The Boötes Void & Cosmic Supervoids

How did the giant Boötes Void form and is it completely empty?

The Boötes Void (discovered by Kirshner et al. 1981) is an approximately spherical cosmic supervoid roughly 100 megaparsecs (330 million light-years) in diameter centered at redshift z ≈ 0.052 (~700 million light-years away). It is not a total vacuum: deep redshift surveys have identified ~60 star-forming galaxies within its volume—roughly 10–15% of the cosmic mean galaxy density—arranged along tenuous internal sub-filaments evacuated by divergent peculiar velocity flows.

Physical Mechanism & Dynamics

Supervoids evolve from primordial troughs in the Gaussian density field (δ_i < 0). Because a region with lower-than-average matter density experiences weaker self-gravity than the surrounding background universe, its effective local Hubble expansion rate H_void exceeds the global rate H(t). Matter flows outward from the void center toward the bounding filamentary walls, deepening the interior underdensity toward δ_m ≈ -0.8 to -0.9.

As smaller adjacent sub-voids expand and collide, the tenuous sheets separating them are stretched and drained—a process called the 'void-in-void' hierarchy (Sheth & van de Weygaert 2004). In the Boötes Void, residual tubular sub-filaments survive inside the supervoid, hosting isolated, gas-rich, low-metallicity late-type galaxies that have escaped ram-pressure stripping and major mergers.

Quantitatively, this mechanism is governed by Nonlinear Spherical Void Expansion & Evacuation (1 + δ_v(t) ≈ (1 - δ_lin(t) / 3)^(-3), v_outflow(r) ≈ (1/3) H(z) Ω_m(z)^0.55 |δ_v| r). Describes how a linear underdensity δ_lin < 0 maps into a deep nonlinear void density contrast δ_v → -0.85 with linear radial outflow velocity toward the bounding shell.

Nonlinear Spherical Void Expansion & Evacuation

1 + δ_v(t) ≈ (1 - δ_lin(t) / 3)^(-3), v_outflow(r) ≈ (1/3) H(z) Ω_m(z)^0.55 |δ_v| r

Describes how a linear underdensity δ_lin < 0 maps into a deep nonlinear void density contrast δ_v → -0.85 with linear radial outflow velocity toward the bounding shell.

Quantitative Benchmarks & Parameters

Parameter / ObservableMeasured Value / ScaleMethod & Context
Boötes Void diameter~100 Mpc (330 million ly)Kirshner et al. (1981, 1987) redshift survey
Center redshift & distancez ≈ 0.052 (~215 Mpc / 700 Mly)Heliocentric recession velocity cz ≈ 15,500 km/s
Known interior galaxies~60 galaxies (vs ~2,000 at mean density)Hα, H I 21-cm, and SDSS spectroscopic surveys
Interior matter density contrastδ_m ≈ -0.75 to -0.85Void galaxy counts & weak lensing profiles

Observational Evidence & How Scientists Know

VLA 21-cm neutral hydrogen (H I) mapping and optical spectroscopy of Boötes Void galaxies (Szomoru et al. 1996) demonstrate that void galaxies have normal H I gas masses and elevated specific star formation rates compared to cluster galaxies of identical stellar mass, confirming that cosmic environment governs late-stage galaxy quenching.

Across reference datasets (Planck 2018 Cosmological Parameters (PR3), SIMBAD Astronomical Database (CDS)), quantitative benchmarks for the boötes void & cosmic supervoids are anchored by: Boötes Void diameter (~100 Mpc (330 million ly), via Kirshner et al. (1981, 1987) redshift survey); Center redshift & distance (z ≈ 0.052 (~215 Mpc / 700 Mly), via Heliocentric recession velocity cz ≈ 15,500 km/s); Known interior galaxies (~60 galaxies (vs ~2,000 at mean density), via Hα, H I 21-cm, and SDSS spectroscopic surveys); Interior matter density contrast (δ_m ≈ -0.75 to -0.85, via Void galaxy counts & weak lensing profiles).

Uncertainties, Systematics & Open Questions

Measuring the exact dark-matter floor inside deep supervoids requires stacking weak-lensing tangential shear profiles across thousands of SDSS/DESI/Euclid voids to separate luminous galaxy bias from true total matter density.

Real Astronomical Benchmarks & Cross-Domain Links

Guided Learning Path

Scientific Sources & Provenance

  1. Planck 2018 Cosmological Parameters (PR3) (PR3 (2020 A&A 641, A6)) — Planck Collaboration, Aghanim, N., et al. 2020, A&A, 641, A6. