The solar chromosphere at high resolution with IBIS

K. P. Reardon; H. Uitenbroek; G. Cauzzi

doi:10.1051/0004-6361/200811223

Free Access

Issue		A&A Volume 500, Number 3, June IV 2009


Page(s)		1239 - 1247
Section		The Sun
DOI		https://doi.org/10.1051/0004-6361/200811223
Published online		11 March 2009

III. Comparison of Ca II K and Ca II 854.2 nm imaging

K. P. Reardon^1,2 - H. Uitenbroek² - G. Cauzzi^1,2

1 - INAF - Osservatorio Astrofisico di Arcetri, 50125 Firenze, Italy
2 - National Solar Observatory, PO Box 62, Sunspot nm 88349, USA

Received 24 October 2008 / Accepted 13 February 2009

Abstract
Aims. Filtergrams obtained in Ca II H, Ca II K, and H $\alpha$ are often employed as diagnostics of the solar chromosphere. The vastly disparate appearance between the typical filtergrams in these different lines calls into question the nature of what is actually being observed. We investigate the lack of obvious structures of magnetic origin such as fibrils and mottles in on-disk Ca II H and K images.
Methods. We directly compare a temporal sequence of classical Ca II K filtergrams with a co-spatial and co-temporal sequence of spectrally resolved Ca II 854.2 images obtained with the Interferometric Bidimensional Spectrometer (IBIS), considering the effect of both the spectral and spatial smearing. We analyze the temporal behavior of the two series by means of Fourier analysis.
Results. The lack of fine magnetic structuring in Ca II K filtergrams, even with the narrowest available filters, is due to observational effects, primarily contributions from the bright, photospheric wings of the line that swamp the small and dark chromospheric structures. Signatures of fibrils remain, however, in the temporal evolution of the filtergrams, in particular with the evidence of magnetic shadows around the network elements. The Ca II K filtergrams do not appear, however, to properly reflect the high-frequency behavior of the chromosphere. Using the same analysis, we find no significant chromospheric signature in the Hinode/SOT Ca II H quiet-Sun filtergrams.
Conclusions. The picture provided by H $\alpha$ and Ca II 854.2, which show significant portions of the chromosphere dominated by magnetic structuring, appears to reflect the true and essential nature of the solar chromosphere. Data that do not resolve this aspect, whether spatially or spectrally, may misrepresent the behavior the chromosphere.

Key words: Sun: chromosphere - Sun: magnetic fields - instrumentation: high angular resolution - line: formation - techniques: spectroscopic

1 Introduction

The Ca II H and K resonance spectral lines have long been used for diagnostics of the solar chromosphere. The crucial results obtained with these strong lines, particularly those based on observations using slit-based spectrographs, have been summarized by Rutten & Uitenbroek (1991). Imaging observations, most often using Lyot-type filters (0.03-0.2 nm FWHM), have also been widely employed. Their use is much increased in recent years due in part to the availability of efficient image stabilizing systems and image reconstructions techniques, both of which allow high spatial resolution to be maintained over long period of times.

Several studies have used filter observations in an effort to assess the characteristics of the chromosphere via the examination of the spatial distribution and temporal evolution of structures in the two-dimensional field of view (e.g. Ermolli et al. 1998; Wöger et al. 2006; de Wijn et al. 2005a; Tritschler et al. 2007). Most recently, a broadband Ca II H filter (0.22 nm FWHM) has been flown on the Hinode satellite, allowing acquisition of long time series free of terrestrial atmospheric distortions. Novel results from this instrument include small-scale penumbral jets (Katsukawa et al. 2007), the spatial patterning of chromospheric umbral oscillations (Nagashima et al. 2007), the rapid evolution of spicules (De Pontieu et al. 2007), and more.

However, the on-disk images obtained in the H and K lines with these filters are always significantly different from the appearance of the chromosphere in the other preeminent chromospheric line, H $\alpha$ . Observations in this line, using even relatively broad filters (0.1 nm FWHM) show a highly structured environment including fibrils, mottles, and filaments across the full solar disk. This is consistent with the growing dominance of the magnetic field at increasing heights in the atmosphere. Most contemporary images in the Ca II H and K lines, instead, do not typically show many examples of such structuring by the magnetic field, even when using the narrowest available passbands (cf. the images shown in Wöger et al. 2006). Looking further back, fibrils were sometimes seen in Ca II H and K images using spectroheliograms (Beckers 1964; Bumba & Howard 1965; Bailey & Sheely 1969) or filtergrams (Zirin 1974; Marsh 1976), though predominantly around active regions or close to the limb and with reduced contrast compared to H-alpha fibrils. Rutten (2007) remarks that the fibrils seen in Ca II H and K filtergrams are at best visible only as ghostly impressions of their counterparts observed in H $\alpha$ . Why does the observed scene differ so greatly between these two sets of ``chromospheric'' lines?

