The BINGO Stage 0 group is dedicated to developing the instrumental components of the BINGO radio telescope, which is designed to detect Baryon Acoustic Oscillations (BAOs). The telescope will map the intensity of neutral hydrogen at cosmological distances, targeting the detection of BAOs from 980 MHz to 1260 MHz frequency range, which corresponds to a redshift interval of 0.127 < z < 0.449.
The Stage 0 group is responsible for the initial phases of the project, including site preparation, radio frequency interference (RFI) measurements, and the structural assembly of the telescope. BINGO employs a “single dish, many horns” design, consisting of a pair of 40-meter mirrors and around 28 horn antennas. These horns are the telescope’s primary receiving elements, playing a crucial role in capturing the faint radio signals associated with BAOs. In addition, the group also works on the development of other key radio frequency components—such as filters and receivers—as well as the backend systems, including analog-to-digital converters, real-time digital signal processing using FPGAs, with data storage infrastructure being the final component of Stage 0.

Leaders: 

This working group focuses on analyzing the raw data (time domain), detecting Fast Radio Bursts, Pulsars, and other transients. We also work on the development of the BINGO outriggers

Coordinator: Jiajun Zhang
Vice Coordinator: Alessandro Marins

After preliminary treatment of the radio signal, we get the spectrum of the received energy, which means we know the luminosity at every
different frequencies. At the same time, we also know where the signal coming from, by looking at the pointing direction of the telescope. In stage II, we need to combine these two kinds of information and make a map of the sky. The map can tell us which part of the sky is brighter and which part is dimmer. From now on, the numbers transmitting from the telescope become beautiful images of out universe. 
From the maps, we are looking for 21cm signal from the atomic hydrogen in the universe, however, the other sources are much brighter than the 21cm signal. For example, our Milky Way galaxy is very bright in the sky, the other galaxies are also bright, covering the 21cm signal. In fact, 21cm signal is no more than 1 out of 10000 in the collected radio signal. Our goal is pick it out magically, just like pick a needle from the bottom of the sea. This process is called foreground removal. 
Our team has developed several different methods to make maps and remove the foreground, they are tested to be successful in our simulation data. 

Coordinator: Jiajun Zhang
Vice Coordinator: Linfeng Xiao

How do we know what the universe looks like and how do we know our method can pick out the correct information from the data? The answer is, create an universe by ourselves and test if we can find the secrets. This is what Stage III is doing. By running cosmological simulations using super computers, we can create multiple universes and make the mock observations. According to our understanding, we can add all kinds of ingredients. In this way, we test ourselves, see if we can find the 21cm signal correctly, and also calculate the probability of getting the right answer. 
Every time creating the simulated universe, we know the exact parameters for cooking it. Then we develop the method of guess. According the statistical information, such as power spectrum, wiggles in the curves (called baryon acoustic oscillation), correlation functions, etc., we have a taste of the universe. We compare it to our model predictions, try it again and again, until we find the correct parameters in the model. This is called cosmological inference. 
Our team has developed several different methods simulate the universe and make mock observations. We also developed methods to statistically measure the universe and figure out the embedded parameters.

Coordinator:Chang Feng

The BINGO Stage IV group is dedicated to uncovering new physics through 21 cm intensity mapping. By analyzing the distribution of neutral hydrogen across cosmic time—particularly at low redshifts—we investigate how subtle imprints of beyond-Standard-Model physics may manifest in the matter distribution. Our research emphasizes the development of novel theoretical frameworks and data analysis algorithms designed to detect signatures of new dark matter particles, dark sector interactions, and deviations from general relativity. Through measurements of the 21 cm power spectrum and cross-correlations with other cosmological probes, we aim to establish 21 cm cosmology as a powerful and precise tool for testing fundamental physics.

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