title: The Low Frequency Instrument in the ESA Planck mission

abstract:
  Measurements of the cosmic microwave background (CMB) allow high precision
observation of the cosmic plasma at redshift z~1100. After the success of the
NASA satellite COBE, that in 1992 provided the first detection of the CMB
anisotropy, results from many ground-based and balloon-borne experiments have
showed a remarkable consistency between different results and provided
quantitative estimates of fundamental cosmological properties. During the
current year the team of the NASA WMAP satellite has released the first
improved full-sky maps of the CMB since COBE, leading to a deeper insight in
the origin and evolution of the Universe. The ESA satellite Planck, scheduled
for launch in 2007, is designed to provide the ultimate measurement of the CMB
temperature anisotropy over the full sky, with an accuracy that will be limited
only by astrophysical foregrounds, and robust detection of polarisation
anisotropy. Planck will observe the sky with two instruments over a wide
spectral band (the Low Frequency Instrument, based on coherent radiometers,
from 30 to 70 GHz and the High Frequency Instrument, based on bolometric
detectors, from 100 to 857 GHz). The mission performances will improve
dramatically the scientific return compared to WMAP. Furthermore the LFI
radiometers (as well as some of the HFI bolometers) are intrinsically sensitive
to polarisation so that by combining the data from different receivers it will
be possible to measure accurately the E mode and to detect the B mode of the
polarisation power spectrum. Planck sensitivity will offer also the possibility
to detect the non-Gaussianities imprinted in the CMB.


title: Simulations of dust-trapping vortices in protoplanetary discs

abstract:
  Local three-dimensional shearing box simulations of the compressible coupled
dust-gas equations are used in the fluid approximation to study the evolution
of different initial vortex configurations in a protoplanetary disc and their
dust-trapping capabilities. The initial conditions for the gas are derived from
an analytic solution to the compressible Euler equation and the continuity
equation. The solution is valid if there is a vacuum outside the vortex. In the
simulations the vortex is either embedded in a hot corona, or it is extended in
a cylindrical fashion in the vertical direction. Both configurations are found
to survive for at least one orbit and lead to accumulation of dust inside the
vortex. This confirms earlier findings that dust accumulates in anticyclonic
vortices, indicating that this is a viable mechanism for planetesimal
formation.


title:
The ESO Nearby Abell Cluster Survey. XII. The mass and
  mass-to-light-ratio profiles of rich clusters

abstract:
  We determine the mass profile of an ensemble cluster built from 3056 galaxies
in 59 nearby clusters observed in the ESO Nearby Abell Cluster Survey. The mass
profile is derived from the distribution and kinematics of the Early-type
(elliptical and S0) galaxies only, which are most likely to meet the conditions
for the application of the Jeans equation. We assume that the Early-type
galaxies have isotropic orbits, as supported by the shape of their velocity
distribution. The brightest ellipticals (with M_R < -22+5 log h), and the
Early-type galaxies in subclusters are excluded from the sample. Application of
the Jeans equation yields a non-parametric estimate of the cumulative mass
profile M(<r), which has a logarithmic slope of -2.4 +/- 0.4 in the density
profile at the virial radius. We compare our result with several analytical
models from the literature (NFW, Moore et al. 1999, softened isothermal sphere,
and Burkert 1995) and find that all are acceptable. However, our data do not
provide compelling evidence for the existence of a core; as a matter of fact,
the best-fitting core models have core-radii well below 100/h kpc. The upper
limit we put on the size of the core-radius provides a constraint for the
scattering cross-section of dark matter particles. The total-mass density
appears to be traced remarkably well by the luminosity density of the
Early-type galaxies. On the contrary, the luminosity density of the brightest
ellipticals increases faster towards the center than the mass density, while
the luminosity density profiles of the early and late spirals are somewhat
flatter than the mass density profile. (Abridged)


title:
Evaluating GAIA performances on eclipsing binaries. III. Orbits and
  stellar parameters for UW LMi, V432 Aur and CN Lyn

abstract:
  The orbits and physical parameters of three detached F and G-type eclipsing
binaries have been derived combining Hipparcos H(P) photometry with 8480-8740
Ang ground-based spectroscopy, simulating the photometric+spectroscopic
observations that the GAIA mission will obtain. Tycho B(T) and V(T) light
curves are too noisy to be modeled for the three targets, and only mean Tycho
colors are retained to constrain the temperature. No previous combined
photometric+spectroscopic solution exists in literature for any of the three
targets. Quite remarkably, CN Lyn turned out to be an equal masses F5 triple
system. Distances from the orbital solutions agree within the astrometric error
with the Hipparcos parallaxes.


title: First evidence for dusty disks around Herbig Be stars

abstract:
  We have carried out a high-sensitivity search for circumstellar disks around
Herbig Be stars in the continuum at 1.4mm and 2.7mm using the IRAM
interferometer at the Plateau de Bure (PdBI) . In this letter, we report data
on three well studied B0 stars, MWC 1080, MWC 137 and R Mon. The two latter
have also been observed in the continuum at 0.7 cm and 1.3 cm using the NRAO
Very Large Array (VLA) . We report the detection of circumstellar disks around
MWC 1080 and R Mon with masses of Md ~ 0.003 and 0.01 Msun, respectively, while
for MWC 137 we estimate a disk mass upper limit of 0.007 Msun. Our results show
that the ratio Md/M* is at least an order of magnitude lower in Herbig Be stars
than in Herbig Ae and T Tauri stars.


title: Non-Gaussian velocity shears in the environment of low mass dense cores

abstract:
  We report on a novel kind of small scale structure in molecular clouds found
in IRAM-30m and CSO maps of 12CO and 13CO lines around low mass starless dense
cores. These structures come to light as the locus of the extrema of velocity
shears in the maps, computed as the increments at small scale (about 0.02 pc)
of the line velocity centroids. These extrema populate the non-Gaussian wings
of the shear probability distribution function (shear-PDF) built for each map.
They form elongated structures of variable thickness, ranging from less than
0.02 pc for those unresolved, up to 0.08 pc. They are essentially pure velocity
structures. We propose that these small scale structures of velocity shear
extrema trace the locations of enhanced dissipation in interstellar turbulence.
In this picture, we find that a significant fraction of the turbulent energy
present in the field would be dissipating in structures filling less than a few
% of the cloud volume.


title: Telescopic system with a rotating objective element

abstract:
  The angular resolution is tha ability of a telescope to render detail: the
higher the resolution the finer is the detail. it is, together with the
aperture, the most important characteristic of telescopes. We propose a new
construction of telescopes with improved ratio of angular resolution and area
of the primary optical element (mirror or lense). For this purpose we use the
rotation of the primary optical element with one dominating dimension. The
length of the dominating dimension of the primary optical element determines
the angular resolution. During the rotation a sequence of images is stored in a
computer and the images of observed objects can be reconstructed using a
relatively simple software. The angular resolution is determined by the maximal
length of the primary optical element of the system. This construction of
telescopic systems allows to construct telescopes of high resolution with lower
weight and fraction of usual costs.


title: Formaldehyde emission from low mass protostars

abstract:
  We present a survey of the formaldehyde emission in nine class 0 protostars
obtained with the IRAM 30m and the JCMT millimeter telescopes. Using a detailed
radiative transfer code of the envelopes surrounding the protostars, we show
that all but one of the observed objects show an inner warm evaporation region
where the formaldehyde is much more abundant (up to three orders of magnitude)
than in the outer cold part. The largest inner formaldehyde abundances are
associated with the sources having the lowest submillimetric to bolometric
luminosity ratio, i.e. with sources closer to the class I border. These
abundances are compared with predictions from recent models of hot core
chemistry.


title: The Structure of Cold Molecular Cloud Cores

abstract:
  A brief summary is presented of our current knowledge of the structure of
cold molecular cloud cores that do not contain protostars, sometimes known as
starless cores. The most centrally condensed starless cores are known as
pre-stellar cores. These cores probably represent observationally the initial
conditions for protostellar collapse that must be input into all models of star
formation. The current debate over the nature of core density profiles is
summarised. A cautionary note is sounded over the use of such profiles to
ascertain the equilibrium status of cores. The magnetic field structure of
pre-stellar cores is also discussed.


title: Unveiling the Inner Disk Structure of T Tauri Stars

abstract:
  We present near-infrared spectra of the excess continuum emission from the
innermost regions of classical T Tauri disks. In almost all cases, the shape of
the excess is consistent with that of a single-temperature blackbody with T ~
1400 K, similar to the expected dust sublimation temperature for typical dust
compositions. The amount of excess flux roughly correlates with the accretion
luminosity in objects with similar stellar properties. We compare our
observations with the predictions of simple disk models having an inner rim
located at the dust sublimation radius, including irradiation heating of the
dust from both the stellar and accretion luminosities. The models yield inner
rim radii in the range 0.07-0.54 AU, increasing with higher stellar and
accretion luminosities. Using typical parameters which fit our observed sample,
we predict a rim radius ~ 0.2 AU for the T Tauri star DG Tau, which agrees with
recent Keck near-infrared interferometric measurements. For large mass
accretion rates, the inner rim lies beyond the corotation radius at (or within)
which magnetospheric accretion flows are launched, which implies that pure
gaseous disks must extend inside the dust rim. Thus, for a significant fraction
of young stars, dust cannot exist in the innermost disk, calling into question
theories in which solid particles are ejected by a wind originating at the
magnetospheric radius.


title: The Evolution of Nova Ejecta

abstract:
  In this paper I review the basic parameters of Classical Novae and then move
on to describe the evolution of their ejected envelopes. The early shaping of
the remnant, thought to be a consequence of a common envelope phase, and with
analogies to what may occur in PNe with binary star nuclei, is then described.
Finally, the curious case of Nova GK Persei (1901) and its potential to aid our
understanding of both nova and long-term PN evolution is discussed.


title:
CCD photometric search for peculiar stars in open clusters. V. NGC 2099,
  NGC 3114, NGC 6204, NGC 6705 and NGC 6756

abstract:
  We have investigated 1008 objects in the area of five intermediate age open
clusters (NGC 2099, NGC 3114, NGC 6204, NGC 6705 and NGC 6756) via the narrow
band Delta a-system. The detection limit for photometric peculiarity is very
low (always less than 0.009mag) due to the high number of individual frames
used (193 in total). We have detected six peculiar objects in NGC 6705 and NGC
6756 from which one in the latter is almost certainly an unreddened late type
foreground star. The remaining five stars are probably cluster members and bona
fide chemically peculiar objects (two are lambda Bootis type candidates).
Furthermore, we have investigated NGC 3114, a cluster for which already
photoelectric Delta a-measurements exist. A comparison of the CCD and
photoelectric values shows very good agreement. Again, the high capability of
our CCD Delta a-photometric system to sort out true peculiar objects together
with additional measurements from broad or intermediate band photometry is
demonstrated.


