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All issues Volume 10 (2020) J. Space Weather Space Clim., 10 (2020) 31 Full HTML
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J. Space Weather Space Clim.
Volume 10, 2020
Topical Issue - Space Weather Instrumentation
Article Number 31
Number of page(s) 11
DOI https://doi.org/10.1051/swsc/2020032
Published online 05 August 2020

© J.-M. Malherbe et al., Published by EDP Sciences 2020

Licence Creative CommonsThis is an Open Access article distributed under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

1 Introduction

Solar activity is the primary driver of space weather and space climate (e.g., Schrijver et al., 2012; Pomoell & Poedts, 2018). It varies over a wide range of time scales from several minutes with solar flares and Coronal Mass Ejections (CMEs; e.g., Shibata & Magara, 2011) to hundreds of years with the ≈100-year modulation (Gleissberg cycle) of the 11-year solar cycle (e.g., Hathaway, 2015). Both short-term and long-term full-disk observations of the Sun are thus critical for improving our understanding of solar activity at all time scales, but also for monitoring and predicting it in space weather forecast applications (e.g., Ueno et al., 2010; Malherbe et al., 2019).

Ground-based observations of the chromosphere are of particular interest, because this layer is the source of solar activity. Two international networks are already operating with several ground-based stations at various longitudes: the Global Hα Network (GHN, http://ghn.njit.edu) and the GONG Hα network (http://halpha.nso.edu). Counterparts in the hot corona above are observed in EUV by Solar Dynamics Observatory (SDO/AIA, NASA, since 2010) or radiotelescopes (e.g., Nançay, Nobeyama). Events at large distance of the Sun (up to 30 rad) are tracked by several wide angle, white light space coronographs (SoHO/LASCO, ESA/NASA, since 1996; STEREO/NASA since 2006). Parker Solar Probe (NASA, launched in 2018) observes in situ the far corona and the Solar Orbiter mission (ESA) started early 2020. SDO/HMI provides in addition photospheric magnetograms and dopplergrams.

We summarize below the interest of chromospheric observations in the scope of space weather research and applications. Then we review the state of instrumentation dedicated to this task at Paris (OP) and Côte d’Azur (OCA) observatories in the context of the upcoming solar cycle 25. Section 2 presents new instrumentation for short-term, high-cadence monitoring of solar activity. The widely open data will be used by the french Air Force for space weather forecast and by the scientific community to investigate unstable phenomena as flares, Moreton waves or CMEs. Section 3 describes the long-term, low-cadence Spectroheliograph while Section 4 develops the wavelength calibration of new datacubes.

1.1 Short-term, high-cadence chromospheric observations

High-cadence Hα observations are widely used in the context of solar flare/CME analyses and monitoring (e.g., Deng et al., 2002; Huang et al., 2014). In the case of filament eruptions, such data allow one to follow the pre-, and early-, eruptive dynamics of the filament, which provide insights into both the CME triggering and driving mechanisms when combined with the analysis of other datasets such as photospheric magnetic field data (e.g., Joshi et al., 2014; Chen et al., 2018). Adopting the framework of the Torus Instability (one of the main models considered for CME trigger/driver; Kliem & Török, 2006; Démoulin & Aulanier, 2010), then Hα imaging can further be used to monitor the slow rise of the filament and predict when it will reach the critical height for the onset of the instability (e.g., Filippov & Zagnetko, 2008; McCauley et al., 2015).

More generally, high-cadence Hα observations are further interesting because they also register the chromospheric response to solar flares/CMEs, as flare ribbons (e.g., Wang et al., 2003; Jiang et al., 2014) and Moreton waves (e.g., Narukage et al., 2008; Muhr et al., 2010). Flare ribbons are “surface” brightenings (often observed in EUV and Hα) caused by the interaction of energetic particles and thermal energy (emitted at the coronal reconnection region) with the lower and denser layers of the solar atmosphere (e.g., Schmieder et al., 1987; Fletcher et al., 2011). Moreton waves are large-scale disturbances that appear as arc-shaped, bright fronts in the center and blue wing of the Hα line (e.g., Moreton, 1960; Zhang et al., 2011) and which physical nature is still not yet fully understood (e.g., Liu et al., 2013; Warmuth, 2015). Both Hα flare ribbons and Moreton waves are chromospheric signatures of the coronal dynamics. Their spatial and temporal evolution thus provide crucial information on the flare/CME energetics (e.g., Gilbert et al., 2008; Veronig & Polanec, 2015), which can be used to estimate the potential impact of the flare/CME on the Earth’s magnetosphere in space weather forecast applications.

