197 research outputs found
Searching for visual companions of close Cepheids. VLT/NACO lucky imaging of Y~Oph, FF~Aql, X~Sgr, W~Sgr and ~Aql
Aims: High-resolution imaging in several photometric bands can provide color
and astrometric information of the wide-orbit component of Cepheid stars. Such
measurements are needed to understand the age and evolution of pulsating stars.
In addition, binary Cepheids have the potential to provide direct and
model-independent distances and masses. Methods: We used the NAOS-CONICA
adaptive optics instrument (NACO) in the near-infrared to perform a deep search
for wide components around the classical Cepheids, Y~Oph, FF~Aql, X~Sgr, W~Sgr,
and ~Aql, within a field of view (FoV) of ( for ~Aql). Results: We were able to reach contrast -8\,mag and -7\,mag in the radius range ,
which enabled us to constrain the presence of wide companions. For Y~Oph,
FF~Aql, X~Sgr, W~Sgr, and ~Aql at , we ruled out the presence
of companions with a spectral type that is earlier than a B7V, A9V, A9V, A1V,
and G5V star, respectively. For , no companions earlier than
O9V, B3V, B4V, B2V, and B2V star, respectively, are detected. A component is
detected close to ~Aql at projected separation \,mas and a position angle . We estimated its
dereddened apparent magnitude to be and derived a
spectral type that ranges between an F1V and F6V star. Additional photometric
and astrometric measurements are necessary to better constrain this star and
check its physical association to the ~Aql system.Comment: Accepted for publication in Astronomy and Astrophysic
Investigating Cepheid Carinae's Cycle-to-cycle Variations via Contemporaneous Velocimetry and Interferometry
Baade-Wesselink-type (BW) techniques enable geometric distance measurements
of Cepheid variable stars in the Galaxy and the Magellanic clouds. The leading
uncertainties involved concern projection factors required to translate
observed radial velocities (RVs) to pulsational velocities and recently
discovered modulated variability. We carried out an unprecedented observational
campaign involving long-baseline interferometry (VLTI/PIONIER) and spectroscopy
(Euler/Coralie) to search for modulated variability in the long-period (P
35.5 d) Cepheid Carinae. We determine highly precise angular diameters
from squared visibilities and investigate possible differences between two
consecutive maximal diameters, . We characterize the
modulated variability along the line-of-sight using 360 high-precision RVs.
Here we report tentative evidence for modulated angular variability and confirm
cycle-to-cycle differences of Carinae's RV variability. Two successive
maxima yield = 13.1 0.7 (stat.) {\mu}as for
uniform disk models and 22.5 1.4 (stat.) {\mu}as (4% of the total angular
variation) for limb-darkened models. By comparing new RVs with 2014 RVs we show
modulation to vary in strength. Barring confirmation, our results suggest the
optical continuum (traced by interferometry) to be differently affected by
modulation than gas motions (traced by spectroscopy). This implies a previously
unknown time-dependence of projection factors, which can vary by 5% between
consecutive cycles of expansion and contraction. Additional interferometric
data are required to confirm modulated angular diameter variations. By
understanding the origin of modulated variability and monitoring its long-term
behavior, we aim to improve the accuracy of BW distances and further the
understanding of stellar pulsations.Comment: Accepted for publication in MNRAS. 19 pages, 13 figures, 10 table
Cepheid limb darkening, angular diameter corrections, and projection factor from static spherical model stellar atmospheres
Context. One challenge for measuring the Hubble constant using Classical
Cepheids is the calibration of the Leavitt Law or period-luminosity
relationship. The Baade-Wesselink method for distance determination to Cepheids
relies on the ratio of the measured radial velocity and pulsation velocity, the
so-called projection factor and the ability to measure the stellar angular
diameters. Aims. We use spherically-symmetric model stellar atmospheres to
explore the dependence of the p-factor and angular diameter corrections as a
function of pulsation period. Methods. Intensity profiles are computed from a
grid of plane-parallel and spherically-symmetric model stellar atmospheres
using the SAtlas code. Projection factors and angular diameter corrections are
determined from these intensity profiles and compared to previous results.
