submillimeter astronomy in france p. encrenaz 434 first international symposium on space terahertz...

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Page 434 First International Symposium on Space Terahertz Technology Submillimeter Astronomy in France P. ENCRENAZ Laboratoire de Radioastronomie Millimetrique OBSERVATOIRE DE PARIS - Section de Meudon 92195 MEUDON FRANCE ABSTRACT: Submillimeter astronomy has been selected as the top priority for the next decade by the french space agency (CNES). A balloon borne telescope of 2m of diameter is built by Matra-Space, using the lightest CFRP materials. The petals of the telescope have been recently delivered: the telescope will be diffraction limited at 150 gm, and the pannels will be adjusted during flight. A pointing accuracy of 5" is anticipated. The first flight from Sicily to Spain is scheduled for 1992 with a set of bolometers cooled to He3. The first heterodyne receiver will fly in 1993. It consists of a cooled schottky receiver at 380 GHz to observe simultaneously H20 and 02. The trilayer Nb/Al203/Nb junctions may be used for the first flight. In collaboration with Cal Tech and Jet Propulsion Laboratory, a proposal for a small submillimeter satellite called SM3 (T. Phillips in the P.1) has been selected for a phase A by CNES. Related technological developments are funded in the area of cryo coolers, adjustable pannels in flight, quantum well devices and local oscillator sources, and manufacturing of SIS junctions. Work on different subsystems of the cornerstone FIRST is also in progress.

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Page 434 First International Symposium on Space Terahertz Technology

Submillimeter Astronomy in France

P. ENCRENAZ

Laboratoire de Radioastronomie Millimetrique

OBSERVATOIRE DE PARIS - Section de Meudon

92195 MEUDON FRANCE

ABSTRACT:

Submillimeter astronomy has been selected as the top priority forthe next decade by the french space agency (CNES). A balloon bornetelescope of 2m of diameter is built by Matra-Space, using the lightestCFRP materials. The petals of the telescope have been recentlydelivered: the telescope will be diffraction limited at 150 gm, and thepannels will be adjusted during flight. A pointing accuracy of 5" isanticipated. The first flight from Sicily to Spain is scheduled for 1992with a set of bolometers cooled to He3. The first heterodyne receiverwill fly in 1993. It consists of a cooled schottky receiver at 380 GHz toobserve simultaneously H20 and 02. The trilayer Nb/Al203/Nb junctionsmay be used for the first flight.

In collaboration with Cal Tech and Jet Propulsion Laboratory, aproposal for a small submillimeter satellite called SM3 (T. Phillips in theP.1) has been selected for a phase A by CNES. Related technologicaldevelopments are funded in the area of cryo coolers, adjustable pannelsin flight, quantum well devices and local oscillator sources, andmanufacturing of SIS junctions.

Work on different subsystems of the cornerstone FIRST is also inprogress.

First International Symposium on Space Terahertz Technology Page 435

PRONAOS

A French Balloon - Borne Space Project

1) Generalities

PRONAOS is a scientific space project for astrophysical observations in

submillimeter wavelength region with instrumentation borne on a stratospheric

balloon gondola.

The PRONAOS architecture consists of three parts •

- a carry away vehicle : the stabilized gondola

- a common facility : the submillimeter telescope

- a scientific payload : 2 focal plane instruments

A 900 000 m 3 balloon will permit first flights in transmediterranean campaigns from

Sicilia to south Spain (about 20 hours of ceiling at an altitude of 40 km and a latitude of

38° N), in july 1992 and 1993.

2) "Naps" gondoll :

The main characteristics of the vehicle are

- an azimuthal gondola with two stages stabilization delivering a diurnal pointing with

an accuracy RMS in arc seconds on two axes

. absolute 7"

. stability 5"

. drift rate 5" hour)

- the dry mass is 1600 kg for a lauching mass of 2200 kg

- the mass of the pointed set including Telescope, 1 focal-plane instrument and various

equipments is approximatly 500 kg.

- The gondola dimensions are typically : 4m x 4m x 7m (see Fig 111-1.1 and 1.2) and the

on-board energy permits a capacity of 30 kWh by a set of lithium batteries.

Page 436First International Symposium on Space Terahertz Technology

E t EoF.

git

First International Symposium on Space Terahertz Technology Page 437

3) Thq telescope

It is a 2m class submillirneter telescope. The main characteristics are

Cassegrain type telescope with a focal length of 20m, with f10,9 primary aperture

and 2.8 m back focus. The pointing (accuracy goal : 5 arc second) is obtained by stellar

sensor.

The 2m of diameter primary mirror has a surface accuracy of 10 g m RMS

including all defects.

The image quality of the telescope will be limited by the diffraction at 300 gm .

Light weight technology is used for the primary mirror realization : carbon fibre

by a replica-technique.

