A&A 487, 357-362 (2008)
DOI: 10.1051/0004-6361:200809762
I. A. G. Snellen - S. Albrecht - E. J. W. de Mooij - R. S. Le Poole
Leiden Observatory, Leiden University, Postbus 9513, 2300 RA, Leiden, The Netherlands
Received 11 March 2008 / Accepted 16 April 2008
Abstract
Context. The first detection of an atmosphere around an extrasolar planet was presented by Charbonneau and collaborators in 2002. In the optical transmission spectrum of the transiting exoplanet HD 209458b, an absorption signal from sodium was measured at a level of
%, using the STIS spectrograph on the Hubble Space Telescope. Despite several attempts, so far only upper limits to the Na D absorption have been obtained using telescopes from the ground, and the HST result has yet to be confirmed.
Aims. The aims of this paper are to re-analyse data taken with the High Dispersion Spectrograph on the Subaru telescope, to correct for systematic effects dominating the data quality, and to improve on previous results presented in the literature.
Methods. The data reduction process was altered in several places, most importantly allowing for small shifts in the wavelength solution. The relative depth of all lines in the spectra, including the two sodium D lines, are found to correlate strongly with the continuum count level in the spectra. These variations are attributed to non-linearity effects in the CCDs. After removal of this empirical relation the uncertainties in the line depths are only a fraction above that expected from photon statistics.
Results. The sodium absorption due to the planet's atmosphere is detected at >5,
at a level of
(
Å band), 0.07
(
.5 Å band), and
(
Å band). There is no evidence that the planetary absorption signal is shifted with respect to the stellar absorption, as recently claimed for HD 189733b.
Conclusions. The STIS/HST measurements are confirmed. The measurements of the Na D absorption in the two most narrow bands indicate that some signal is being resolved. Due to variations in the instrumental resolution and intrinsic variations in the stellar lines due to the Rossiter-McLauglin effect, it will be challenging to probe the planetary absorption on spectral scales smaller than the stellar absorption using conventional transmission spectroscopy.
Key words: techniques: spectroscopic - stars: atmosphere - stars: planetary systems
Transiting extrasolar planets are of great scientific value.
While the radial velocity method continues to be very successful in finding
planets and characterising their orbits, only transits can currently
reveal the properties of the planets themselves. In addition to the basic
planetary parameters that can be determined, such as planet mass, size, and
average density, the atmospheres of transiting planets can be probed through
either secondary eclipse observations (e.g. Charbonneau et al. 2005; Deming et al. 2005; Knutson et al. 2007) or atmospheric transmission
spectroscopy, the subject of this paper.
In transmission spectroscopy, the depth of a planet transit
is measured as function of wavelength. It is expected that at certain
wavelengths, a transit will be slightly deeper due to absorption
in the planet's atmosphere. In the optical transmission spectrum of hot
Jupiters,
the strongest of these absorption features was predicted to come from the
sodium D lines at 5889 and 5896 Å (Brown 2001; Seager & Sasselov 2000).
Indeed, Charbonneau et al. (2002) detected Na D absorption
in the transmission spectrum of the transiting exoplanet HD 209458b, at a level
of 0.02.006% in a 12 Å wide band, using the STIS spectrograph
on the Hubble Space Telescope (HST).
This constitutes the first detection of an atmosphere around an extrasolar
planet. Subsequently, strong absorption features have been detected
in HD 209458b from hydrogen, oxygen, and carbon at a level of 5-15%,
thought to be caused by an evaporating exosphere (Vidal-Madjar
et al. 2003, 2004). Recently, hot hydrogen has been detected by
Ballester et al. (2007), also using HST data.
A claim by Tinetti et al. (2007) of the
detection of water vapour from a comparison of transit depths at several
wavelengths
in the infrared, as measured with Spitzer, has been disputed by Ehrenreich
et al. (2007). This, while Swain et al. (2008) identify both water and methane
from NICMOS/HST data.
Despite several attempts from ground-based observatories, no confirmation has
yet been obtained of the Na D planetary absorption feature in the transmission spectrum of HD 209458b.
