Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://mavr.sao.ru/hq/lsfvo/devices/scorpio/0502095.pdf Äàòà èçìåíåíèÿ: Sat May 13 15:37:22 2006 Äàòà èíäåêñèðîâàíèÿ: Fri Dec 28 18:47:54 2007 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: astro-ph

Astronomy Letters, vol. 31, No.3, 2005, pp.193-203 Translated from Pis'ma v Astronomicheskii Zhurnal, vol.31, No.3, 2005, pp. 214-225

April 30, 2006

The SCORPIO Universal Focal Reducer of the 6-m Telescope
Afanasiev V.L. and Moiseev A.V.
Sp ecial Astrophysical Observatory, RAS, Nizhnii Arkhyz, Karachai-Cherkessian Republic, 357147 Russia

arXiv:astro-ph/0502095 v1 4 Feb 2005

Abstract. We describ e the SCORPIO focal reducer that has b een used since the fall of 2000 for observations on the 6-m Sp ecial Astrophysical Observatory telescop e. We give parameters of the instrument in various observing modes (direct images, long-slit and multislit sp ectroscopy, sp ectrop olarimetry, Fabry-Perot panoramic sp ectroscopy). Observations of various astronomical ob jects are used as examples to demonstrate the SCORPIO capabilities.

1. INTRODUCTION
The idea of using a focal reducer on a telescope was suggested and implemented by Georg Court´s as the 50e 60 of the last century (see, for example, Court´s, 1960, e 1964). The focal reducer allows several problems to be solved simultaneously. Firstly, the equivalent focal ratio of the system becomes faster and the field of view increases, which is important for studying faint extended ob jects. Secondly, the off-axis aberrations of the primary mirror can be corrected by using specially calculated optics. Thirdly, it becomes possible to install dispersing elements (grisms, Fabry-Perot interferometer (FPI) etc.) in the parallel beam between the collimator and the camera, which turns the focal reducer into a universal spectrograph. Instruments based on this scheme, which are primarily designed for the spectroscopy and photometry of faint extended ob jects, have gained wide acceptance in the last two decades. It will suce to mention the EFOSC camera of the 3.6-m ESO telescope (Buzzoni et al. 1984); in many respects, it became the prototype of modern spectrographs for 8-10-m telescopes, such as FORS on VLT (Nicklas et al. 1997). The first focal reducer for interferometric observations on the 6-m BTA telescope was created at the Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences in the mid-1980s using commercially available photographic lenses. Despite such shortcomings as poor image quality at the edge of the field of view, low optical transmittance (about 30% at maximum), and the absence of any automation, the reducer had been used on the 6-m BTA telescope for more than ten years until the question of its upgrading arose. In 1999, work on the creation of a new focal reducer for the prime focus of the 6-m BTA telescope began at the SAO. The
requests to : Alexei Moiseev, e-mail:

new SCORPIO (Spectral Camera with Optical Reducer for Photometric and Interferometric Observations) focal reducer has allowed the following types of observations of extended and starlike ob jects to be performed at the prime focus of the 6-m telescope: ­ Direct images in broad-, medium- and narrow-band filters. ­ Panoramic spectroscopy with the FPI. ­ Long-slit spectroscopy. ­ Slitless spectroscopy. ­ Multiob ject spectroscopy with 16 slits moved remotely in the focal plane. ­ Polarimetry in the filtres and spectropolarimetry. The mechanical and optical parts of SCORPIO were produced at the SAO breadboard workshops. The first BTA observations were performed in September 2000 with the old version of the prime-focus adapter. A new adapter platform came into use in May 2001. The first successful multislit spectroscopic observations were carried out in September 2003; in the summer of 2004, the spectropolarimetric mode was implemented, and the first observations were performed. In the next section, we consider the optomechanical layout of SCORPIO and its basic characteristics. Subsequently, we consider the peculiarities of observations in various modes; these are illustrated using specific results obtained with the 6-m telescope when the instrument was tested. In the last section we consider prospects for further upgrading SCORPIO .

2. Description of the sp ectrograph
Constructionally, SCORPIO consists of three parts each of which can be used independently: a focal reducer, a prime-focus adapter platform, and a CCD detector. Basic parameters of the instrument are given in Table 1.

