Radio Telescopes of the Future

Transcription

1 Radio Telescopes of the Future Cristina García Miró Madrid Deep Space Communications Complex NASA/INTA AVN Training School HartRAO, March 2017

2 Radio Telescopes of the Future Characteristics FAST SKA (EHT) Space antennas: Millimetron Lowest frequencies: Let s go outside!

3 Radio Telescopes of the Future

4 Radio Telescopes of the Future Complement and enhance actual radio telescopes

5 Radio Telescopes of the Future Complement and enhance actual radio telescopes High sensitivity and adequate spatial resolution: complement actual arrays (moderate spatial resolution, more sensibility, better quality radio images). Several simultaneous wide field of views (beamforming) to improve observing efficiency and survey speed. Support several projects with the same data set.

6 Radio Telescopes of the Future Complement and enhance actual radio telescopes High sensitivity and adequate spatial resolution: complement actual arrays (moderate spatial resolution, more sensibility, better quality radio images). Several simultaneous wide field of views (beamforming) to improve observing efficiency and survey speed. Support several projects with the same data set. Dual polarization, circular and/or linear. Observation at many frequency bands simultaneously, or broadband receivers. Flexibility: simultaneous configurations for high and low spatial resolution with high sensitivity, adaptive beamforming.

7 Radio Telescopes of the Future Complement and enhance actual radio telescopes Span the observing frequency range, e.g. frequencies not possible from the Earth. RFI control (terrestrial and LEO/MEO satellites): RFI effect mitigation techniques for weak signals.

8 Radio Telescopes of the Future Complement and enhance actual radio telescopes Span the observing frequency range, e.g. frequencies not possible from the Earth. RFI control (terrestrial and LEO/MEO satellites): RFI effect mitigation techniques for weak signals. Appropriate antenna elements: hybrid feed horns with b/w 2:1, polarizers with large and narrow bandwidths, microstrip antenna elements or dipoles, reflectors with multiple beams (single dish or array), phase-array feeds, etc. Antenna calibration: large number of unknown parameters dependent on frequency and observing direction: antenna gains and phases as well as the atmospheric and ionospheric disturbances.

9 FAST: Five hundred meter Aperture Spherical Telescope in China (first light Sep. 2016) Largest and most sensitive filled-aperture radio telescope (500m):

10 FAST: Five hundred meter Aperture Spherical Telescope in China (first light Sep. 2016) Largest and most sensitive filled-aperture radio telescope (500m): in testing and commissioning, 70MHz-3GHz, 3x Arecibo sensitivity, with active surface to create 300m paraboloids pointing to different directions, focusing radio waves on a receiver suspended 140 m above it. Pointing within ±40 from the Zenith, with 4 arcsec pointing precision, with 9 arcsec resolution for 21cm.

11 The largest the better? Greenbank telescope, EEUU 300 feet = 91m

12 The largest the better? Greenbank telescope, EEUU 300 feet = 91m 1998

13 The largest the better? Greenbank telescope, EEUU 300 feet = 91m 1998

14 SKA: Square Kilometer Array The Square Kilometer Array (SKA) project is an international effort to build the world s largest radio telescope, with eventually over a square kilometer of collecting area.

15 SKA: location Location selection: Free of RFI: low population areas, in a long period of time. Atmosphere characteristics (ionosphere and troposphere). Physical characteristics, climate and subsoil temperature change. Connectivity.

16 SKA: location Location selection: Free of RFI: low population areas, in a long period of time. Atmosphere characteristics (ionosphere and troposphere). Physical characteristics, climate and subsoil temperature change. Connectivity. Cost of infrastructure, operations and maintenance. Study of the Galactic Center: Southern Hemisphere Large, flat extension of ~ 5000 Km radius Politically stable country

17 SKA: location South Africa s Karoo region Western Australia s Murchison shire MHz (64 dishes) MHz MHz (36 dishes)

18 SKA: location South Africa s Karoo region Western Australia s Murchison shire MHz (64 dishes) MHz MHz (36 dishes)

19 SKA Project World leading scientists and engineers from around 100 organizations across about 20 countries are participating in the design and development of the SKA. It will be built in two phases, with cost of about 650M for SKA1. Fully operational in late 2020s, start construction in 2018, first science observations in 2020 with a partial array.

20 SKA Project World leading scientists and engineers from around 100 organizations across about 20 countries are participating in the design and development of the SKA. It will be built in two phases, with cost of about 650M for SKA1. Fully operational in late 2020s, start construction in 2018, first science observations in 2020 with a partial array. 240M SKA1 ~ 3 PEPAS!!!