1.2 Long-term, low-cadence chromospheric observations

On the other hand, long-term, low-cadence full-disk observations of the chromosphere in CaII K and Hα lines, such as the centennial Kodaikanal (Hasan et al., 2010) and Meudon collections (Malherbe & Dalmasse, 2019), are gold mines for research on the solar cycle and its variability. The CaII K1v imaging (blue wing) allows us to derive the sunspots number and area (e.g., Bertello et al., 2016; Chatterjee et al., 2016), while the Hα imaging enables us to compute the number of filaments and their lengths (e.g., Mouradian & Soru-Escaut, 1993; Hao et al., 2015). All these quantities are good tracers of solar activity that permit us to probe the properties of the solar cycle (amplitude, duration, activity level). The accumulation of such data series and products over very long periods is thus essential to study and improve our understanding of the solar cycle variability and modulation (including the Gleissberg modulation or the occurrence of grand minima such as the Maunder minimum; e.g., Clette et al., 2015; Webb et al., 2018), both of which directly affect space weather.

The study of rare events is yet another research field to which long-term, full-disk CaII K1v and Hα archives contribute. Determining the frequency of rare events such as large sunspot groups is key to both solar dynamo and climatology (e.g., Jiang et al., 2015; Schmieder, 2018). Recent work by Nagy et al. (2017) shows that the emergence of a large-scale bipolar active region into the solar atmosphere can have major effects on the properties of the solar cycle and its cycle-to-cycle variability. It can introduce an activity asymmetry and time lag between the North and South solar hemispheres (similar to the one already observed; e.g., McIntosh et al., 2013; Svalgaard & Kamide, 2013), or trigger a grand minimum in the subsequent cycles (similar to the Maunder minimum; e.g., Spoerer & Maunder, 1890; Ribes & Nesme-Ribes, 1993).

CaII K3 (line center) and Hα imaging can also be used to probe the magnetic properties of solar active regions and the energy of solar flares in old archives, both of which are essential to research on extreme solar flares for the development of space weather prediction tools (e.g., Gopalswamy, 2017; Tsiftsi & De la Luz, 2018). For instance, CaII K spectroheliograms provide a means to estimate the magnetic flux in plages and sunspots, thus enabling the construction of pseudo-magnetograms (e.g., Harvey & White, 1999; Pevtsov et al., 2016). Using empirical laws derived from observations and MHD models, one can further quantify the flare-energy release from Hα bright ribbons (e.g., Toriumi et al., 2017), and/or the maximum energy available for a solar flare from the CaII K size and area of an active region (e.g., Aulanier et al., 2013).

2 MeteoSpace at Calern

The MeteoSpace instrument will operate in 2021 at Calern (OCA, 1270 m elevation, the sunniest station in France). It is a fully automated system dedicated to short-term, high-cadence monitoring of chromospheric activity. For that purpose, three telescopes will be available (Malherbe et al., 2019): two for Hα line and one for CaII K line.

MeteoSpace will complete the world-wide Hα survey with enhanced features. It will join the GHN network, composed of many heterogeneous instruments in terms of cadence, spatial resolution, seeing, filter type and bandwidth. In terms of capabilities, MeteoSpace is close to the homogeneous GONG Hα network (same filters), but it will offer improved temporal resolution (15 s) and two Hα channels (line center and blue wing). MeteoSpace will also propose CaII K systematic images, with faster cadence (60 s) than previous routines (such as PSPT); CaII K is more chromospheric than the space-borne SDO/AIA 1600 and 1700 Å channels.