title:
Relativistic Collapse of Rotating Supermassive Stars to Supermassive
  Black Holes

abstract:
  There is compelling evidence that supermassive black holes (SMBHs) exist. Yet
the origin of these objects, or their seeds, is still unknown. We are
performing general relativistic simulations of gravitational collapse to black
holes in different scenarios to help reveal how SMBH seeds might arise in the
universe. SMBHs with ~ 10^9 solar masses must have formed by z > 6, or within
10^9 yrs after the Big Bang, to power quasars. It may be difficult for gas
accretion to build up such a SMBH by this time unless the initial seed black
hole already has a substantial mass. One plausible progenitor of a massive seed
black hole is a supermassive star (SMS). We have followed the collapse of a SMS
to a SMBH by means of 3D hydrodynamic simulations in post-Newtonian gravity and
axisymmetric simulations in full general relativity. The initial SMS of
arbitrary mass M in these simulations rotates uniformly at the mass--shedding
limit and is marginally unstable to radial collapse. The final black hole mass
and spin are determined to be M_h/M ~ 0.9 and J_h/M_h^2 ~ 0.75. The remaining
mass goes into a disk of mass M_{disk}/M ~ 0.1. This disk arises even though
the total spin of the progenitor star, J/M^2 = 0.97, is safely below the Kerr
limit. The collapse generates a mild burst of gravitational radiation.
Nonaxisymmetric bars or one-armed spirals may arise during the quasi-stationary
evolution of a SMS, during its collapse, or in the ambient disk about the hole,
and are potential sources of quasi-periodic waves, detectable by LISA.


title: GALICS III: Predicted properties for Lyman Break Galaxies at redshift 3

abstract:
  This paper illustrates how mock observational samples of high-redshift
galaxies with sophisticated selection criteria can be extracted from the
predictions of GALICS, a hybrid model of hierarchical galaxy formation that
couples the outputs of large cosmological simulations and semi-analytic recipes
to describe dark matter collapse and the physics of baryons respectively. As an
example of this method, we focus on the properties of Lyman Break Galaxies at
redshift 3. With the MOMAF software package described in a companion paper, we
generate a mock observational sample with selection criteria as similar as
possible to those implied in the actual observations of z = 3 LBGs by Steidel
et al.(1995). Our model predictions are in good agreement with the observed
number density and 2D correlation function. We investigate the optical/IR
luminosity budget as well as several other physical properties of LBGs and find
them to be in general agreement with observed values. Looking into the future
of these LBGs we predict that 75% of them end up as massive ellipticals today,
even though only 35% of all our local ellipticals are predicted to have a LBG
progenitor. In spite of some shortcomings, this new 'mock observation' method
clearly represents a necessary first step toward a more accurate comparison
between hierarchical models of galaxy formation and real observational surveys.


title:
Pulsating White Dwarfs in Cataclysmic Variables: The Marriage of ZZ Cet
  and Dwarf Nova

abstract:
  There are now four dwarf novae known with white dwarf primaries that show
large amplitude non-radial oscillations of the kind seen in ZZ Cet stars. We
compare the properties of these stars and point out that by the end of the
Sloan Digital Sky Survey more than 30 should be known.


title:
Arecibo 430 MHz Pulsar Polarimetry: Faraday Rotation Measures and
  Morphological Classifications

abstract:
  We have measured Faraday Rotation Measures (RMs) at Arecibo Observatory for
36 pulsars, 17 of them new. We combine these and earlier measurements to study
the galactic magnetic field and its possible temporal variations. Many RM
values have changed significantly on several-year timescales, but these
variations probably do not reflect interstellar magnetic field changes. By
studying the distribution of pulsar RMs near the plane in conjunction with the
new NE2001 electron density model, we note the following structures in the
first galactic longitude quadrant: (1) The local field reversal can be traced
as a null in RM in a 0.5-kpc wide strip interior to the Solar Circle, extending
\~7 kpc around the Galaxy. (2) Steadily increasing RMs in a 1-kpc wide strip
interior to the local field reversal, and also in the wedge bounded by 42<l<52
deg, indicate that the large-scale field is approximately steady from the local
reversal in to the Sagittarius arm. (3) The RMs in the 1-kpc wide strip
interior to the Sagittarius arm indicate another field reversal in this strip.
(4) The RMs in a final 1-kpc wide interior strip, straddling the Scutum arm,
also support a second field reversal interior to the Sun,between the
Sagittarius and Scutum arms. (5) Exterior to the nearby reversal, RMs from
60<l<78 deg show evidence for two reversals, on the near and far side of the
Perseus arm. (6) In general, the maxima in the large-scale fields tend to lie
along the spiral arms, while the field minima tend to be found between them. We
have also determined polarized profiles of 48 pulsars at 430 MHz. We present
morphological pulse profile classifications of the pulsars, based on our new
measurements and previously published data.


title: Binarity and Symbiotics in Asymmetrical Planetary Nebulae

abstract:
  We show that there are strong links between certain types of asymmetrical
Planetary Nebulae (PNe) and symbiotic stars. Symbiotics are binaries and
several have extended optical nebulae all of which are asymmetrical and ~-40%
are bipolar. Bipolar PNe are likely to be formed by binaries and share many
properties with symbiotic nebulae (SyNe). Some PNe show point symmetry which is
naturally explained by precession in a binary system. M2-9 has both point and
plane symmetry, and has been shown to have a binary central object. We show
that inclination on the sky affects the observed properties of bipolar nebulae
due to enhanced equatorial densities, and compare observations of a sample of
BPNe with a simple model. Good agreement is obtained between model predicted
and observed IR/optical flux ratios and apparent luminosities, which further
confirms the binary hypothesis.


title: Orientation effects in bipolar nebulae: Can disks do it?

abstract:
  In this work we investigate how a circumstellar disk affects the radiation
emitted by an embedded star. We show correlations obtained from broad-band
observations of bipolar nebulae indicating that an orientation effect is at
play in these systems. The FIR radiation relative to total radiation increases
with inclination while the NIR and BVR fractions decrease. This is an expected
effect if we consider the system as being made up of a dense dusty disk being
irradiated by a hot star. We calculate 2-D models to try and reproduce the
observed behavior with different disk and star configurations.


title: Kinematics and Proper Motion of the Ansae in NGC7009

abstract:
  We have measured the expansion velocities and proper motion of the ansae in
NGC7009 using high dispersion echelle spectra and archive narrow band HST
images. Assuming that the ansae are moving at equal and opposite velocities
from the central star we obtain an average system radial velocity of -54 +-2
km/s, the eastern ansa approaching and the western ansa receding at Vr = 5.5
+-1 km/s relative to this value. Only the proper motion of the eastern ansa
could be measured, leading to 2.8 +- 0.8 arcsec/century, or Vt=130 +- 40.d
km/s, where d is the distance to the nebula in kpc. Additionally, the electron
temperature and density for each ansa was measured using line intensity ratios.
The results are Te = 9000 K and ne = 2000 /cm3 for both ansae within the
errors.


title: Searching for the Intra-Group Medium in Loose Groups of Galaxies

abstract:
  We have conducted a study with the VLA, DRAO Synthesis Telscope, and the FUSE
satellite to search for the intra-group medium in two loose groups of galaxies:
GH 144 and GH 158. No HI was detected near the background AGN in GH 158,
however two previously unknown dwarf galaxies were detected in GH 144.
Lyman-alpha, -beta, CIII and NV absorption was detected in GH 144 by FUSE.
Using this data and previously published data we found that the virial mass of
GH 144 is 2x10^12 M(sun). Of this 8% lies in the individual group galaxies, and
less than 8% is in the dense neutral intra-group medium. From our absorption
line data we constrain the diffuse IGM to have a volume density greater than
log n = -5.2 in a layer less than 22 kpc thick assuming a metallicity of 0.4
solar. While these values are uncertain, it is unlikely that this diffuse gas
contributes a significant fraction of the group mass. Given the depth of the
absorbing material and its separation from the nearest galaxies, it seems most
likely it originates from a small-clump in the IGM, perhaps an ionized
high-velocity cloud. (abridged)


title: On Intrinsic Magnetic Moments In Black Hole Candidates

abstract:
  In previous work we found that many of the spectral properties of low mass
x-ray binaries, including galactic black hole candidates could be explained by
a magnetic propeller model that requires an intrinsically magnetized central
object. Here we describe how the Einstein field equations of General Relativity
and equipartition magnetic fields permit the existence of highly red shifted,
extremely long lived, collapsing, radiating objects. We examine the properties
of these collapsed objects and discuss characteristics that might lead to their
confirmation as the source of black hole candidate phenomena.


title:
High energy cosmic-rays: puzzles, models, and giga-ton neutrino
  telescopes

abstract:
  The existence of cosmic rays of energies exceeding 10^20 eV is one of the
mysteries of high energy astrophysics. The spectrum and the high energy to
which it extends rule out almost all suggested source models. The challenges
posed by observations to models for the origin of high energy cosmic rays are
reviewed, and the implications of recent new experimental results are
discussed. Large area high energy cosmic ray detectors and large volume high
energy neutrino detectors currently under construction may resolve the high
energy cosmic ray puzzle, and shed light on the identity and physics of the
most powerful accelerators in the universe.


title:
Global, Exact Cosmic Microwave Background Data Analysis Using Gibbs
  Sampling

abstract:
  We describe an efficient and exact method that enables global Bayesian
analysis of cosmic microwave background (CMB) data. The method reveals the
joint posterior density (or likelihood for flat priors) of the power spectrum
$C_\ell$ and the CMB signal. Foregrounds and instrumental parameters can be
simultaneously inferred from the data. The method allows the specification of a
wide range of foreground priors. We explicitly show how to propagate the
non-Gaussian dependency structure of the $C_\ell$ posterior through to the
posterior density of the parameters. If desired, the analysis can be coupled to
theoretical (cosmological) priors and can yield the posterior density of
cosmological parameter estimates directly from the time-ordered data. The
method does not hinge on special assumptions about the survey geometry or noise
properties, etc. It is based on a Monte Carlo approach and hence parallelizes
trivially. No trace or determinant evaluations are necessary. The feasibility
of this approach rests on the ability to solve the systems of linear equations
which arise. These are of the same size and computational complexity as the
map-making equations. We describe a pre-conditioned conjugate gradient
technique that solves this problem and demonstrate in a numerical example that
the computational time required for each Monte Carlo sample scales as
$n_p^{3/2}$ with the number of pixels $n_p$. We test our method using the
COBE-DMR data and explore the non-Gaussian joint posterior density of the
COBE-DMR $C_\ell$ in several projections.