Send offprint moisav@sao.ru


2

Afanasiev & Moiseev: The SCORPIO focal reducer

Table 1. The main characteristics of SCORPIO
Total focal ration F /2.6 Field of view: full 6.1 â 6.1 in mutlsilit mode 2.9 â 5.9 Image scale 0.18 /px Sp ectral range 3 600 - 10 000° A Sp ectral resolution with grisms ° (for slit width 1 ) 1.5 - 20A with Fabry-Perot interferometers 0.8 - 2.5° A Maximal quantum efficiency (telescop e+SCORPIO +CCD) Direct imaging 70% Sp ectroscopy 40% Observations with FPI 20%

2.1. The focal reducer
The optical layout of the focal reducer (Fig.1) includes a field lens and a collimator ­ a four-lens apochromat (F/2.2) that forms the exit pupil of the system, a camera ob jective ­ a six-lens apochromat (F/1.8), and replaceable optical elements ­ FPI, diffraction gratings, filters, a polarization analyzer, phase plates ant etc. The equivalent focal ratio of the system at the prime focus of the 6-m telescope is F/2.6. The optical surfaces are coated with seven antireflecting layers1 that work in the wavelength range 3500 - 10 000°. The laboratory measurements of A the SCORPIO spectral transmission curve are shown in Fig.2. Since the collimator optics corrects the coma and field curvature of the primary mirror of the telescope, we can abandon the use of the standard lens corrector without antireecting coating. The diameter of the collimated beam is 40 mm. The working focal length of the camera is 14 mm. The equivalent focal length of the BTA reducer is 15.6 m, which corresponds to an image scale of 75µm/. The linear size of the nonvignetted field of view is 28 â 28 mm in the plane of the detector. Constructionally, the reducer was made in the form of separate remotely controlled units mounted in a single case: ­ a multislit unit placed in front of the focal plane; ­ two rotating wheels,each with six positions; ­ a polarization analyzer placed in front of the collimator; ­ the collimator focusing mechanism; ­ the mechanism of putting/withdrawing a dispersive element in/from the collimated beam. The multislit unit, which is designed for multiob ject spectroscopy, is an arrangement that consists of 16 metal
The antireecting layers were put on the surfaces at the Nizhnii Novgorod Institute of Applied Physics.
1

strips with slits located in the focal plane and moved in a 2. 9 â 5. 9 field. The slit height is about 18 . The position of each slit is fixed using two (holding and catching) electromagnets. The holding magnets are fixed; the catching magnets are fastened to the frame that is moved along one coordinate by a stepping motor. A separate electromagnet simultaneously fixes the positions of all slits in the focal plane. The arrangement is put in the beam using a stepping motor. The wheels installed in the spectrograph are designed to put various replaceable elements in the beam ­ filters, slits, masks, etc. All of the elements installed in the wheel are mounted in bayonet-type holder with a clear aperture of 72 mm, which allows them to be replaced on the fly. Medium- and narrow-band interference filters as well as a slit for spectroscopic observations are generally installed in the wheel located in the focal plane of the telescope. Broad-band glass filters, a phase plate, and a mask for slitless spectroscopy are installed in the second wheel (behind the field lens and in front of the collimator). One position in each wheel always remains free in order that all of the installed filters could be used in observations. A 14-mm-thick Savart plate that separates the beams in two mutually perpendicular planes of polarization by 9 in the focal plane is used as the polarization analyzer. The analyzer can be turned around the optical axis through 45 .A stepping motor is used to put the analyzer in and withdraw from the beam and to turn it. The collimator focusing mechanism provides a linear displacement of the collimator within 12 mm with an accuracy of 0.01 mm. A slide with two switchable positions to put dispersive elements (FPI or direct-vision grisms) in the beam is located between the collimator and the camera. A built-in neon lamp is used to visually adjust the FPI. A central electromagnetic shutter with a shutter cycle of 0.1 s is located at the flange of the instrument closest to the primary mirror in front of the mutislit unit.