The optical diameter of the three imagers is 100 mm with 985 mm equivalent focal length. The filters bandwidth, optical resolution on the Sun and observing cadence are given by Table 1. Instruments are enclosed in a temperature controlled box (active heating, passive cooling) supported by an equatorial mount. The detectors are QSI 660i and 690i air cooled cameras using shutterless interline CCD sensors from Sony (3000 dynamic range, 12 bits).

Table 1

Capabilities of the MeteoSpace and Spectroheliograph instruments.

MeteoSpace is the first solar automatic station in France. All operations are fully robotized: weather checking, opening and closing the dome, catching the Sun, solar tracking, data acquisition, processing and transfer to the archive, and website update. MeteoSpace is supervised by a main computer connected to several sub-systems, for environment (weather station and full-sky camera), mount steering, instrument and camera control, data archiving and webservice. Two scintillometers (AiryLab company) provide an estimate of flux and seeing conditions (1″ typical at Calern) for each image. The instrument is protected by many house-keeping procedures, including weather phenomena; in case of failure, a short messaging service (SMS) generates an alert to the local staff.

Quick look data (JPEG) will be available in real time, while scientific images (FITS) will be delivered a few hours later after calibration and corrections of dark current, geometric distorsion and rotation to present solar north up. Data will be processed and stored at Nice (30 Tera bytes available) but accessed through the BASS2000 national database dedicated to ground-based observations (http://bass2000.obspm.fr); a real-time channel is under development to disseminate high-cadence Hα images for space weather applications.

Figure 1 displays the two Hα imagers. They are enclosed in a 1.7 × 0.5 × 0.5 m3 box at 27 °C temperature (maximum value at Calern in summer), with active heating but passive cooling. The entrance objective (L1) is a Takahashi TSA102. Both incorporate an afocal magnifying system (L2/L3, ×1.2) for the temperature regulated Fabry-Pérot filter working in the F/30 beam (DayStar company, Quantum Pro series). The filter (F) is located in the pupil plane of the chamber, which includes L3, the filter plus a motorized field corrector/focuser (L4, M, Fig. 2). Flares, filament eruptions and CMEs will be observed with the first Hα, line centered filter. The second filter is blue wing shifted (−0.5 Å) and dedicated to the detection of fast Moreton waves by running differences of consecutive images, as explained by Malherbe et al. (2019). The wavelength transmission curves of both filters are displayed in Figure 3. They were computed from Hα line profiles observed with the 14 m spectrograph (0.02 Å spectral resolution) of the Meudon Solar Tower. The curves derive from filter scans by the slit, after surface averaging, because the setup is a pupil plane application.

thumbnail Fig. 1

Top: the MeteoSpace overall structure (0.5 × 0.5 × 1.7 m) enclosing three instruments; H = Hα; Ca = CaII K. Middle: details of the two Hα telescopes; E = energy rejection filter (Baader); L1 = entrance objective (Takahashi TSA102); L2/L3 = afocal magnifying system; F = DayStar Quantum PE Fabry Pérot filter; L4 = field corrector/focuser; M = focuser motor; C = cooled CCD camera (QSI 660i). Bottom: optical design of the Hα telescopes.

thumbnail Fig. 2

The chamber of MeteoSpace Hα telescopes. L3 = chamber objective; F = DayStar Quantum PE Fabry Pérot filter; L4 = field corrector/focuser; M = focuser motor; C = cooled CCD camera (QSI 660i).

thumbnail Fig. 3

The transmission curves of the line centered filter (black) and of the blue-shifted filter (blue) as a function of wavelength. The dashed line is the observed Hα line profile.

The CaII K filter has a bandwidth four times larger than Hydrogen filters and provides a proxy of chromospheric magnetic fields covering facular regions. The entrance objective of the telescope is a Takahashi FS102. The interference filter (from Barr Associates) is located in the image plane of the motorized magnifier/focuser (×1.2, not shown).

