First scientific operation and performances of the Javalambre Panoramic Camera (JPCam) are presented in this paper. JPCam, deployed on the 2.6m large field-of-view Javalambre Survey Telescope (JST250) at the Observatorio Astrof´ısico de Javalambre (OAJ), is a 1.2 Gpixel camera conceived to perform the Javalambre Physics of the Accelerated Universe Astrophysical Survey (J-PAS). J-PAS in an unprecedented photometric sky survey of several thousand square degrees of the northern sky in 56 optical bands, 54 of them narrow-band filters (145 Å FWHM). The innovative designs of the J-PAS instrument and filter system has been optimized to accurately measure photometric redshifts for galaxies up to z∼1 and to study stellar populations in nearby galaxies. As a result, J-PAS will provide a low-resolution spectroscopy for hundreds of millions of other galaxies. The data set produced by this survey will have a unique legacy value, allowing a wide range of astrophysical studies. To this aim, JPCam is equipped with a mosaic of 14 large format 9.2k x 9.2k, 10μm pixel, low noise detectors from Teledyne-E2V, providing an unvignetted Field of View of 3.4 square degrees with a plate scale of 0.2267′′/pix. Its filter unit admits 5 filter trays, each mounting 14 filters corresponding to the 14 CCDs of the mosaic and allowing all the J-PAS filters to be permanently installed. To optimize image quality during the observations, the position of the JST250 secondary mirror and JPCam focal plane are maintained optically aligned by means of two hexapod systems. To perform this task, JPCam includes 12 auxiliary detectors, 4 for autoguiding and 8 for image quality control through wavefront sensing. JPCam commissioning was successfully completed and first scientific operation started in summer 2023. This paper shows JPCam on-sky operation and first J-PAS Science Verification results, demonstrating fulfilment of the main J-PAS scientific requirements.
Commissioning results, on-sky performance and first operations of the Javalambre Panoramic Camera (JPCam) are presented in this paper. JPCam is a 1.2 Gpixel camera deployed on the 2.6m, large field-of-vie Javalambre Survey Telescope (JST250) at the Observatorio Astrof´ısico de Javalambre. JPCam has been conceived to perform J-PAS, a photometric survey of several thousand square degrees of the northern sky in 56 optical bands, 54 of them narrow-band filters (145 ˚A FWHM), contiguous and equi-spaced between 370 and 920nm, producing a low resolution photo-spectrum of every pixel of the observed sky, hence promising crucial breakthroughs in Cosmology and galaxy formation and evolution. JPCam has been designed to maximize field-of-view and wavelength coverage while guaranteeing a high image quality over the entire focal plane. To this aim, JPCam is equipped with a mosaic of 14 9.2k x 9.2k, 10µm pixel, low noise detectors from Teledyne-E2V, providing a FoV of 4.1 square degrees with a plate scale of 0.2267′′/pix. In full frame mode, camera electronics allows read times of 10.9s at 633kHz read frequency (16.4s at 400kHz) with a readout noise of 5.5e− (4.3e−). Its filter unit admits 5 filter trays, each mounting 14 filters corresponding to the 14 CCDs of the mosaic and allowing all the J-PAS filters to be permanently installed. To fully optimize image quality, position of JST250 secondary mirror and JPCam focal plane are maintained optically aligned by means of two hexapod systems. To perform this task, JPCam includes 12 auxiliary detectors, 4 for autoguiding and 8 for image quality control through wavefront sensing.
The presented new 1% narrowband filter centered at 1254nm with a FWHM of 11nm required and achieved excellent maximum transmission and deep out of band blocking. Magnetron sputtering was used for the filter coating process. The filter was used in the fully cryogenic near-infrared camera CIRCE of the Gran Telescopio Canarias (GTC) Telescope. The goal of the project is to detect very distant galaxies at the dawn of the Universe. These remote and extremely faint galaxies are selected by their Ly-alpha emission. We report on the spectral and interferometric results of the filter, and provide the spectacular first deep image taken with the 10.4m GTC telescope.
Spectral and radiometric requirements of optical filters for space applications are always more demanding. Multispectral bandpass filters require very steep edges, a high accuracy in the central wavelength position, a high average transmittance as well as a very good level of blocking outside of the bandpass region.
Realization of such filters implies to design the layer stacks in a way that reduces sensitivity to the production deviations and to be able to properly control the coating conditions in the machine.
In order to optimize the design, a pre-production error analysis can be performed, to assess the weight of each layer in the global filter properties and therefore modify the design until a good stability level is achieved. We discuss different insitu optical monitoring strategies and process conditions depending on the coating technology. The realization phase needs a precise control of the coating machine such as well-characterized deposited materials, stable deposition rates, a reliable layer thickness monitoring system in addition to a good coating uniformity over all the coating positions inside the machine.
