TECHNOLOGICAL DEVELOPMENTS AT IGN INSTRUMENTATION AND TECHNOLOGICAL DEVELOPMENTS AT THE IGN

Transcription

1 INSTRUMENTATION AND TECHNOLOGICAL DEVELOPMENTS AT THE IGN

2 Yebes Observatory is a Fundamental Geodetic Station where Astronomical, Geodetic and Geophysical techniques are combined. Yebes, Guadalajara, Spain 980 meters height

3 Yebes Observatory development areas: Radio astronomy Technological developments. VLBI & SD observations. Geodesy Differential GPS station. Permanent GNSS Station maintenance. Geophysics Collecting data from gravimeters. Gravimeters maintenance.

4 FACILITIES 14 meters radio telescope. 40 meters radio telescope. Gravimeters. Satellite laser ranging (SLR)

5 Laboratories 40m 14m Double Astrograph Solar telescope Guest house Gravimetry Visitors Center

6 14 METERS RADIOTELESCOPE Inside radome Observations since 1976 VLBI since 1990: SiO masers EVN member (1994) and JIVE (1993) Next participation in VSOP-2 OBSERVATIONS SINGLE DISH: VLBI: Stellar formation SiO masers SiO masers CORE, EUROPE Galactic center

7 SPACE VLBI : 14m AS A LINK STATION VLBI Link system High Gain Antenna Diameter: 80cm Astro-G VSOP-2 Phase Transfer Uplink Frequency 40 GHz No Modulation TX-Power 10 W VLBI Data Downlink Frequency GHz Bit Rate 1 Gbps Modulation QPSK TX-Power 20 W Ground Link Station Diameter >10m H Maser Data Storage Data Storage Capacity 4 TB / 8 hours Phase Comparison

8 40m radio telescope Nasmyth-Cassegrain Diameter: 40m Subreflector: 3.28m Mount Alt-azimuth Turning head over bearing Operation: Primary & Nasmyth Aperture efficiency: 150 microns RMS 70% a 7mm 50% a 3mm Pointing: Requirements: 5 at 10m/s 1 servo system error

9 Construction: Budget 12M More than 20 companies: Engineering, Mechanics, Electronic, Electricity, Civil works,

10 Weight : 500 tones Main dish: 420 high precision panels < 65 microns.

11 Receiver cabin Large size Frequency band from 2 GHz to 120 GHz.

12 M4 branch 6 receivers 2.2 (S), 3.3,5-6 (C), 8.4 (X), 22 & 100 GHz Double polarization LCP & RCP

13 Control room

14 First light: June 2007 (The Moon at 22 GHz) First VLBI observation: June 2008

15 VLBI sessions Astronomical S/X, 22 GHz Geodetic S/X e-vlbi at C band (4-6 GHz)

16 Gravimetry laboratory

17 Mechanical stability. Seven isolated concrete pillars foundations. Thermal stability. Two isolated rooms one inside the other.

18 Absolute gravimeter FG5 Superconductive gravimeter (in 2010)

19 Satellite Laser Ranging, SLR The installation of a SLR station is one of our new projects. It allows the measurement of distances to satellites. It offers information of: ITRF (station coordinates, movement vectors, geocenter variations) Orbits determination EOP (xp, yp)

20 TECHNOLOGICAL DEVELOPMENTS Receivers Antennas Electronic components (LNA amplifiers, MMIC, feed antennas, )

21 Yebes Observatory has more than 500 square meters for laboratories and a mechanical workshop for the development of astronomical, geodetic, and geophysical instrumentation.

22 The labs have RF instrumentation for microwave circuits characterization covering the frequency band to 140 GHz. Among others, there are also laser prototyping and bonding machines for the construction of these microwave and millimeter circuits.

23 The workshop is equipped with milling and laith machines for the instrumentation construction. A CNC machine for the LNA boxes construction is also available.

24 ANTENNA DEVELOPMENTS Feed Design Phased-array Antenna measurement Holography

25 The feeds installed at the 40 meter are designed at Yebes Observatory. Commercial software, GRASP, or home-made software (QuasiOptica) are used for system feed design. Commercial software like CORRUG o HFSS is employed for antenna design.

26 Feed Systems Dichroic CH C S X

27 Antennas

28 Phased arrays IGN takes part in SKADS for the design of 1Km x 1Km telescope array in the 0.1 to 20 GHz band. IGN contribution has been the development of a planar array in the 0.3 to 1 GHz band.