2.2. The platform-adapter
The platform adapter is fixed on a turning table in the BTA prime-focus cage and is used for guiding based on offaxis stars and for illuminating the spectrograph by calibration lamps. Both the focal reducer and other equipment can be mounted on it. The adapter is equipped with an electromagnetic shutter that works independently of the central shutter of the focal reducer. The adapter contains two rectangular fields to search for guiding stars2 ; the centers of the fields are offset by 12 from the center of the field of view. A fiber bundle displaced by step motors in a rectangular coordinate system is located in each of the fields. The off-axis lens correction
2 Since th the p osition field of view two guiding

e 6-m telescop e has an altazimuth mounting, b oth of the telescop e in A and z and the rotation of the should b e controlled during the guiding. Therefore, stars are used.


Afanasiev & Moiseev: The SCORPIO focal reducer

3

Fig. 1. Optical layout of SCORPIO . (1) ­ tip-tilt plate, (2) ­ calibration optics, (3) ­ flat mirror, (4) ­ field lens, (5) ­ collimator, (6) ­ camera, (7) ­ CCD, (8) ­ filter wheels, (9) ­ FPI, (10) ­ grism, (11) ­ multislit unit, (12) ­ polarization analyzer. placed in front of each guiding field corrects the coma of the telescope's primary mirror. The fiber displacement range is 8. 5 â 4. 5, and the diameter of the field of view of each fiber is about 40 . The flat diagonal mirror (denoted by number 3 in Fig.1) has two fixed positions. At one of these positions, the mirror throws the images from the fiber bundles to the TV view. This mode is used when exposing ob jects. At the other position, the mirror blocks the central beam of light from the telescope and throws the image of the field center of the instrument to the TV view, which is needed to roughly point the telescope at the required object. In addition, the light from the calibration lamps is thrown to the spectrograph at this position of the mirror. The adapter contains the calibration illuminator optics that forms a convergent beam with a focal ratio of F/4 at the entrance of the focal reducer, which is telecentrically equivalent to the beam formed by the primary mirror of the telescope. This scheme of the calibration unit forms the system's pupil at the same position where the image of the telescope's main mirror is located. This allows us not only to properly calibrate the wavelength scale using a line-spectrum lamp, but also to calibrate the system's transmission in various operating modes (flat field). The entrance area of the calibration unit is illuminated through an integrating sphere (Ulbricht's sphere) by two calibration lamps: a He-Ne-Ar-filled lamp to calibrate the wavelength scale and a continuum halogen lamp to produce a flat field. The SCORPIO control system contains a relatively large number of various electromechanical mechanisms (13 motors, two shutters, two calibration lamps, three crossillumination LEDs, 33 electromagnets in the multislit unit) that are controlled as follows. Each of the listed units (the focal reducer, the platform, and the multislit unit) includes electronic boards with a microprocessor that controls the mechanisms of the corresponding unit. Instructions to the microprocessor are issued from a remote personal computer using the standard RS232 data connection protocol. This implementation of the instrument's remote control allows the required stability to be achieved when working with the existing long communication lines of the 6-m telescope. No continuous control of the motors and their state polling are required: the microprocessor takes over these functions. At the same time, any possible changes of the observing technique and the software on the controlling computer requires no reprogramming of the microprocessors.

2.3. The CCD detector
From 2000 until 2003, the detector was a TK1024 1024 â 1024-pixel CCD array. Since April 2003, an EEV 4240 2048 â 2048-pixel CCD array has been mainly used on SCORPIO . Basic parameters of the two detectors are given in Table 2. It should be noted that a programmed choice of modes with different gain and readout speeds and noise is possible for EEV 42-40. Figure 2 shows a plot of the quantum efficiency for EEV 4240. The detector is cooled with liquid nitrogen. The entire complex for CCD observations (the cryostat, the electronics, and the control software) were designed and


4

Afanasiev & Moiseev: The SCORPIO focal reducer

Fig. 2. Transmission curve for the SCORPIO optics (1); the quantum efficiency curve for the EEV 42-40 CCD, as provided by the producer (2); the combined quantum efficiency curve for SCORPIO +CCD (3); and the quantum efficiency curve in a spectral mode for observations with VPHG550G (4) and VPHG550R (5) low-resolution grisms. Table 2. Parameters of the CCDs
The detector TK1024 EEV-42-40 Typ e Thin, back-illuminated Size 1024 â 1024 2048 â 2048 Pixel size, µ 24 13.5 Scale1 , /px 0.32 0.18 Field of view1 , arcmin 5.4 6.1 Max DQE, % 80 83 Readout noise, ¯ e 3 1.8-4 Dark current, ¯/min e 0.1 0.03 1 Till Septemb er 2003 the optics supp orted the focal ratio F /2.9 was used. In this case the scale on CCD TK1024 was 0.28 /px, with the field of view 4.8

