Compact multi-band visible camera for 1m-class fast telescopes
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1 Compact multi-band visible camera for 1m-class fast telescopes Alberto Riva *a, Paolo Spanò a a INAF - Osservatorio Astronomico di Brera, Via E. Bianchi 46, I Merate, ITALY ABSTRACT Most of the small 1m-class telescopes designed for fast tracking of transient object, like GRBs, are equipped with infrared and visible cameras, fed through a dichroic. We studied a new concept for a fast and compact multi-band visible camera, using successive dichroics, to cover simultaneously many visible bands (U,B,V,R, and I), sampled with one more CCD detectors. This extended spectral coverage will help to observe transient faint objects. To keep envelope size, weight and overall cost at a reasonable level, a trade-off has been carried out. Keywords: Visible camera, 1m-class telescopes, multi-band, dichroic, GRB 1. INTRODUCTION This paper presents the study and design of some optical elements necessary in order to build instruments with the possibility to produce simultaneous acquisitions of the same source in different spectral customizable bands. Many astrophysical fields can benefit from such an instrument, mainly in the monitoring of fast transient sources. In particular, we can gain the possibility to measure the spectral energy distribution in one exposure. Some of the most appealing sources to be monitored with this kind of instruments will be the Gamma Ray Bursts (GRB), the Active Galactic Nuclei (AGN), variable stars, objects with peculiar spectral features. One of the pioneering instruments that use the principle of simultaneous acquisition in different bands is GROND, a seven-channel instrument installed at MPI/ESO 2.2m, at La Silla (Chile) [1]. We are proposing the translation of the principle into instruments suitable for smaller 1-m class telescopes. This idea comes from the availability of small telescopes dedicated to the monitoring of fast transient like GRB. In this paper we will present solutions for the optical arm for the two 60-cm telescopes, REM and BOOTES, respectively installed on La Silla (Chile) and Sierra Nevada (Spain). 2. SPLITTING THE BEAM The core of multi-band instruments with simultaneous acquisition stands in the definition and design of the element that splits the beam into the desired bands. This element has the function to separate the white beam into the desired number of colored arms. The splitting element has been thought to be placed in the collimated part of the system, in order to reduce at minimum the aberrations. In this paper we present two alternative solutions in order to split the beam into four channels. 2.1 Wavelength selection As a first step, we studied how to split light vs. wavelength, deriving the number of useful arms that can be observed at a time. A strong constraint comes from the telescope mirror coatings. As example, we use the case of two similar telescopes. The first is REM described in Zerbi et al. [2], and the second is BOOTES-IR described in Castro Tirado et al. [3]. The coatings of REM mirrors are made in protected Silver. This kind of coatings has a cutoff below 400 nm. * alberto.riva@brera.inaf.it; phone ; fax ; Ground-based and Airborne Instrumentation for Astronomy II, edited by Ian S. McLean, Mark M. Casali, Proc. of SPIE Vol. 7014, , (2008) X/08/$18 doi: / SPIE Digital Library -- Subscriber Archive Copy Proc. of SPIE Vol
2 IvI I I 400 S *aveteth IN NflCMETERS 900 Fig. 1. Melles-Griot typical protected Silver curve. This converts the minimum wavelength for the instrument design at 400 nm. In order to maximize observational efficiency, instead of classical Johnson Cousins filters BVRI, we can adopt a better suited Sloan filters. Due to the stated minimum wavelength, the only available filters will be g,r,i,z. 100 go o Sloan filters Xnm Fig. 2. Sloan Digital Sky Survey (SDSS) filters. Filter Table 1. SDSS filters parameters [4]. Central wavelength (nm) FWHM bandpass (nm) Peak efficiency Recipe (glass + coating) g >90% 2mm GG mm BG38 + short-pass cutoff 550 nm r >95% 4mm OG mm BK7 (**) + short-pass cutoff 700 nm i >95% 4mm RG mm BK7 (**) + short-pass cutoff 850 nm z 835 (*) - >95% 4mm RG mm BK7 (**) (*) cut-off wavelength (**) to have the same overall thickness Proc. of SPIE Vol
