Pulsar Receiver Unit

NEW PRODUCT

Pulsar receiver package, the powerful integrated system can work with any radio telescope with L-Band output, you need to connect the RF cable to the Pulsar receiver, install PRS software on your PC, and then your system is ready for observation and recording Radio Pulsars data.

In the case of working with other frequency bands rather than L-Band, transferring the input frequency to L-Band ( with the centre frequency of 1420MHz and 100MHz bandwidth) needs to use the up/down conversion unit; for more information, please get in touch with us to discuss in detail.

Main Features:

L-Band Input
100MHz bandwidth
Sample rate 2GSa/s ( Maximum )
Input impedance 50Ω
Up to 50,000wfms/s waveform capture rate
Up to 60,000 frames of real-time waveform record, replay & analysis functions
Auto measurement of 25 waveform parameters, with statistics
Built-in FFT with a choice of window functions
Various waveform math functions
Connectivity mode USB
4U Rackmount case
Power Voltage 100 V to 240 V, 45 Hz to 65 Hz
Power Maximum 50 W, 250 V
Environment Temperature Range: 0℃ to +50℃ ( Operating )
Humidity Range: ≤95% relative humidity

Please contact us for more information.

The Package includes:

Pulsar receiver unit
PRS software
USB cable
Power cable
User manual
One year warranty
Up/down conversion unit ( Optional )

IR Telescope

Infrared (IR) Telescope

Ground-based IR telescopes are somewhat limited because carbon dioxide and water in the atmosphere absorb much of the incoming infrared radiation. However, there is the possibility of doing IR observations at high altitudes in areas with dry climates with cooled IR detector cameras. In addition, since infrared telescopes are not affected by light, they can be used during the day and at night.

Our IR telescopes can be designed to work in LWIR or MWIR bands with various sizes from 6" to 24" to meet the customer's requirement.

Please contact us for more information.

16" IR Telescope working in MWIR (3µm – 5µm)

Gold coating mirror for the highest reflectivity in IR

Solar Telescope

Solar Radio Telescopes * NEW RELEASE *

All POAM's radio telescopes from 3m to 12m can convert to a solar telescope. This kind of telescope eventually supplies LCP and RCP feed in the frequency band of interest from 100 MHz to 23 GHz to cover most science targets in solar radio astronomy.

The solar receiver can record data with a maximum sampling rate of 5 GSa/S in the form of time and frequency domain data, FFT data and much more ...

With POAM's solar software, the Sun can be tracked continuously, and data will be recorded and stored automatically or manually.

For more information about our range of solar telescopes, please contact us.

4.5 meter wideband solar telescope

11m Antenna designed for Solar observation

UWB Feed

Ultra-Wide Band Feed for Reflector Antenna

Professor Per-Simon Kildal designs this special feed antenna from Chalmers University in Sweden. The antenna has a fixed phase centre and can cover over a decade BW. This means that it can operate over an extensive band. Furthermore, its small size makes it easy to fit, move and cool down. The application areas of this antenna span from Radio Astronomy - Cryogenic feed in reflector antennas to Surveillance (military) and EMC Test chambers. This antenna can be designed for several frequency bands, from 100MHz to 20GHz.

UWB-1 100 MHz to 1 GHz

UWB-2 500 MHz to 5 GHz

UWB-3 1 GHz to 10 GHz

UWB-4 2 GHz to 20 GHz

UWB-2 Dual Polarised 500MHz to 5GHz feed

suitable for RTP53 ( 5.3m Radio telescope )

Low Frequency Feed

Low Frequency Feed for big Reflector Antenna

A novel low-frequency dual-polarization feed with symmetrical E&H plane patterns is presented in reflector antennas. This work describes the design, construction and characterization of a low-frequency feed for GMRT antennas covering the frequency range of 30 to 90 MHz. The main goals of our strategy are, 1) the physical dimension is suitable for mounting it along with one of the existing feeds on the GMRT antenna turret, with minimum interference to its operation, 2) the feed has symmetrical E & H plane patterns with reasonable aperture efficiency (0.5 < ηap < 0.7), and 3) the sky power transmitted from feed to receiver dominates the system temperature (Tsky > 5 TRec ) in the frequency range of interest. Currently, four GMRT antennas are equipped with these low-frequency feeds. Preliminary testing indicates that we have met most of our design goals.