NooElec SAWbird+ H1 - Premium SAW Filter & Cascaded Ultra-Low Noise Amplifier (LNA) Module for Hydrogen Line (21cm) Applications. 1420MHz Center Frequency. Designed for Software Defined Radio (SDR)

Works very well to specification.

El LNA llegó acompañado de un latiguillo adaptador USB/conector de barríl de 5,5mm para la conexión de alimentación externa y un barrilete SMA macho/macho. El rendimiento de nuestra unidad honra los valores anunciados: ganancia sensiblemente superior a los 40dB en la banda de trabajo, con un ancho de 67MHz. Como se aprecia en las imágenes, la banda de trabajo está sensiblemente desplazada hacia abajo respecto a la frecuencia de funcionamiento nominal. Ahora, ¡a montarlo en una antena!

It did what it said on the box. I was able to finish my homebuilt telescope and see the hydrogen line!

excellent produit, faible bruit, et bien filtré, ne laisse passer que la bande SHF du H1, pour les radioastronomes, et les amateurs du SETI.

Low noise amplifier with essential filter for observing Hydrogen 1 line on 1.42 GHz. Reduces great amount of noises all around wanted spectra. Great amplification (40 dB+).

Amateur radio enthusiasts now have amazing and powerful technical capabilities at their disposal. My initial plan was to replicate some of the results documented by a group of students on the Internet. Their project demonstrated how the native H1 frequency (1420.4 Mhz) of neutral hydrogen can become red and blue-shifted due to the Doppler effect and the rotation of our Milky Way galaxy (MWG). Likewise used the spectrometer software from the West Virginia University Radio Astronomy project (WVU RAIL) which employs the polyphase filter bank technique to enhance harvesting of weak astronomical signals from the noise clutter. Instead of a horn antenna, a simple grid-wifi dish was used in conjunction with a dipole feed element tuned to 1420 Mhz via return-loss testing. The Sawbird+H1 served as the upstream LNA because of its lower published noise figure and a spectrum analyzer confirmed a relatively flat 30 db passband. Downstream devices included a Raspberry Pi-4 running the spectrometer software and an NESDR Smartee sampling at 2.4 MSPS. The accompanying image has the dish pointed in the vicinity of the star Alya near the galactic plane with coordinates of approximately +35 degrees longitude and 0 degrees latitude. There is a noticeable peak at roughly 1420.56 Mhz, followed by a dip, and then another slight peak at 1420.59 Mhz. These blue-shifted frequencies appear related to H1 concentrations in regions of the spiral arms of the MWG that are moving toward the observer. The frequency deviations from the baseline H1 correspond to a tangential (line-of-sight) velocity of 33.8 km/sec and 40.1 km/sec, respectively. By factoring in the Sun's velocity relative to the galactic core, the rotational speed of the galaxy can be estimated. Calibration of the spectrometer using its "hot" and "cold" benchmark temperatures is vital prior to observation.