A&A 453, 309-319 (2006)
DOI: 10.1051/0004-6361:20054333
N. Nardetto1 - D. Mourard1 - P. Kervella2 - Ph. Mathias1 - A. Mérand2 - D. Bersier3,4
1 - Observatoire de la Côte d'Azur, Dept. Gemini, UMR 6203,
06130 Grasse, France
2 -
Observatoire de Paris-Meudon, LESIA, UMR
8109, 5 place Jules Janssen, 92195 Meudon Cedex, France
3 -
Space Telescope Science Institute, 3700 San Martin Drive,
Baltimore, MD
21218, USA
4 -
Astrophysics Research Institute, Liverpool John Moores
University, Twelve Quays House, Egerton Wharf, Birkenhead,
CH41 1LD, UK
Received 11 October 2005 / Accepted 11 March 2006
Abstract
Context. The ratio of pulsation to radial velocity (the projection factor) is currently limiting the accuracy of the Baade-Wesselink method, and in particular of its interferometric version recently applied to several nearby Cepheids.
Aims. This work aims at establishing a link between the line asymmetry evolution over the Cepheids' pulsation cycles and their projection factor, with the final objective to improve the accuracy of the Baade-Wesselink method for distance determinations.
Methods. We present HARPS high spectral resolution observations (R=120 000) of nine galactic Cepheids: R Tra, S Cru, Y Sgr,
Dor,
Gem, Y Oph, RZ Vel,
Car and RS Pup, having a good period sampling (P=3.39d to P=41.52d). We fit spectral line profiles by an asymmetric bi-Gaussian to derive radial velocity, Full-Width at Half-Maximum in the line (FWHM) and line asymmetry for all stars. We then extract correlations curves between radial velocity and asymmetry. A geometric model providing synthetic spectral lines, including limb-darkening, a constant FWHM (hereafter
)
and the rotation velocity is used to interpret these correlations curves.
Results. For all stars, comparison between observations and modelling is satisfactory, and we were able to determine the projected rotation velocities and
for all stars. We also find a correlation between the rotation velocity (
)
and the period of the star:
[km s-1]. Moreover, we observe a systematic shift in observational asymmetry curves (noted
), related to the period of the star, which is not explained by our static model:
.
For long-period Cepheids, in which velocity gradients, compression or shock waves seem to be large compared to short- or medium-period Cepheids we observe indeed a greater systematic shift in asymmetry curves.
Conclusions. This new way of studying line asymmetry seems to be very promising for a better understanding of Cepheids atmosphere and to determine, for each star, a dynamic projection factor.
Key words: techniques: spectroscopic - stars: atmospheres - stars: oscillations - stars: variables: Cepheids - stars: distances
Long-baseline interferometers currently provide a new quasi-geometric way to calibrate the Cepheid Period-Luminosity relation. Indeed, it is now possible to determine the distance of galactic Cepheids up to 1kpc with the Interferometric Baade-Wesselink method, hereafter IBW method (see for e.g. Sasselov & Karovska 1994; and Kervella et al. 2004, hereafter Paper I). Interferometric measurements lead to angular diameter estimations over the whole pulsation period, while the stellar radius variations can be deduced from the integration of the pulsation velocity. The latter is linked to the observational velocity deduced from line profiles by the projection factor p. In this method, angular and linear diameters have to correspond to the same layer in the star to provide a correct estimate of the distance.
Table 1: Observed sample of Cepheids sorted by increasing period.
The spectral line profile, in particular its asymmetry, is critically affected by the dynamical structure of Cepheids' atmosphere: photospheric pulsation velocity (hereafterThe interferometric definition of the projection factor is of crucial importance in the IBW method, as it can induce a bias of up to 6% on the derived distance (Nardetto et al. 2004; Mérand et al. 2005). Otherwise, the limb-darkening is also required to derive a correct estimation of the angular diameter of the star. With the latest generation of long-baseline interferometers, studying its phase-dependence is of crucial importance (Marengo et al. 2002, 2003; Nardetto et al. 2006).
Line asymmetry was first observed for short-period cepheids by Sasselov et al. (1989). Then, Sasselov et al. (1990) studied the impact of the asymmetry on radius and distances determinations. The link between line profiles asymmetry and the projection factor has been studied by Albrow et al. (1994). Finally, an error analysis of the IBW method is given in Marengo et al. (2004).