title:
Quasi-Periodic Oscillations from Rayleigh-Taylor and Kelvin-Helmholtz
  Instability at a Disk-Magnetosphere Interface

abstract:
  We consider the interface between an accretion disk and a magnetosphere
surrounding the accreting mass. We argue that such an interface can occur not
only with a magnetized neutron star but also sometimes with an unmagnetized
neutron star or a black hole. The gas at the magnetospheric interface is
generally Rayleigh-Taylor unstable and may also be Kelvin-Helmholtz unstable.
Because of these instabilities, modes with low azimuthal wavenumbers m are
expected to grow to large amplitude. It is proposed that the resulting
nonaxisymmetric structures contribute to the high frequency quasi-periodic
oscillations that have been seen in neutron-star and black-hole X-ray binaries.
The mode oscillation frequencies are calculated to be approximately equal to m
\Omega_m, where \Omega_m is the angular velocity of the accreting gas at the
magnetospheric radius. Thus, mode frequencies should often be in the
approximate ratio 1:2:3, etc. If the pressure of the gas in the disk is not
large, then the m = 1 mode will be stable. In this case, the mode frequencies
should be in the approximate ratio 2:3, etc. There is some observational
evidence for such simple frequency ratios.


title: Primordial nuggets survival and QCD pairing

abstract:
  We revisit the problem of boiling and surface evaporation of quark nuggets in
the cosmological quark-hadron transition with the explicit consideration of
pairing between quarks in a color-flavor locked (CFL) state. Assuming that
primordial quark nuggets are actually formed, we analyze the consequences of
pairing on the rates of boiling and surface evaporation in order to determine
whether they could have survived with substantial mass. We find a substantial
quenching of the evaporation + boiling processes, which suggests the survival
of primordial nuggets for the currently considered range of the pairing gap
$\Delta$. Boiling is shown to depend on the competition of an increased
stability window and the suppression of the rate, and is not likely to dominate
the destruction of the nuggets. If surface evaporation dominates, the fate of
the nuggets depend on the features of the initial mass spectrum of the nuggets,
their evaporation rate, and the value of the pairing gap, as shown and
discussed in the text.


title: Variable Stars in the Magellanic Clouds: Results from OGLE and SIRIUS

abstract:
  We have performed a cross-identification between OGLE-II data and
single-epoch SIRIUS JHK survey data in the LMC and SMC. After eliminating
obvious spurious variables, we determined the pulsation periods for 9,681 and
2,927 variables in the LMC and SMC, respectively. Based on these homogeneous
data, we studied the pulsation properties and metallicity effects on period-K
magnitude (PK) relations by comparing the variable stars in the LMC and SMC.
The sample analyzed here is much larger, and we found the following new
features: (1) variable red giants in the SMC form parallel sequences on the PK
plane, just like those found by Wood (2000) in the LMC; (2) both of the
sequences A and B of Wood (2000) have discontinuities, and they occur at the
K-band luminosity of the TRGB; (3) the sequence B of Wood (2000) separates into
three independent sequences B+- and C'; (4) comparison between the theoretical
pulsation models (Wood et al. 1996) and observational data suggests that the
variable red giants on sequences C and newly discovered C' are pulsating in the
fundamental and first overtone mode, respectively; (5) the theory can not
explain the pulsation mode of sequences A+- and B+-, and they are unlikely to
be the sequences for the first and second overtone pulsators, as was previously
suggested; (6) the zero points of PK relations of Cepheids in the metal
deficient SMC are fainter than those of LMC ones by ~0.1 mag but those of SMC
Miras are brighter than those of LMC ones by ~0.13 mag, which are probably due
to metallicity effects.


title:
Detection of Intermediate-Period Transiting Planets with a Network of
  Small Telescopes: transitsearch.org

abstract:
  We describe a project (transitsearch.org) currently attempting to discover
transiting intermediate-period planets orbiting bright parent stars, and we
simulate that project's performance. The discovery of such a transit would be
an important astronomical advance, bridging the critical gap in understanding
between HD209458b and Jupiter. However, the task is made difficult by
intrinsically low transit probabilities and small transit duty cycles. This
project's efficient and economical strategy is to photometrically monitor stars
that are known (from radial velocity surveys) to bear planets, using a network
of widely-spaced observers with small telescopes. These observers, each
individually capable of precision (1%) differential photometry, monitor
candidates during the time windows in which the radial velocity solution
predicts a transit if the orbital inclination is close to 90 degrees. We use
Monte Carlo techniques to simulate the performance of this network, performing
simulations with different configurations of observers in order to optimize
coordination of an actual campaign. Our results indicate that transitsearch.org
can reliably rule out or detect planetary transits within the current catalog
of known planet-bearing stars. A distributed network of skilled amateur
astronomers and small college observatories is a cost-effective method for
discovering the small number of transiting planets with periods in the range
10d < P < 200d that orbit bright (V < 11) stars.


title:
The Three Spectral Regimes Found in the Stellar Black Hole XTE
  J1550--564 in its High/Soft State

abstract:
  The present paper describes the analysis of multiple RXTE/PCA data of the
black hole binary with superluminal jet, XTE J1550-564, acquired during its
1999--2000 outburst. The X-ray spectra show features typical of the high/soft
spectral state, and can approximately be described by an optically thick disk
spectrum plus a power-law tail. Three distinct spectral regimes, named standard
regime, anomalous regime, and apparently standard regime, have been found from
the entire set of the observed spectra. When the X-ray luminosity is well below
6E38 erg/s (assuming a distance of 5 kpc), XTE J1550-564 resides in the
standard regime, where the soft spectral component dominates the power-law
component and the observed disk inner radius is kept constant. When the
luminosity exceeds the critical luminosity, the apparently standard regime is
realized, where luminosity of the optically thick disk rises less steeply with
the temperature, and the spectral shape is moderately distorted from that of
the standard accretion disk. In this regime, radial temperature gradient of the
disk has been found to be flatter than that of the standard accretion disk. The
results of the apparently standard regime are suggestive of a slim disk (e.g.,
Abramowicz et al. 1988, Watarai et al. 2000) which is a solution predicted
under high mass accretion rate. In the intermediate anomalous regime, the
spectrum becomes much harder, and the disk inner radius derived using a simple
disk model spectrum apparently varies significantly with time. These properties
can be explained as a result of significant thermal inverse Comptonization of
the disk photons, as was found from GRO J1655-40 in its anomalous regime by
Kubota, Makishima and Ebisawa (2001).


title: The ISO-LWS far-infrared spectra of pre-Main Sequence objects

abstract:
  The Long Wavelength Spectrometer (LWS) on board the Infrared Space
Observatory (ISO) satellite has allowed for the first time to investigate the
whole far infrared (FIR) part of the spectrum (from 43 to 197 um), inaccessible
from the ground. The FIR spectrum is crucial for the study of the early phases
of protostellar evolution since the peak of the continuum emission of the
protostars falls around 100 um and many molecular species emit in this range.
In this paper we review the main results of the spectroscopic observations
carried out with the LWS on a sample of pre-Main Sequence objects in different
evolutionary stages. The FIR spectra are characterized by a strong continuum
with superimposed atomic and molecular emission lines. The fine structure lines
emitted by the OI and CII atoms are present in all the objects of our sample
while emission from molecular species (CO, H_2O and OH) dominate the spectrum
of the younger and more embedded objects; lines of highly ionized atoms (OIII,
NIII, NII) are present only in high luminosity sources. We will show how both
the FIR continuum and the emission lines are powerful indicators of the
evolutionary status of young embedded objects. The analysis of the LWS spectra
has allowed to study only the average properties of the young stellar objects,
due to the large field of view (~ 80 arcsec), the limited sensitivity and the
poor spectral resolution (~ 200) of the instrument in its grating mode. The
higher spatial and spectral resolutions of the instruments on board the
Herschel satellite will allow to address in deeper detail the scientific
problems highlighted by the ISO results.


title: The quasars are neutron stars embedded in clouds of hydrogen

abstract:
  The accretion of a cloud of hydrogen at the surface of a small, heavy star
produces a high energy mostly dissipated by electromagnetic radiation. The
combination of the absorption and the redshift of this radiation by hydrogen
explains all spectral observations: shapes of the broad lines, and their
anti-correlation with the radio-loudness, lack of lines in front of the Lyman
forest, value zb = 0.062 of the periodicity of the redshifts, correlation of a
high redshift with a thermal spectrum attributed to dust. These properties are
deduced from usual laws of physics without new parameters, they do not require
any non baryonic matter.


title:
Remarkable changes in the near-infrared spectrum of the nova-like
  variable V4332 Sgr

abstract:
  We report on recent near-IR observations of V4332 Sgr - the nova-like
variable that erupted in 1994. Its rapid, post-outburst evolution to a cool M
type giant/supergiant, soon after its outburst, had showed that it was an
unusual object differing from other eruptive variables like classical/symbiotic
novae or born-again AGB stars. The present study of V4332 Sgr was motivated by
the keen interest in the recent eruption of V838 Mon - which along with V4332
Sgr - is believed to belong to a new class of objects (we propose they may be
called "quasi-novae"). Our observations show new developments in the evolution
of V4332 Sgr. The most striking feature is the detection of several molecular
bands of AlO - a rarely seen molecule in astronomical spectra - in the JHK
spectra. Many of these bands are being detected for the first time. The only
other detection of some of these AlO bands are in V838 Mon, thereby showing
further spectral similarities between the two objects. JHK photometry shows the
development of a new dust shell around V4332 Sgr with a temperature of ~ 900K.
This dust shell does not appear to be associated with ejecta of the 1994
outburst but is due to a second mass-loss episode which is not expected in a
classical nova outburst. The cold molecular environment, suggested by the AlO
emission, is also not expected in novae ejecta. We model the AlO bands and also
discuss the possible formation mechanism of the AlO.


title:
Current Status and Perspectives of Cosmic Microwave Background
  Observations

abstract:
  Measurements of the cosmic microwave background (CMB) radiation provide a
unique opportunity for a direct study of the primordial cosmic plasma at
redshift z ~1000. The angular power spectra of temperature and polarisation
fluctuations are powerful observational objectives as they encode information
on fundamental cosmological parameters and on the physics of the early
universe. A large number of increasingly ambitious balloon-borne and
ground-based experiments have been carried out following the first detection of
CMB anisotropies by COBE-DMR, probing the angular power spectrum up to high
multipoles. The recent data from WMAP provide a new major step forward in
measurements percision. The ESA mission Planck Surveyor, to be launched in
2007, is the third-generation satellite devoted to CMB imaging. Planck is
expected to extract the full cosmological information from temperature
anisotropies and to open up new fronteers in the CMB field.