In general, ground-based transmission spectroscopy has not been a great success.
Typically, upper limits to a Na D absorption signal of 0.1-1% have
been reached (Moutou et al. 2001; Snellen 2004; Narita et al. 2005),
implying that systematic effects dominate the error budgets.
A modern Echelle spectrograph on a 8-10 m. class telescope can provide
spectra from the brightest transiting exoplanet systems with signal-to-noise ratios,
,
within a few minutes of exposure time.
Integrating over a few Angstrom and over the duration of a transit, this would
mean that photon noise statistics should allow detections down to a few times
10-4. Although the HST detection of the Na D absorption feature is only
just at this level, it is expected that its width is only a fraction of
the 12 Å passband used by Charbonneau et al. (2002), as recently shown by
re-analysis of the STIS data (Sing et al. 2008).
This means that the Na absorption
within a 2-3 Å band should be at the
10-3 level.
In this paper we re-analyse a data-set from the High Dispersion Spectrograph on the Subaru telescope, that covers one transit of HD 209458b. The aim is to identify and correct for possible systematic effects, and to improve on the results previously presented by Narita et al. (2005, NAR05). Their analysis resulted in spectra with an SNR of a few hundred in the stellar continuum. However, near strong absorption lines, such as the Na D doublet, clear coherent structures were visible (Fig. 2 in NAR05), well in excess of the photon shot noise. While NAR05 argued that the positions of the spectral lines are stable to within 0.01 Å, spectral shifts at only a fraction of this level (e.g. due to slit-centering variations) could cause these effects. This encouraged us to analyse this data again. In Sect. 2, the observations, data reduction and analysis are described. The result on the Na D absorption are presented and discussed in Sect. 3, together with a comparison with the STIS/HST results, and with a recent detection of Na D absorption in exoplanet HD 189733b (Redfield et al. 2008).
HD 209458 was observed on the night of October 24, 2002, using the High
Dispersion Spectrograph (HDS; Noguchi et al. 2002) on the Subaru telescope.
We obtained the data using the SMOKA archive system (Baba et al. 2002).
The observations have been described in Winn et al. (2004) and
Narita et al. (2005; NAR05). Thirty-two spectra were taken in Yb mode
(without the iodine cell), of which the last thirty were made with an exposure time
of 500 s. The entrance slit was 4'' long and 0.8'' wide, oriented
with a constant position angle, resulting in a spectral resolution
of
with 0.9 km s-1 per pixel. We concentrated on the
data from the red CCD, which contains 21 orders of 4100 pixels covering
Å. Twelve of the thirty spectra fall outside
the transit (nine before ingress and three after egress), and eighteen
during the transit. The uncertainty in the transit timing is neglegible.
For the initial data reduction we followed the procedure of NAR05. First the frames were processed using the IRAF software package, including the extraction of the one-dimensional spectra. These spectra have signal-to-noise ratios that vary between 300 and 450 per pixel in the continuum. Subsequent analyses were conducted using custom-built procedures in the Interactive Data Language (IDL). Winn et al. (2004) and NAR05 describe a good method to correct for time-dependent variations of the instrumental blaze function (possibly caused by flexure of the spectrograph) using the adjacent orders, which we also use here. We do not apply a global wavelength solution to the spectra. Only for the analysis of the strength of telluric absorption features (see below) did we apply the wavelength solution to the order containing the Na D doublet. The Na D spectral surroundings of HD 209458 are shown in Fig. 1.
The variations in observing conditions during the night are shown in Fig. 2. The solid line indicates the variation in airmass, and the dashed line the variation in the 1-dimensional stellar profile along the slit (a measure of the seeing). The dotted line shows the normalised variation in continuum count level in the spectra, indicating that it varies up to a factor of two from spectrum to spectrum.
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Figure 1: Spectrum of HD 209458 around the Na D doublet. The shaded areas indicate the narrow, medium, and wide passbands as used in our analysis. In all cases, the comparison bands are located directly adjacent to the central band, and have the same width. The upper line shows a synthetic telluric spectrum constructed from the line list of Lundstrom et al. (1991). Note that the telluric sodium absorption can show strong seasonable variability. |
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Figure 2:
Variations of observing conditions over the 30 spectra.