Table 3. The limiting magnitudes in broad-band filters (Fatkhullin, 2002)
Filter B V RC IC Texp , 2500 1500 1260 1800 mags 27.0m 26.3m 26.4m 25.1m

3. Observations in various mo des 3.1. Direct Images
SCORPIO is equipped with several filter sets that can be used for photometric observations. Broad-band glass filters allow the Johnson-Cousins photometric UBVRc Ic system to be implemented in direct imaging mode (see Bessell 1990). Table 3 gives the limiting magnitudes for the detection of faint ob jects at a signal-to-noise ratio of 3 at 1.3 seeing. This table is based on the work of Fatkhullin (2002), who studied the capabilities of SCORPIO (with a TK1024 CCD) for the photometry of faint starlike and extended ob jects. The set of medium-band interference filters with a bandwidth of 160-400 ° and central waveA lengths of 3700-9700 ° was produced at the Research A Institute of Applied Instrument Making (Moscow). In direct imaging mode, these filters can be used for various tasks, such as constructing the spectral energy distribution for faint ob jects in the field or imaging extended ob-

produced in the SAO Laboratory of Advanced Design (http://www.sao.ru/hq/adlab/). As we see from Table 2, the detectors used have a high quantum efficiency (see Fig.2), low noise, and low dark current. In addition, both detectors have an almost perfect surface: the numbers of bad columns and hot pixels are very small. Perhaps the only shortcoming is the interference of the transmitted light (fringes) that is observed at wavelengths longer than 7500 ° for TK1024 and longer A than 6600 ° for EEV 42-40. An appropriate observing A technique (see the section 4) is required to properly subtract the interference pattern.


Afanasiev & Moiseev: The SCORPIO focal reducer

5

jects in various emission lines (H , [OIII], etc.) and in the continuum. Examples of such images obtained with SCORPIO are given in the paper by Lozinskaya et al. (2002). I.D. Karachentsev (SAO) provided a filter with a bandwidth of 75 ° centered at the wavelength of the A H line, which is used to map the distribution of ionized hydrogen in nebulae and nearby galaxies. The main problem of photometric observations is the interference pattern (fringes) during observations in red photometric bands (see the section 4). Thus, for example, during Ic band observations with an EEV 42-40 CCD, the fringes level reaches 8% of the sky background level.

3.2. Long-Slit and Slitless Sp ectroscopy
The preimaging possibility proves to be very useful in slit spectroscopy of both extended ob jects (since the slit position is known exactly) and starlike ob jects if the latter are too faint to be visible on the TV-view. Thus, for example, 1-2 minutes trial exposure in the filter Rc is enough for reliable pointing to ob jects of 22-23m at a moderate seeing. In the pointing process, the ob ject under study is set on the detector where the slit image is pro jected. Subsequently, the slit is set in place of the filter, and a grism (the combination of a transparent grating and two prisms) is inserted in the collimated beam, which turns the focal reducer into a fast spectrograph. So, the change of the "direct imaging"-"long slit" configurations takes about one minute. Figure 3 sequentially shows the process observational data using the spectroscopy galaxy RCJ 1154+0431 (the observations a of Yu.N. Pariiskii) as an example. The total is 19.8m, its measured redshift is z=1.0 (see al., 2003a). of obtaining of the radio t the request V magnitude Afanasiev et