3 2.2 The Quadrichroic One of the solution studied use the internal reflections of a single cube as shown in Fig. 3. The splitting scheme is shown in Fig. 4. Incoming beam Counter- disp ers or Second Ann Wedge(s) Reflected Beam (tirst ann) Fourth Ann Third Ann Fig. 3. The optical layout of the quadrichroic system. One dichroic layer is between air and glass, while the other two are inside the glass assembly > Fig. 4. Scheme of separation of light for the quadrichroic Proc. of SPIE Vol
4 The light comes from the collimator and goes on the counter-disperser prism. This prism has two functions: the first is to compensate for the dispersion introduced by the material of the cube, the second one is to present the chief ray inside the cube at a 45 degrees with respect to each face. On the first face of the wedge we assumed to place the first dichroic coating. It makes the surface reflective for the light that must go into the first arm and transmissive for the remaining part of the spectrum. Once passed in the counter-disperser, the beam goes in the cube with the proper angle. When the light comes to the first face of the cube it is split in two beams through another dichroic coating. The coating is deposed on the face of a wedge in contact with the cube. The presence of the wedge is necessary because otherwise the light coming out from the cube has a strong anamorphism. The introduction of the wedge help in the manufacturing of the system. Indeed this solution avoids the deposition of different coatings on different faces of the cube itself. The manufacturing process of deposition of a multilayer dichroic coating is performed through a massive heating of the substrate. The different multilayer coatings (due to different wavelengths cut off) are deposed in separate processes and the heating of the cube can damage the previous deposition. The light coming out from the wedge feeds the second arm of the instruments, while the other parts continue its path inside the cube going to the other face where it finds another dichroic coating deposed on the wedge attached to the face. The considerations made for the second arm are the same for the third arm, obviously except for the wavelength range. The last crossing of the light on the face of the cube is slightly different. In this case we don t need a dichroic coating but we want all the light passing and going into the wedge that has the only function of giving an acceptable angle to the outcoming beam that will form the fourth arm. Fig. 5. This figure shows different perspectives of the assembling for the quadrichroic. Proc. of SPIE Vol
5 > Fig. 6. Scheme of separation of light for the multi-cube. Fig. 7. Optical layout of the dichroic system Proc. of SPIE Vol
6 2.3 The Multicube An alternative solution studied consists in the use of multiple dichroic cubes in order to produce four arms. In this configuration, the light coming from the collimator comes to a cube-dichroic that separates the light into two arms. The difference with the previous scheme stands in the cut-wavelength. Indeed it separates the spectrum into two equal parts. In this solution each arm will pass through two dichroics, while in the other solution the number of dichroics per each arm will vary. The choice between the two configurations can be done analyzing the performances of each dichroic coating. In order to simplify the layout for the incoming and outcoming beams, three 45 total internal reflection prisms (eventually silver coated onto the hypotenuse of the triangle) has been added, one after the first dichroic, the other two after the remaining dichroics. For the reduction of costs and manufacturing issues, this dichroic train is composed by standard BK7 right angle prisms with a standard dimension (30mm, in this layout). During manufacturing only custom coatings need to be applied: dichroic coatings for splitting elements, and anti reflection (A/R) coatings on the external surfaces. Non optical surfaces can be black painted to reduce scattered light. Prisms will be cemented together to give better stability. Folding prisms are used as total internal reflection prisms if the Total Internal Reflection (TIR) condition is met. If smaller incidence angles will be present, prisms with aluminized hypotenuse can be used. 