title: Kinematics and binaries in young stellar aggregates. II. NGC 6913 = M29

abstract:
  Between 1996 and 2003 we have obtained 226 high resolution spectra of 16
stars in the field of the young open cluster NGC 6913, to the aim of
constraining its main properties and study its internal kinematics. Twelve of
the program stars turned out to be members, one of them probably unbound. Nine
are binaries (one eclipsing and another double lined) and for seven of them the
observations allowed to derive the orbital elements. All but two of the nine
discovered binaries are cluster members. In spite of the young age (a few Myr),
the cluster already shows signs that could be interpreted as evidence of
dynamical relaxation and mass segregation. However, they may be also the result
of an unconventional formation scenario. The dynamical (virial) mass as
estimated from the radial velocity dispersion is larger than the cluster
luminous mass, which may be explained by a combination of the optically thick
interstellar cloud that occults part of the cluster, the unbound state or
undetected very wide binary orbit of some of the members that inflate the
velocity dispersion and a high inclination for the axis of a possible cluster
angular momentum. All discovered binaries are hard enough to survive average
close encounters within the cluster and do not yet show sign of relaxation of
the orbital elements to values typical of field binaries.


title: Inverse temperature dependence of the dust submillimeter spectral index

abstract:
  We present here a compilation of PRONAOS-based results concerning the
temperature dependence of the dust submillimeter spectral index, including data
from Galactic cirrus, star-forming regions and a circumstellar envelope. We
observe large variations of the spectral index (from 0.8 to 2.4) in a wide
range of temperatures (12 to 80 K). These spectral index variations follow a
hyperbolic-shaped function of the temperature, large spectral indices (1.5-2.4)
being observed in cold regions (12-20 K) while small indices (0.8-1.6) are
observed in warm regions (35-80 K). Three interpretations are proposed: one is
that the grain sizes change in warm and rather dense environments, another is
that the chemical composition of the grains is not the same in different
environments, a third one is that there is an intrinsic dependence of the dust
spectral index on the temperature due to quantum processes.


title: Polarimetric evolution of V838 Mon

abstract:
  We present the results of our polarimetric and spectropolarimetric monitoring
of V838 Monocerotis, performed at Asiago and Crimean observatories during and
after the multiple outbursts that occurred in January-March 2002.
  The polarization of the object is mainly due to interstellar polarization
(P=2.48%). Intrinsic polarization up to 0.7% at 5000 A is present during the
second maximum of the object (February 2002). This intrinsic component
increases toward shorter wavelengths but our limited spectral coverage
(5000-7500 A) does not allow conclusive inferences about its origin. A strong
depolarization across the Halpha profile is observed. The interstellar
polarization gives a lower limit to the reddening of E(B-V)>0.28, with
E(B-V)=0.5 being the most probable value. A normal ratio of total to selective
absorption (R_V=3.22+-0.17) was derived from the wavelength of maximum
interstellar polarization. This suggests a low (if any) contribution by
circumstellar material with peculiar dust to gas ratio. A polarimetric map of a
portion of the light echo shows a complex polarization distribution reaching
P_max=45%.


title: Long-Term Timing of 374 Pulsars

abstract:
  We have analysed the arrival times for 374 pulsars that have been observed
for more than six years using the 76-m Lovell telescope at Jodrell Bank
Observatory. Here we present a qualitative analysis of structures seen in the
timing residuals.


title: An HI census of Loose Groups of Galaxies

abstract:
  We present results from our Parkes Multibeam HI survey of 3 loose groups of
galaxies that are analogous to the Local Group. This is a survey of groups
containing only spiral galaxies with mean separations of a few hundred kpc, and
total areas of approximately 1 sq. Mpc; groups similar to our own Local Group.
We present a census of the HI-rich objects in these groups down to an M(HI),
1-sigma sensitivity ~7x10^5 M(sun), as well as the detailed properties of these
detections from follow-up Compact Array observations. We found 7 new HI-rich
members in the 3 groups, all of which have stellar counterparts and are,
therefore, typical dwarf galaxies. The ratio of low-mass to high-mass gas-rich
galaxies in these groups is less than in the Local Group meaning that the
``missing satellite'' problem is not unique. No high-velocity cloud analogs
were found in any of the groups. If HVCs in these groups are the same as in the
Local Group, this implies that HVCs must be located within ~300-400 kpc of the
Milky Way.


title:
Helioseismic Probing of Solar Variability: The Formalism and Simple
  Asses sments

abstract:
  We derive formulae connecting the frequency variations in the spectrum of
solar oscillations to the dynamical quantities that are expected to change over
the solar activity cycle. This is done for both centroids and the asymmetric
part of the fine structure (so-called even-a coefficients). We consider the
near-surface, small-scale magnetic and turbulent velocity fields, as well as
horizontal magnetic fields buried near the base of the convective zone. For the
centroids we also discuss the effect of temperature variation. We demonstrate
that there is a full, one-to-one correspondence between the expansion
coefficients of the fine structure and those of both the averaged small-scale
velocity and magnetic fields. Measured changes in the centroid frequencies and
the even-a's over the rising phase solar cycle may be accounted for by a
decrease in the turbulent velocity of order 1%. We show that the mean
temperature decrease associated with the net decrease in the efficiency of
convective transport may also significantly contribute to the increase of the
centroid frequencies. Alternatively, the increase may be accounted for by an
increase of the small-scale magnetic field of order 100 G, if the growing field
is predominantly radial. We also show that global seismology can be used to
detect a field at the level of a few times 10^5 G, if such a field were present
and confined to a thin layer near the base of the convective envelope.


title: In flight calibration of the ISGRI camera

abstract:
  ISGRI, the IBIS low energy camera (15 keV - 1 MeV) on board INTEGRAL, is the
first large CdTe gamma-ray imager in orbit. We present here an overview of the
ISGRI in-flight calibrations performed during the first months after launch. We
discuss the stability of the camera as well as the CdTe pixels response under
cosmic radiation. The energy calibra tions were done using lead and tungsten
fluorescence lines and the $\mathrm{^{22}Na}$ calibration unit. Thermal effects
and charge correction algorithm are discussed, and the resulting energy
resolution is presented. The ISGRI background spatial and spectral
non-uniformity is also described, and some image correction results are
presented.


title: The Ellipticity of the Disks of Spiral Galaxies

abstract:
  The disks of spiral galaxies are generally elliptical rather than circular.
The distribution of ellipticities can be fit with a log-normal distribution.
For a sample of 12,764 galaxies from the Sloan Digital Sky Survey Data Release
1 (SDSS DR1), the distribution of apparent axis ratios in the i band is best
fit by a log-normal distribution of intrinsic ellipticities with ln epsilon =
-1.85 +/- 0.89. For a sample of nearly face-on spiral galaxies, analyzed by
Andersen and Bershady using both photometric and spectroscopic data, the best
fitting distribution of ellipticities has ln epsilon = -2.29 +/- 1.04. Given
the small size of the Andersen-Bershady sample, the two distribution are not
necessarily inconsistent. If the ellipticity of the potential were equal to
that of the light distribution of the SDSS DR1 galaxies, it would produce 1.0
magnitudes of scatter in the Tully-Fisher relation, greater than is observed.
The Andersen-Bershady results, however, are consistent with a scatter as small
as 0.25 magnitudes in the Tully-Fisher relation.


title:
Comparison of two optical cluster finding algorithms for the new
  generation of deep galaxy surveys

abstract:
  We present a comparison between two optical cluster finding methods: a
matched filter algorithm using galaxy angular coordinates and magnitudes, and a
percolation algorithm using also redshift information. We test the algorithms
on two mock catalogues. The first mock catalogue is built by adding clusters to
a Poissonian background, while the other is derived from N-body simulations.
Choosing the physically most sensible parameters for each method, we carry out
a detailed comparison and investigate advantages and limits of each algorithm,
showing the possible biases on final results. We show that, combining the two
methods, we are able to detect a large part of the structures, thus pointing
out the need to search for clusters in different ways in order to build
complete and unbiased samples of clusters, to be used for statistical and
cosmological studies. In addition, our results show the importance of testing
cluster finding algorithms on different kinds of mock catalogues to have a
complete assessment of their behaviour.


title:
AWM 4 and MKW 4 - two very different poor clusters observed with
  XMM-Newton

abstract:
  We present observations of two poor clusters, AWM 4 and MKW 4, observed by
XMM-Newton. Both systems are relaxed, with little substructure evident in their
X-ray halos or galaxy populations. However, their temperature structures are
markedly different, with AWM 4 isothermal to the resolution of the EPIC
instruments while MKW 4 shows a strong decline in temperature towards the core.
Metal abundance also increases more strongly in the core of MKW 4 than AWM 4.
Three dimensional models show further differences, suggesting that gas in the
core of AWM 4 has been heated and has expanded outwards. The dominant
elliptical galaxy of AWM 4 hosts an AGN with large-scale radio jets, while the
central cD of MKW 4 shows no current AGN activity. We therefore conclude that
the difference in activity cycle of the AGN in the two galaxies is responsible
for the difference in IGM properties between the two clusters.


title:
Influence of the neutron star 1E 161348-5055 in RCW 103 on the
  surrounding medium

abstract:
  We have carried out a study of the neutral hydrogen in the direction of the
X-ray source 1E 161348-5055, a compact central object (CCO) located in the
interior of the supernova remnant (SNR) RCW 103. The HI 21 cm line observations
were carried out using the Australia Telescope Compact Array, complemented with
single dish data from the Parkes radio telescope to recover information at all
spatial scales. We derive a distance to RCW 103 of 3.3 kpc, in agreement with
previous distance measurements. We have also detected a small hole in the HI
emission which is positionally and kinematically coincident with the location
of the CCO which confirms the association between the SNR and the CCO. This is
the third case of a depression in HI emission seemingly associated with CCOs in
SNRs. The characteristic parameters of the holes such as their size,
eccentricity and evacuated mass are similar in all three cases. We estimate the
absorbing HI column density towards 1E 161348-5055 to be ~6 x 10^{21} cm^{-2},
a value compatible with a blackbody solution for the CCO X-ray emission.
However, the implied brightness temperature is very high comparedto most
neutron stars. Moreover, the strong long-term variability in X-rays favours the
hypothesis that 1E 161348-5055 is an accreting binary sourcerather than an
isolated, cooling neutron star. An analysis of the continuum image obtained at
1.4 GHz from these observations shows no trace of a pulsar wind nebula around
1E 161348-5055, in spite of it being a young object.


title: Turbulence and Fossil Turbulence in Oceans and Lakes

abstract:
  Turbulence is defined as an eddy-like state of fluid motion where the
inertial-vortex forces of the eddies are larger than any of the other forces
that tend to damp the eddies out. Energy cascades of irrotational flows from
large scales to small are non-turbulent, even if they supply energy to
turbulence. Turbulent flows are rotational and cascade from small scales to
large, with feedback. Viscous forces limit the smallest turbulent eddy size to
the Kolmogorov scale. In stratified fluids, buoyancy forces limit large
vertical overturns to the Ozmidov scale and convert the largest turbulent
eddies into a unique class of saturated, non-propagating, internal waves,
termed fossil-vorticity-turbulence. These waves have the same energy but
different properties and spectral forms than the original turbulence patch. The
Gibson (1980, 1986) theory of fossil turbulence applies universal similarity
theories of turbulence and turbulent mixing to the vertical evolution of an
isolated patch of turbulence in a stratified fluid as its growth is constrained
and fossilized by buoyancy forces. These theories apply to the dynamics of
atmospheric, astrophysical and cosmological turbulence.