SCORPIO is equipped with set of grisms ensuring observations with different spectral resolution (from 1.5 to ° 20A with the slit width 1 ) in different regions of an optical spectrum. Before 2003, observations were performed using transparent gratings with profiled grooves with the number of grooves from 300 to 1200 per mm. The gratings are replicas from cut gratings and were produced at the S.I. Vavilov State Optical Institute (St.Petersburg). The maximum quantum efficiency of the entire system (telescope+SCORPIO+CCD) with such gratings was 30% for low-resolution ( = 15 - 20°) spectra and only A ° about 3-5% for higher-resolution ( = 5 - 6A) spectra. Observations with grisms using volume phase holographic gratings (VPHGs) were begun in 2003-2004; these have a high transmission and a low level of scattered light (Barden et al. 2000; Habraken et al. 2001). The number of lines for the available VPHGs ranges from 550 to 3000 per mm; in this case, a quantum efficiency of 20-50% is achieved with both low (see Fig.2) and high resolutions. The main set of gratings was produced by Wasath Photonics (USA, http://wasatchphotonics.com); two

gratings were kindly provided by the University of Padova (Italy). The achieved quantum efficiency of the instrument has allowed one to continuously determine the redshifts and spectral classification of extragalactic radio sources, since the required low-resolution spectra of 19 - 21m ob jects can be obtained even at moderate atmospheric transparency and at 3 - 5 seeing; the total exposure time is only 10-20 min (see, e.g., Afanasiev et al., 2003b; Amirkhanyan et al. 2004). At the same time, at 1.5 seeing in low-resolution spectroscopy of starlike ob jects, a limiting magnitude of Rc = 24m is achieved over a two-hour exposure time (the signal-to-noise ratio is 10 in the continuum of the spectra obtained). The stability of the instrumental profile of the spectrograph, which affects both the accuracy of subtracting the night-sky lines and the possibility of allowance for the interference pattern in the detector material (see the section 4), plays a crucial role in obtaining the spectra of such faint ob jects. The technique of displacing an ob ject along the slit between exposures helps greatly in such observations. During the subsequent reduction, a pure spectrum, i.e., the spectrum of the sky taken from the same location, but on the displaced frame, is subtracted from the spectrum of the ob ject. A good test for the capabilities of the spectrograph is to study the kinematics of galactic stellar disks, since absorption spectra with a relatively high signal-to-noise ratio and a spectral resolution of at least = 2 - 4° should A be obtained here for regions with a surface brightness of 21-23m/2 . Figure 4 shows an example of measuring the parameters of the stellar kinematics along the ma jor axis of a barred lenticular galaxy, NGC 3412. Over a 1.5-h total exposure time on SCORPIO (using VPHG2310), we can measure the radial velocities and the radial-velocity dispersions of stars for regions with a V-band surface brightness of 23m /2 . Slitless spectroscopy, where the slit is replaced with a circular mask about 30 in diameter, is used during the observations of spectrophotometric standard stars. This technique allows one to completely get away from the problems of light losses on the slit and distortion of the spectral energy distribution due to the effect of differential atmospheric refraction.

3.3. Multislit Sp ectroscopy
The available set of grisms can also be used in multislit observations, although the total spectral range decreases in comparison with the long-slit case due to the slit displacement in the field. An IDL-based package of the programs was written for the preliminary determination of the optimal position angle of the multislit unit concerning observed. In such observations, a direct image of the area under study is obtained, a multislit unit is introduced in the focal plane of the telescope, and the slits are set according to the coordinates of the chosen ob jects measured on the CCD array. The time of the complete slit arrange-


6

Afanasiev & Moiseev: The SCORPIO focal reducer

Fig. 3. Spectroscopy for the radio galaxy RCJ 1154+0431 with SCORPIO: (a) a fragment of an RC (Texp = 60 s) image, the position of the spectrograph slit is shown; the radio galaxy is marked by the arrow; (b) a low-resolution spectrum (the sum of two 600-s exposures); (c) the same after the subtraction of the night-sky spectrum; (d) the integrated spectrum on the wavelength scale. ment (at the required accuracy of 0.2 - 0.3 ) is about 10 min. The spectra obtained are illustrated in Fig.5. interference (near the H line) and olution in this line of 2.5 and 0.7° A from order overlapping 28 and 13 are successfully used to study both clusters) and extragalactic ob jects. FPI observations with SCORPIO , provide a spectral resfor spectral ranges free ° respectively. These A Galactic (nebulae, star For more details on the see Moiseev (2002).