Another multiplet of Ca II lines, the so-called ``infrared triplet'' around 850 nm, may provide for the resolution of this apparent discrepancy. Like H $\alpha$ , the Ca II IR triplet lines are subordinate, but whereas the lower level of the former is coupled to the hydrogen ground level via the extremely strong Ly $\alpha$ radiative transition, the lower level of these latter lines is metastable and only coupled to the Ca II ground level via electronic collisions. This accounts for a stronger coupling of the Ca II IR triplet to local conditions and allows a more straightforward interpretation of the line formation (Uitenbroek 1989). Observationally, the use of the infrared lines also provides several significant advantages with respect to H and K, including a typically better response of digital detectors in the red, a reduction in atmospheric turbulence, and a higher photon flux. Indeed, in recent years, the use of the infrared triplet for solar studies has increased notably (see, e.g. Uitenbroek 2006b; Socas-Navarro et al. 2006; Tziotziou et al. 2006), although studies combining spatial and spectral high resolution over extended fields of view (FOV) are still scarce.

In Papers I and II of this series (Cauzzi et al. 2008; Vecchio et al. 2009) we presented novel observations of the Ca II 854.2 nm line of the infrared triplet, obtained with the Interferometric Bidimensional Spectrometer (IBIS, Cavallini 2006). These studies established the suitability of imaging spectroscopy in this line for high-resolution investigations of chromospheric diagnostics. A central finding of Paper I was the nearly ubiquitous occurrence of fibrilar structures. They originate from even the smallest magnetic elements, and appear to fill large portions of the chromospheric volume, even in ``quiet'' areas. Their presence indicates that even at the relatively low chromospheric heights sampled by the Ca II 854.2 line, the atmosphere is already highly structured by the pervasive magnetic fields, entirely consistent with the picture provided by H $\alpha$ images. The fibrils in turn play a crucial role in shaping the chromospheric dynamics, in particular producing a strong reduction in the oscillatory power at periods around three minutes, correlated with the absence of chromospheric acoustic shocks (Vecchio et al. 2007; Paper I; Paper II).

The question is then why this subordinate line would display a more ``chromospheric'' scene than the resonance H and K lines, which have a far larger opacity. In Paper I we put forward the hypothesis that a large part of the problem lies in the strong observational limitations that still affect Ca II H and K imaging. Namely, while the chromospheric contribution of the Ca II H and K is limited to a narrow core of less than 0.02 nm width, virtually all the imaging is performed with much broader filters, having FWHM passbands in the range of 0.03-0.3 nm. Further, the decreased photon flux and low filter transmission lead to long exposures (often one second or more) that, combined with the increased seeing disturbances at shorter wavelengths, severely limits the spatial resolution that can be consistently achieved.

In this paper, we explore these and other effects by a direct comparison between spatially and spectrally resolved IBIS Ca II 854.2 data and cotemporal Ca II K filtergrams. This builds on the preliminary results that have been reported in Reardon et al. (2007) and allows us to compare the clear chromospheric signatures seen in the IBIS spectra with the behavior observed in the Ca II K filtergrams.

2 Observations

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1223_f1.eps} \end{figure}$

Figure 1:

Top panel: Ca II 854.2 nm atlas profile (black line) from the FTS atlas (Wallace et al. 1993,1998), the IBIS transmission profile (orange line), and the ``synthetic'' instrumental profile (blue line), derived as described in the Sect. 3.1. The red crosses show the observed spectral profile averaged over a portion of the field of view at the 27 sampled spectral positions. Bottom panel: Atlas profile for the core of Ca II K (black line) and theoretical instrumental passband of the Halle filter (blue line). The plotted wavelength range is scaled according to the wavelengths of the two lines. In both plots, the transmission of the filter passband has been arbitrarily scaled to accommodate the plotted range of the atlas profile.

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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1223_f2.eps} \end{figure}$	Figure 2: Simultaneous individual images from the full observing sequence: a) Ca II 854.2 nm blue wing -0.07 nm from line core; b) Ca II K filtergram; c) Ca II 854.2 line core. The orange squares, yellow ovals, and pink triangles indicate respectively: structures present in the Ca II line wing images; in the Ca II line core images; or in both. The spatial scale is given in Mm.
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The observations were obtained on 2 June 2004, starting around 15:00 UT, at the Dunn Solar Telescope (DST) of the US National Solar Observatory. Seeing conditions were excellent during most of the approximately one-hour-long sequence, aided by a high order adaptive optics system (Rimmele 2004). The target region was a quiet area at disk center that included some portions of enhanced, bipolar network, well observed in the MDI high resolution magnetic maps. At continuum wavelengths a few transient pores appeared and disappeared repeatedly during the course of the observations. In coronal images, the region appeared as a fading coronal bright point.