Figure 4 shows a simulation based on (x, y, λ) dadacubes of the Meudon Spectroheliograph recorded on 13 Nov 2013 (near solar maximum) during a test campaign (Sect. 3). The two Hα images (core and blue wing centered) are obtained applying the wavelength transfer function of the respective filters (Malherbe et al., 2019) to line profiles. Then, both images can be combined in order to provide enhanced contrast pictures of filaments, plages and prominences at the limb. For that purpose, the blue wing is subtracted to the line core image after normalization by mean intensities measured in a large area around disk center. The CaII K image is obtained also by integration of the spectrum over the filter transmission curve. The result is intermediate between K1v and K3 spectroheliograms (Sect. 3); sunspots and bright active regions are well visible, but the filter bandpass make the filaments vanish.

thumbnail Fig. 4

Simulation of typical data that will be produced by the MeteoSpace instrument. Top (left to right): Hα core and Hα blue wing (−0.5 Å). Bottom (left to right): composite Hα image showing enhanced structures (line center minus blue wing) and CaII K.

The simulation allows to quantify the loss of structure contrast resulting from spectral integration over the Lorentzian transmission of filters in comparison with spectroscopic observations (Table 2). For Hα, it reveals a loss for filaments and faculae. On the contrary there is a gain for sunspots, because the visibility of sunspots is better in the continuum and wings than in the line core. The same conclusions are amplified for CaII K, because the filter is broader. The visibility of prominences at the limb is not affected for Hα but is degraded in CaII K for the same reason.

Table 2

Contrast loss of MeteoSpace structures compared to the Spectroheliograph at line center.

3 Meudon Spectroheliograph

Meudon Spectroheliograph operates daily since 1908 in CaII K and Hα chromospheric lines. It is not a filtergraph, but a spectrograph (Fig. 5) providing classical (λ, x) spectra (x abscissa along the slit). The second direction y, necessary to form solar images, comes from the scan of the solar surface. The main characteristics are reported in Table 1.

thumbnail Fig. 5

The Spectroheliograph and optical scheme. S = entrance slit; SP = spectrograph; F = interference filters; M = neutral density “moon” translator for prominences; O1 = entrance objective and translator; O2 = collimator; O3 = chamber objective; A1, A2 = historical “arms” with old photographic 13 × 18 cm plate systems.

This instrument provided monochromatic images using glass and later film plates until 2001. The photographic device was replaced by a CCD array in 2002 (Malherbe & Dalmasse, 2019). Since mid 2017, the detector is a fast SCMOS sensor which records full line profiles, so that (x, y, λ) datacubes are registered in 3D FITS files, as shown by the online movie (see Supplementary Material, Movie S1 for details). Images are derived from the datacubes for precise wavelength positions along the line profiles.

The spectrograph is fixed and fed by a coelostat (two flat mirrors) and a 250 mm diameter objective (O1, 4 m focal length). The slit (S) of the spectrograph (30 microns or 1.5″ width) is located in the solar image (37.2 mm diameter). The entrance objective (O1) is mounted on a motorized translator in order to scan the solar surface in 60 s typically.

The spectrograph has a 1.3 m focal length (O2) and uses a 300 groves/mm grating (17°27′ blaze angle). Spectral lines form at interference orders 3 (Hα) or 5 (CaII K and H). Orders are selected by filters (F). The spectral resolution is about R = 40,000. The detector is a fast SCMOS sensor (PCO water cooled camera, 150,00 dynamic range, 14 bits) mounted on a SkyWatcher 0.4 m apochromatic objective (O3). The throughput is 100 (λ, x) spectra/s. CaII K and H are always observed simultaneously (see Fig. 6 with solar atlas comparison). Long exposure observations are also done for prominences (5–10 times fainter) at the limb; in order to preserve the structures of the disk, an artificial “moon” (neutral density 0.9) is put against the solar image and is mechanically coupled to the objective translator O1.

thumbnail Fig. 6

Spectrum (λ, x) between 3900 and 4000 Å displaying CaII K and H lines near disk center. Top: high resolution atlas (R = 2 × 106, Delbouille et al., 1973). Bottom: Spectroheliograph (R = 40,000).