We present design strategies and means of pre-production error analysis for typical multispectral bandpass specifications as well as transmittance curves.
In support of a spaceborne astrophysics instrument design, we have studied high UV filter efficiency and strong transmission blocking out to the end of Si response at 1100nm. For filters at wavelengths 297.5nm/338.5nm/379.5nm, these attributes are achieved with the combination of hard sputtered dielectric coatings on colored glass substrates. The filterglass substrates can be used to suppress ghost images caused by reflection at the exit face which is a common problem of all interference filter designs. Known disadvantages of filterglasses like solarization or autofluorescence are discussed and possible ways to mitigate are discussed. At two shorter wavelengths, 215.5nm and 256.5nm, metaldielectric Fabry-Perot stacks are applied on fused silica. Those traditional designs are advantageous due to their efficient blocking up to the mid IR range and economic low number of layers. We discuss the different design possibilities of metal-dielectric filters and ways to improve the steepness of the slopes. Resulting spectra are expressed.
The importance of high performance interference bandpass filters in the UV is growing recently. For the CETUS project a set of bandpass filters with a clear aperture of 70 mm is required centered at the wavelengths 215.5 nm / 256.5 nm / 297.5 nm / 338.5 nm / 379.5 nm with a FWHM of 41 nm and blocked as good as possible up to 1100 nm. We present a design study based on all-dielectric hard sputtered coatings on colorglass substrates for the wavelengths 297.5 nm / 338.5 nm / 379.5 nm. The colorglass substrates where chosen to suppress ghost images by reflection on the exit face and to improve the blocking in the required range. For the wavelengths 215.5 nm and 256.5 nm a conventionally evaporated design of metal-dielectric Fabry-Perot stacks was chosen on fused silica substrates. We comment on how system requirements are leading to filter specifications and show theoretical spectra of the chosen filter designs.
We present the first results using a new SCHOTT 1% narrow band filter in the near infrared for the CIRCE camera of the 10.4m GTC telescope. The goal of the project is to detect very distant galaxies at the dawn of the Universe. These remote and extremely faint galaxies are selected by their Ly-alpha emission. For this project SCHOTT manufactured a high transmission 11 nm narrow band filter which has been used in the fully cryogenic near-infrared camera CIRCE of the Gran Telescopio Canarias Telescope. A steep interference filter Bandpass with FWHM 11nm centered at 1254nm was coated on a fused silica substrate. The filter achieved excellent maximum transmission and deep out of band blocking. This was achieved by using magnetron sputtering for the filter coating process. We report on the spectral and interferometric results of the filter and the scientific results achieved with a first set of observations.
On the Javalambre mountain in Spain, the Centro de Estudios de Fisica del Cosmos de Aragon has setup two telescopes, the JST/T250 and the JAST/T80. The JAST/T80 telescope integrates T80Cam, a large format, single CCD camera while the JST/T250 will mount the JPCam instrument, a 1.2Gpix camera equipped with a 14-CCD mosaic using the new large format e2v 9.2k×9.2k10-μm pixel detectors. Both T80Cam and JPCam integrate a large number of filters in dimensions of 106.8×106.8 mm2 and 101.7×95.5 mm2, respectively. For this instrument, SCHOTT manufactured 56 specially designed steep edged bandpass interference filters, which were recently completed. The filter set consists of bandpass filters in the range between 348.5 and 910 nm and a longpass filter at 915 nm. Most of the filters have full-width at half-maximum (FWHM) of 14.5 nm and a blocking between 250 and 1050 nm with optical density of OD5. Absorptive color glass substrates in combination with interference filters were used to minimize residual reflection in order to avoid ghost images. In spite of containing absorptive elements, the filters show the maximum possible transmission. This was achieved by using magnetron sputtering for the filter coating process. The most important requirement for the continuous photometric survey is the tight tolerancing of the central wavelengths and FWHM of the filters. This insures each bandpass has a defined overlap with its neighbors. A high image quality required a low transmitted wavefront error (<λ/4 locally and <λ/2 on the whole aperture), which was achieved even by combining two or three substrates. We report on the spectral and interferometric results measured on the whole set of filters.