We present here a new original study of the line asymmetry using the very high spectral resolution of HARPS (R=120 000). We have observed 9 galactic Cepheids with periods ranging from P=3.39 d to P=41.52 d. Radial velocity, full-width at half-maximum (hereafter FWHM) and line asymmetry are presented for all stars in Sect. 2.
Section 3 deals with modelling and Sect. 4 with observations interpretation. Through a geometric model different definitions of the projection factor are proposed and compared in order to find the best procedure. Then the model is used to interpret observational radial velocity and asymmetry correlation curves. A set of parameters is thus derived for all stars. Taking into account the whole sample of stars we discuss general properties and in particular the period-dependencies.
HARPS is a spectrometer dedicated to the search for extrasolar planets by means of radial velocity measurements. It is installed at the Coudé room of the 3.6 m telescope at La Silla. The resolution is R=120 000 and the average Signal to Noise Ratio we obtain over all observations in the continuum (292 spectra) is 300 per pixel. The observed sample of Cepheids is presented in Table 1.
We have used the standard ESO/HARPS pipe-line reduction package with a special attention for the normalization process. We have noted on metallic line profiles of all stars a good reproduction from cycle-to-cycle. Therefore, spectra for a given star have been recomposed into an unique cycle.
Using Kurucz models (1992) we have identified about 150 unblended spectral lines. This first study considers only the unblended metallic line Fe I 6056.005 Å.
Several methods have been used to measure radial velocities of
Cepheids, each having advantages and drawbacks. Among these methods
there is the line minimum (usually determined via a parabolic fit to
a few pixels near the bottom of the line) a Gaussian fit (obviously
not adequate for asymmetric lines), the line centroid, determined
from the integration of the line profile (requires high
ratio), and the line bisector where one measures the
width of the line at one or several depths. Our bi-Gaussian approach
combines advantages of methods useful for low
data while
providing information usually associated with high resolution and
high
data (asymmetry).
Radial velocity, full width at half-maximum (FWHM) and asymmetry
have been derived simultaneously applying a classical minimization algorithm between the observed line profile (
)
and a modelled spectral line profile (
).
The corresponding reduced
is:
The analytic line profile is defined by:
There are different ways to define the line asymmetry (see e.g.
Sasselov et al. 1990; Sabbey et al. 1995). The advantage of the
bi-Gaussian method is that it offers the possibility to derive
statistical uncertainties directly from the minimization process.
Moreover, all parameters (
,
FWHM, D and A) are fitted simultaneously leading to a very consistent set
of information. The largest reduced
we obtain with this
method is of about 10 corresponding to a
of 438, but in
most cases we have a reduced
or 2 corresponding
to a
ranging from 75 to 350. That means that our analytic
model is well suited to the data quality. We note also that the
reduced
is not sensitive to the spectral line resolution.
As an example, Fig. 1 presents line profile
variation for Dor together with the analytic spectral line
profile. We find that the asymmetry is insensitive to the choice of
the continuum. However, this one has to be correctly defined to
derive correct values of the
and line depth D.
![]() |
Figure 1:
Spectral line evolution of ![]() |
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Another radial velocity definition, the centroid velocity (
)
or, the first moment of the spectral line
profile, has been estimated as:
As indicated in the previous section, we can derive three types of
radial velocity: the velocity associated to the Gaussian fit (
), the line minimum (
)
and the
barycenter of the spectral line (
). Figure 2 shows these radial velocity curves obtained in the
case of
Dor. Figure 3 represents for each
star of our sample, the
variation (arbitrary
shifted). The solid lines are the interpolated curves using a
periodic cubic spline function. This function is calculated either
directly on the observational points (e.g.
Dor) or using
arbitrary pivot points (e.g. RZ Vel). In the latter case, a
classical minimization process between observations and the
interpolated curve is used to optimize the position of the pivot
points. All the interpolated curves presented in this study are
derived using one of these two methods. The only exception is Y Oph
(too few points) for which we performed a linear interpolation.