2.4 Efficiency A simple comparison between the two configurations can be performed analyzing the efficiencies. In the following table we show the results for the two alternatives.designs. The first calculation is done through parametric numbers, and then we show results for mean values. This because the efficiency curves depend from the multilayer coatings and the substrates chosen. We will use α for the reflection in air, β for the reflection into a glass and γ for the transmission. We tried to introduce some typical numbers for the mean efficiency, assuming 0.98 for reflection in air, 0.97 for reflection in glass and 0.95 for transmission. These are obviously representative numbers, but according to the formulas they can be changed depending on real numbers. Table 2. Evaluation of efficiencies for the two configurations Quadrichroic Multi-cube Parameters Numbers Parameters Numbers First channel α 0.98 β Second channel γ βγ 0.92 Third channel βγ βγ 0.92 Fourth channel β 2 γ γ A POSSIBLE INNOVATIVE SOLUTION FOR UPDATING REM-ROSS ROSS is the visible camera currently installed on the REM telescope. Its design is described in Tosti et al. [5]. The camera layout is mainly a relay 1:1 optics that matches the infrared field of view onto the visible arm. We propose an alternative solution in order to update the existing instrument. The camera is fed by an initial dichroic that separate the infrared beam for REMIR and the visible one for ROSS. After that, a focal plane is formed 150 mm Proc. of SPIE Vol
7 from the REMIR optical axis. Then a collimator with two identical doublets creates a collimated beam with a diameter of 14mm. To optimize image quality and reduce chromatic effects within the selected wavelength range ( nm), doublets are made with S-FPL53/S-LAL14 (Ohara preferred glasses). Then light passes through the multi-cube dichroic system, being split into four similar beams. To focus light onto the detector, four very similar cameras (only distances between elements can vary, to optimize image quality) are used, made by two doublets and a singlet. Doublets are again in S- FPL53/S-LAL14, while the S-BSM14 can control residual chromatism. Some surfaces are flat to reduce the number of manufacturing steps. Finally, to send light towards the same detector, four displacing prisms are used, made by two right angle prisms. In order to maximize the effective field of view, we need to reduce the dead gaps between the four images. This can be achieved with a proper size of these prisms, and a rotation of them with respect to axes defined by the 2 by 2 matrix camera system. This, in turn, requires a rotation of the dichroic system of the same angle. Table 3 Estimated final paremeters for ROSS2 FoV: 9.1 x 9.1 arcmin 2 Plate scale: 0.56 arcsec/pixel CCD: 2048 x 2048, 13 micron Wavelength: nm Channels: 4 (Sloan g, r, i, z ) Fig. 8. Optical layout of the unfolded collimator-camera system Image quality is diffraction-limited over the whole field of view. Proc. of SPIE Vol
8 Fig. 9. Spot diagrams of the overall system. Boxes are two pixels wide. Disks show the Airy disk. The different configurations refer to different wavelength range because the four cameras will see different bands. Configuration 2 refers to two channels with identical cameras. Ii Fig. 10. Layout of the ROSS2 camera with the REM telescope layout Proc. of SPIE Vol
9 Dichroic system /4 a REM focal plane Cameras 4- collimator Folding prisms CCD Fig. 11. Layout of the ROSS2 camera. Fig. 12. Layout of folding prisms to recollect light from different cameras to the same detector REFERENCES [1] [2] [3] [4] [5] Greiner J., Borrenmann W., Clemens C., Deuter M., Hasinger G., et al., GROND - a 7-channel imager, The PASP Vol 120, Issue 866, Zerbi F.M., Chincarini G., Ghisellini G., Rodonò S., et al, REM telescope, a robotic facility to monitor the prompt afterglow of Gamma Ray Bursts, Proc. SPIE 4841, (2003). Castro Tirado A.J., et al., "BOOTES-IR: a robotic nir astronomical observatory devoted to follow up of transient phenomena", Proc. SPIE 6267, 62670I (2006). Fukugita M., et al, The Sloan Digital Sky Survey Photometric System, AJ 111, 1748 Tosti G., et al, The REM optical slitless spectrograph (ROSS), Proc. SPIE 5492, (2004). Proc. of SPIE Vol
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