The Ca II 854.2 data utilized in this paper have been described in detail in Paper I. We thus summarize here only the most important aspects of the observations. The field of view covered an 80 $^{\prime\prime}$ diameter circle on the Sun with a plate scale of 0.166 $^{\prime\prime}$ /pixel. The Ca II 854.2 nm line was sampled with 27 spectral points (see Fig. 1), which were acquired in a total of 7 s. The repetition time between scans was 19 seconds (the entire sequence also included scans of two photospheric lines). A total of 175 scans of the spectral line were obtained for a total duration of 55 min. The instrumental spectral profile of IBIS is described in Reardon & Cavallini (2008) and at this wavelength has an FWHM of 4.4 pm, with spectrally scattered light less than 1.5% of the total transmission.

Simultaneously with the IBIS spectral data, Ca II K images were obtained through a Halle filter with a nominal ${\it FWHM} = 0.06$ nm, centered 0.03 nm from line core. The spatial scale was set at 0.08 $^{\prime\prime}$ /pix, and a FOV of approximately $82{\hbox{$^{\prime\prime}$ }}\times~82{\hbox{$^{\prime\prime}$ }}$ . Given the overall low light level with this setup, the exposure time for each image was 1.2 s. Images were obtained every 2 s during the same one hour period, producing a sequence of 1576 frames.

Both sequences of data were subjected to destretching, to remove residual distortions introduced by the terrestrial atmosphere. For the narrowband IBIS data, reference images were provided by strictly simultaneous white light images. The Ca II K data were destretched with respect to an averaged image and then interpolated to the same spatial scale as the IBIS data using images of a reference grid acquired for this purpose. Finally, the Ca II K filtergram closest in time to the moment of acquisition of the Ca II 854.2 line core images was selected for each of the 175 spectral scans.

Figure 2 shows the full FOV of the observations, at one time during the observing sequence. Figure 2a displays the intensity image acquired at -0.07 nm from the Ca II 854.2 line core. As described in Paper I, this position in the line wing originates at an average height of $\sim$ 200 km. The photospheric reversed granulation pattern (Cheung et al. 2007; Janssen & Cauzzi 2006) and magnetic flux concentrations (Paper I; Leenaarts et al. 2006) are easily discernible throughout the field. Figure 2c displays instead the intensity at the nominal Ca II 854.2 line core wavelength formed at a height of roughly 1200 km. At the center of the line, fibrils are seen to occupy a large fraction of the FOV, strongly reminiscent of the structures commonly seen in H $\alpha$ . The fibrils can be seen as both bright and dark elongated structures originating from even the small magnetic network elements. For how this region appears at other wavelengths within the line, we refer the reader to Fig. 3 in Paper I.

Figure 2b shows the Ca II K filtergram closest in time to the displayed IBIS images. An essential aspect of this comparison is the presence in the Ca II K image of features that can be associated either with photospheric structures seen in the Ca II 854.2 line wing (squares) or chromospheric structures in the line core images (ovals) or both (triangles). In particular, some of the strongest fibrils observed in the Ca II 854.2 core are also discernable in the K filtergram.

3 Data comparison

The net effect of any instrumental spectral profile is to mix information from different portions of a spectral line and thus arising from different layers in the solar atmosphere. This is in addition to the ``smearing'' produced from the line formation itself (Uitenbroek 2006a). Such mixing is particularly relevant for the Ca II H and K lines because the large passband of the filters generally employed sums over a significant portion of the entire line profile. In such an integration, the very low residual intensity of the chromospheric line center will be swamped by the much higher flux of the line wings originating in the photosphere. This will strongly dilute the chromospheric signal when observing on the disk. In Paper I we put forward the hypothesis that the scarcity of fibrils observations in H and K filtergrams is mainly due to this effect.

$\begin{figure} \par\includegraphics[width=8.4cm,height=6cm,clip]{1223_f3.eps} \end{figure}$	Figure 3: Temperature response functions for the Ca II K filtergrams (solid) and the Ca II 854.2 nm synthetic filtergrams (dashed) (see Sect. 3.1). The x axis represents heights from the solar surface ( $\tau _{500}=1$ ) in km. Both curves have been computed for the FALC model.
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On the other hand, IBIS data do not suffer this limitation: the filter passband is comparable to that of a spectrograph and can effectively isolate the chromospheric portions of the line and resolve fine details in the spectral profiles of Ca II 854.2 (Papers I and II). Currently, it is not possible to obtain similar measurements in the H and K lines since no such narrow filters exist in this wavelength range. It is also difficult to obtain spectroheliograms with similar spatial or temporal resolution. Therefore, we compare the observations in these two lines by attempting to replicate the Ca II K filtergram images from the spectrally resolved Ca II 854.2 data.