21 SKA Project World leading scientists and engineers from around 100 organizations across about 20 countries are participating in the design and development of the SKA. It will be built in two phases, with cost of about 650M for SKA1. Fully operational in late 2020s, start construction in 2018, first science observations in 2020 with a partial 620M array. in 2016

22 SKA Project World leading scientists and engineers from around 100 organizations across about 20 countries are participating in the design and development of the SKA. It will be built in two phases, with cost of about 650M for SKA1. Fully operational in late 2020s, start construction in 2018, first science observations in 2020 with a partial array. Full SKA: Over a square kilometer of collecting area (unprecedented sensitivity), spawning over 3,000 km in extension (adequate resolution): ~2000 high and mid frequency parabolic dishes and aperture arrays. ~1 million low frequency antennas. Precursors: MeerKAT in South Africa, Murchison Widefield Array (MWA) and ASKAP in Australia.

23 SKA SKA will produce 1 Exabyte of data / day

24 SKA Retail price Hard drive available in Equivalent to HD photos in cellular Data produce by an SME with 30 employees in one day

25 SKA x 1024 Retail price Hard drive available in Equivalent to 8000 millions of tweets 120 hours English course in HD

26 SKA x 1024 Retail price Hard drive available in Equivalent to 40% human brain storage capacity Data from HST during 455 years

27 SKA x 1024 Retail price Hard drive available in Equivalent to 20 times size of all times books written until times the cultural material storage by Internet Archive It will produce 1 Exabyte of data / day: Double the daily world internet traffic

28 SKA

29 SKA

30 SKA: adaptive beamforming The relative phases of the signals arriving at the telescope are varied to constructively interfere the directions of interest, and destructively interfere the non-interesting ones.

31 Science with SKA SKA1 LOW (Australia): ): Reach as deep as 400 million after the Big Bang when the first stars and galaxies formed (13 billion years ago). SKA1 MID (Sudáfrica): versatile array... current and future science cases: pulsars and transients observations, detection of gravitational waves, clues about life in our Galaxy?

32 (EHT: Event Horizon Telescope) Earth-sized array, GHz high-frequency observations to improve resolution, 16Gbps recording (very sensitive).

33 (EHT: Event Horizon Telescope) Earth-sized array, GHz high-frequency observations to improve resolution, 16Gbps recording (very sensitive).

34 (EHT: Event Horizon Telescope) 10 mas Earth-sized array, GHz high-frequency observations to improve resolution, 16Gbps recording (very sensitive).

35 (EHT: Event Horizon Telescope) 10 mas Earth-sized array, GHz high-frequency observations to improve resolution, 16Gbps recording (very sensitive).

36 Space antennas: Millimetron Millimetron observatory ( Spektr-M project)

37 Space antennas: Millimetron Millimetron observatory ( Spektr-M project) 10-meter space telescope near L2, 10mm surface accuracy Millimeter and infrared wavelengths: 0.02 to 17 mm. High sensitivity, passive and active cooling systems, 0.5-4K

38 Space antennas: Millimetron Millimetron observatory ( Spektr-M project) 10-meter space telescope near L2, 10mm surface accuracy Millimeter and infrared wavelengths: 0.02 to 17 mm. High sensitivity, passive and active cooling systems, 0.5-4K Two operational modes: the single-dish: maximum sensitivity Space-Earth interferometer modes: ultra-high angular resolution, 0.1marcsec at 13cm

39 Lowest frequencies: where do we go? Solar emissions RFI Ionospheric limit: maximum baseline length below 100 MHz to 5 Km

40 Lowest frequencies: where do we go? Solar emissions RFI Ionospheric limit: maximum baseline length below 100 MHz to 5 Km Outside the atmosphere!

41 Lowest frequencies: where do we go? Solar emissions RFI Ionospheric limit: maximum baseline length below 100MHz to 5 Km RADIO ASTRONOMY EXPLORER B (1973) Outside the atmosphere!

42 Lowest frequencies: where do we go? Solar emissions RFI Ionospheric limit: maximum baseline length below 100MHz to 5 Km Outside the atmosphere!

43 Lowest frequencies: precursors New Mexico USA New Mexico USA Australia

44 Lowest frequencies: New Lunar Surface Concepts DALI

45 Lowest frequencies: DALI, 2025 Dark Ages Lunar Interferometer Array of 100,000 dipoles on the hidden side of the Moon (50 km diameter), 21cm HI line, MHz, z Average emission of the HI line in absorption over the CMB. Absorption occurs in areas of high density of dark matter that gave rise to the first stars.

46 Lowest frequencies: DARE, 2020 RFI, ionosphere & solar emissions Satellite in lunar orbit, averaged 21cm HI emission in absorption, at high z (35-11), MHz.

47 Radio Telescopes of the Future MANY THANKS! Cristina García Miró Madrid Deep Space Communications Complex NASA/INTA AVN Training School HartRAO, March 2017