3.4. Panoramic Sp ectroscopy
The scanning FPI is a highly efficient instrument for studying the kinematics of extended ob jects. The observations consist in sequentially obtaining several tens of images of the interferentic rings from the ob ject under study (or a calibration lamp) for various optical paths between the parallel reflecive plates. The radius of the rings is a function of the wavelength and the FPI plates' gap. After special reduction, these interferograms can be represented as a data cube in which two coordinate axes are located in the plane of the sky and the wavelengths (or the Doppler velocities measured from the redshifts of spectral lines) are the third coordinate. In other words, an individual spectrum is related to each image pixel. The Queensgate ET-50 scanning piezoelectric interferometer is placed between the collimator and the camera where the exit pupil of the optical system is located. There are two scanning FPIs at the SAO provided by the Marseilles (France) and Burakan (Armenia) Observatories. These FPIs work in 235 and 501 orders of

Narrow-band filters with a bandwidth of 10 - 20° are A used to separate out the required portion of the spectrum. A set of filters centered at the wavelength of the redshifted emission line under study is needed for the observations of various galaxies. With the filters available at the SAO, objects with radial velocities from -200 to +10 000 km s-1 s1 and from +3500 to +11 000 km s-1 are currently observable in the H and [OIII]5007 lines, respectively. Most of the narrow-band filters were produced at the Research Institute of Applied Instrument Making (Moscow); several filters were provided by our colleagues from the Burakan Observatory (T.Movsesyan) and the Padova University (G.Barbieri). Figure 6 shows the FPI observations of the nearby s ral galaxy NGC 6951. The constructed velocity field is good agreement with similar observations by Rozas et (2002). Here, the radial velocities were measured with piin al. an


Afanasiev & Moiseev: The SCORPIO focal reducer

7

Fig. 4. Kinematics of the stellar component in the galaxy NGC 3412: the distribution of radial velocities (a) and radial-velocity dispersion (b) along the ma jor axis. The solid and dashed lines represent the published measurements by Aguerri et al. (2003) and Neistein et al. (1999), respectively.

Fig. 5. Spectroscopy for globular clusters in the nearby galaxy NGC 147 (the observations at the request of M.E. Sharina): A V-band image of the galaxy with marked slit positions (a) and multislit spectra of the ob jects (b). accuracy of about 5 km s-1 . For a detailed discussion of the data obtained, see Moiseev et al. (2004).

3.5. Polarization observations
In spectropolarimetric observations, a mask that forms a dotted slit is placed in front of the SCORPIO slit. The height of each slit is 7.5 , and the separation between the


8

Afanasiev & Moiseev: The SCORPIO focal reducer

Fig. 6. FPI observations of the galaxy NGC 6951 with SCORPIO in the H : (a) image in the emission line, (b) the line-of-sight velocity field. Table 4. Polarization observations with SCORPIO
ob ject BD+59d389 VICyg#12 BD+64d106 BD+28d4211 SCORPIO measu P, % 6.61 ± 0.11 8.80 ± 0.16 5.35 ± 0.41 0.33 ± 0.3 rements , 97 ± 1 117 ± 2 86 ± 5 ­ Schmidt et al.( P, % 6.701 ± 0.015 8.947 ± 0.088 5.627 ± 0.037 0.054 ± 0.030 1992) , 98.09 115.03 96.63 ­

slit centers is 9.8 . After the introduction of a polarization analyzer in the beam, a series of pairs of spectra in mutually perpendicular polarization planes is obtained at the exit of the spectrograph. Comparing the spectra taken at different orientations of the analyzer, 0 and 45 , we unambiguously determine the degree of linear polarization and the position angle of the polarization plane for the ob ject as a function of the wavelength. Apart from the count statistics determined by the exposure, the actual accuracy of measuring the degree of polarization depends on the level of scattered light in the spectrograph, the accuracy of correcting the spectra for the flat field, the presence of ghosts in the analyzer (their level is about 0.2%), and the accuracy of extracting the spectra from the image. As our measurements show, the measurement threshold for the degree of linear polarization in SCORPIO is 0.2-0.3%, and the measurement accuracy is 0.1-0.3% (depending on the exposure). Table 4 gives the measurements of polarization standards with VPHG550G (the dispersion is 2 °/px) in the V band. The degrees of polarization that A are compared with their published values were obtained by integrating the spectra in the V band. Figure 7 illustrates the integrated spectrum of the central region in Seyfert 2 galaxy Mrk 573 obtained when the SCORPIO polarization mode was tested in August 2004. This figure shows the wavelength dependence of the degree of linear polarization. The spectra were obtained at