The Centro de Estudios de Fisica del Cosmos de Aragon will conduct a photometric sky survey with two new telescopes recently set up on the Javalambre mountain in Spain: the JST/T250 is a 2.55-m telescope with a plate scale of 22.67 arcsec/mm and a 3-deg-diameter field of view (FoV) and the auxiliary telescope JAST/T80 with a 82-cm primary mirror and an FoV of 2 deg diameter. A multiple CCD (9k-by-9k array size, 10-μm pixel size) mosaic camera is used in combination with filter trays or filter wheels, each containing a multitude of filters in dimensions of 101.7×96.5 mm or 106.8×106.8 mm. For this project, Schott manufactured 56 specially designed narrow band steep-edged bandpass interference filters and five broadband Sloan-filters which were completed only recently. We report here on the results of the broadband Sloan-filters with transmission bands of 324 to 400 nm (Sloan-u), 400 to 550 nm (Sloan-g), 550 to 700 nm (Sloan-r), 695 to 850 nm (Sloan-i), and 830 to 1200 nm (Sloan-z). The filters are composed of Schott filterglasses and clearglass substrates coated with interference filters and represent an improvement of broadband Sloan filters commonly used in astronomy. In spite of the absorptive elements, the filters show maximum possible transmissions achieved by magnetron sputtered filter coatings. In addition, the blocking of the filters is better than OD5 (transmission <10 to −5) in the range 250 to 1050 nm which was achieved by combining up to three substrates. A high image quality required a low transmitted wavefront error (<λ/8 locally, respectively <λ/2 globally). We report on the spectral and interferometric results measured on the filters.
On the Javalambre mountain in Spain, the Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA) has setup a new wide field telescope, the JST/T250: a 2.55 m telescope with a plate scale of 22.67”/mm and a 3° diameter field of view. To conduct a photometric sky survey, a large format mosaic camera made of 14 individual CCDs is used in combination with filter trays containing 14 filters each of theses 101.7 x 96.5 mm in size. For this instrument, SCHOTT manufactured 56 specially designed steep edged bandpass interference filters which were recently completed. The filter set consists of bandpass filters in the range between 348,5 nm and 910 nm and a longpass filter at 915 nm. Most of the filters have FWHM of 14.5 nm and a blocking between 250 and 1050 nm with optical density of OD5. Absorptive color glass substrates in combination with interference filters were used to minimize residual reflection in order to avoid ghost images. Inspite of containing absorptive elements, the filters show the maximum possible transmission. This was achieved by using magnetron sputtering for the filter coating process. The most important requirement for the continuous photometric survey is the tight tolerancing of the central wavelengths and FWHM of the filters. This insures each bandpass having a defined overlap with its neighbors. In addition, the blocking of the filters is better than OD5 in the range 250–1050 nm. A high image quality required a low transmitted wavefront error (</4 locally and </2 on the whole aperture) which was achieved even by combining 2 or 3 substrates. We report on the spectral and interferometric results measured on the whole set of filters. λλ
The Centro de Estudios de Fisica del Cosmos de Aragon (CEFCA) will conduct a photometric sky survey with 2 new telescopes recently setup on the Javalambre mountain in Spain: the JST/T250 is a 2.55m telescope with a plate scale of 22.67”/mm and a 3° diameter field of view (FoV) and the auxiliary telescope JAST/T80 with a 82cm primary mirror and a FoV of 2 deg diameter. A multiple CCD (9k-by-9k array size, 10μm pixel size) mosaic camera is used in combination with filter trays or filter wheels, each containing a multitude of filters in dimensions of 101.7x96.5mm or 106.8x106.8mm. For this project, SCHOTT manufactured 56 specially designed narrow band steep edged bandpass interference filters and 5 broadband sloan-filters which were completed only recently. We report here on the results of the broadband sloanfilters with transmission bands of 324-400nm (sloan-u), 400-550nm (sloan-g), 550-700nm (sloan-r), 695-850nm (sloan-i) and 830-1200nm (sloan-z). The filters are composed of SCHOTT filterglasses and clearglass substrates coated with interference filters and represent an improvement of broadband sloan filters commonly used in astronomy. Inspite of the absorptive elements, the filters show maximum possible transmissions achieved by magnetron sputtered filter coatings. In addition the blocking of the filters is better than OD5 in the range 250–1050nm. A high image quality required a low transmitted wavefront error (<λ/8 locally, respectively <λ/2 globally) which was achieved by combining up to 2 substrates. We report on the spectral and interferometric results measured on the filters.
SCHOTT was one of the interference filters inventors starting around 1935. Based on this legacy optical bandpass filters were design, manufactured, and integrated into optical instruments in satellites. In addition a special blocking coating was developed reducing cross talk and ghost. For ground based telescopes steep-edge narrow bandpass filters with low transmitted wavefront error and about 100 mm x 100 mm size were manufactured pushing the filter design and the technology to its limits. The reached results for design and measurements will be shown on an H-alpha filter.