Standard corrections include dark current, curvature of spectral lines and rotation (solar north up). Line profile datacubes (3D FITS) of Hα, CaII H and CaII K, as well as classical images (JPEG and 2D FITS derived from datacubes at line center, wings or continuum) are freely available to the community through BASS2000 at http://bass2000.obspm.fr. Raw datacubes (TIF) are also stored online for specific use at ftp://ftpbass2000.obspm.fr/pub/meudon/spc/tiff. Datacubes of Hβ line are scheduled for 2021.

In order to illustrate the Spectroheliograph capabilities, we chose datasets recorded near the last solar maximum (13 Nov 2013) with the new SCMOS detector (which was, at this moment, only available for tests). Figure 7 shows images extracted from Hα line profiles, with many sunspots, filaments and active regions. The composite image comes out from the difference between line core and the sum of the red and blue wings, after normalization by the average values computed in a quiet Sun region near disk center. This method makes all structures of the Sun appear together in a single frame (prominences, chromosphere at the limb, spots, filaments, faculae) with enhanced contrast. The Doppler velocity proxy is made of the contrast of line wings (ratio between the difference and sum of red and blue wings, after normalization by disk center values).

thumbnail Fig. 7

Typical images issued from Hα datacubes produced by the Spectroheliograph. Top (left to right): continuum (−1.07 Å), blue wing (−0.43 Å) and line core. Bottom (left to right): limb prominences, composite image (line center minus red and blue wings) and Doppler proxy (contrast between both wings).

Figure 8 displays images derived from CaII K line profiles (CaII H line is also available, as observed simultaneously, and provides similar results). K1v and K3 are respectively the blue wing and line core. The composite image comes out from the difference between line center (K3) and the sum of the red and blue wings (K1r + K1v at ±1.0 Å), after normalization by the average values measured in a quiet region near disk center. As for Hα, this method reveals all solar structures in a synthetic image (prominences, chromosphere at the limb, spots, filaments, bright plages) with better contrast.

thumbnail Fig. 8

Typical images issued from CaII K datacubes of the Spectroheliograph. Top (left to right): K1v (blue wing, −1.0 Å) and K3 (line core). Bottom (left to right): limb prominences (K3) and composite image (line center minus red and blue wings).

4 Wavelength calibration of Spectroheliograph datacubes

Let us call C[i, j, k] the datacubes provided by the Spectroheliograph FITS files with i, j, k varying from 1 to respectively NAXIS1, NAXIS2 and NAXIS3 (pixel numbers). They need to be calibrated along the wavelength axis (k) in order to compute header CRPIX3 and CRVAL3 keywords (line center in pixel unit and in Å, respectively, see Greisen & Calabretta, 2002). They are roughly known in advance but can be precisely determined. We first locate the minimum of the integrated intensities of the cube images:

(1)

(2)

The minimum of S obs at index k min may not be strictly at the line core location λ c (keyword WAVELNTH). The idea is then to fit the observed line profile with a reference one S ref(λ) in order to identify precisely the location of the minimum and assign to it the value of λ c . The reference spectrum is taken from the visible atlas by Delbouille et al. (1973) available online at the BASS2000 website (http://bass2000.obspm.fr) with a resolution of = 0.002 Å. The bandwidth of the cube is assumed unknown and therefore the reference spectrum is smoothed over a number of points n that we also have to determine. We define the smoothed reference spectrum to which we want to compare the observed one by:

(3)

The minimum value of this smoothed spectra is located at λ s (n) which is a function of n and is slightly different from λ c . The wavelengths corresponding to the different images of the cube are obtained by

where Δλ (the wavelength increment in Å) is given by the FITS keyword CDELT3:

(4)and k min is an unknown fractional index. We assign λ c to the keyword CRVAL3 and compute CRPIX3 through:

A linear scaling between the smoothed reference spectra and the observed one may not be always appropriate far from the line core. We allow a wavelength dependence of the linear term and write (see top panel of Fig. 9):