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Figure 2:
![]() ![]() ![]() ![]() ![]() ![]() |
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Figure 3:
Radial velocity curves (
![]() |
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Figure 4 presents the FWHM curve as a function of
phase for all stars. We note that the largest FWHM values are
obtained for the maximum contraction velocities. RS Pup, the longest
period Cepheid of our sample, seems to present an important
compression or shock wave signature. Figure 5
presents line profile variation for this star. Unfortunately the
phase coverage is not very good, but we can clearly see a strong
increase of the FWHM at .
Such phenomenon has been
already detected in
Cepheids (Fokin et al. 2004).
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Figure 4: FWHM versus phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to a zero FWHM. Note the particular case of RS Pup, which may present the signature of an important compression or shock wave. RS Pup has the longest period of our sample. |
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Figure 5:
FeI 6056.005 Å spectral line evolution of RS Pup. The
vertical line at the top corresponds to a differential flux of 0.2. We note the broadening of the line at ![]() |
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Figure 6: Asymmetry against phase for all stars. Curves have been arbitrarily shifted vertically. The horizontal lines correspond to an asymmetry of zero. |
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Figure 6 shows the asymmetry variation for all stars.
Generally speaking, the shape of the aymmetry curve is similar to
the shape of the velocity curve
.
As already mentioned in Sect. 2.3, the radial velocity
according to the choice of the method considered is sensitive to the
line asymmetry. Figure 7 shows the
correlation between the differences of radial velocity (
)
and the asymmetry of the line. We
have only presented here the case of
Car and RS Pup. Each
star presents a similar behavior. A typical difference in velocity
of about 4 km s-1 can be obtained for an asymmetry of
in extreme cases (Y Sgr and R TrA). The relation between the radial
velocity difference and the asymmetry is certainly affected by star
characteristics (rotation, FWHM, velocity gradients) present in the
line asymmetry. In particular RS Pup signature is certainly affected
by strong velocity gradient effects. The fact that the
and
radial velocities present such differences
as a function of the pulsation phase is an additional difficulty
concerning an average projection factor and its time-dependence
determination. With the centroid estimator of the radial velocity
(
or
)
results are quite similar.
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Figure 7:
Difference between the radial velocity obtained with the
line minimum and the Gaussian fit methods as a function of the
asymmetry in the case of ![]() ![]() |
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In next sections, we summarize all observational results in correlation diagrams between radial velocity and asymmetry. These correlations are interpreted using the geometric model in order to determine some physical parameters of our stars and to obtain information about dynamical effects in Cepheids atmosphere.
We consider a limb-darkened pulsating star in rotation with an one-layer atmosphere. Our model has four parameters:
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Figure 8:
The weighting or the synthetic spectral line profile in
different cases, considering a) the pulsation velocity, b) the
limb-darkening, c) the rotation and, d) an intrinsic width for the
line (
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We now consider a pulsation velocity curve defined by:
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Figure 9:
The projection factor corresponding to the centroid
velocity (![]() ![]() |
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Figure 10:
Results of the geometric model of pulsating star. a), b)
The radial velocity-asymmetry correlation curves for different
![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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Firstly, we note that the
of the line and the
rotation have different effects on the slope and/or shape of the
correlation curves.
Secondly, correlation curves are slightly different from one
definition of
radial velocity to another. But the interesting point
is that the
velocity does not depend of
and/or rotation. This behavior is clearly seen
on diagrams 10b and 10d: the centroid
projection factor
is constant with the
and the rotation while the Gaussian and the
minimum projection factors,
and
,
are
varying. For the Cepheids of our sample the centroid projection
factor ranges from
(
uV=0.64;
R TrA) to
(
uV=0.75;
Car),
through the following relation:
This behavior is of great importance in the context of the IBW
method. Indeed, the community has often used the
value of the projection factor (Burki et al. 1982)
using the Gaussian method instead of the centroid method. As seen
here, and already pointed out by Burki et al. (1982), this
estimator is biased by the rotation velocity, even if Cepheids are
supposed to be slow rotators, and also by the
.
We thus recommend the centroid based methods (spectral observable
and p-factor) for the analysis of Cepheid radial velocities. For
the present work, we have therefore chosen the
definition of the radial velocity. Even though this requires
substantial S/N, its advantages outweigh the drawback of spending
more telescope time to acquire the data.