title: A Large Extension of the CfA Galactic CO Survey

abstract:
  The Galactic CO survey of Dame, Hartmann, & Thaddeus (2001; hereafter DHT) is
composed of both large-scale unbiased surveys, mainly concentrated within
10-deg of the Galactic plane, and targeted observations of clouds at higher
latitudes. Analysis of all-sky IRAS and 21 cm maps suggests that the DHT survey
is nearly complete for clouds larger than ~1 deg, even though roughly half of
the total area at |b| < 30 deg was not observed. In October 2001 we began a new
survey of all of this unobserved area that is accessible to the northern 1.2
meter telescope, approximately 6,600 deg^2 between l = 0 deg and 230 deg,
mainly in the latitude range |b| = 10-30 deg. At least 12 hours per day is
being dedicated to this large project, which is sampled every 1/4-deg (every
other beamwidth) to an rms sensitivity of 0.19 K at a velocity resolution of
0.65 km/s. As of May 2003, we have obtained 90,000 of the 106,000 spectra
required to complete the survey. While, as expected, the new observations do
not substantially change the DHT map, ~68 relatively small and isolated
molecular clouds at intermediate latitudes have so far been discovered.
  The survey has also been extended to b < -30 deg in two regions, one in the
vicinity of the large MBM clouds 53-55 at l ~ 90 deg and the other south of the
Taurus clouds at l ~170 deg. Substantial amounts of molecular gas were detected
in both of these high-latitude regions.


title: The Aligned z ~ 1 Radio Galaxy 3C 280

abstract:
  The z~1 radio galaxy 3C280 has a striking rest-frame UV morphology, with
multiple line and continuum components precisely aligned with the radio
structure, including an obvious semi-circular arc. We explore the nature of
these various components by bringing together HST and ground-based imaging,
ground-based spectroscopy, and radio mapping. From plausible decompositions of
the spectra, we show that the continuum of the nuclear component is likely
dominated by a combination of nebular thermal continuum, quasar light, and
light from old stars. A component that falls directly on the probable path of
the radio jet shows mostly nebular thermal continuum and includes contributions
from a relatively young stellar population with an age around 100 Myr. The arc
appears to be completely dominated by line emission and nebular thermal
continuum, with no evidence for a significant stellar contribution. Though much
of the aligned light is in UV components, the underlying old elliptical is also
well-aligned with the radio axis. The elliptical is well-fit by a de
Vaucouleurs profile, probably has a moderately old stellar population (~3 Gyr),
and is a massive system with a velocity dispersion of sigma ~ 270 km/s that
implies it contains a supermassive black hole. Although the arc and the
extended emission surrounding the eastern lobe suggest that interactions
between the radio lobe and jet must have been important in creating the UV
morphology, the ionization and kinematic properties in these componentsare more
consistent with photoionization than shock excitation. 3C280 may be a
transition object between the compact steep-spectrum radio galaxies which seem
to be shock-dominated, and the extended radio sources which may have evolved
past this phase and rarely show shock signatures.


title: Magnetic Interaction between Stars and Accretion Disks

abstract:
  In this review I consider modern theoretical models of coupled star--disk
magnetospheres. I discuss a number of models, both stationary and
time-dependent, and examine what physical conditions govern the selection of a
preferred model.


title:
Molecular Hydrogen Emission Lines in Far Ultraviolet Spectroscopic
  Explorer Observations of Mira B

abstract:
  We present new Far Ultraviolet Spectroscopic Explorer (FUSE) observations of
Mira A's wind-accreting companion star, Mira B. We find that the strongest
lines in the FUSE spectrum are H2 lines fluoresced by H I Lyman-alpha. A
previously analyzed Hubble Space Telescope (HST) spectrum also shows numerous
Lyman-alpha fluoresced H2 lines. The HST lines are all Lyman band lines, while
the FUSE H2 lines are mostly Werner band lines, many of them never before
identified in an astrophysical spectrum. We combine the FUSE and HST data to
refine estimates of the physical properties of the emitting H2 gas. We find
that the emission can be reproduced by an H2 layer with a temperature and
column density of T=3900 K and log N(H2)=17.1, respectively. Another similarity
between the HST and FUSE data, besides the prevalence of H2 emission, is the
surprising weakness of the continuum and high temperature emission lines,
suggesting that accretion onto Mira B has weakened dramatically. The UV fluxes
observed by HST on 1999 August 2 were previously reported to be over an order
of magnitude lower than those observed by HST and the International Ultraviolet
Explorer (IUE) from 1979--1995. Analysis of the FUSE data reveals that Mira B
was still in a similarly low state on 2001 November 22.


title: Aborted jets and the X-ray emission of radio-quiet AGNs

abstract:
  We propose that radio-quiet quasars and Seyfert galaxies have central black
holes powering outflows and jets which propagate only for a short distance,
because the velocity of the ejected material is smaller than the escape
velocity. We call them "aborted" jets. If the central engine works
intermittently, blobs of material may be produced, which can reach a maximum
radial distance and then fall back, colliding with the blobs produced later and
still moving outwards. These collisions dissipate the bulk kinetic energy of
the blobs by heating the plasma, and can be responsible (entirely or at least
in part) for the generation of the high energy emission in radio-quiet objects.
This is alternative to the more conventional scenario in which the X-ray
spectrum of radio-quiet sources originates in a hot (and possibly patchy)
corona above the accretion disk. In the latter case the ultimate source of
energy of the emission of both the disk and the corona is accretion. Here we
instead propose that the high energy emission is powered also by the extraction
of the rotational energy of the black hole (and possibly of the disk). By means
of Montecarlo simulations we calculate the time dependent spectra and light
curves, and discuss their relevance to the X-ray spectra in radio-quiet AGNs
and galactic black hole sources. In particular, we show that time variability
and spectra are similar to those observed in Narrow Line Seyfert 1 galaxies.


title: Two Active Nuclei in 3C294

abstract:
  The z=1.786 radio galaxy 3C294 lies <10 arsec from a 12th mag star and has
been the target of at least three previous investigations using adaptive-optics
imaging. A major problem in interpreting these results is the uncertainty in
the precise alignment of the radio structure with the H or K-band AO imaging.
Here we report observations of the position of the AO guide star with the HST
Fine Guidance Sensor, which, together with positions from the U. S. Naval
Observatory's UCAC2 catalog, allow us to register the infrared and radio frames
to an accuracy of better than 0.1 arcsec. The result is that the nuclear
compact radio source is not coincident with the brightest discrete object in
the AO image, an essentially unresolved source on the eastern side of the light
distribution, as Quirrenbach et al. (2001) had suggested. Instead, the radio
source is centered about 0.9 arcsec to the west of this object, on one of the
two apparently real peaks in a region of diffuse emission. Nevertheless, the
conclusion of Quirrenbach et al. that 3C294 involves an ongoing merger appears
to be correct: analysis of a recent deep Chandra image of 3C294 obtained from
the archive shows that the nucleus comprises two X-ray sources, which are
coincident with the radio nucleus and the eastern stellar object. The
X-ray/optical flux ratio of the latter makes it extremely unlikely that it is a
foreground Galactic star.


title: Outflows and Jets I: a personal take

abstract:
  As a session chair I have the privilege to write down a few comments on four
talks that were delivered under the general title of "outflows and jets I".
This and the session that followed it, grouped work on circumstellar
environments of, post-AGB stars, proto-PNe and PNe. After summarizing some of
the highlights, I pose the question of which observations, if any,reveal the
presence of a common envelope ejection in the past of a PN. Finally, I point
out that the finding that most or all PNe have a binary origin, while solving
some of our problems, might be in contrast with the number of known close main
sequence binaries.


title:
A Low Frequency Survey of the Galactic Plane Near l=11 degrees:
  Discovery of Three New Supernova Remnants

abstract:
  We have imaged a 1 deg^2 field centered on the known Galactic supernova
remnant (SNR) G11.2-0.3 at 74, 330, and 1465 MHz with the Very Large Array
radio telescope (VLA) and 235 MHz with the Giant Metrewave Radio Telescope
(GMRT). The 235, 330, and 1465 MHz data have a resolution of 25 arcsec, while
the 74 MHz data have a resolution of 100 arcsec. The addition of this low
frequency data has allowed us to confirm the previously reported low frequency
turnover in the radio continuum spectra of the two known SNRs in the field:
G11.2-0.3 and G11.4-0.1 with unprecedented precision. Such low frequency
turnovers are believed to arise from free-free absorption in ionized thermal
gas along the lines of site to the SNRs. Our data suggest that the 74 MHz
optical depths of the absorbing gas is 0.56 and 1.1 for G11.2-0.3 and
G11.4-0.1, respectively. In addition to adding much needed low frequency
integrated flux measurements for two known SNRs, we have also detected three
new SNRs: G11.15-0.71, G11.03-0.05, and G11.18+0.11. These new SNRs have
integrated spectral indices between -0.44 and -0.80. Because of confusion with
thermal sources, the high resolution (compared to previous Galactic radio
frequency surveys) and surface brightness sensitivity of our observations have
been essential to the identification of these new SNRs. With this study we have
more than doubled the number of SNRs within just a 1 deg^2 field of view in the
inner Galactic plane. This result suggests that future low frequency
observations of the Galactic plane of similar quality may go a long way toward
alleviating the long recognized incompleteness of Galactic SNR catalogs.


title:
The structure of the NGC1333-IRAS2 protostellar system on 500 AU scales:
  an infalling envelope, a circumstellar disk, multiple outflows, and chemistry

abstract:
  This paper investigates small-scale structures of dense gas and dust around
the low-mass protostellar binary NGC1333-IRAS2 using millimeter-wavelength
aperture-synthesis observations from the OVRO and BIMA interferometers. The
detected 3 mm continuum emission is consistent with models of the envelope
around IRAS2A, based on previously reported submillimeter continuum images,
down to the 3", or 500 AU, resolution of the interferometer data. Our data
constrain the contribution of an unresolved point source to 22 mJy. Within the
accuracy of the parameters describing the envelope model, the point source flux
has an uncertainty by up to 25%. We interpret this point source as a cold disk
of mass \gtrsim 0.3 M_\odot. The same envelope model also reproduces
aperture-synthesis line observations of the optically thin isotopic species
C34S and H13CO+. The more optically thick main isotope lines show a variety of
components in the protostellar environment: N2H+ is closely correlated with
dust concentrations as seen at submillimeter wavelengths and is particularly
strong toward the starless core IRAS2C. We hypothesize that N2H+ is destroyed
through reactions with CO that is released from icy grains near the
protostellar sources IRAS2A and B. CS, HCO+, and HCN have complex line shapes
apparently affected by both outflow and infall. In addition to the east-west
jet from IRAS2A, a north-south velocity gradient near this source indicates a
second, perpendicular outflow. This suggests the presence of a binary companion
within 0.3" (65 AU) from IRAS2A as driving source of this outflow. Alternative
explanations of the velocity gradient such as rotation in a circumstellar
envelope or a single, wide-angle outflow are less likely.


title:
The eclipsing massive X-ray binary M33 X-7: New X-ray observations and
  optical identification

abstract:
  The eclipsing X-ray binary M33 X-7 was in the field of view during several
observations of our XMM-Newton M33 survey and in the archival Chanfdra
observation 1730 which cover a large part of the 3.45 d orbital period. We
detect emission of M33 X-7 during eclipse and a soft X-ray spectrum of the
source out of eclipse that can best be described by bremsstrahlung or disk
blackbody models. No significant regular pulsations of the source in the range
0.25-1000 s were found. The average source luminosity out of eclipse is 5E37
erg/s (0.5-4.5 keV). In a special analysis of DIRECT observations we identify
as optical counterpart a B0I to O7I star of 18.89 mag in V which shows the
ellipsoidal heating light curve of a high mass X-ray binary with the M33 X-7
binary period. The location of the X-ray eclipse and the optical minima allow
us to determine an improved binary period and ephemeris of mid-eclipse as HJD
(2451760.61+-0.09)+- N * (3.45376+-0.00021). The mass of the compact object
derived from orbital parameters and the optical companion mass, the lack of
pulsations, and the X-ray spectrum of M33 X-7 may indicate that the compact
object in the system is a black hole. M33 X-7 would be the first detected
eclipsing high mass black hole X-ray binary.


title: Cold Atom Clocks, Precision Oscillators and Fundamental Tests

abstract:
  We describe two experimental tests of the Equivalence Principle that are
based on frequency measurements between precision oscillators and/or highly
accurate atomic frequency standards. Based on comparisons between the hyperfine
frequencies of 87Rb and 133Cs in atomic fountains, the first experiment
constrains the stability of fundamental constants. The second experiment is
based on a comparison between a cryogenic sapphire oscillator and a hydrogen
maser. It tests Local Lorentz Invariance. In both cases, we report recent
results which improve significantly over previous experiments.


title:
A Numerical Gamma-Ray Burst Simulation Using Three-Dimensional
  Relativistic Hydrodynamics: The Transition from Spherical to Jet-like
  Expansion

abstract:
  We present the first unrestricted, three-dimensional relativistic
hydrodynamical calculations of the blob of gas associated with the jet
producing a gamma-ray burst. We investigate the deceleration phase of the blob
corresponding to the time when afterglow radiation is produced, concentrating
on the transition in which the relativistic beaming 1/gamma goes from being
less than theta, where gamma is the bulk Lorentz factor and theta is the
angular width of the jet, to 1/gamma > theta. We study the time dependent
evolution of the physical parameters associated with the jet, both parallel to
the direction of motion and perpendicular to it. We calculate light curves for
observers at varying angles with respect to the velocity vector of the blob,
assuming optically thin emission that scales with the local pressure. Our main
findings are that (i) gas ahead of the advancing blob does not accrete onto and
merge with the blob material but rather flows around the blob, (ii) the decay
light curve steepens at a time corresponding roughly to 1/gamma equals theta
(in accord with earlier studies), and (iii) the rate of decrease of the forward
component of momentum in the blob is well-fit by a simple model in which the
gas in front of the blob exerts a drag force on the blob, and the cross
sectional area of the blob increases quadratically with laboratory time (or
distance).


title: New Data and Improved Parameters for the Transiting Planet OGLE-TR-56b

abstract:
  We report new spectroscopic observations of the recently discovered
transiting planet OGLE-TR-56b with the Keck/HIRES instrument. Our radial
velocity measurements with errors of ~100 m/s show clear variations that are in
excellent agreement with the phasing (period and epoch) derived from the OGLE
transit photometry, confirming the planetary nature of the companion. The new
data combined with measurements from the previous season allow an improved
determination of the mass of the planet, M_p = 1.45 +/- 0.23 M_Jup. All
available OGLE photometry, including new measurements made this season, have
also been analyzed to derive an improved value for the planetary radius of R_p
= 1.23 +/- 0.16 R_Jup. We discuss the implications of these results for the
theory of extrasolar planets.


title: Angular clustering in the SUMSS radio survey

abstract:
  We measure the angular correlation function of radio galaxies selected by the
843 MHz Sydney University Molonglo Sky Survey (SUMSS). We find that the
characteristic imprint of large-scale structure is clearly detectable, and that
the survey is very uniform. Through comparison with similar analyses for other
wide-area radio surveys - the 1400 MHz NRAO VLA Sky Survey (NVSS) and the 325
MHz Westerbork Northern Sky Survey (WENSS) - we are able to derive consistent
angular clustering parameters, including a steep slope for the clustering
function, $w(\theta) \propto \theta^{-1.1}$. We revise upwards previous
estimates of the NVSS clustering amplitude, and find no evidence for dependence
of clustering properties on radio frequency. It is important to incorporate the
full covariance matrix when fitting parameters to the measured correlation
function. Once the redshift distribution for mJy radio galaxies has been
determined, these projected clustering measurements will permit a robust
description of large-scale structure at $z \sim 0.8$, the median redshift of
the sources.


title:
Analysing the database for stars in open clusters I. General methods and
  description of the data

abstract:
  We present an overview and statistical analysis of the data included in
WEBDA. This database includes valuable information such as coordinates,
rectangular positions, proper motions, photometric as well as spectroscopic
data, radial and rotational velocities for objects of open clusters in our
Milky Way. It also contains miscellaneous types of data like membership
probabilities, orbital elements of spectroscopic binaries and periods of
variability for different kinds of variable stars. Our final goal is to derive
astrophysical parameters (reddening, distance and age) of open clusters based
on the major photometric system which will be presented in a follow-up paper.
For this purpose we have chosen the Johnson UBV, Cousins VRI and Stroemgren
uvbybeta photometric systems for a statistical analysis of published data sets
included in WEBDA. Our final list contains photographic, photoelectric and CCD
data for 469820 objects in 573 open clusters. We have checked the internal
(data sets within one photometric system and the same detector technique) and
external (different detector technique) accuracy and conclude that more than
97% of all investigated data exhibit a sufficient accuracy for our analysis.
The way of weighting and averaging the data is described. In addition, we have
compiled a list of deviating measurements which is available to the community
through WEBDA.


title:
Highly extinguished supernovae in the nuclear regions of starburst
  galaxies

abstract:
  A handful of nearby supernovae (SNe) with visual extinctions of a few
magnitudes have recently been discovered. However, an undiscovered population
of much more highly extinguished (A(V) > 10) core-collapse supernovae (CCSNe)
is likely to exist in the nuclear (central kpc) regions of starburst galaxies.
The high dust extinction means that optical searches for such SNe are unlikely
to be successful. Here, we present preliminary results from our ongoing
near-infrared Ks-band search programme for nuclear SNe in nearby starburst
galaxies. We also discuss searches for SNe in Luminous and Ultraluminous
Infrared Galaxies.


title:
Varying G, accelerating Universe, and other relevant consequences of a
  Stochastic Self-Similar and Fractal Universe

abstract:
  In this paper the time dependence of G is presented. It is a simple
consequence of the Virial Theorem and of the self-similarity and fractality of
the Universe. The results suggest a Universe based on El Naschie's Cantorian
space-time. Moreover, we show the importance of the Golden Mean in respect to
the large scale structures. Thanks to this study the mass distribution at large
scales and the correlation function are explained and are natural consequences
of the evaluated varying G. We demonstrate the agreement between the present
hypotheses of segregation with a size of astrophysical structures, by using a
comparison between quantum quantities and astrophysical ones. It appears clear
that the Universe has a memory of its quantum origin. This appears in the G
dependence too. Moreover, we see that a G=G(t) in El Naschie's Cantorian
space-time can imply an accelerated Universe.


title:
The orbital period of the dipping, bursting, globular cluster X-ray
  source XB 1746-371 from Rossi X-ray Timing Explorer observations

abstract:
  We present results from two long observations of XB 1746-371 by the Rossi
X-ray Timing Explorer (RXTE) in 2002 January and May, lasting 4 and 5 days
respectively. Dips are observed in the X-ray light curves with a depth of 25
per cent, largely independent of energy within the usable band of the PCA
instrument of 2.1 - 16.0 keV. X-ray bursting and flaring activity are also
evident. The dips define the orbital period of the system, and using a power
spectral analysis and a cycle counting technique we derive an accurate period
of P_orb = 5.16 +/- 0.01 hr. The previously-reported candidate period of
5.73$\pm$0.15 hr, obtained using Ginga data, is inconsistent with our
determination, perhaps due to the weakness of the dipping and the variability
of the source during that observation. The dips in the RXTE observations
presented here do not align with the Ginga period, however our improved period
is consistent with a wide range of archival data.


title: Cometary panspermia explains the red rain of Kerala

abstract:
  Red coloured rain occurred in many places of Kerala in India during July to
September 2001 due to the mixing of huge quantity of microscopic red cells in
the rainwater. Considering its correlation with a meteor airbust event, this
phenomenon raised an extraordinary question whether the cells are
extraterrestrial. Here we show how the observed features of the red rain
phenomenon can be explained by considering the fragmentation and atmospheric
disintegration of a fragile cometary body that presumably contains a dense
collection of red cells. Slow settling of cells in the stratosphere explains
the continuation of the phenomenon for two months. The red cells under study
appear to be the resting spores of an extremophilic microorganism. Possible
presence of these cells in the interstellar clouds is speculated from its
similarity in UV absorption with the 217.5 nm UV extinction feature of
interstellar clouds.


title:
The apsidal corotation in mean motion resonance: the 55 Cancri as an
  example

abstract:
  The inner two planets around the 55 Cancri were found to be trapped in the
3:1 mean motion resonance. In this paper, we study the dynamics of this
extra-solar planetary system. Our numerical investigation confirms the
existence of the 3:1 resonance and implies a complex orbital motion. Different
stable motion types, with and without the apsidal corotation, are found. Due to
the high eccentricities in this system, we apply a semi-analytical method based
on a new expansion of the Hamiltonian of the planar three-body problem in the
discussion. We analyse the occurrence of the apsidal corotation in this mean
motion resonance and its influence on the stability of the system.