The solid line
indicates the airmass, and the dotted line shows the normalised variation
in continuum count level. The dashed line indicates the seeing (in ![]() |
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Figure 3: The top panel shows the normalized count level of the continuum in the spectra versus the measured weighted mean-strength of 59 deep stellar absorption lines. A strong inverse correlation is present, with the more flux in the spectra, the deeper the absorption lines. We believe that this is due to a non-linearity effect in the CCD. The solid line indicates the linear least squares fit to the correlation, used to correct the measured line strengths. The lower panel shows the same average strength of these 59 absorption lines as function of orbital phase, where the grey band indicates the planetary transit. Those data points corrected for the correlation with count level (thick squares) have a reduced chi-squared of 1.06, while the uncorrected data exhibit a reduced chi-squared of 6.11. |
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We subsequently selected 59 strong stellar lines and the Na D doublet to
perform our analysis. First, for each line, the line center, ,
was
determined through Gaussian fitting. Subsequently, the total flux was
integrated within
a spectral band,
,
and divided by the average of two
equally wide bands to the left and right of the line.
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(1) |
The variations from spectrum to spectrum, away from spectral lines, are, as expected, dominated by photon noise. However, at and around strong lines, systematic effects play a role. This is in addition to the fact that the signal-to-noise ratios in the cores of deep lines are significantly lower. Most importantly, it was noticed that the observed depths of the Na D lines are a clear function of the overall count level in the spectra. The same effect is visible in the average of the 59 reference lines. In the top panel of Fig. 3, for each spectrum, the normalised continuum level is plotted against the weighted (by line-strength) mean depth of the lines. It shows that the higher the count levels in the spectra, the deeper the lines. Firstly, we convinced ourselves that this is not due to scattered light residuals. It would need about 300 counts per spectral bin to cause this effect, two orders of magnitude above the uncertainties in the scattered light removal. Instead, several other possible causes are identified, but we believe that non-linearity of the CCD is the most likely cause. Other potential systematic effects are caused by variations in the seeing and/or spectral resolution, and intrinsic variations of the stellar spectral line due to the Rossiter-McLaughlin effect (Rossiter 1924). The latter two effects result in strong variations across deep spectral lines, making atmospheric transmission spectroscopy very challenging at spectral scales shorter than the width of the stellar lines.
Most likely, the non-linearity of the pixels in the HDS CCD is causing the
effect seen in the top panel of Fig. 3. Since it was not possible
to directly measure the non-linearity of the CCD, we corrected for it
in an empirical way, by performing a least-squares fit to the correlation
between line depth and count level.
For the weighted mean of the 59 strong comparison lines, the reduced
chi-squared drops from
to
.05 after
this correction. The bottom panel of Fig. 3 shows the
remaining residuals. Although there is some correlated
variation still visible, it averages out over the transit.
Since we integrate over the total extent of the lines, we do not
expect variations in the seeing to affect our results. Nevertheless, since
the seeing influences how much flux of the star enters the slit, the seeing
is anti-correlated with the count level in the spectra. Therefore,
a correlation between the seeing and the average line strength is also
present. However, the resulting reduced chi-squared is
.90,
significantly higher than that resulting from the continuum count level,
indicating that changes in seeing are not the underlying cause of the line
variations.
In a similar manner as for the weighted mean of the reference lines, the correlation between line depth and continuum count level was removed for the Na D doublet. We subsequently determined the depth of the transit for the three Na D passbands separately. A least-squares fit was performed on the data using as a model a scaled version of the HST light curve as presented by Brown et al. (2001). The best fitting model is subsequently removed from the data, revealing low-level variations due to changing telluric contaminations most evident at the end of the night. This telluric residual was found to scale with the airmass and with the strength of some strong telluric lines in the red part of the spectrum (as shown in Fig. 2). A linear fit was performed between the average strength of the strong telluric lines and the Na D residuals to remove the telluric contribution. Note that the fitting of the continuum count level, transit signal, and telluric contamination was performed in a iterative way, but the solutions did not significantly change after the first round.
