GENERAL INFO

RESEARCH TASKS

INSTRUMENTS

ORBIT AND LAUNCH

GROUND SEGMENT

COOPERATION

DOCUMENTS

MEETINGS

LINKS

 

SCIENTIFIC PAYLOAD

 T-170M Telescope

The T-170M telescope is based on the classic Ritchey-Chretien scheme. Main parameters of the telescope are the following 

Primary mirror diameter  170 cm
Focal length 1700 cm
Field of view  30 arcmin
Image quality diffraction limited at the center of the field of view

General view of the T-170M telescope

 

The telescope is under development by Lavochkin Association (Russia). The main units of the structural model of the T-170 prototype telescope have successfully passed vibrostatic and thermal vacuum tests. The primary mirror and other optical elements is being manufactured by the Lytkarino Optical Glass Factory (Russia).The T-170M telescope has assimilated the successful experience gained during the fulfillment of the "Astron" project. 

Instrumental compartment

 

Spectrographs

Spectrograph unit comprises three different single spectrographs: two high-resolution spectrographs - UVES and VUVES (Germany), and a long-slit spectrograph LSS (China).

 

 

Spectrograph wavelength range resolution
VUVES 102-172 55000
UVES 174-310 50000
LSS 102-310 2500

Such characteristics will make it possible to perform detailed spectral analysis of UV stellar spectra (up to 15-17m) including e.g. bright stars in Magellanic Clouds. LSS is aimed at observations of faint objects (e.g. distant galaxies) with the moderate dispersion.

Field Camera Unit (ISSIS)

The WSO-UV field camera unit (Spain) named ISSIS (Imaging and Slitless Spectroscopy Instrument for Surveys) is being developed to carry out UV and optical diffraction limited imaging of astronomical objects. The ISSIS incorporates three channels:

  • High Sensitivity Far-UV Channel: 120-200nm;

  • Channel for Surveys (FUV): 120-600 nm, optimized for 120-270 nm;

  • Channel for Surveys (UVO): 120-600 nm, optimized for 270-600 nm.
     

FUV and UVO channels for surveys work through the beam splitter and have the same field of view. In addition to direct imaging, ISSIS will provide slitless spectroscopic capabilities. Polarimetric modes are under study as well as coronography.
 

ISSIS REQUIREMENTS (preliminary)

Camera Far-UV Channel Channel for Surveys (FUV) Channel for Surveys (NUV)
Detector type MCP (CsI) CCD Thinned, back-illuminated, uncoating CCD Thinned, back-illuminated, AR coating
Wavelength range 120-200 nm 120-600 nm optimized for 120-270 nm 20-600 nm optimized for 270-600 nm
Array size 2048 x 2048 4096 x 4096 4096 x 4096
Pixel size, mkm 15 15 15
Field of View 2'.2 (TBC) 3'.4 3'.4
Scale 0.05"/pixel 0.05"/pixel 0.05"/pixel

 

Fine Guidance System


The Fine Guidance Sensors System (FGS) is intended for precise pointing and stabilization of the telescope during a scientific observation session. 

The Fine Guidance System consists of 3 guiding sensors located near the central part of the telescope focal surface, and the common Data Processor Unit (DPU). Every sensor is based on 1 megapixel rad-hard CMOS image sensor STAR 1000, fabricated by Fillfactory. The Master catalogue for the Fine Guidance System is stored in the Data Processor Unit and contains coordinates of guiding stars over all the sky up to 17 magnitude.

Fig. 1 Rad-hard CMOS image sensor STAR 1000 for Fine Guiding system.

Sensitive surfaces of guide sensors are located close to the spectrographs entrance slits on their cases. It provides high stability of mutual position of the entrance slits and GS receivers.


Main characteristic of Fine Guide system are presented in the following table

Pointing and stabilization accuracy  0.03"
The period of information updating 0.5 - 2 sec
Spectral range 450 - 750 nm
Guide stars Up to 17 magnitude

The Fine Guidance System is under development by Russian Space Research Institute (IKI RAS). 

 
 

www.inasan.r