3.1 Synthetic Ca II 854.2 filtergrams

To perform this comparison, we introduce a ``synthetic spectral filter'' that can be applied to the Ca II 854.2 spectra to provide a diagnostic as close as possible to that of the K data. We adopted two criteria for the construction of this synthetic filter: 1 - that it have the same spectral shape as the Halle filter, namely a sync function with a large central peak and secondary transmission orders that introduce signal from the far wings; 2 - that the run with height of the response function to temperature variations for the two Ca II lines, once convolved with the respective filter passbands, is as similar as possible. To this end, we synthesized both spectral lines in the static 1-D FALC model of the quiet solar atmosphere (Fontenla et al. 1991). The best match for the temperature response function was obtained when using a sync function of 0.04 nm FWHM, centered at -0.025 nm from the core of the line. Figure 3 shows the response functions obtained in this case, for the K line (solid) and the 854.2 line (dashed). Using a broader passband for the Ca II 854.2 synthetic filter would move the peak of the temperature response function to deeper layers, while positioning it further towards the core of the line would increase the chromospheric contribution (heights above 800-900 km) well above the Ca II K case. Although our choice of filter function is dictated by the hydrostatic FAL model, this conclusion would not change much if we would have taken snapshots from chromospheric dynamics simulations as a template, since the source function of the Ca II 854.2 line is strongly dominated by the K line (Uitenbroek 1989), and the response functions of the two lines would change in similar fashion.

Figure 1, which showed these two spectral lines, also includes the spectral passbands of the respective filters (the actual passband of the Halle filter for Ca II K, and the ``synthetic'' passband for Ca II 854.2). The top panel further displays the actual IBIS passband at this wavelength, as well as the spectral positions at which the line was sampled during the observations. The spectral range plotted for each of the two lines is proportionate to their wavelength, showing how the position of the K_2V and K_2R features in the Ca II K line correspond to the ``knees'' of 854.2 line. Uitenbroek (1989) illustrates this scaling and the behavior of the corresponding line source functions in a quiet-Sun model atmosphere (his Fig. 2).

We then summed the monochromatic images obtained with IBIS after applying the relative weighting given by the synthetic spectral filter in order to generate ``synthetic filtergrams'' for the 854.2 line. Only 3% of the total filter transmission lay outside of the range of the IBIS spectral scan and was not included in the construction of the filtergrams.

3.2 Spatial smearing

Both the long exposure times of the Ca II K data (compounded by the worse seeing at shorter wavelengths), as well astigmatism introduced by the Halle filter produce a loss of spatial resolution in the K images with respect to the IBIS data. The magnitude of the optical degradation was estimated by comparing the images of the reference grids taken in the two lines. The additional seeing degradation for the K data has been estimated by analyzing the spatial profile in the Ca II K images of the sharpest bright features visible in the wings of 854.2. The composite smearing can be effectively described by an asymmetric 2-D Gaussian with widths of 1.0 and 1.6 arcsec along the two orthogonal axes of the distribution. The Ca II 854.2 synthetic filtergrams were then convolved with this PSF to produce spatially smeared images.

3.3 Radiation temperature

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{1223_f4.eps} \end{figure}$	Figure 4: Radiation temperature maps derived from a) the synthetic 854.2 filtergram and b) the observed K filtergram's intensity. The shapes indicate the same features as in Fig. 2. Average values are 4540 and 4600 K, respectively.
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$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1223_f5.eps} \end{figure}$	Figure 5: Temporally averaged radiation temperature maps summed over the 175 realizations obtained during the one hour time series. a) Ca II 854.2 synthetic filtergrams, b) Ca II K filtergrams, and c) Ca II 854.2 line minimum intensity. The two filtergrams are both scaled between 4400 and 4900 K and the line minimum intensity is scaled between 3500 and 4800 K.
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The intensity variations in the two Ca II lines reflect the different sensitivity to velocity, density and temperature variations. This latter is mostly due to the different slope of the Planck function at the two different wavelengths. In order to partially account for this effect, we translated the intensity maps into radiation temperature maps. First each set of images was normalized to the spatio-temporal average intensity over their entire duration. The radiation temperature corresponding to the average intensity has been derived from the line profiles calculated in the FALC model, after convolution with the spectral transmission profiles, and corresponds to 4540 and 4600 K for the Ca II K and 854.2, respectively. The close match between these two average radiation temperatures indicates that our choice of synthetic filter for the Ca II 854.2 as derived from the temperature response functions was indeed proper. The final result is displayed in Fig. 4 showing the radiation temperature map obtained for the synthetic 854.2 filtergram (Fig. 4a) and the observed K filtergram (Fig. 4b), at the same temporal step of Fig. 2. The overplotted symbols represent the same features as in Fig. 2. The Ca II K filtergram now shows smaller amplitude intensity excursions than that of the synthetic Ca II 854.2 filtergram, because the former is much less sensitive to the intensity variations induced by Doppler shifts. Indeed, the small spectral features in the core of the Ca II H and K lines (e.g. K₂V and K₂R) create multiple crosstalk signatures of opposite sign that tend to cancel when summed together by the spectral transmission profile, rendering filtergrams in these lines highly insensitive to such crosstalk. The more classical absorption profile of Ca II 854.2 (at least for an averaged atlas profile) still produces a significant velocity crosstalk signature in the synthetic filtergrams (also because the synthetic filter is narrower than the Ca II K filter). Taking into account as well the increased amplitude of the Doppler shifts at longer wavelengths, for typical chromospheric velocities the magnitude of the velocity-to-intensity crosstalk is four times greater in the Ca II 854.2 nm synthetic filtergrams than the Ca II K filtergrams.

