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carried out an exhaustive study to define the characteristics required by such a telescope in order to participate actively in the international astronomy community. Once the appropriate homology and applications of the telescope had been selected a feasibility study was carried out with the fundamental objective of determining whether or not it was practical to construct such a telescope in Spain and if so how to maximize the participation of
Spanish industry in said project. This study was undertaken by INISEL Espacio and finally the contract for the detailed design and construction was awarded to a German company with a long experience of design and maintenance of radio telescope and radar dishes, MAN Technologie. Thus the initial construction work began in 2000 with the pouring of foundations and the placement of the concrete pedestal, built by ACS, that would support the telescope reflectors and associated support structure. The same year saw the production of the azimuth and elevation bearings by Rothe-Erde and FAQ of Germany respectively. 2000 also saw the construction of the steel back-support structure for the telescope by Schwartz-Hautmont Construcciones Metálicas of Spain. The contract for the design of the focal plane optics was awarded to ESTI of the Technical University of Telecommunications in Madrid to couple the Cassegrain focal plane radiation to the receivers. In 2001 the contract for the manufacturing of the surface panels of the primary and secondary reflectors was awarded to Schwartz-Hautmont and then installation of the servo-motors to BBH of Germany. Finally in 2003 the electrical installation was completed by ELIMCO of Spain.
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two orthogonal components of the incoming circularly polarised beam. The two linear polarisations are then fed directly to two low noise cryogenically cooled amplifiers. Following 2nd stage amplification, conditioning and filtering the astronomical signal is mixed with a Local
Oscillator signal at 2.555 GHz to give a 170 MHz IF bandwidth centred at 750 MHz. This IF is then re-routed to the backends in the control room some 5 metres below via a cable wrap. A phasecal signal is also injected to the IF module to remove phase errors. This band is important for observing the three Ch molecular lines which are considered extremely important in understanding the chemistry of the
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University of Madrid. The horn antenna is then coupled to a waveguide to coaxial polariser that separates out the two orthogonal components of the incoming circularly polarised beam. The two linear polarisations are then fed directly to two low noise cryogenically cooled amplifiers. Following 2nd stage amplification, conditioning and filtering the astronomical signal is mixed with a Local
Oscillator signal to give a 500 MHz IF in the standard band and a 330 MHz IF bandwidth in the expanded band. This IF is then re-routed to the backends in the control room some 5 metres below via a cable wrap. A phasecal signal can also be injected to the IF module to remove phase errors.
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polariser that separates out the two orthogonal components of the incoming circularly polarised beam. The two linear polarisations are then fed directly to two low noise cryogenically cooled amplifiers. Following 2nd stage amplification, conditioning and filtering the astronomical signal is mixed with a Local
Oscillator signal to give a 200 MHz or 500 MHz IF bandwidth centred at 750 and 800 MHz respectively. This IF is then re-routed to the backends in the control room some 5 metres below via a cable wrap. A phasecal signal can also be injected to the IF module to remove phase errors. This band is particularly important for the observation of formaldehyde (H
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the structure of the telescope housing, via a beam-guide. The optical configuration of the tertiary
Nasmyth system is such that the focus is always maintained in the same place as the flat Nasmyth mirrors track the movement of the principal axis of the dual reflector to ensure a constant illumination of the receivers. This allows the receiver antennas to remain fixed in position and greatly simplifies the opto-mechanical design of the receiver suite.
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size and comes in at 53 microns RMS. It has two nominal movement phase ; firstly a fine motion to correct for defocusing as a small defocus at the secondary is magnified 21 times at the
Cassegrain focus and which can result in large coupling losses especially at high frequencies. Secondly a large axial displacement is also possible (1 metre) which allows the holographic receptor to be placed in the focus of the parabolic reflector.
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346:. It is located at an altitude of 931 meters above sea level and benefits from exceptional observing conditions throughout the year. The precipitable water vapor (PWV) level remains below 6 mm, dropping to a minimum of 2 mm during winter. The wind velocity is generally below 5 m/s for most of the year, and the occurrence of rainy or snowy days is less than one week annually.
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that separates out the two orthogonal components of the incoming circularly polarised beam. The two linear polarisations are then fed directly to two low noise cryogenically cooled amplifiers. Following 2nd stage amplification, conditioning and filtering the astronomical signal is mixed with a Local
Oscillator signal at 1.53 GHz to give a 170 MHz
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skeleton and each panel is associated with a mechanical actuator that allows precision movements and orientation of each panel to 14 microns. The primary focus is located 15 metres from the parabolas vertex and is coincident with one of the foci of the secondary. The entire primary reflector and support structure weighs 200 tons.