title: Galactic magnetic fields, from radio polarimetry of the WIM

abstract:
  Multi-frequency radio polarimetry of the diffuse Galactic synchrotron
background gives new viewpoints on the Galactic magnetic field. Rotation
measure maps reveal magnetic structures on arcminute to degree scales, such as
a ring in polarization that we interpret as a magnetic tunnel. A complication
using this technique is depolarization across the beam and along the line of
sight. The influence of beam depolarization has been estimated using numerical
models of the magneto-ionic ISM, through which polarized radiation propagates.
The models show that depolarization canals similar to those observed can be
caused by beam depolarization, and that the one-dimensional gradients in RM
needed to produce these canals are ubiquitous in the medium.


title: Radio Polarimetry in the Southern Galactic Plane Survey

abstract:
  We present radio polarimetric observations of a test region for the Southern
Galactic Plane Survey (SGPS), a radio survey in the Galactic plane in HI and
polarized continuum at 1.4 GHz with the Australia Telescope Compact Array
(ATCA) and the Parkes 64m dish. Ubiquitous structure in linearly polarized
intensity is often uncorrelated with structure in total intensity, indicating
Faraday rotation and depolarization. The one-dimensional second order structure
function of rotation measure for different position angles of the distance lag
shows a very shallow slope of the structure function on small scales and an
anisotropy in the slope on large scales. The anisotropy on large scales is
indicative of a gradient or large filament across the field. The shallow slope
can be explained by contributions of two separated Faraday screens. Assuming
that the two Faraday screens are the local and Carina spiral arms, the
structure function suggests an outer scale of structure in the local arm of
about 2 pc. This scale is similar to the typical scale of a Stroemgren sphere
of a B1-2 star. Therefore, we suggest that HII regions possibly dominate the
scale of structure in spiral arms.


title: The Evolution of Cluster Substructure with Redshift

abstract:
  Using Chandra archival data, we quantify the evolution of cluster morphology
with redshift. To quantify cluster morphology, we use the power ratio method
developed by Buote and Tsai (1995). Power ratios are constructed from moments
of the two-dimensional gravitational potential and are, therefore, related to a
cluster's dynamical state. Our sample will include 40 clusters from the Chandra
archive with redshifts between 0.11 and 0.89. These clusters were selected from
two fairly complete flux-limited X-ray surveys (the ROSAT Bright Cluster Sample
and the Einstein Medium Sensitivity Survey), and additional high-redshift
clusters were selected from recent ROSAT flux-limited surveys. Here we present
preliminary results from the first 28 clusters in this sample. Of these, 16
have redshifts below 0.5, and 12 have redshifts above 0.5.


title:
Cosmological parameters from lensing power spectrum and bispectrum
  tomography

abstract:
  We examine how lensing tomography with the bispectrum and power spectrum can
constrain cosmological parameters and the equation of state of dark energy. Our
analysis uses the full information at the two- and three-point level from
angular scales of a few degrees to 5 arcminutes (50 < l < 3000), which will be
probed by lensing surveys. We use all triangle configurations, cross-power
spectra and bispectra constructed from up to three redshift bins with
photometric redshifts, and relevant covariances in our analysis.
  We find that the parameter constraints from bispectrum tomography are
comparable to those from power spectrum tomography. Combining the two improves
parameter accuracies by a factor of three due to their complementarity. For the
dark energy parameterization w(a) = w0 + wa(1-a), the marginalized errors from
lensing alone are sigma(w0) = 0.03 fsky^{-1/2} and sigma(wa) = 0.1 fsky^{-1/2}.
We show that these constraints can be further improved when combined with
measurements of the cosmic microwave background or Type Ia supernovae. The
amplitude and shape of the mass power spectrum are also shown to be precisely
constrained. We use hyper-extended perturbation theory to compute the nonlinear
lensing bispectrum for dark energy models. Accurate model predictions of the
bispectrum in the moderately nonlinear regime, calibrated with numerical
simulations, will be needed to realize the parameter accuracy we have
estimated. Finally, we estimate how well the lensing bispectrum can constrain a
model with primordial non-Gaussianity.


title:
Thermal Timescale Mass Transfer and the Evolution of White Dwarf
  Binaries

abstract:
  The evolution of binaries consisting of evolved main sequence stars (1 <
M_d/Msun < 3.5) with white dwarf companions (0.7 < M_wd/Msun < 1.2) is
investigated through the thermal mass transfer phase. Taking into account the
stabilizing effect of a strong, optically thick wind from the accreting white
dwarf surface, we have explored the formation of several evolutionary groups of
systems for progenitors with initial orbital periods of 1 and 2 days. The
numerical results show that CO white dwarfs can accrete sufficient mass to
evolve to a Type Ia supernova and ONeMg white dwarfs can be built up to undergo
accretion induced collapse for donors more massive than about 2 Msun. For
donors less massive than ~2 Msun the system can evolve to form a He and CO or
ONeMg white dwarf pair. In addition, sufficient helium can be accumulated (~0.1
Msun) in systems characterized by 1.6 < M_d/Msun < 1.9 and 0.8 < M_wd/Msun < 1
such that sub Chandrasekhar mass models for Type Ia supernovae, involving off
center helium ignition, are possible for progenitor systems evolving via the
Case A mass transfer phase. For systems characterized by mass ratios > 3 the
system likely merges as a result of the occurrence of a delayed dynamical mass
transfer instability. A semi-analytical model is developed to delineate these
phases which can be easily incorporated in population synthesis studies of
these systems.


title:
The Exact Evolution Equation of the Curvature Perturbation for Closed
  Universe

abstract:
  As is well known, the exact evolution equation of the curvature perturbation
plays a very important role in investigation of the inflation power spectrum of
the flat universe. However, its corresponding exact extension for the non-flat
universes has not yet been given out clearly. The interest in the non-flat,
specially closed, universes is being aroused recently. The need of this
extension is pressing. We start with most elementary physical consideration and
obtain finally this exact evolution equation of the curvature perturbation for
the non-flat universes, as well as the evolutionary controlling parameter and
the exact expression of the variable mass in this equation. We approximately do
a primitive and immature analysis on the power spectrum of non-flat universes.
This analysis shows that this exact evolution equation of the curvature
perturbation for the non-flat universes is very complicated, and we need to do
a lot of numerical and analytic work for this new equation in future in order
to judge whether the universe is flat or closed by comparison between theories
and observations.


title:
Tests of stellar model atmospheres by optical interferometry: VLTI/VINCI
  limb-darkening measurements of the M4 giant psi phe

abstract:
  We present K-band interferometric measurements of the limb-darkened intensity
profile of the M4 giant star psi Phoenicis obtained with VLTI/VINCI.
High-precision squared visibility amplitudes in the second lobe of the
visibility function were obtained employing two 8.2 m UTs. This succeeded one
month after light from UTs was first combined for interferometric fringes. In
addition, we sampled the visibility function at small spatial frequencies using
the 40cm test siderostats. Our measurement constrains the diameter of the star
as well as its CLV. We construct a spherical hydrostatic PHOENIX model
atmosphere based on spectrophotometric data from the literature and confront
its CLV prediction with our interferometric measurement. We compare as well CLV
predictions by plane-parallel hydrostatic PHOENIX, ATLAS9, and ATLAS12 models.
We find that the Rosseland angular diameter as predicted by comparison of the
spherical PHOENIX model with spectrophotometry is in good agreement with our
interferometric diameter measurement. The shape of our measured visibility
function in the second lobe is consistent with all considered PHOENIX and ATLAS
model predictions, and significantly different from UD and FDD models. We
derive high-precision fundamental parameters for psi Phe, namely a Rosseland
angular diameter of 8.13 +/- 0.2 mas, with the Hipparcos parallax corresponding
to a Rosseland linear radius R of 86 +/- 3 Rsun and an effective temperature of
3550 +/- 50 K, with R corresponding to a luminosity of log (L/Lsun)=3.02 +/-
0.06. Together with evolutionary models, these values are consistent with a
mass of 1.3 +/- 0.2 Msun, and a surface gravity of log g = 0.68 +/- 0.11.


title: The Luminosity Function of PNe with different morphology

abstract:
  We have analyzed the behaviour of various parameters of PNe in the Magellanic
Clouds (MCs) and the Galaxy as a function of their morphology. The luminosity
function of different morphological types has been built, finding that
elliptical and round PNe dominate the bright cutoff both in the MCs and in the
Galaxy. The dependence of the [OIII] absolute magnitude on chemical abundances
has been investigated.


title: The ANTARES neutrino project: status report

abstract:
  The ANTARES project aims to build a deep underwater Cherenkov neutrino
telescope in the Mediterranean Sea. Currently the experiment is in the
construction phase and has recently achieved two important milestones. The
electro-optical cable to shore and the junction box that will distribute power
to detector strings and allow data transmission have been deployed at the sea
floor. A prototype string and a string for environmental parameter measurement
have been deployed, connected to the cable using a manned submarine. Data have
been sent to shore. The final ANTARES detector consisting in 12 strings each
equipped with 75 photomultiplier tubes is planned to be fully deployed and
taking data by the end of 2006.


title: High-z massive galaxies in the HDF-South

abstract:
  [abr] We report the analysis of three galaxies selected in the Hubble Deep
Field South at Ks<22 on the basis of their unusually red near-IR color J-K>3.
We have used population synthesis models to constrain their redshifts and their
stellar masses. One galaxy is at redshift z_p~2.4 while the other two are at
z_p~2.9-3.0. All three galaxies have already assembled a stellar mass of about
10^{11} M_sun at the observed redshift placing the possible merging event of
their formation at z>3.5. The inferred mass weighted age of their stellar
populations implies that the bulk of the stars formed at z_f>3.5. The resulting
co-moving density of M_{stars}>10^{11} M_sun galaxies at <z>~2.7 is
rho=1.2(+-0.7)x10^{-4} Mpc^{-3}, about a factor two higher than the predictions
of hierarchical models. The comparison with the local density of galaxies
implies that the three galaxies must have already formed most of their stellar
mass and that they cannot follow an evolution significantly different from a
passive aging.The comparison with the density of local L>L* early types
(passively evolved galaxies) suggests that their co-moving density cannot
decrease by more than a factor 2.5-3 from z=0 to z~3 and that up to 40% of the
stellar mass content of bright (L>L*) local early type galaxies was already in
place at z>2.5.


title: A puzzling periodicity in the pulsating DA white dwarf G 117-B15A

abstract:
  We present time-resolved optical spectrophotometry of the pulsating hydrogen
atmosphere (DA) white dwarf G 117-B15A. We find three periodicities in the
pulsation spectrum (215s, 272s, and 304s) all of which have been found in
earlier studies. By comparing the fractional wavelength dependence of the
pulsation amplitudes (chromatic amplitudes) with models, we confirm a previous
report that the strongest mode, at 215s, has l=1. The chromatic amplitude for
the 272s mode is very puzzling, showing an increase in fractional amplitude
with wavelength that cannot be reproduced by the models for any l at optical
wavelengths. Based on archival HST data, we show that while the behaviour of
the 215s mode at ultra-violet wavelengths is as expected from models, the weird
behaviour of the 272s periodicity is not restricted to optical wavelengths in
that it fails to show the expected increase in fractional amplitude towards
shorter wavelengths. We discuss possible causes for the discrepancies found for
the 272s variation, but find that all are lacking, and conclude that the nature
of this periodicity remains unclear.