The Observatorio Astrofisico de Javalambre in Spain will conduct an all-sky astronomical surveys using multi-bands, where optical filters are needed. 54 narrow bandpass (FWHM = 14.5 nm) filters will continuously populate the spectrum between 370 to 920 nm with 10.0 nm steps. Here results on 2 filters with center wavelength of 460 nm and 470 nm and blocking from 250 to 1050 nm with OD5 will be shown. The filters have a maximum transmission of larger than 85% and a transmitted wavefront error of better than λ/2 over an aperture >~ 100mm.
The Observatorio Astrofisico de Javalambre in Spain will conduct an all-sky astronomical survey using multi-bands, where optical filters are needed. These filters are narrow bandpass steep edge filters (FWHM = 14.5 nm) in a spectrum between 390 to 920 nm with 10.0 nm steps. In order to fulfill the demanding requirements for final scientific image quality and transmitted wavefront error a new white-light Shack Hartmann sensor and difficult refractive index measurements of the sub-assembly were needed. In addition due to the spectral requirements the design and manufacturing of the filters were pushed at its technological limit.
KEYWORDS: Bandpass filters, Coating, Optical filters, Spectral resolution, Sputter deposition, Planets, Linear filtering, Electronic filtering, Ion beams, Control systems
Ion Beam Sputtering (IBS) offers a deposition process yielding optical thin films with stable optical parameters, near bulk density, and ppm level optical loss. Recently higher throughput systems with higher deposition rate and larger substrate fixtures have been developed. The higher deposition rates make accurate layer control essential. This is most readily achieved by using an optical monitoring system (OMS).
Multiple optical bandpass, edge filters and notch filters have been deposited in a high throughput IBS system with four 333mm diameter planetary using both a single wavelength (SWLOMS) as well as a broadband OMS (BBOMS). A wavelength repeatability of less than 0.1% for five subsequent short wave pass filters is demonstrated. Results for a multi notch filter coated using the BBOMS are also presented. A control strategy utilizing a mix of a broadband and a single wavelength model was used successfully in the deposition.
Spectral performance of multiple bandpass filters using turning point control is presented. A 2D mapping of a 15nm FWHM bandpass filter centered at 830nm shows a +/-0.05% variation in the center wavelength across the central 180mm diameter and a +/-0.35nm variation in the FWHM to the edge of the wafer. A variation of the standard turning point monitoring that enables control of filters with narrower bandwidth than the spectral resolution of the OMS system has been developed. A 0.8nm FWHM bandpass filter centered at 532nm controlled using a BBOMS with a ~1.5nm FWHM spectral resolution of the spectrometer is demonstrated.
The Observatorio Astrofisico de Javalambre in Spain observes with its telescope galaxies in the Local Universe plans to
perform a multi-band survey, where optical filters are needed. Different filters with a full width half maximum between
10-20 nm with central wavelengths at 395 nm, 410 nm, 430 nm, 515 nm, and an average transmission Tave larger than
85 % in the passband and blocking from 250 nm to 1050 nm of OD5 (T < 10-5) will be shown. The edges are steep for a
narrow transition from 5 % to 80 % and the transmitted wavefront error of the optical filter are less than λ/2 over an
aperture > 100 mm.
The Observatorio Astrofisico de Javalambre in Spain observes with its JAST/T80 telescope galaxies in the Local
Universe in a systematic study. This is accomplished with a multi-band photometric all sky survey called Javalambre
Photometric Local Universe Survey (J-PLUS). A wide field camera receives the signals from universe via optical filters.
In this presentation the development and design of a narrow bandpass steep edge filter with wide suppression will be
shown. The filter has a full width half maximum in the range of 13-15 nm (with <1 nm tolerance) with central
wavelengths in the range 350-860nm and an average transmission larger than 90% in the passband. Signals beyond the
passband (blocking range) have to be suppressed down to 250nm and up to 1050nm (spectral regime), where a blocking
of OD 5 (transmission < 10-5) is required. The edges have to be steep for a small transition width from 5% to 80%. The
spectral requirements result in a large number of layers which are deposited with magnetron sputtering. The transmitted
wavefront error of the optical filter must be less than lambda/2 over the 100mm aperture and the central wavelength
uniformity must be better than +/- 0.4% over the clear aperture. The filter consists of optical filter glass and a coated
substrate in order to reach the spectral requirements. The substrate is coated with more than 120 layers. The total filter
thickness was specified to be 8.0mm. Results of steep edge narrow bandpass filters will be demonstrated fulfilling all
these demanding requirements.