Table 2: Optimized parameters obtained for each sample Cepheid through the confrontation of HARPS observations with our geometric model.
Modeling results obtained in the previous section are now helpful to elaborate a strategy in a comparison of observations and models.
Firstly, the effective temperature
and the surface
gravity
have been used to derive the intensity profile of
stars through linear limb-darkening coefficients
of
Claret et al. (2000) (see Table 2).
Secondly, we determine the projection factor
using
Eq. (6). The pulsation velocity is then derived through
,
where
is the observational radial velocity corrected from the
heliocentric velocity given in Table 2. The pulsation velocity
and the projection factor
(see
Table 2) obtained are not physically realistic, because our model
does not include dynamical effects and in particular velocity
gradients in the atmosphere, nevertheless this procedure imposes the
surimposition of observational and modelled radial velocity curves
.
Moreover, as a very good agreement is observed for
each phase (better than 1%), it validates the use of a constant projection factor (
). We find also that the poor
description of the pulsation velocity (Eq. (5)) used to
derive
has no incidence on the resulting modelled
curve. By this procedure, we can thus concentrate only on the
asymmetry, making the interpretation easier. Note that Nardetto et al. (2004) already gave an indication of the impact of
velocity gradients on the projection factor, and thus on the
distance determination, in the case of
Cep (about
).
In Table 2, we also indicate for each star the corresponding
projection factors
and
for
comparison.
Thirdly,
and
are
determined together from the observational RV-A and FWHM curves. We
first consider the minimum of the observational FWHM curve to obtain
an indication on the value of
.
We then find the
rotation which gives the best slope and shape for the RV-A curve.
But as the rotation has also an impact on the FWHM (about 0.02 Å),
we have then to slightly readjust
accordingly.
By this process we finally find the best and unique values for
and
.
The uncertainties on
and
,
associated to the minimization process, were estimated to be
respectively 1 km s-1 and 0.02 Å. Similar uncertainties
are found if one considers several metallic lines. Note however that
our toy model is too simple to provide secure and precise values of
the rotation, which is the most interesting parameter. In particular
the broadening of the spectral line due to the macro-turbulence can
certainly affect our rotation values (Bersier & Burki
1996). Nevertheless our principal and first objective is
to probe the dynamical effects by a direct comparison of our static
model with observations.
We now apply our methodology to each Cepheid of our sample. Results
are indicated in Table 2. RV-A plot are
represented in Figs. 11 and 12. Note that
RV-A plot deduced from the model have been shifted in asymmetry to
match the observations (this point is discussed in next section).
For R TrA and Y Sgr, we can notice a very small slope for the RV-A
plot and a very large value for the observational FWHM. It indicates
a large rotational velocity
and a properly
small value for
(see Figs. 10a,c).
Thus, the corresponding Gaussian and minimum projection factors
(
and
)
are lower than for others
stars (see Figs. 10b,d). Conversely, for Y Oph and RZ Vel
the RV-A plot have relatively large slope while the observational
FWHM is typical (about 0.3). This has a direct consequence on the
rotation, which is then very small, and on the projection factors
(
and
)
which are then relatively
large. Comparatively, S Cru,
Dor and
Gem can be
considered as intermediate cases. For
Car and RS Pup, we
obtain an atypical RV-A plot which is greatly shifted in asymmetry.
For RS Pup, we obtain a specific RV-A plot characterized by a strong
curvature which can be interpreted by our geometric model as a very
slow rotation velocity
km s-1. Note that
atypical points which are observed at the top of the RV-A plot are
certainly due to dynamical effects since they corresponds to phases
of outwards acceleration.
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Figure 11:
Radial velocity (
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As observed in the particular case of Car and RS Pup, an
important systematic shift in asymmetry can be present between
observations and models. We define respectively
and
the averaged value of the observational and computed
asymmetry curves [in
]. Note that the phases are sampled in the
same way for data and model. Results are indicated in
Table 2. We have also calculated for each
star the residuals between the observational and computed asymmetry
curves, noted O-C curves (Fig. 13). We define
,
the average value of these residual curves.