4 Results

4.1 Temporally averaged images

In Fig. 5, we display the time-averaged radiation temperature maps for the Ca II 854.2 synthetic filtergrams, the Ca II K filtergrams, and, as a further chromospheric indicator, the Ca II 854.2 line minimum intensity. This latter is derived from the minimum position of the core as determined for each spectral profile and removes any effects of velocities in the conversion to $T_{\rm rad}$ .

The average $T_{\rm rad}$ map for the line minimum still shows a wealth of resolved, darker fibrils surrounding the extended bright network, even in this one hour average. Some of the regions of intermediate intensity (primarily at the top and bottom of the field) indicate the fibril-free portions of the internetwork (see Paper II for further details).

The image of the temporally averaged Ca II 854.2 synthetic filtergrams in Fig. 5a also shows the bright network surrounded by darker regions of fibrils, though their extent is smaller. The dark streaks surrounding the network are the result of the strong velocity crosstalk from the upflows arising from the base of the chromospheric fibrils.

Figure 5b shows the temporally averaged Ca II K filtergram and again the most obvious features are the areas of bright network outlining the magnetic field concentrations. In this image, individual fibrils are not visible, but the network is surrounded by darker regions that correspond closely to the fibril-dominated areas in the Ca II 854.2 image. This indicates that the signature of the fibrils may be present in the Ca II K filtergrams, even if they are not always resolved as individual structures due to the various effects described above.

4.2 Power maps

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{1223_f6.eps} \end{figure}$

Figure 6:

Power maps from integration of 1-D Fourier power at each pixel over three frequency bands arranged in columns ( left) five-minute, 1.8-3.5 mHz; ( center) three-minute, 4.0-7.5 mHz; and ( right) short period, 7.5-15 mHz. The four rows show the maps calculated for Ca II 854.2 line core minimum intensity; Ca II 854.2 synthetic filtergrams; 175 Ca II K filtergrams matched to times of synthetic filtergrams; 1576 Ca II K filtergrams taken with a strict 2 s cadence. The scales are given in Mm.

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$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f7.eps} \end{figure}$	Figure 7: Observed intensities on 18 April 2007: a) IBIS narrowband image -0.07 nm from Ca II 854.2 nm line core (height of formation $\sim$ 200 km); b) SOT Ca II H filtergram; and c) IBIS map of line minimum intensity of Ca II 854.2 (height of formation $\sim$ 1200 km).
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Since Ca II H and K images are often used for studies of chromospheric dynamics using Fourier and other temporal analysis, it is important to understand to what extent the chromospheric behavior is encoded in such filtergrams. We therefore compare the Fourier power of the intensity signals in several different frequency bands.

For each time sequence of radiation temperature maps, we calculate the Fourier power of the temperature modulation, separately for each spatial pixel in the FOV. We normalize by the mean intensity in each pixel in order to evaluate the modulation power (see de Wijn et al. 2005b). We then integrate the power over each of three ranges of frequencies: 1.8-3.5 mHz; 4.0-7.5 mHz; and 7.5-15 mHz (five-minute, three-minute, and ``high-frequency'' bands). The calculated power maps are shown in Fig. 6 for the Ca II 854.2 line minimum intensity (first row), the 854.2 synthetic filtergrams (second row), and the Ca II K filtergrams at both the same 19 s cadence as the Ca II 854.2 data (third row) and at the full 2 s cadence (fourth row).

Our ``pure'' chromospheric indicator, the 854.2 line core minimum intensity, shows a relative enhancement of the power in the magnetic network in the five-minute regime and the suppression of the three-minute oscillations in the fibrils surrounding the network (the ``magnetic shadows'', see Judge et al. 2001). This is consistent with the behavior found by Vecchio et al. (2009,2007) in the chromospheric velocities for this same dataset.

The power maps generated using the Ca II 854.2 synthetic filtergrams and the Ca II K filtergrams show comparable behavior in the five-minute and three-minute bands, with roughly similar spatial distributions of enhanced and suppressed power. There are also some interesting differences, such as clearer enhancement of the five-minute power in the network in the Ca II K filtergrams as compared to the Ca II 854.2 synthetic filtergrams (though still less pronounced then in the line minimum power maps).

We also note that the shadows are more spatially limited and less pronounced in both of the filtergram power maps as compared to the Ca II 854.2 line minimum power maps. Using the regions defined in Reardon et al. (2008), we find that the relative modulation power in the fibril region is reduced by a factor of six relative to the power of the quiet internetwork in the line core intensities, while the equivalent reductions in the Ca II 854.2 synthetic filtergrams and the Ca II K filtergrams are only a factor of five and three, respectively. Still, this shows that the signature of fibrils remains in the power maps for the Ca II K filtergrams, even if they are not visible in the individual intensity images.