(5)where:

thumbnail Fig. 9

Example of wavelength calibration of CaII K spectral line. The red crosses represent the observed disk-integrated intensities S obs (Eq. (1)). The black lines are the scaled smoothed reference spectrum (Eq. (5)). Top panel: S obs and are plotted as a function of the intensities of the smoothed reference spectrum (Eq. (3)). Middle and bottom panels: S obs and are plotted as a function of wavelength. The coefficients a, b, c and d of the fit are shown. The vertical blue line gives the line core position at λ c = 3933.663 Å. The corresponding FITS index is given by CRPIX3. The interval over which the reference spectra is smoothed is given by δλ. WSSR is the resulting weighted sum of squared residuals. The top and middle panels give the fit with the initial parameters and the bottom panel gives the fit and parameters after optimization (lower WSSR).

The six free parameters of the model are therefore: a, b, c, d, n and k min. They could be obtained by minimizing the sum of squared residuals:

(6)

This quantity however will depend on the scaling parameters and will not permit an easy comparison for the goodness of the fit between different data cubes (quality index). We therefore prefer instead to build, from the observed profile, a profile that can always be compared to the reference one. From equation (5), we can define:

(7)

Furthermore, we use a weighting function chosen in order to give maximum weight to the points close to the line core:

The six model parameters are thus obtained by minimizing a weighted sum of squared residuals (WSSR):

We perform a multidimensional minimization using the Nelder-Mead simplex algorithm (Gao & Han, 2012). For the initial parameters we take n = 2Δλ/, k min is obtained from equation (2) and, given these two values, a, b, c, d are the least-squares solution to the linear matrix (5) which minimizes the SSR of equation (6).

For CaII K spectral line, Figure 9 shows the observed integrated intensities S obs compared to the scaled smoothed reference spectrum using the initial parameters (middle panel) and after optimization (bottom panel). Such calibrations are performed daily for CaII H, K and Hα lines; the result is available at ftp://solar-ftp.oca.eu/SHG/.

5 Conclusions

New solar cycle 25 will be intensively observed at Paris and Côte d’Azur observatories with new and fast automatic instruments (MeteoSpace at Calern in 2021) or with improved capabilities existing ones (Meudon Spectroheliograph).

The MeteoSpace instrument is a new set of three automated telescopes using narrow Fabry-Pérot filters and dedicated to short-term, high-cadence (20 s) imagery of fast events such as flares, filament eruption, CME onset and Moreton waves. Simulations of Hα blue wing and line core images, as well as CaII K (magnetic proxy), are shown. In comparison with spectroscopic data, the Lorentzian shape of filters reduces the contrast of structures (−40% on filaments and faculae in Hα), but we suggest a simple method combining them to produce composite and enhanced images. Low cost pre-filters could also be added to limit the contrast loss to −30%. Capabilities could be extended at the end of the space-borne SDO mission by a fourth telescope for Stokes V measurements (magnetograms) in the blue wing of NaD1 5896 Å line.

The Spectroheliograph is dedicated to long-term, low-cadence observations of the chromosphere and now delivers (x, y, λ) datacubes of Hα, CaII H and K spectral lines, from which classical images are derived. A precise wavelength calibration method of datacubes, using comparison with atlas spectra, is proposed. Observation of Hβ line is the next extension.

All data are (or will be) freely available to the scientific community through a dedicated web service (BASS2000), which will offer an additional real-time channel to disseminate high cadence MeteoSpace images for space weather applications.

Acknowledgments

We are indebted to the referees and to the editor for helpful comments and suggestions. We thank the observers operating the Spectroheliograph and the technical team of the MeteoSpace project. We acknowledge financial support of several institutions as DGA, CNRS/INSU (PNST), Paris and Côte d’Azur observatories, Ile de France DIM/ACAV. This work has been supported through the UCA/JEDI investments managed by the National Research Agency (ANR) with the reference number ANR-15-IDEX-01. If you use data for publication, please insert the following sentence: “Spectroheliograph and MeteoSpace data are courtesy of Paris and Côte d’Azur observatories”. The editor thanks two anonymous reviewers for their assistance in evaluating this paper.