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370:, quasi-optics etc.) that allows the dedicated team of more than 20 engineers and astronomers present to develop and optimize new and existing receivers. The R&D undertaken in the CDT under the mandate of the OAN permits it to share information and resources with the other important radio observatory in Spain, the
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and horizon to horizon coverage in elevation (180 degrees total or slightly less?). As previously mentioned the telescope is
Nasmyth-Cassegrain model that consists of a parabolic primary reflector and a hyperbolic secondary reflector that brings the dual system to a focus some 11 metres below, within
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The C-H band is a dual polarisation channel that covers from 3.22 – 3.39 GHzThe receiver consists of a choke ring axial corrugated horn that was designed by the
Antenna Group at the Technical University of Madrid. The horn antenna is coupled to a waveguide to coaxial polariser that separates out the
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The tertiary optics are responsible for the efficient coupling of the sky to the horn antennas of the 5 frequency bands of ARIESXXI. The first element encountered is an offset-parabolic with a focal length of 1.36 metres which converts the incoming quasi-plane wave to a converging beam which is then
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The sub-reflector can be displaced axially through focus to aid in correcting defocusing effects during telescope slewing caused by gravitational/elevation deformations. It is a hollow structure that permits the mounting of a holographic receptor within which will be used for determining the surface
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The project "A Radio
Telescope for Spain" was conceived from a series of National Development Plans for Radio Astronomy undertaken in the mid and late 90s. These plans culminated in a technical meeting in Madrid in the late 90s where the CAY personnel in conjunction with experts from all over Europe
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ARIESXXI boasts an unusually large receiver cabin (8 × 9 x 3.5 metres) which permits the housing of a large number of receivers. The cabin currently houses six receivers all of which reside in one of the two optical branches available (M and M'). The orientation of the Nasmyth mirrors can
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The S-Band is a dual polarization band with observable frequencies between 2.2 and 2.37 GHz. The S-Band receiver consists of a choke ring axial corrugated horn designed by the Antenna Group at the Technical University of Madrid. The horn antenna is coupled to a waveguide to coaxial polariser
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M2 is the hyperbolic sub-reflector of the dual reflector Cassegrain system and has a diameter of 3.28 metres. It is made from a carbon fibre shell covered in a thin layer of aluminium foil. The requirement on the surface flatness is tighter than for the primary due to the scaling of the main beam
635:
accuracy of the primary reflector panels. The telescope design follows the principle of homology. It can operate in winds up to 15 m/s and a maximum wind speed of up to 50 m/s can be withstood without structural damage being sustained. The surface accuracy can reach at least 150 microns
365:
network (EVN) as well as operating as a single dish. It currently has active receivers in S-Band (2.2–2.37 GHz), CH-Band (3.22–3.39 GHz), C band which is split in two sub-bands (4.56–5.06 GHz and 5.9–6.9 GHz), X-band (8.15–9.00 GHz) and K-Band (split in four bands between
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with a maximum accuracy of 75 microns RMS achievable. In order to attain this level of planarity each individual panel must fulfill a surface accuracy of 60 microns. A minimum planarity of 150 microns allows operation up to 125 GHz applying the Ruze condition of λ/16 with an upper threshold
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The X-Band has two simultaneously observable dual polarization sub-bands from 8.18 – 8.65 GHz called the Standard band and from 8.65 – 8.98 GHz called the expanded band. The X-Band receiver consists of a smooth walled conical horn and was designed by the Antenna Group at the Technical
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M3 and M4/M4' are the Nasmyth mirrors which redirect the incoming beam from the sky to the Nasmyth focus which is in essence the Cassegrain focus but displaced. Both mirror are flat and have a diameter of 2.65 metres and form a 45 degree angle with the optical axis of the telescope. The primary
665:
M1 is a 40 metre main parabolic reflector made up of 420 aluminium panels organized in 10 concentric rings. Each panel is fabricated from an aluminium plate approximately 1.8 mm thick and is covered with an epoxy to protect against the elements. The panels are mounted on a re-enforced aluminium
760:
simultaneously observable from 4.56 – 5.06 GHz, 5.9 – 6.4 GHz and 6.4 – 6.9 GHz. The C-Band receiver also consists of a choke ring axial corrugated horn and was designed by the Antenna Group at the University of Navarra. The horn antenna is then coupled to a waveguide to coaxial
731:(IF) bandwidth centred at 755 GHz. This IF is then re-routed to the backends in the control room some 5 metres below via a cable wrap. A phasecal signal is also injected to the IF module to remove phase errors. This band is primarily used for atmospheric calibration of VLBI observations?¿.
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frequency of 250 GHz in the case of 75 microns accuracy. The measured inefficiencies of ARIESXXI are ?% at ? GHz which compare to a theoretical maximum of 78% for a blocked Gaussian illumination and with a constant edge taper of −10.9 dB at the sub-reflector.
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in Granada. This collaboration also permits the free exchange of ideas and personnel with IRAM's facilities in France and Spain and facilitates technology exchanges between sister institutes in other European countries which participate in the
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also be altered to 0° and 20° if required to include additional optical paths and which substantially increases the number of receptors which can potentially be placed in the cabin. The receiver currently installed are as follows :
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function of these mirrors is to ensure a continuous illumination of the tertiary optical system. Currently only the M4 branch is furnished with receivers with M4' reserved for future high frequency and/or multi-beam receivers
361:. The most powerful telescope is the newly constructed 40 m telescope which was completed in 2005 and saw first light in ¿May 2007?. ARIESXXI was specifically designed to be integrated in the European
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The telescope observes both as a stand-alone telescope, and as part of VLBI networks. Up to 30% of its observing time is available to astronomers on a global basis.