The most striking difference in Fig. 6 is in the high-frequency regime, where magnetic shadows are still present in the power maps calculated for both the line minimum intensity and synthetic filtergrams but are almost nonexistent in the Ca II K power map. We test whether this lack of clear fibril signature might be due to a lower signal-to-noise ratio in the Ca II K filtergrams or perhaps caused by the irregular temporal sampling of the Ca II K sequence (in order to match the 19 s cadence of the Ca II 854.2 data). We calculate the same power maps using the full sequence of 1576 Ca II K images (bottom row in Fig. 6) taken with a strict two-second cadence. The shadows are only marginally more visible in this case and the overall resemblance to the chromospheric power maps derived from the Ca II 854.2 line core intensity is still poor. It appears that at higher frequencies the Ca II K filtergrams do not accurately represent the behavior of the chromosphere itself. We note that Cram (1978), using a slit spectrograph, observed a similar decreased in the high-frequency power in the Ca II K₃v intensity, even though the Ca II 854.2 nm line core intensity fluctuations remained significant. This indicates the lack of high-frequency power is perhaps due to a line-formation effect, such as the increased opacity of Ca II K leading to contributions over a larger range of heights, resulting in the cancellation of high-frequency oscillations with a mixtures of phases throughout the contribution region.

4.3 Hinode/SOT Ca II H filtergrams

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f8.eps} \end{figure}$	Figure 8: As in Fig. 7, but with the intensities integrated over the one hour duration of the observations.
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$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f9.eps} \end{figure}$	Figure 9: As in Fig. 7, but maps of 1-D Fourier power at each pixel integrated over the range 4.0-7.5 mHz.
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Through comparison with the Ca II 854.2 data, we have determined that some chromospheric signatures do appear in Ca II K filtergrams acquired with narrow filters ( $\sim$ 0.05 nm FWHM). The question remains of whether any such signature persists when using broader filters.

To examine this question, we utilize a sequence of Ca II H filtergrams obtained with Hinode/SOT (Kosugi et al. 2007; Tsuneta et al. 2008). These data were obtained on April 18, 2007 near disk center in an equatorial coronal hole. We select a one hour interval of simultaneous observations covering from 16:39-17:38 UT in which time we obtained 500 scans of the Ca II 854.2 line with IBIS while the SOT/BFI acquired 176 Ca II H filtergrams. Since the SOT Ca II H filter has an FWHM of 0.22 nm, we are not able to construct similar synthetic filtergrams with the IBIS data because of the limits of their spectral coverage. However, we can apply some of the techniques described in previous sections to search for chromospheric signatures in the SOT filtergrams. In particular, we compare the filtergrams to the most similar ``monochromatic'' IBIS images, those acquired in the Ca II 854.2 blue wing at 0.07 nm from the line core, which is formed in the middle photosphere at an average height of 200 km (see Fig. 5 of Paper I). We also compare them to the chromospheric Ca II 854.2 line core minimum intensity.

In Fig. 7 we display single images taken at 17:13 UT in each of the three diagnostics. The Ca II 854.2 line core intensity in Fig. 7c shows a wealth of diffuse structures, fibrils surrounding magnetic concentrations, and regions of patchy internetwork. These chromospheric features are entirely absent in the cotemporal line wing and Ca II H filtergram, which both show primarily the photospheric reversed granulation and the magnetic bright points.

In Sect. 4.1 we saw how temporally averaging Ca II K filtergrams was able to bring out a faint signature of the canopy surrounding the magnetic network. The results of a similar average with these data is shown in Fig. 8, but with this broader filter even the temporal averaging is not able to clearly bring out any clear chromospheric structuring from the Ca II filtergrams (Fig. 8b) when compared to the averaged Ca II 854.2 line core intensity (Fig. 8c).

As a final test, we also calculate the three-minute power maps in the same way as in Sect. 4.2 for the Ca II H filtergrams as well as the Ca II 854.2 line core and line wing intensities. Even in this very quiet region the magnetic shadows are again clearly visible in the line core intensity power (Fig. 9c), but there is little trace of them in the Ca II H power maps (Fig. 9b). The Ca II power map is highly similar, even in the small details, to the photospheric power map derived from the wing of the line (Fig. 9a). Observing on the solar disk, such a broad filter apparently captures very little of the chromospheric dynamics.

5 Conclusions

In this Paper we examine the causes of the very different appearance of on-disk filtergrams obtained with the Ca II H or K lines and those that use other chromospheric lines such as H $\alpha$ and Ca II 854.2. Given the widespread use of filtergrams in investigations of the solar atmosphere, it is important to ask to what extent these kind of data actually represent the structure and behavior of the chromosphere.

We used a series of repeated imaging spectral scans through the Ca II 854.2 nm line in the quiet chromosphere with IBIS and compared them with a simultaneous sequence of Ca II K filtergrams. Our main conclusion is that the lack of well defined chromospheric features in the K filtergrams, such as fibrils and mottles, is essentially due to observational limitations. We confirmed this by generating synthetic Ca II 854.2 ``filtergrams'' by applying a suitably chosen simulated filter profile to the spectrally resolved 854.2 images. Both the observed Ca II K and synthetic Ca II 854.2 intensities were then transformed into radiation temperature, in order to partially account for the different sensitivity of the Planck function at the different wavelengths of the two lines.

Filters sum contributions from different points throughout a line profile. This is particularly important in the Ca II H or K lines given the widths of the filters presently available and the broad range of heights over which the line is formed. Using the shape and position of the spectral transmission of the Halle filter used at the DST, we derived the temperature response function for the Ca II K line in the reference FALC static atmosphere, and showed that it has a broad contribution with a peak at around 400 km, but spanning from the deep photosphere ( $\sim$ 100 km) to the lower chromosphere ( $\sim$ 1100 km). This effect has long been known and has also been recently investigated by Carlsson et al. (2007) in a study of high frequency acoustic waves in the quiet chromosphere. They performed a similar calculation for the broader Ca II H filter on Hinode/SOT and found an average response height of 250 km, with a weaker, broad contribution extending up to 600 km. We confirm this by direct comparison of SOT Ca II H images with images from different positions in the Ca II 854.2 line profile and further show that there is negligible chromospheric signature in the quiet-Sun images taken with the Ca II H filter on SOT.

This summing of contributions results in many chromospheric structures being ``swamped'' by the stronger photospheric signals from the wings of the line. Dark structures, such as fibrils and filaments, may be most strongly affected by this mixing, since their contribution becomes increasingly negligible compared to the that from the wings of the lines. Brighter chromospheric structures instead tend to persist, especially magnetic structures which show relative brightness enhancement both at chromospheric heights as well as at the mid-photospheric regions that make a significant contribution to the overall filtergram intensity. This explains many of the typical characteristics of Ca II H and K filtergrams: the bright network is clearly defined, but only traces of the strongest chromospheric fibrils are seen. Away from the magnetic network, the filtergrams contain a mixture of the reversed granulation arising from the mid-photosphere, enhancements caused by small internetwork magnetic elements, and the intermittent brightenings due to acoustic events in the chromosphere. There is no way to distinguish whether a brightening observed in a Ca II H or K filtergram is of chromospheric or photospheric origin.

Our results are noteworthy for at least two reasons: first, we prove that this effect is important even for the narrowest available K filters ( $\sim$ 0.05 nm FWHM); and second, we do so by direct comparison with the features observed in a subordinate Ca II line directly related to the resonance lines. No chromospheric model is yet capable of reproducing the spectral characteristics of magnetic features in the quiet atmosphere.

Beyond the effect of the filter transmission profile, there is additional degradation of the chromospheric signal in the Ca II K filtergrams due to other observational effects. The spatial resolution in Ca II K filtergrams often suffers due to the significantly longer exposure times (arising from a combination of the dropoff of the Planck function, reduced atmospheric transparency, low filter transmission, and decreased detector efficiency) and the worsening of the atmospheric seeing at shorter wavelengths. There are still differences between the observed and synthetic filtergrams, primarily the greater visibility of the chromospheric fibrils in the Ca II 854.2 filtergrams. This is due in large part to a factor of four increase in the velocity-to-intensity crosstalk in the Ca II 854.2 synthetic filtergrams.

However, even if not immediately visible, the Ca II K filtergrams obtained with the Halle filter do contain several signatures of the chromospheric fibrils. Some of the darkest fibrils in the Ca II 854.2 images can be seen to correspond to direct counterparts in the Ca II K filtergrams. The distribution of fibrils becomes clearer when taking a temporal average of the Ca II K filtergrams, which shows a slightly decreased intensity surrounding the network magnetic patches corresponding to the location of the fibrils in the Ca II 854.2 line core. A further signature is the presence of the ``magnetic shadows'' (Judge et al. 2001) in the map of three-minute Fourier power derived from the modulation of the radiation temperature in the Ca II K filtergrams. These shadows are similar to those seen in the analogous power maps derived from the Ca II 854.2 line core intensities, but with a more limited spatial extent and an amplitude reduced by one half. These shadows correlate with the presence of the chromospheric fibrils (Vecchio et al. 2007) and indicate that the presence of the fibrils can be extracted in the overall time series of filtergrams. The relatively stable intensity of the fibrils was also discussed in Paper II.

It is also important to note that the power maps at higher frequencies from the Ca II K filtergrams display little of the structuring seen in the same range using the Ca II 854.2 line. In the latter line, the intensity variations in the 7.5-15 mHz range show a continued dependence on the chromospheric fibril structures, with magnetic shadows still prominent, while in the Ca II K maps this chromospheric signature is almost completely absent. This indicates that on-disk filtergrams in the Ca II H and K lines, even with relatively narrow filters, may not be suitable for investigation of the high-frequency behavior of the chromosphere.

