93 research outputs found
The Hipparcos parallax for Polaris
This letter follows a recent claim that the Hipparcos parallax for Polaris
could be too small by 2.5 mas. It examines in detail the Hipparcos epoch
astrometric data for Polaris, as well as the viability of other observations
that were put forward to support a larger parallax. The Hipparcos determination
of the Polaris parallax is shown to be sufficiently robust to fully exclude a
significantly larger parallax, and there is no observational support from other
observations, such as a supposed presence of a cluster, either.Comment: 3 pages, 6 figures, Accepted for publication by A&
Cepheid Parallaxes and the Hubble Constant
Revised Hipparcos parallaxes for classical Cepheids are analysed together
with 10 HST-based parallaxes (Benedict et al.). In a reddening-free V,I
relation we find that the coefficient of logP is the same within the
uncertainties in our Galaxy as in the LMC, contrary to some previous
suggestions. Cepheids in the inner region of NGC4258 with near solar
metallicities (Macri et al.) confirm this result. We obtain a zero-point for
the reddening-free relation and apply it to Cepheids in galaxies used by
Sandage et al. to calibrate the absolute magnitudes of SNIa and to derive the
Hubble constant. We revise their result from 62 to 70+/-5 km/s/Mpc. The
Freedman et al. 2001 value is revised from 72 to 76+/-8 km/s/Mpc. These results
are insensitive to Cepheid metallicity corrections. The Cepheids in the inner
region of NGC4258 yield a modulus of 29.22+/-0.03(int) compared with a
maser-based modulus of 29.29+/-0.15. Distance moduli for the LMC, uncorrected
for any metallicity effects, are; 18.52+/-0.03 from a reddening-free relation
in V,I; 18.47+/-0.03 from a period-luminosity relation at K; 18.45+/-0.04 from
a period-luminosity-colour relation in J,K. Adopting a metallicity correction
in V,I from Marci et al. leads to a true LMC modulus of 18.39+/-0.05.Comment: 9 pages, 1 figure, on-line material from [email protected].
Accepted for MNRA
Impact of basic angle variations on the parallax zero point for a scanning astrometric satellite
Determination of absolute parallaxes by means of a scanning astrometric
satellite such as Hipparcos or Gaia relies on the short-term stability of the
so-called basic angle between the two viewing directions. Uncalibrated
variations of the basic angle may produce systematic errors in the computed
parallaxes. We examine the coupling between a global parallax shift and
specific variations of the basic angle, namely those related to the satellite
attitude with respect to the Sun. The changes in observables produced by small
perturbations of the basic angle, attitude, and parallaxes are calculated
analytically. We then look for a combination of perturbations that has no net
effect on the observables. In the approximation of infinitely small fields of
view, it is shown that certain perturbations of the basic angle are
observationally indistinguishable from a global shift of the parallaxes. If
such perturbations exist, they cannot be calibrated from the astrometric
observations but will produce a global parallax bias. Numerical simulations of
the astrometric solution, using both direct and iterative methods, confirm this
theoretical result. For a given amplitude of the basic angle perturbation, the
parallax bias is smaller for a larger basic angle and a larger solar aspect
angle. In both these respects Gaia has a more favourable geometry than
Hipparcos. In the case of Gaia, internal metrology is used to monitor basic
angle variations. Additionally, Gaia has the advantage of detecting numerous
quasars, which can be used to verify the parallax zero point.Comment: 8 pages, 2 figures; Accepted for publication in Astronomy &
Astrophysic
Fiber Optic Spectroscopy for the Optimization of Photodynamic Therapy
__Abstract__
Photodynamic
therapy
(PDT)
is
a
treatment
modality
for
cancer
and
premalignant
lesions
that
utilizes
a
photoactive
drug,
the
photosensitizer,
in
combination
with
light.
PDT
has
become
the
treatment
of
choice
for
various
malignancies.
Furthermore,
PDT
is
under
investigation
as
a
potential
(palliative)
treatment
in
situations
where
the
possibilities
of
chemo-Â
and
radiotherapy
are
limited
or
exhausted.
Since
both
photosensitizer
and
light
have
to
be
present
to
cause
tissue
damage,
selective
damage
to
the
lesion
can
be
achieved
by
controlling
the
presence
of
either
one
of
them
to
the
treatment
area.
Selective
damage
can
be
reached
by
i)
choosing
a
photosensitizer
that
is
mainly
present
in
the
lesion,
or
ii)
preventing
normal
tissue
from
being
illuminated.
However,
the
success
of
PDT
in
reducing/removing
(pre-Ââ)malignant
lesions
has
been
variable.
Treatment
efficacy
can
range
form
non-âobservable
effects
to
severe
damage
to
normal
tissue.
Considering
the
complexity
of
both
the
execution
of
the
treatment
and
damage
pathways
involved
in
PDT,
some
variability
in
treatment
efficacy
is
not
unexpected.
However,
given
the
fact
that
clinical
applications
of
PDT
that
have
proved
successful
remain
small
in
number,
more
work
is
necessary
to
optimize
therapeutic
efficacy
AGB Variables and the Mira Period-Luminosity Relation
Published data for large amplitude asymptotic giant branch variables in the
Large Magellanic Cloud are re-analysed to establish the constants for an
infrared (K) period-luminosity relation of the form: Mk=rho[log P-2.38] +
delta. A slope of rho=-3.51+/-0.20 and a zero point of delta=-7.15+/-0.06 are
found for oxygen-rich Miras (if a distance modulus of 18.39+/-0.05 is used for
the LMC). Assuming this slope is applicable to Galactic Miras we discuss the
zero-point for these stars using the revised Hipparcos parallaxes together with
published VLBI parallaxes for OH Masers and Miras in Globular Clusters. These
result in a mean zero-point of delta=-7.25+/-0.07 for O-rich Galactic Miras.
The zero-point for Miras in the Galactic Bulge is not significantly different
from this value.
Carbon-rich stars are also discussed and provide results that are consistent
with the above numbers, but with higher uncertainties. Within the uncertainties
there is no evidence for a significant difference between the period-luminosity
relation zero-points for systems with different metallicity.Comment: 15 pages, 3 figures, accepted for MNRA
A study of the F-giant star Ξ Scorpii A: a post-merger rapid rotator?
We report high-precision observations of the linear polarization of the F1III star Ξ Scorpii. The polarization has a wavelength dependence of the form expected for a rapid rotator, but with an amplitude several times larger than seen in otherwise similar main-sequence stars. This confirms the expectation that lower-gravity stars should have stronger rotational-polarization signatures as a consequence of the density dependence of the ratio of scattering to absorption opacities. By modelling the polarization, together with additional observational constraints (incorporating a revised analysis of Hipparcos astrometry, which clarifies the system's binary status), we determine a set of precise stellar parameters, including a rotation rate Ï (= Ω/Ωc â„ 0.94, polar gravity log (gp)= 2.091 +0.042-0.039 (dex cgs), mass 3.10 +0.37-0.32 Mâ, and luminosity log (L/Lâ) =3.149+0.041-0.028. These values are incompatible with evolutionary models of single rotating stars, with the star rotating too rapidly for its evolutionary stage, and being undermassive for its luminosity. We conclude that Ξ Sco A is most probably the product of a binary merger
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