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incident on a shaped dichroic lens that passes S/C/CH frequency for coupling to their respective feeds and reflects the X-band radiation towards the X-band feed.
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21.77 and 24.45 GHz). A 100 GHz receiver is currently being installed for millimetre wave VLBI. The CDT has advanced receiver laboratories on site (
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ARIESXXI utilizes the MarkV correlator backend system based on solid-state storage (as opposed to the MarkIV system which used magnetic tapes.
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is an alt-azimuthal design with a rotating head above an azimuthal bearing or turning head. It has full 360-degree movement in
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OH) whose interstellar distributions can yield important information about the structure of the galaxy.
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The observatory is located around 50 kilometres (31 mi) to the North-East of Madrid in the
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The Technological Development Centre (CDT) facilities include two radio telescopes, a
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Dual polarization (LCP & RCP) receiver of the 41-49 GHz band.
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Dual polarization (LCP & RCP) receiver of the 18-26 GHz band.
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The values of the most important optical parameters of the telescope
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Single polarization (RCP) receiver of the 78-110 GHz band.
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The C-Band has three dual polarization sub-bands that are
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The optical system consists of three main components:
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International VLBI Service for Geodesy and Astrometry
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Commissioning began in ¿2005? and finished in 2007.
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918:. Observation types (frequencies and objectives).
999:. Ministry of Public Works and Transport (Spain)
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969:Ministry of Public Works and Transport (Spain)
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997:"Yebes Observatory RT40m CALL FOR PROPOSALS"
965:"The Yebes Observatory 40-m radio telescope"
870:Since 2008, the telescope has been used for
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898:The telescope is also used to observe
333:National Geographic Institute of Spain
209:1,250 m (13,500 sq ft)
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1029:Astronomical observatories in Spain
261:Location of Yebes Observatory RT40m
196:40 m (131 ft 3 in)
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872:Very-long-baseline interferometry
363:Very Long Baseline Interferometry
329:Centro Astronómico de Yebes (CAY)
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342:in the autonomous community of
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461:3.7" in winds of 10 m/s
120:Instituto Geográfico Nacional
323:The telescope is located at
137:931 m (3,054 ft)
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712:The S/CH/C band receivers.
308:, Spain. It is a 40-metre
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894:Single Dish Observations
278:Related media on Commons
908:circumstellar envelopes
874:for both astronomy and
671:The Secondary Reflector
340:province of Guadalajara
298:Yebes Observatory RT40m
63:Province of Guadalajara
19:Yebes Observatory RT40m
904:interstellar molecules
729:Intermediate Frequency
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95:40.525208°N 3.088725°W
916:extragalactic sources
880:European VLBI Network
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660:The Primary Reflector
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37:European VLBI Network
884:Global mm VLBI Array
878:. It is part of the
765:CO) and methanol (CH
450:Aperture Efficiency
437:Primary and Masmyth
399:Telescope properties
368:low-noise amplifiers
206:Collecting area
171:Cassegrain reflector
167:Telescope style
100:40.525208; -3.088725
912:interstellar medium
744:interstellar medium
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421:Nasmyth-Cassegrain
374:radio telescope at
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842:. You can help by
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116:Organization
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1003:9 September
974:9 September
944:9 September
376:Pico Veleta
351:solar tower
98: /
74:Coordinates
55:Location(s)
1018:Categories
922:References
886:, and the
359:Gravimeter
355:astrograph
327:(Spanish:
224:astronomia
83:40°31′31″N
815:Back ends
704:Receivers
490:Parameter
407:Parameter
313:telescope
154:1999–2007
150:1999–2007
86:3°05′19″W
528:25.396m
319:Location
302:ARIESXXI
193:Diameter
134:Altitude
876:geodesy
823:Science
736:CH-Band
628:azimuth
616:3.621°
608:7.129m
600:6.667m
557:Feq/Dm
520:1.204m
474:Weight
426:Monunt
418:Optics
387:History
219:Website
152: (
69:, Spain
33:Part of
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910:, the
882:, the
805:W-Band
795:Q-Band
785:K-Band
774:X-Band
751:C-Band
721:S-Band
644:Optics
613:Theta
584:11.6m
576:26.6m
568:21.09
552:316.6
536:0.375
533:Fm/Dm
512:3.28m
357:and a
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902:from
592:6.6m
495:Value
412:Value
353:, an
306:Yebes
300:, or
285:[
147:Built
59:Yebes
1005:2015
976:2015
946:2015
866:VLBI
565:Mag
560:7.9
549:Feq
544:15m
504:40m
445:7.9
442:F/D
372:IRAM
296:The
226:.ign
906:in
846:.
758:not
637:RMS
605:hs
597:hp
589:g'
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541:Fm
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509:Ds
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228:.es
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