In addition, a consistency check was performed to see whether our telluric line contamination removal was reasonable. Many telluric lines are present around the Na D doublet, in both the line and reference bands. We used the telluric line list of Lundstrom (1991) to construct a synthetic telluric spectrum. We then constructed a reference spectrum from the average of all exposures which was subsequently removed from the 30 frames. Although the absolute telluric contamination is now lost, all information on the change in telluric contamination becomes clearly visible in this way. The synthetic telluric spectrum was then fitted to these frames, and the change in telluric contribution in the various spectral bands determined. This gives very similar results as the method described above. We use the former method in our final analysis since the contribution of telluric sodium relative to that of water and oxygen undergoes seasonal variations, but within one night is expected to vary following the other telluric lines. Note that NAR05 used the spectrum of the rapidly rotating B5 star HD 42545 to remove the telluric contamination around the Na D doublet, however the sodium absoption towards this star is dominated by interstellar contributions (although this is unlikely to have influenced their results).
We measured the depth of the Na D features in the transmission spectrum
within three spectral passbands centered on the two stellar lines,
with widths of 0.75 Å, 1.5 Å, and 3.0 Å. The results are presented in
Fig. 4.
The sodium absorption due to the planet's atmosphere is detected at >5,
at a level of 0.05
.007% (
Å band),
0.07
.011% (
.5 Å band), and 0.13
.017% (
.75 Å band). The quoted uncertainties are 1
error intervals as
determined from the SNR in the spectra using chi-square analysis.
The resulting reduced chi-squares values,
,
are 47/28=1.63, 31/28=1.10, and 45/28=1.75 respectively, and
indicate that the residual noise levels are 10-30% higher than expected
from Poisson statistics. A way to take this residual noise into account in the
error budget is to scale the error bars up such that
.
This would increase the uncertainties by 10-30%, resulting in
conservative estimates of the significance of the sodium detection of
6
in each individual passband.
A crucial part of our data analysis is the empirical correction for the
correlation of line depth with the continuum count level in the spectra,
attributed to non-linearity effects in the CCD.
To assess the robustness of our result we performed a slightly different
empirical correction by directly correlating the weighted mean-strength
of the 59 reference lines with that of the Na D lines.
Depending on the passband, this alternative analysis results in a transit
depth 20-30% lower than determined above, also with
20-30% higher
values. Since this would still be
5
detections, it further supports the detection.
Since the
first method gives significantly less noisy results, we believe that
method it is more reliable.
In our analysis we do not take into account the variation
in radial velocity of the planet (and its atmospheric absorption) relative to that
of the star. During the
transit, the radial velocity of the planet varies from about -14 to +14 km s-1. For a Lorentzian shaped planetary absorption profile with a width
comparable to that of the star (see below), the strength of the absorption
signal will have been underestimated by 4% in the narrowest passband.
Therefore this is just a minor effect.
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Figure 4:
Transit photometry averaged in two bands centered on the
Na D doublet, with spectral widths of 3 ![]() ![]() ![]() |
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Figure 5:
The three measurements of the Na D absorption in
the transmission spectrum of HD 209458b in passbands of
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Our results are in excellent agreement with the STIS/HST results presented by
Charbonneau et al. (2002) and Sing et al. (2008a).
Figure 5 shows our three measurements of the planetary Na D
absorption as a function of the spectral passband.
The solid line and grey band shows the STIS/HST result and its uncertainty
corrected to our passbands, assuming that the planetary absorption is
unresolved and completely within them.
If there were no stellar Na D lines, then the expected absorption strength as a function of passband would simply scale as
.
However, since most absorption occurs near the cores of the stellar
Na D doublet, where there is already little flux present,
the relative contribution of the absorbed part of the spectrum varies more
steeply than as 1/
.
Our measurement in the
widest passband is perfectly consitent with an unresolved HST absorption,
but some absorption appears to be missing in the two smallest passbands,
about 40% in the
Å band and about 60% in the
Å passband, indicating that the planetary absorption is
partially being resolved out.
We modelled this by measuring the absorbed flux as function of passband
for a planetary Lorentzian line profile with a width
equal, 2
and 4
times the width of the stellar Na D absorption,
normalised to the STIS/HST value.
These simulations are shown as the dotted lines a, b, c in Fig. 5, and indicate that
planetary absorption is likely
to be about as broad (within a factor of 2) as the stellar absorption.
Also presented in Fig. 5 are two measurements from the re-analysis of
the HST/STIS data (Sing et al. 2008a,b), within a band pass of 4.4 and 9
.
The analysis of Sing et al. is fully consistent with our results,
but indicates that the Na line profiles may not be Lorentzian on wide scales.
Instead they present narrow cores extending over a broader plateau.
The observations presented here are not sensitive to absorption on these large
spectral scales.
Recently, Redfield et al. (2008) measured Na D absorption in the
transmission spectrum of the other known bright transiting hot Jupiter
HD 189733b, at a level of
% in a passband of 12 Å.
Note that their in-transit data originate from short observations of eleven
different transit events, but in total reach a similar SNR as the data
presented in this paper.
The detection of
Redfield et al. is about a factor of 3 higher than that measured for HD 209458b.
From their Fig. 1 we conclude that they have derived the strength of the
Na D feature by integrating
instead of
integrating
.
This means
that their result cannot be directly compared to the results of HD 209458b,
since it puts much higher weights (>10
)
on the pixels in the center of the stellar absorption lines where most planetary absorption
is seen.
The number of
absorbed photons for a
1% planetary absorption at the stellar line
center would be equal to the number of absorbed photons for a
0.1% planetary absorption at the stellar continuum.
By multiplying the data points from
their Fig. 1 by the stellar flux at each wavelength, we estimate that
the measured Na D absorption from HD 189733b is only a factor
2 above that measured for HD 209458b. This remaining difference
however does not mean that the
planets have a different Na atmosphere. Physically, these
levels of absorption correspond to a variation in the apparent planetary radius
of 0.8% (
750 km) for HD 209458b, and 1.0% (
780 km) for
HD 189733b. Hence the results for both
planets are actually very similar.
Remarkably, Redfield et al. (2008) find a significant blueshift of their
planetary absorption signal, of the order of 38 km s-1
(corresponding to
0.75 Å).
No such shift of the planetary absorption is present in
the transmission spectrum of HD 209458b. If this velocity shift is real,
it is rather puzzling how it could be produced, since it is about
an order of magnitude higher than the expected sound speed in the
upper layer of the planet's atmosphere (Brown 2001). We note that the
data analysis of Redfield et al. is affected by the intrinsic variations
in stellar line shapes due to the Rossiter-McLaughlin effect, due
to the use of the
integral, which
does not have to integrate down to zero, even if there is no additional
planetary absorption (see section 2). If the spectra are not evenly
distributed over the
transit, this can also lead to spurious velocity offsets,
although it is difficult to see how these could become larger than the
of the star.
We present the first ground-based detection of the Na D absorption feature in
the transmission spectrum of the extrasolar planet HD 209458b,
fully consistent with the HST measurements by Charbonneau et al. (2002).
The absorption is measured at a level of
%,
%,
and
% in three passbands of
Å,
Å, and
Å wide,
indicating that the absorption is partially resolved out in the two smallest bands.
Crucial in our analysis was the removal of an empirical correlation between
line depth and the continuum count level in the spectra, likely to be caused
by non-linearity of the CCD. We show that due to either
changes in the spectral resolution, or intrinsic changes in the stellar line
profiles during the transit due to the Rossiter-McLaughlin effect,
it is crucial
to integrate the atmospheric absorption over a wide-enough passband
to avoid spurious effects.
Acknowledgements
We thank the anonymous referee for his or her insightful comments. Based on data collected at the Subaru Telescope and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan.