Large Telescope (SALT), we obtained the first optical spectra of the
proposed optical counterparts of two candidate Be stars associated with SUZAKU
J0105-72 and XMMU J010147.5-715550, respectively a transient and a recurrent
SSS, and confirmed the proposed Be classification and Small Magellanic Clouds
membership. We also obtained new optical spectra of two other Be stars proposed
as optical counterparts of the transient SSS XMMU J052016.0-692505 and
MAXI-J0158-744. The optical spectra with double peaked emission line profiles,
are typical of Be stars and present characteristics similar to many high mass
X-ray binaries with excretion disks, truncated by the tidal interaction with a
compact object. The presence of a massive WD that sporadically ignites nuclear
burning, accreting only at certain orbital or evolutionary phases, explains the
supersoft X-ray flares. We measured equivalent widths and distances between
lines' peaks, and investigated the variability of the prominent emission lines'
profiles. The excretion disks seem to be small in size, and are likely to be
differentially rotating. We discuss possible future observations and the
relevance of these objects as a new class of type Ia supernovae progenitors.Comment: Accepted for publication in teh Astrophysical Journa
Detecting metal-rich intermediate-age globular clusters in NGC4570 using K-band photometry
âThe original publication is available at www.springerlink.comâ. Copyright Springer. DOI: 10.1007/s10509-009-0093-8Globular cluster systems (GCSs) of most early-type galaxies feature two peaks in their optical colour distributions. Blue-peak globular clusters (GCs) are believed to be old and metal-poor, whereas the ages, metallicities, and the origin of the red-peak GCs are still being debated. We obtained deep K-band photometry and combined it with Hubble Space Telescope observations in g and z to yield a full spectral energy distribution from the optical to the near-infrared. This now allows us to break the ageâmetallicity degeneracy. We used our evolutionary synthesis models galev for star clusters to compute a large grid of models with different metallicities and a wide range of ages. Comparing these models to our observations revealed a large population of intermediate-age (1â3 Gyr) and metal-rich (âsolar-metallicity) GCs, that will give us further insights into the formation history of this galaxy.Peer reviewe
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