The mirror, segmented in 6 parts semi-active (in flight, aligment of the 6

segments considered as rigid, controlled by an on-board servo-loop), is equiped with 18

actuators and 30 dispacement captors.

Each segment is realized in composite structure (carbon fibre : honeycomb and

skins) on a replica mould : the mass is 3.3 kg, with a coating of 0.15 gm thickness gold

deposit.

4) Instruments,

Two instruments could be used on the focal plane of the telescope

SPM : (Multiband Photometric System)

The spectral resolution v/Av is 1 to 10 on the field : 200 gm to 1.5 mm (in 5 bands).

The photometer employs cooled bolometers at 0.5 K (or 0.1 K).

SMH : (Heterodyne Spectrometer)

With a high spectral resolution (v/Av., 106)

The submillimeter heterodyne radiometer will operate in the first generation at

380 GHz with a next goal of operating to 550 GHz. Noise temperatures as low as 500 K at the

lower frequency and 1000 K at the high end of the frequency range are expected. The

heterodyne radiometer mixes the input signal with a local oscillator (LO) signal at

approximately the same frequency to generate an output at the difference or

intermediate frequency (IF) which is then amplified and processed.

An ambient thermal load and a cold load will be used for absolute calibrations of

the radiometer. The mixer subsystem consists of a cooled Schottky diode, or three element

arrray of superconducting - insulating - superconducting tunnel junctions (SIS)

Page 438 First International Symposium on Space Terahertz Technology

operating at 3.5 K. The IF subassembly includes the cooled low-noise preamplifiers

which are followed by warm amplifiers. The LO subsystem contains the injection optics,

a set of frequency multipliers, Gunn oscillator to drive the multipliers , and a phase

locking system for the Gunn oscillator.

Acousto-optic spectrometers (AOS) will be used for the spectral analysis of the

heterodyne radiometers. The instrument block diagram is shown in Fig. 111-2. Following

are descriptions of the heterodyne radiometers and the AOS.

5) SMH main characteristics and description, •

The first interstellar molecules in galactic sources studied with SMH are H20 and

02 at 380.2 and 368.5 GHz respectively.

Atmospheric attenuation for different sites, shown on Fig. 111-3, indicates the

necessity to observe from space.

Using the double side band operation on the submillimeter heterodyne receiver,

both lines will be observed simultaneously by a optimized choice of the intermediate

frequency of the receiver (see picture below)

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first a cooled Schottky diode followed by an HEMT 6 GHz amplifier will be used. In this

case a over-all 500 K noise temperature will permit to detect a line in half of hour. For

the second flight, an SIS mixer will be used to increase the sensitivity..

Local oscillators

Optimum performance of a Schottky or an SIS mixer is achieved with an absorbed

LO power of about 300 p.W in the first case or less 10 jiW in the second case. To provide

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Page 440 First International Symposium on Space Terahertz Technology

even this level of power over the 300 GHz band is a challenge ; however, an approach

based on frequency multiplication of phase-locked solid-state millimeter-wave sources is

adequate and should be sufficiently reliable for space applications.

IF amplifiers

The IF frequency will be set at about 6 GHz with a bandwidth of 500 MHz . To take

advantage of the low noise performance of the mixers devices, the first IF stage, with 30

dB gain, will be cooled to about 40 K and located close to the mixers. HEMT devices are

being developped in the frequency range with noise temperatures less than 20 K and

low power dissipation.

Spectrum analysis

Acousto-optic spectrometers (AOS) will be used to analyze the spectra from the

heterodyne radiometers. In the AOS, the IF signal modulates a transducer which

generates a beam of acoustic waves in a crystalline material. These acoustic waves

diffract a separately injected laser beam. The deflected laser light is then detected by a

linear array of photodiodes to integrate the signal power in each frequency

channel.The signals from each diode are read out to a computer for the processing of the

spectral data.

The spectrum resolution of 500 kHz with 1000 pixels is obtained by 2 acousto-

optical spectrometers (Fig 111-4). The AOS bandwith is 180 MHz with a PbMo04 bragg cell.

To obtain high spectrum resolution, all local oscillators are stabilized by a phase

and frequency loop on a quartz reference. (stability of 10 4 is required).

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First International Symposium on Space Terahertz TechnologyPage 44/

Data acquisition and controls An in-board computer can control the receiver

(house keeping) and compact the data to send them to the ground station. The

transmission flow from the instrument is about 150 kbyte/s.

Cryogenics

The constraints and requirements for the cryogenic system 3.5 K operating

temperature with a 40 hours lifetime. The baseline design is a liquid Helium Dewar with a

40 K stage for the IF cooled amplifier.

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Page 442 First International Symposium on Space Terahertz Technology

First International Symposium on Space Terahertz Technology Page 443

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Page 446First International Symposium on Space Terahertz Technology

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