2 seeing with VPHG550G. We took a series of 10-min exposures at successive rotation angles of the analyzer (0 and 45 ). The total exposure time was 2 h, and the total V-band brightness of the galactic nucleus in the slit was about 16m . A broad component of the hydrogen lines is distinguished in Fig.7 (c). The result obtained is in satisfactory agreement with the observations of other authors (Nagao et al., 2004)

4. Data Reduction
The observational data are written in the FITS format. Various standard astronomical image reduction systems, such as MIDAS or IRAF, can be used for their reduction. The primary data reduction can be easily automated, since all of the necessary information about the spectrograph configuration is written in the FITS-headers. In the IDL environment, we wrote software packages for SCORPIO data reduction and analysis. The programs for the reduction of FPI, long-slit, and multiob ject spectroscopy have a user-friendly interface and can be used by users that are not familiar with the IDL language itself. The reduction sequence of FPI observations with SCORPIO was described by Moiseev (2002). In the reduction of observations, it is important to take into account the fringe pattern in the sensitive layer of the CCD array in the red spectral range (see above). In the case of spectroscopic observations, to correct this effect,


Afanasiev & Moiseev: The SCORPIO focal reducer

9

B

C

D

Fig. 7. Spectropolarimetry of the Seyfert 2 nucleus in the galaxy Mrk 573. The grism is VPHG550G, the exposure time is 120 min, and the slit is 1 â 7.5 : (a) the initial spectrum with the analyzer at position 0; (b) the integrated spectrum of the nucleus (V = 16m ) minus the spectrum of the surrounding galaxy (I ); (c) the degree of polarization of the nucleus (P ); (d) the spectrum of polarized emission (I â P ). ADU=0.5¯. e the frames with the ob ject's spectra are divided by the frames with the accumulated spectra of the built-in lamp, a spectral flat field. In this way, the fringes can be reduced by more than an order of magnitude, which is enough in most cases. We can also get rid of the fringe pattern by the flat field division in the case of direct imaging, although using the frames illuminated by the inner lamp or the twilight sky as a flat field is often not enough, particularly in the case of broad-band filters, since the spectral energy distribution of the night-sky background emission differs markedly from that of the calibration frames. In this case, an optimal imaging technique is to form an image of the averaged interference pattern using a series of all accumulations in the corresponding filter during the observing night.

5. Further upgrading of the instrument
A standard autoguiding system using images on the TVview (Shergin & Maksimova 2001) is used during observations with the 6-m telescope. It allows the displacement of stars in the field to be compensated by the corresponding motions of the entire telescope. This is a slow guiding, since the oscillations of the centers of stellar images at a frequency of 0.1 Hz are suppressed. In 2005, we planned to put into operation a fast guiding system based on a tip-tilt fused quartz plate. This system will allow the os-


10

Afanasiev & Moiseev: The SCORPIO focal reducer

cillations with frequencies up to 10 Hz to be compensated. This will make it possible to significantly reduce the effect of the telescope's natural oscillations, thereby improving the quality of stellar images. For an example, using a local tip-tilt corrector at the Nasmyth-2 focus of the 6-m BTA telescope would allow the limiting magnitude of the spectrograph located there to be increased by 0.5 - 1m (Ivanov et al., 2001). Equipping the spectrograph with a "semi-thin" CCD detector seems promising. This detector combines the advantages of both "thick" (directly illuminated) devices, the absence of a interference pattern, and "thin" devices (back-illuminated) with a high quantum efficiency. Such a detector has a much smaller amplitude of fringes and a higher (up to 80% at 9000°) sensitivity in the red specA tral range, which will allow the SCORPIO efficiency to be increased during near-infrared observations.