title: Neutrino physics from cosmology

abstract:
  Cosmological observations have in the past few years become an increasingly
powerful method for determining parameters within the neutrino sector, such as
the presence of sterile states and the mass of neutrinos. I review the current
status of the field in light of recent measurements of the cosmic microwave
background by the WMAP collaboration, as well as current large scale galaxy
surveys.


title: A fitting function for the SNAP data

abstract:
  A mathematically motivated fitting function for analyzing supernovae
distance-redshift data is suggested. It is pointed out that this function can
be useful in analyzing SNAP data. To illustrate our method, we analyze current
experimental data which includes 78 supernovae and 20 radio galaxies. From
these data we obtain vacuum equation of state in a model independent way. We
show that the flat Universe model with a cosmological constant is in a good
agreement with observations.


title: Dust during the Reionization

abstract:
  The possibility that population III stars have reionized the Universe at
redshifts greater than 6 has recently gained momentum with WMAP polarization
results. Here we analyse the role of early dust produced by these stars and
ejected into the intergalactic medium. We show that this dust, heated by the
radiation from the same population III stars, produces a submillimetre excess.
The electromagnetic spectrum of this excess could account for a significant
fraction of the FIRAS (Far Infrared Absolute Spectrophotometer) cosmic far
infrared background above 700 micron. This spectrum, a primary anisotropy
($\Delta T$) spectrum times the $\nu^2$ dust emissivity law, peaking in the
submillimetre domain around 750 micron, is generic and does not depend on other
detailed dust properties. Arcminute--scale anisotropies, coming from
inhomogeneities in this early dust, could be detected by future submillimetre
experiments such as Planck HFI.


title:
The XMM/2dF survey III: Comparison between optical and X-ray cluster
  detection methods

abstract:
  We directly compare X-ray and optical techniques of cluster detection by
combining SDSS photometric data with a wide-field ($\sim 1.8$ deg$^{2}$)
XMM-{\em Newton} survey in the North Galactic Pole region. The optical cluster
detection procedure is based on merging two independent selection methods - a
smoothing+percolation technique, and a Matched Filter Algorithm. The X-ray
cluster detection is based on a wavelet-based algorithm, incorporated in the
SAS v.5.2 package. The final optical sample counts 9 candidate clusters with
richness of more than 20 galaxies, corresponding roughly to APM richness class.
Three, of our optically detected clusters are also detected in our X-ray
survey. The most probable cause of the small number of optical cluster
candidates detected in our X-ray survey is that they are relatively poor
clusters, fainter than the X-ray flux limit (for extended sources) of our
survey $f_{x}(0.3-2 {\rm keV}) \simeq 2 \times 10^{-14} erg cm^{-2} s^{-1}$.


title:
GRB optical and IR rapid follow-up with the 2 m Liverpool Robotic
  Telescope

abstract:
  The Liverpool Telescope, owned and operated by Liverpool John Moores
University and situated at Roque de los Muchachos, La Palma, is the first 2-m,
fully instrumented robotic telescope. We plan to use the LT in conjunction with
Gamma Ray Observatories (HETE-2, INTEGRAL, Swift) to study GRB physics. A
special over-ride mode will enable observations commencing less than a minute
after the GRB alert, including optical and near infrared imaging and
spectroscopy. These observations, together with systematic monitoring of the
burst through the afterglow, will help to unravel the nature of prompt optical
flashes, short bursts, optically dark bursts, redshift distribution, GRB -
supernova connection and other questions related to the GRB phenomenon. In
particular, the combination of aperture, instrumentation and rapid automated
response makes the Liverpool Telescope excellently suited to the investigation
of optically dark bursts and currently optically unstudied short bursts.


title: Kinematics of the faintest gas rich galaxy in the Local Group: DDO210

abstract:
  We present deep, high velocity resolution (~1.6 km/s) Giant Meterwave Radio
Telescope (GMRT) HI 21cm synthesis images of the faint (M_B ~ -10.6) local
group dwarf galaxy DDO210. We find that the HI distribution in the galaxy is
not axi-symmetric, but shows density enhancements in the eastern and southern
halves of the galaxy. The optical emission is lopsided with respect to the HI,
most of the bright optical emission arises from the eastern half of the HI
disk. The velocity field of the galaxy is however quite regular and shows a
systematic large scale pattern, consistent with the rotational motion. The
rotation curve for the galaxy shows a peak (inclination corrected) rotation
velocity of only ~8 km/s, comparable to the random motions in the HI gas. After
correcting for the dynamical support provided by random motions (the
``asymmetric drift'' correction), we find the corrected peak rotation velocity
of ~16.0 km/s. Mass modeling of the corrected rotation curve shows that the
kinematics of DDO210 can be well fit with either a modified isothermal halo
(with a central density rho_0 ~ 29 X 10^{-3} M_\odot pc^{-3} for a stellar mass
to light ratio of 3.4) or an NFW halo. In the case of the NFW halo however, a
good fit is obtained for a wide range of parameters; the halo parameters could
not be uniquely determined from the fit. Density profiles with inner slope
steeper than ~1.2 however provide a poor fit to the data. Finally, the rotation
curve derived using MOND also provides a reasonable fit to the observed
rotation curve.


title: Polar Ring Galaxies and the Tully-Fisher relation

abstract:
  We have investigated the Tully-Fisher relation for Polar Ring Galaxies
(PRGs), based on near infrared, optical and HI data available for a sample of
these peculiar objects. Many PRGs show larger HI line-widths than expected for
the observed K band luminosity, and this result is confirmed by a larger sample
of objects, based on B-band data. This observational evidence may be related to
the dark halo shape and orientation in these systems: the larger rotation
velocities observed in PRGs can be explained by a flattened polar halo, aligned
with the polar ring.


title: A new population of X-ray transients in the Galactic Centre

abstract:
  A comparison of the XMM-Newton and Chandra Galactic Centre (GC) Surveys has
revealed two faint X-ray transients with contrasting properties. The X-ray
spectrum of XMM J174544-2913.0 shows a strong iron line with an equivalent
width of ~2 keV, whereas that of XMM J174457-2850.3 is characterised by a very
hard continuum with photon index ~1.0. The X-ray flux of both sources varied by
more than 2 orders of magnitude over a period of months with a peak X-ray
luminosity of 5 x 10^34 erg/s. We discuss the nature of these peculiar sources.


title: The broad OVI absorber at z = 3.02 toward CTQ 325

abstract:
  We report on the multiphase absorption-line system detected at a redshift z =
3.021 in the spectrum of the quasi-stellar object CTQ 325 (z_em = 3.212). The
system is displaced by ~14,000 km/s to the blue of the systemic velocity
defined by the center of the symmetric OI quasar emission line. It consists of
shallow and broad (~700 km/s, FWHM) absorption lines of HI 1215, CIV 1548,1550,
and OVI 1032,1038, produced by collisionally ionized gas and of narrow
absorption lines (FWHM < 20 km/s) of Ly-alpha, Ly-beta, ..., Ly-6, SiIII 1206,
and CIII 977 produced by photoionized gas. Possible origins of this system are
discussed.


title: Magnetorotational mechanism of supernova type II exlosion

abstract:
  Results of 2D simulations of the magnetorotational mechanism of supernova
type II are presented. Amplification of toroidal magnetic field of the star due
to differential rotation of the star leads to the transformation of the
rotational (gravitational) energy to the energy of the supernova explosion. In
our simulation the energy of the explosion is $1.12 \cdot 10^{51}erg$. The
explosion ejects about $0.11 M_\odot$.


title: Intracluster Stellar Population

abstract:
  I shall review the latest results for the presence of diffuse light in nearby
clusters, and the evidence of ongoing star formation in an intracluster Virgo
field. I shall discuss how intracluster planetary nebulae can be used as
excellent tracers of the diffuse stellar population in nearby clusters. Their
number density distribution, density profile and radial velocity distribution
provide observational constraints to models for cluster formation and
evolution. The preliminary comparison of the avaliable ICPN samples with high
resolution N-body models of a Virgo-like cluster in a Lambda CDM cosmology
supports ``harassment'' as the most likely mechanism for the origin of diffuse
stellar light in clusters.


title:
The hard quiescent spectrum of the neutron-star X-ray transient EXO
  1745-248 in the globular cluster Terzan 5

abstract:
  We present a Chandra observation of the globular cluster Terzan 5 during
times when the neutron-star X-ray transient EXO 1745-248 located in this
cluster was in its quiescent state. We detected the quiescent system with a
(0.5-10 keV) luminosity of ~2 x 10^{33} ergs/s. This is similar to several
other neutron-star transients observed in their quiescent states. However, the
quiescent X-ray spectrum of EXO 1745--48 was dominated by a hard power-law
component instead of the soft component that usually dominates the quiescent
emission of other neutron-star X-ray transients. This soft component could not
conclusively be detected in EXO 1745-248 and we conclude that it contributed at
most 10% of the quiescent flux in the energy range 0.5-10 keV. EXO 1745-248 is
only the second neutron-star transient whose quiescent spectrum is dominated by
the hard component (SAX J1808.4-3658 is the other one). We discuss possible
explanations for this unusual behavior of EXO 1745-248, its relationship to
other quiescent neutron-star systems, and the impact of our results on
understanding quiescent X-ray binaries. We also discuss the implications of our
results on the way the low-luminosity X-ray sources in globular clusters are
classified.


title: A Flux Limited Atlas of Galaxy Cluster Temperature Maps

abstract:
  An atlas of gas temperature maps is presented for a flux limited catalog of
galaxy clusters. The sample of clusters is based on the Edge et al. (1990)
sample, with the inclusion of five additional clusters, all with fluxes
f_X(2-10 keV)>= 1.7x10**-11 ergs sec**-1 cm**-2, drawn from a variety of other
sources. The temperature maps are derived from ASCA GIS observations using a
common methodology to correct for the Point-Spread Function and calculate the
local projected gas temperature in such a way so as to make each cluster
directly comparable to all others in the sample. Variations in the temperature
distribution, when present at > 90% confidence, are characterized by their
severity and extent. We find that 70% of the clusters in our sample have
significant variations in the projected gas temperature. The presence of these
variations increases with increasing luminosity, as does the spatial scope and
severity within a cluster. For a more limited sample we find that one third of
clusters with temperature structure have radio halos. The high rate of
occurance of structure emphasizes the need for caution when using clusters to
measure cosmological parameters.