J-PAS (Javalambre-PAU Astrophysical Survey) is a Spanish-Brazilian collaboration to conduct an innovative
photometric survey of more than 8000 square degrees of northern sky using a system of 57 filters, 54 narrow-band
(FWHM=13.8 nm) filters continuously populating the spectrum between 370 to 920 nm with 10.0 nm steps, plus 3
broad-band filters. Together with the main J-PAS survey, the collaboration is carrying out J-PLUS (the Javalambre
Photometric Local Universe Survey), an all-sky survey using a set of 12 carefully optimized broad- and narrow-band
filters that will be used to perform the calibration tasks for the main survey. The J-PAS survey will be carried out using
JPCam, a 14-CCD mosaic camera using the new e2v 9.2k-by-9.2k, 10μm pixel detectors, mounted on the JST/T250, a
dedicated 2.55-m wide-field telescope at the Observatorio Astrofísico de Javalambre (OAJ) in Teruel, Spain. J-PLUS, on
the other hand, will be carried out using a wide field CCD camera (the T80Cam) equipped with a large format STA 1600
CCD (10.5k-by-10.5k, 9μm pixel) and mounted on the JAST/T80, a dedicated 0.83-m wide-field telescope at the OAJ.
In both cases, the filters will operate close to, but up-stream from the dewar window in a fast converging optical beam.
This optical configuration imposes challenging requirements for the J-PLUS and J-PAS filters, some of them requiring
the development of new filter design solutions. This paper describes the main requirements and design strategies for
these two sets of filters.
The presented work is embedded in the research network “Integrative Ion Processes for Modern Optics”, called IntIon, consisting of 12 partners from the German optics industry and two research institutes. The main target of the IntIon network is the development of new process concepts on the basis of ion assisted deposition (IAD) for the industrial production of optical thin film components. Besides an improvement in efficiency, a major aim is concentrated on the optical characteristics for selected application fields with high economical potential. In this network, different ion and plasma sources are compared with regard to their qualification for ion assisted deposition processes. This work includes the characterization of the ion energy and ion current using Faraday-cup measurements. The selection of investigated coating materials includes a broad variety of standard and non-standard oxides. First results of the network will be presented for adapted deposition materials and different operation characteristics of ion sources.
Scanning acoustic microscopy is used to determine elastic properties of carbon thin films. The films have been deposited by fullerene-argon-ionbeam deposition on crownglass substrates. With V(z) measurements, their elastic constants and experimental dispersion relations can be obtained. These are compared with numerically calculated dispersion relations. Using a simplex method for least- square data fitting the Young's modulus, the shear modulus and Poisson's ratio of the measured carbon thin films were determined.
Tetrahedral carbon thin films in amorphous modifications (ta-C) are ofinterest for applications due to their excellent hardness, chemical inertness, low friction, and low wear rates. They are obtained by mass-selected and monoenergetic carbon ion beam deposition and by laser ablation ofgraphite '' . The need ofan ion beam with a narrow distributed kinetic energy per C-atom is currently a fundamental obstacle for the use of such thin films in large area and high volume applications. More recently, the deposition of ions abstracted from a radio frequency excited acetylene plasma has yield a hydrogenated form oftetrahedral carbon with properties comparable to ta-C '.An important technological progress can be expected if an ion source can be made available that delivers carbon ions with a narrow-distributed kinetic energy per Catom, that can easily be scaled up, and that can be integrated into existing deposition systems. Due to their high vapour pressure, fullerenes can easily be sublimed and introduced into ion beam and plasma systems and thus have a potential for the deposition oftetrahedral carbon films by relatively simple technological means. The first approach to the use of fullerenes for the deposition oftetrahedral carbon was a cluster ion beam experiment ,in which fullerene ions were accelerated and disintegrated at their impact on a substrate. In another way, fullerenes can be used to generate a plasma ofhigh C2-content due to the effective dissociation ofstrongly heated fullerenes by C2-emission 6 The first use of such a plasma was a chemical vapour deposition experiment, in which fullerenes were dissociated in an argon microwave plasma and nanocrystalline diamond was grown6. The films obtained hereby show superior surface smoothness, low friction and low wear rates .Forthe deposition of amorphous carbon, a Kaufmann-source supplied with fu8 and a radio-frequency (RF) plasma source supplied with fullerenes and argon 10have been applied. Here we report on the ion beam deposition of amorphous carbon by using a fullerene argon plasma without the admixture ofhydrogen. The films are characterized regarding their Raman-emission, their plasmon loss structure and valence band spectra acquired by high-resolution X-Ray photoelectron spectroscopy (XPS), their optical absorption in the visible wavelength regime, and their wetting angles.
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