Temirova A.V., Zhelenkova O.P., Goss W.M., 2003a, Astron. Rep orts, 47, 377 Afanas'ev V.L., Dodonov S.N., Moiseev A.V., Chavushyan, V., Mujica, R., Juarez, Y., Gorshkov, A.G., Konnikova, V. K., Mingaliev, M. G., 2003b, Astron. Letters, 29, 579 Afanas'ev V.L., Gazhur E.B., Zhelenov S.R., Moiseev A.V., 2004, Bull. SAO, vol. 58 Aguerri J. A.L., Debattista V. P., Corsini E.M., 2003, MNRAS, 338., 465 Amirkhanyan, V.R, Afanas'ev V.L., Dodonov S.N., Moiseev A.V., Mikhailov V.P., 2004, Astron. Letters, 30, 834 Barden S.C, Arns J.A., Colburn W.S., and Williams J.B., 2000, PASP, 112, 809 Bessell, M.S., 1990, PASP, 102, 1181 Buzzoni, B., Delabre B., Dekker H., et al., 1984, ESO Messenger (ISSN 0722-6691), Dec. 1984, 9. Court´s, G., 1960, Ann. d'Astrophysics, 23, 115 e Court´s, G., 1964, AJ, 69, 325 e Fatkhullin T.A., 2002, Bull. SAO, 53, 5 Ivanov A.A., Panchuk V.E., Shergin V.S., 2001, Preprint SAO RAS, No.155 6. Conclusions Lozinskaya T.A., Arkhip ova V.P., Moiseev A.V., Afanasiev The high efficiency of the new instrument has been V.L., 2002, Astron. Rep orts, 46, 16 confirmed during its continuous practical use. Over Moiseev A.V., 2002, Bull. SAO, 54, 74 (astro-ph/0211104) the period from September 2000 through November Moiseev A.V., Vald´s J.R., Chavushyan V.O., 2004, A&A, 421, e 433 2004, observations were performed at the SAO on more than 240 nights; the results obtained were used in 26 Nagao, T., Kawabata, K.S., Murayama, T. et al., 2004, AJ, 128, 109 papers, three Ph.D. and two doctoral dissertations. A more detailed description of the spectrograph and Neistein E., Maoz D., Rix H.-W., Tonry J.L., 1999, AJ, 117, 2666 the observing technique can be found in the paper Nicklas H., Seifert W., Boehnhardt, H., Kiesewetterby Afanasiev et al. (2004), while the current descripKoebinger, S., Rupprecht, G., 1997, Proc. SPIE, 2871, in tion of the spectrograph is accessible on the Internet at: "Optical Telescop es of Today and Tomorrow" (Eds. Arne http://www.sao.ru/hq/moisav/scorpio/scorpio.html, L. Ardeb erg), Nordic Optical Telescop e SA (Sweden), 1222 a continuously updated gallery of observed ob jects is Rozas M., Relano M., Zurita A., Beckman J.E., 2002, A&A, also given here. A similar instrument (but without the 386, 42 platform-adapter and the multislit unit) produced at Schmidt G.D., Elston R., Lupie O.L.), 1992, AJ, 104, 1563 the SAO is being successfully used in observations with Shergin V.S., Maksimova V.M., 2001, Autoguiding Program TV guide. User's guide SAO the 2.6-m Byurakan Astrophysical Observatory telescope (http://www.sao.ru/hq/vsher/vsher_ru.html) (Armenia). Acknow ledgements. We wish to thank the SAO administration for continuous supp ort and attention when the instrument was designed and produced. Dodonov S.N. and Amirkhanyan V.R. for fruitful discussions in making the instrument, and Gazhur E.B., Zhelenkov S.R., Perep elitsyn E.I., and Fateev V.I., who produced and adjusted the individual parts of the sp ectrograph; to the administration of the Institute of Astronomy RAS for making available of VPH gratings. This work was supp orted in part by the "Astronomy" Federal Science and Technology Program (contract no. 40.022.1.1.1101 from February 1, 2002), the INTAS grant (96-0315) and the Program of the Department of Physical Sciences of the Russian Academy of Sciences. And the Program of the Department of Physical Sciences of the Russian Academy of Sciences. Moiseev A.V. wishes to thanks the Russian Science Supp ort Foundation and the Russian Foundation for Basic Research (pro ject no.0402-16042) for partial supp ort of the work.

Translated by V. Astakhov, V. Shapoval

References
Afanas'ev V.L., Dodonov S.N., Moiseev A.V., Verkhodanov O.V., Kopylov A.I., Pariiskii Yu.N., Sob oleva N.S.,