These O-C asymmetry curves contain the whole dynamical information
present in the observational asymmetry, mainly: the
limb-darkening variation in the spectral line and with the pulsation
phase, the micro- and macro- turbulence, velocity gradient and
temperature effects. For R TrA, S Cru, Y Sgr, RZ Vel and RS Pup, we
note a bump in the O-C asymmetry curves which is approximately
linked to the cross of the compression wave just after the maximum
contraction velocity (see Fig. 3). However
Dor,
Gem and
Car do not present such bump,
which may be interpreted as the presence of a very small compression
wave. In the case of Y Oph the phase sampling seems insufficient to
conclude. Consistent hydrodynamical model would be helpful to
confirm these results.
,
and
are represented as a
function of the pulsation period in Fig. 14a. The
open squares represent
.
We want to emphasize here that
our model produces asymmetry curves with non-zero average
value. Indeed, it is a natural consequence of the shape of the
observational radial velocity curve used to derive the pulsation
velocity. We find a similar behavior for all stars independently of
the period.
The shifts obtained on the observational asymmetry curves (
)
show a very interesting linear dependence with the
logarithm of the pulsation period:
![]() |
Figure 12: Same as Fig. 11 but for RS Pup. RS Pup seems to be a non-rotating star as requested by the shape of its RV-A curve. Note also atypical points in observational RV-A plot, which can certainly be interpreted through the presence of a strong compression or shock wave in the stellar atmosphere. |
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Figure 13: Difference of the Observational and Computed asymmetry curves (O-C curves) for each stars. Curves are arbitrarily shifted. The horizontal dotted lines corresponds to a zero asymmetry for each star. |
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From results of Table 2, it appears also
that the projected rotational velocity varies as a function of the
pulsation period (Fig. 14b). We obtain the
following relationship:
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Figure 14:
a) Average values of the observational (black circles) and
computed (open squares) asymmetry curves, together with the
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We have presented HARPS high spectral resolution (R=120 000)
observations of nine galactic Cepheids having a good period sampling
(P=3.39d to P=41.52d). We fit spectral line profile with an
asymmetric bi-Gaussian to derive radial velocity,
and line
asymmetry for all stars. The presence of a very important
compression or shock wave in the case of RS Pup, the longest period
Cepheid of our sample has been identified. We have also translated
the measured spectroscopic quantities into meaningful correlation
curves between radial velocity and asymmetry.
A simple geometric model providing synthetic spectral lines,
including limb-darkening, the
and the
projected rotation velocity is then used to interpret these
correlations curves.
Firstly, we find that the centroid projection factor ()
is independent of
and the rotation
velocity. This projection factor is thus certainly the best one to
use in the context of the Baade-Wesselink method.
Secondly, we find for each stars an optimized set of parameters
which allows to reproduce observational radial velocity - asymmetry
correlation curves. In particular, we find a dependence of the
derived projected rotation velocities with the period of the star:
[in km s-1].
Finally, by comparing the outputs of our static models and the
observed quantities, we gain access to dynamical effects. In
particular, we found that long-period Cepheids with strong velocity
gradient, like RS Pup, have a systematic shift in their asymmetry
curve. We thus derived a linear relation between the observational
shift in asymmetry and the logarithm of the period:
.
A detailed interpretation of these empirical relation is very
difficult, but forthcoming hydrodynamical models are likely to bring
out important insight in this field.
In conclusion, line asymmetry, which contains most of the physics involved in Cepheid atmosphere, is an important tool. But additional hydrodynamical considerations together with a multi-lines study are now required to have a better understanding of the dynamical processes present in Cepheid atmosphere and in particular to determine realistic projection factors including velocity gradients.
Acknowledgements
Based on observations collected at La Silla observatory, Chile, in the framework of European Southern Observatory's programs 072.D-0419 and 073.D-0136. This research has made use of the SIMBAD and VIZIER databases at CDS, Strasbourg (France). We thank David Chapeau for his helpful collaboration concerning computing aspects, Olivier Chesneau and Philippe Stee for their careful reading of the manuscript, as well as Vincent Coudé du Foresto and Andrei Fokin for useful discussions.
Table 3: HARPS observations results for R TrA, S Cru and Y Sgr.
Table 4:
HARPS observations results for Dor,
Gem, Y Oph, and RZ Vel. See
Table3 for legend.
Table 5:
HARPS observations results for Car and RS Pup.
See Table 3 for legend.