References

Cite this article as: Malherbe J-M, Corbard T & Dalmasse K 2020. Optical instrumentation for chromospheric monitoring during solar cycle 25 at Paris and Côte d’Azur observatories. J. Space Weather Space Clim. 10, 31.

Supplementary material

Supplementary Movie S1

MPEG4 movie showing a typical wavelength exploration of Spectroheliograph datacubes (observation of 13 Nov 2013) in Hα and CaII K lines. The current wavelength (Å) is indicated at the bottom of images. The mean line profile of disk center is superimposed with the moving wavelength index. Filaments appear only in the core of both lines. Access here

All Tables

Table 1

Capabilities of the MeteoSpace and Spectroheliograph instruments.

In the text
Table 2

Contrast loss of MeteoSpace structures compared to the Spectroheliograph at line center.

In the text

All Figures

thumbnail Fig. 1

Top: the MeteoSpace overall structure (0.5 × 0.5 × 1.7 m) enclosing three instruments; H = Hα; Ca = CaII K. Middle: details of the two Hα telescopes; E = energy rejection filter (Baader); L1 = entrance objective (Takahashi TSA102); L2/L3 = afocal magnifying system; F = DayStar Quantum PE Fabry Pérot filter; L4 = field corrector/focuser; M = focuser motor; C = cooled CCD camera (QSI 660i). Bottom: optical design of the Hα telescopes.
In the text
thumbnail Fig. 2

The chamber of MeteoSpace Hα telescopes. L3 = chamber objective; F = DayStar Quantum PE Fabry Pérot filter; L4 = field corrector/focuser; M = focuser motor; C = cooled CCD camera (QSI 660i).
In the text
thumbnail Fig. 3

The transmission curves of the line centered filter (black) and of the blue-shifted filter (blue) as a function of wavelength. The dashed line is the observed Hα line profile.
In the text
thumbnail Fig. 4

Simulation of typical data that will be produced by the MeteoSpace instrument. Top (left to right): Hα core and Hα blue wing (−0.5 Å). Bottom (left to right): composite Hα image showing enhanced structures (line center minus blue wing) and CaII K.
In the text
thumbnail Fig. 5

The Spectroheliograph and optical scheme. S = entrance slit; SP = spectrograph; F = interference filters; M = neutral density “moon” translator for prominences; O1 = entrance objective and translator; O2 = collimator; O3 = chamber objective; A1, A2 = historical “arms” with old photographic 13 × 18 cm plate systems.
In the text
thumbnail Fig. 6

Spectrum (λ, x) between 3900 and 4000 Å displaying CaII K and H lines near disk center. Top: high resolution atlas (R = 2 × 106, Delbouille et al., 1973). Bottom: Spectroheliograph (R = 40,000).
In the text
thumbnail Fig. 7

Typical images issued from Hα datacubes produced by the Spectroheliograph. Top (left to right): continuum (−1.07 Å), blue wing (−0.43 Å) and line core. Bottom (left to right): limb prominences, composite image (line center minus red and blue wings) and Doppler proxy (contrast between both wings).
In the text
thumbnail Fig. 8

Typical images issued from CaII K datacubes of the Spectroheliograph. Top (left to right): K1v (blue wing, −1.0 Å) and K3 (line core). Bottom (left to right): limb prominences (K3) and composite image (line center minus red and blue wings).
In the text
thumbnail Fig. 9

Example of wavelength calibration of CaII K spectral line. The red crosses represent the observed disk-integrated intensities S obs (Eq. (1)). The black lines are the scaled smoothed reference spectrum (Eq. (5)). Top panel: S obs and are plotted as a function of the intensities of the smoothed reference spectrum (Eq. (3)). Middle and bottom panels: S obs and are plotted as a function of wavelength. The coefficients a, b, c and d of the fit are shown. The vertical blue line gives the line core position at λ c = 3933.663 Å. The corresponding FITS index is given by CRPIX3. The interval over which the reference spectra is smoothed is given by δλ. WSSR is the resulting weighted sum of squared residuals. The top and middle panels give the fit with the initial parameters and the bottom panel gives the fit and parameters after optimization (lower WSSR).
In the text

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