Based on the above discussion, it would appear that the picture given by the H $\alpha$ and Ca II 854.2 lines, with significant portions of the chromosphere being dominated by magnetic structuring, represents the true nature of the chromosphere. As a corollary, on-disk images that don't show evidence of such structuring, even in the quiet Sun, cannot be said to realistically portray the chromospheric conditions. We expect that images in Ca II H and K lines taken with higher spatial and spectral resolution will show a silmilar wealth of fibrillar structures (Pietarila et al. 2008). In the absence of such data, and given the observational advantages of working at longer wavelengths (with the one drawback of decreased spatial resolution), the Ca II 854.2 nm line represents an excellent chromospheric indicator.

Acknowledgements

The authors are grateful to the DST observers D. Gilliam, M. Bradford and J. Elrod, whose patience and skills are greatly appreciated. We thank Rob Rutten for insightful discussions on the presence and visibility of fibrils in Ca II K. IBIS was built by INAF-Osservatorio Astrofisico di Arcetriwith contributions from the Università di Firenze and the Università di Roma Tor Vergata. Further support for IBIS operation was provided by the Italian MIUR and MAE, as well as NSO. NSO is operated by the Association of Universities for Research in Astronomy, Inc. (AURA), under cooperative agreement with the National Science Foundation. NSO/Kitt Peak FTS data used here were produced by NSF/NOAO. This research has made use of NASA's Astrophysics Data System (ADS). Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in co-operation with ESA and NSC (Norway).

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All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1223_f1.eps} \end{figure}$	Figure 1: Top panel: Ca II 854.2 nm atlas profile (black line) from the FTS atlas (Wallace et al. 1993,1998), the IBIS transmission profile (orange line), and the ``synthetic'' instrumental profile (blue line), derived as described in the Sect. 3.1. The red crosses show the observed spectral profile averaged over a portion of the field of view at the 27 sampled spectral positions. Bottom panel: Atlas profile for the core of Ca II K (black line) and theoretical instrumental passband of the Halle filter (blue line). The plotted wavelength range is scaled according to the wavelengths of the two lines. In both plots, the transmission of the filter passband has been arbitrarily scaled to accommodate the plotted range of the atlas profile.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1223_f2.eps} \end{figure}$	Figure 2: Simultaneous individual images from the full observing sequence: a) Ca II 854.2 nm blue wing -0.07 nm from line core; b) Ca II K filtergram; c) Ca II 854.2 line core. The orange squares, yellow ovals, and pink triangles indicate respectively: structures present in the Ca II line wing images; in the Ca II line core images; or in both. The spatial scale is given in Mm.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=8.4cm,height=6cm,clip]{1223_f3.eps} \end{figure}$	Figure 3: Temperature response functions for the Ca II K filtergrams (solid) and the Ca II 854.2 nm synthetic filtergrams (dashed) (see Sect. 3.1). The x axis represents heights from the solar surface ( $\tau _{500}=1$ ) in km. Both curves have been computed for the FALC model.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{1223_f4.eps} \end{figure}$	Figure 4: Radiation temperature maps derived from a) the synthetic 854.2 filtergram and b) the observed K filtergram's intensity. The shapes indicate the same features as in Fig. 2. Average values are 4540 and 4600 K, respectively.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=17.5cm,clip]{1223_f5.eps} \end{figure}$	Figure 5: Temporally averaged radiation temperature maps summed over the 175 realizations obtained during the one hour time series. a) Ca II 854.2 synthetic filtergrams, b) Ca II K filtergrams, and c) Ca II 854.2 line minimum intensity. The two filtergrams are both scaled between 4400 and 4900 K and the line minimum intensity is scaled between 3500 and 4800 K.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{1223_f6.eps} \end{figure}$	Figure 6: Power maps from integration of 1-D Fourier power at each pixel over three frequency bands arranged in columns ( left) five-minute, 1.8-3.5 mHz; ( center) three-minute, 4.0-7.5 mHz; and ( right) short period, 7.5-15 mHz. The four rows show the maps calculated for Ca II 854.2 line core minimum intensity; Ca II 854.2 synthetic filtergrams; 175 Ca II K filtergrams matched to times of synthetic filtergrams; 1576 Ca II K filtergrams taken with a strict 2 s cadence. The scales are given in Mm.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f7.eps} \end{figure}$	Figure 7: Observed intensities on 18 April 2007: a) IBIS narrowband image -0.07 nm from Ca II 854.2 nm line core (height of formation $\sim$ 200 km); b) SOT Ca II H filtergram; and c) IBIS map of line minimum intensity of Ca II 854.2 (height of formation $\sim$ 1200 km).
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f8.eps} \end{figure}$	Figure 8: As in Fig. 7, but with the intensities integrated over the one hour duration of the observations.
Open with DEXTER
In the text

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{1223_f9.eps} \end{figure}$	Figure 9: As in Fig. 7, but maps of 1-D Fourier power at each pixel integrated over the range 4.0-7.5 mHz.
Open with DEXTER
In the text

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