phanerozoic/hi-21cm-survey

21cm Hydrogen Line Sky Survey

Continuous 1-second-cadence power spectra of the 21cm neutral hydrogen (HI) line at 1420.405 MHz, recorded 24/7 from a fixed omnidirectional observer on the US East Coast.

What this is

A radio telescope pointed at the whole sky, recording one spectrum per second, indefinitely. The Earth's rotation scans the beam across the galactic plane daily, producing a natural drift scan. Every row is a self-timestamped power spectrum spanning 2 MHz centered on the HI rest frequency.

Hardware

Component	Detail
Antenna	Omnidirectional L-band feed probe (wide-beam, zenith-biased)
LNA	Nooelec SAWbird+ H1 — SAW bandpass + LNA, centered 1420 MHz
SDR	Nooelec SMArTee v5 (RTL2832U + R820T), TCXO 0.5 ppm
Compute	Raspberry Pi 5, Debian, headless
Location	US East Coast, 41.0°N 73.0°W (quantized)

The SAWbird+ H1 provides a ~68 MHz usable passband (1374–1442 MHz) with peak response near 1399 MHz. The observation window sits on the upper slope of this filter. Bias-tee powered from the SMArTee v5.

Schema

Each row is one integration period from rtl_power.

Column	Type	Unit	Description
date	string	—	UTC date (YYYY-MM-DD)
time	string	—	UTC time (HH:MM:SS)
freq_start	int	Hz	Lower band edge (1419500000)
freq_end	int	Hz	Upper band edge (1421500000)
bin_width	float	Hz	Frequency bin spacing (~976.56)
num_samples	int	—	Samples averaged in this integration
power_0..power_2048	float	dB	Power spectral density per frequency bin

Frequency axis: 2049 bins from 1419.500 MHz to 1421.500 MHz at ~976.56 Hz spacing. To reconstruct: freq_mhz[i] = freq_start/1e6 + i * bin_width/1e6.

Power values: Log-scale (dB) relative to the SDR's internal reference. Not flux-calibrated. Relative measurements (e.g., ON-OFF, time differencing) are valid.

What's in the signal

The 21cm line from neutral hydrogen in the Milky Way. The galactic plane contains vast clouds of HI gas at different distances and velocities. Galactic rotation Doppler-shifts each cloud's emission to a slightly different frequency, spreading the line over 400 kHz (100 km/s). The main features:

• Local/Orion arm — nearest gas, dominant contribution, near the rest frequency
• Perseus arm — redshifted (receding), lower frequency
• Outer arm — further redshifted
• Scutum-Centaurus, Sagittarius-Carina — inner galaxy, complex velocities

The signal strength and Doppler structure change throughout the day as Earth's rotation sweeps different galactic longitudes through the beam.

Calibration notes

This is uncalibrated data. The power values include the receiver bandpass shape (SAWbird filter rolloff), gain drift (thermal), and system noise. To extract the HI signal:

1. Earth-rotation OFF: Hours when the galactic plane is below the horizon serve as a natural bandpass reference. Subtract from on-plane hours.
2. Polynomial baseline: Fit and subtract the bandpass shape from each spectrum, excluding the HI frequency range.
3. Matched filter: Cross-correlate against a galactic rotation model for optimal SNR.

Known artifacts:

• SAWbird bandpass slope across the 2 MHz window (higher power at lower frequencies)
• Thermal gain drift (~1–3 dB over hours, correlated with ambient temperature)
• Occasional RFI spikes (narrowband, identifiable by persistence and bandwidth)

Usage

from datasets import load_dataset

ds = load_dataset("phanerozoic/hi-21cm-survey", split="train")

Plot a single spectrum

import numpy as np

row = ds[0]
freqs = np.array([1419.5e6 + i * row["bin_width"] for i in range(2049)]) / 1e6
powers = [row[f"power_{i}"] for i in range(2049)]

import matplotlib.pyplot as plt
plt.plot(freqs, powers)
plt.xlabel("Frequency (MHz)")
plt.ylabel("Power (dB)")
plt.axvline(1420.405, color="r", linestyle="--", alpha=0.5, label="HI rest freq")
plt.legend()
plt.show()

Daily average

df = ds.to_pandas()
df["datetime"] = pd.to_datetime(df["date"] + " " + df["time"])
df["hour"] = df["datetime"].dt.hour

power_cols = [f"power_{i}" for i in range(2049)]
hourly = df.groupby("hour")[power_cols].mean()

Research applications

1. Galactic structure — Doppler tomography of spiral arms via velocity-resolved HI emission
2. Drift-scan mapping — Earth rotation provides full RA coverage; stack days to build sky maps
3. RFI characterization — long-term L-band interference environment near urban areas
4. Receiver stability — thermal drift, gain variation, bandpass evolution over months
5. Scintillation — interstellar scintillation of compact HI features at 1-second cadence
6. Educational — accessible radio astronomy dataset for students (no telescope required to analyze)

Collection method

Automated daemon on Raspberry Pi 5:

• rtl_power runs continuously, 1-second integrations
• Python watchdog handles crash recovery, daily file rotation, health logging
• Daily upload to HuggingFace via huggingface_hub
• Receiver: 49.6 dB gain, 2 MHz bandwidth, 2048-point FFT

Citation

@dataset{hi-21cm-survey,
  title={21cm Hydrogen Line Sky Survey},
  author={Norton, Charles C.},
  year={2026},
  publisher={Hugging Face},
  url={https://huggingface.co/datasets/phanerozoic/hi-21cm-survey}
}