Results. Our predicted geometric period-projection factor relation including
previously published state-of-the-art hydrodynamical predictions is not with
recent observational constraints. We suggest a number of potential resolutions
to this discrepancy. The model atmosphere geometry also affects predictions for
angular diameter corrections used to interpret interferometric observations,
suggesting corrections used in the past underestimated Cepheid angular
diameters by 3 - 5%. Conclusions. While spherically-symmetric hydrostatic model
atmospheres cannot resolve differences between projection factors from theory
and observations, they do help constrain underlying physics that must be
included, including chromospheres and mass loss. The models also predict more
physically-based limb-darkening corrections for interferometric observations.Comment: 8 pages, 6 figures, 2 tables, accepted for publication in A&
The long-period Galactic Cepheid RS Puppis - III. A geometric distance from HST polarimetric imaging of its light echoes
As one of the most luminous Cepheids in the Milky Way, the 41.5-day RS Puppis
is an analog of the long-period Cepheids used to measure extragalactic
distances. An accurate distance to this star would therefore help anchor the
zero-point of the bright end of the period-luminosity relation. But, at a
distance of about 2 kpc, RS Pup is too far away for measuring a direct
trigonometric parallax with a precision of a few percent with existing
instrumentation. RS Pup is unique in being surrounded by a reflection nebula,
whose brightness varies as pulses of light from the Cepheid propagate outwards.
We present new polarimetric imaging of the nebula obtained with HST/ACS. The
derived map of the degree of linear polarization pL allows us to reconstruct
the three-dimensional structure of the dust distribution. To retrieve the
scattering angle from the pL value, we consider two different polarization
models, one based on a Milky Way dust mixture and one assuming Rayleigh
scattering. Considering the derived dust distribution in the nebula, we adjust
a model of the phase lag of the photometric variations over selected nebular
features to retrieve the distance of RS Pup. We obtain a distance of 1910 +/-
80 pc (4.2%), corresponding to a parallax of 0.524 +/- 0.022 mas. The agreement
between the two polarization models we considered is good, but the final
uncertainty is dominated by systematics in the adopted model parameters. The
distance we obtain is consistent with existing measurements from the
literature, but light echoes provide a distance estimate that is not subject to
the same systematic uncertainties as other estimators (e.g. the Baade-Wesselink
technique). RS Pup therefore provides an important fiducial for the calibration
of systematic uncertainties of the long-period Cepheid distance scale.Comment: 14 pages, 14 figures, accepted for publication in Astronomy &
Astrophysic
Using limb darkening to measure fundamental parameters of stars
Context. Limb darkening is an important tool for understanding stellar
atmospheres, but most observations measuring limb darkening assume various
parameterizations that yield no significant information about the structure of
stellar atmospheres. Aims. We use a specific limb-darkening relation to study
how the best-fit coefficients relate to fundamental stellar parameters from
spherically symmetric model stellar atmospheres. Methods. Using a grid of
spherically symmetric Atlas model atmospheres, we compute limb-darkening
coefficients, and develop a novel method to predict fundamental stellar
parameters. Results. We find our proposed method predicts the mass of stellar
atmosphere models given only the radius and limb-darkening coefficients,
suggesting that microlensing, interferometric, transit and eclipse observations
can constrain stellar masses. Conclusions. This novel method demonstrates that
limb-darkening parameterizations contain important information about the
structure of stellar atmospheres, with the potential to be a valuable tool for
measuring stellar masses.Comment: 8 pages, 6 figures, 2 tables, A&A accepte
Mid-infrared interferometry with K band fringe-tracking I. The VLTI MIDI+FSU experiment
Context: A turbulent atmosphere causes atmospheric piston variations leading
to rapid changes in the optical path difference of an interferometer, which
causes correlated flux losses. This leads to decreased sensitivity and accuracy
in the correlated flux measurement. Aims: To stabilize the N band
interferometric signal in MIDI (MID-infrared Interferometric instrument), we
use an external fringe tracker working in K band, the so-called FSU-A (fringe
sensor unit) of the PRIMA (Phase-Referenced Imaging and Micro-arcsecond
Astrometry) facility at VLTI. We present measurements obtained using the newly
commissioned and publicly offered MIDI+FSU-A mode. A first characterization of
the fringe-tracking performance and resulting gains in the N band are
presented. In addition, we demonstrate the possibility of using the FSU-A to
measure visibilities in the K band. Methods: We analyzed FSU-A fringe track
data of 43 individual observations covering different baselines and object K
band magnitudes with respect to the fringe-tracking performance. The N band
group delay and phase delay values could be predicted by computing the relative
change in the differential water vapor column density from FSU-A data.
Visibility measurements in the K band were carried out using a scanning mode of
the FSU-A. Results: Using the FSU-A K band group delay and phase delay
measurements, we were able to predict the corresponding N band values with high
accuracy with residuals of less than 1 micrometer. This allows the coherent
integration of the MIDI fringes of faint or resolved N band targets,
respectively. With that method we could decrease the detection limit of
correlated fluxes of MIDI down to 0.5 Jy (vs. 5 Jy without FSU-A) and 0.05 Jy
(vs. 0.2 Jy without FSU-A) using the ATs and UTs, respectively. The K band
visibilities could be measured with a precision down to ~2%.Comment: 11 pages, 13 figures, Accepted for publication in A&
Calibrating the projection factor for Galactic Cepheids
The projection factor (p), which converts the radial velocity to pulsational
velocity, is an important parameter in the Baade-Wesselink (BW) type analysis
and distance scale work. The p-factor is either adopted as a constant or
linearly depending on the logarithmic of pulsating periods. The aim of this
work is to calibrate the p-factor if a Cepheid has both the BW distance and an
independent distance measurement, and examine the p-factor for delta Cephei --
the prototype of classical Cepheids. We calibrated the p-factor for several
Galactic Cepheids that have both the latest BW distances and independent
distances either from Hipparcos parallaxes or main-sequence fitting distances
to Cepheid-hosted stellar clusters. Based on 25 Cepheids, the calibrated
p-factor relation is consistent with latest p-factor relation in literature.
The calibrated p-factor relation also indicates that this relation may not be
linear and may exhibit an intrinsic scatter. We also examined the discrepancy
of empirical p-factors for delta Cephei, and found that the reasons for this
discrepancy include the disagreement of angular diameters, the treatment of
radial velocity data, and the phase interval adopted during the fitting
procedure. Finally, we investigated the impact of the input p-factor in two BW
methodologies for delta Cephei, and found that different p-factors can be
adopted in these BW methodologies and yet result in the same angular diameters.Comment: 6 pages, 6 figures and 2 tables. A&A accepte
Stellar parameters of Be stars observed with X-shooter
Aims. The X-shooter archive of several thousand telluric star spectra was
skimmed for Be and Be-shell stars to derive the stellar fundamental parameters
and statistical properties, in particular for the less investigated late type
Be stars, and the extension of the Be phenomenon into early A stars. Methods.
An adapted version of the BCD method is used, utilizing the Balmer
discontinuity parameters to determine effective temperature and surface
gravity. This method is optimally suited for late B stars. The projected
rotational velocity was obtained by profile fitting to the Mg ii lines of the
targets, and the spectra were inspected visually for the presence of peculiar
features such as the infrared Ca ii triplet or the presence of a double Balmer
discontinuity. The Balmer line equivalent widths were measured, but due to
uncertainties in determining the photospheric contribution are useful only in a
subsample of Be stars for determining the pure emission contribution. Results.
A total of 78 Be stars, mostly late type ones, were identified in the X-shooter
telluric standard star archive, out of which 48 had not been reported before.
The general trend of late type Be stars having more tenuous disks and being
less variable than early type ones is confirmed. The relatively large number
(48) of relatively bright (V > 8.5) additional Be stars casts some doubt on the
statistics of late type Be stars; they are more common than currently thought:
The Be/B star fraction may not strongly depend on spectral subtype.Comment: Accepted for publication in A&
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