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30 Anechoic chamber for antenna measurement Frequency range: GHz Feed and reflector measurements Cold optics measurement

31 12 GHz Holography receiver for the 40 meters Yebes has also experience in the measurements for the characterization of antenna surface with holography techniques. A dedicated receiver system has been developed including the software for data acquisition. IGN has also participated in the ALMA antennas characterization and in the design of an holography system for ESA.

32 First holography map with the 40 meter.

33 RECEIVER DEVELOPMENTS Microwave components design Cryogenics Radiofrequency Backends VLBI

34 All the receivers for the 40 meter radio telescope have been design and built at Yebes facilities. S-band: Trec: 50K VLBI CH-band: GHz Trec: 50K VLBI/SD C-band: GHz Trec: 50K VLBI/SD GHz X-band: GHz Trec:10K VLBI K-band: GHz VLBI/SD W-band: GHz Trec: 20K GHz SIS Ku-band: GHz Holography

35 Microwave components design

36 Radioastronomical receivers are installed inside cryostats at 20K.

37 Receiver cryostat at 22 GHz Lens corrected conical corrugated horn Septum polarizer Heaters Directional couplers 20 K stage Low noise amplifiers, LNA s Cryogenic cable (steel) 60 K stage Mollecular siege RF vacuum transitions Vacuum DC conectors

38 Receiver cryostat at S/C/CH

39 Radioastronomical receivers need further amplification and mixing. These are the RF and IF racks. Band C receiver

40 Band X receiver

41 The 100 GHz SIS receiver.

42 The last receiver stage is the digital backend. One of them is the Yebes autocorrelator. Ancho de banda Resolución 1024 MHz 2 MHz 512 MHz 0,5 MHz 256 MHz 125 KHz 128 MHz 62,5 KHz

43 AMPLIFIER DESIGN LNA s for IRAM LNA s for ALMA LNA s for the 40 metros LNA s for the DSN LNA s for satellites LNA s new designs

44 YEBES RECENT PROJECTS HERSCHEL (HIFI) (2-4 GHz & 4-8 GHz) IRAM ( GHz PB & GHz PV changed to 4-8 GHz & 4-12 GHz) RT 40 m CAY ( bands from 2.2 GHz to 26 GHz) ALMA (4-8 & 4-12 GHz) (ESOC) X-Band ( GHz) Ka-Band ( GHz) EUROPEAN PROJECTS FP6: AMSTAR (IFs for IRAM & SRON 4-12 GHz) FF7: AMSTAR+ (IF integrated with mixer), APRICOT (33-50 GHz multibeam receiver) Aprox cryogenic amplifiers supplied for different projects.

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53 SKA differential amplifiers

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55 IRAM Pico Veleta 30 meter radio telescope Plateau de Bure interferometer

56 IRAM is an international research institute for radio astronomy. Its overall objective is to explore the universe and to study its origins and evolution. IRAM headquarters in Grenoble, France IRAM was founded in 1979 by the French CNRS (Centre National de la Recherche Scientifique), the German MPG (Max- Planck-Gesellschaft) and the Spanish IGN (Instituto Geográfico Nacional) - initially an associate member, becoming a full member in 1990.

57 With a staff of more than 120 scientists, engineers, technicians and administrative personnel, IRAM maintains and develops the instrumentation for two observatories: the 30-meter telescope located on Pico Veleta near Granada in Spain, and the Plateau de Bure interferometer (an array of six 15-meter antennas) in the French Alps. SIS Laboratorie New PdB 4 bands receiver IRAM PdB correlator

58 Leader in the field of high frequency technologies, IRAM also develops receiver systems for the ALMA project in the southern hemisphere. 2SSB mixer block ALMA Band 7 cartridge SIS Junction

59 The 30-meter telescope on Pico Veleta in the Spanish Sierra Nevada is one of today s largest and most sensitive radio telescopes for tracing millimeter waves.

60 30meter cable spiral room The 30-meter telescope is equipped with a series of single pixel receivers operating at 3, 2, 1 and 0.8 millimeters and with two cameras working at 1 millimeter: HERA with 9 pixels and MAMBO, a camera with 117 pixels. 30meter receiver cabin

61 The other observatory of IRAM, the Plateau de Bure interferometer, is the most advanced facility existing today for millimeter radio astronomy. Consists of six antennas, each 15 meters in diameter. Each antenna is equipped with state-of-the-art high-sensitivity receivers.

62 The NOEMA project (Northern Extended Millimeter array) will transform the PdB into a completely new and extremely powerful facility, providing significant improvements in two key areas: sensitivity and spatial resolution

63 Muito Obrigado!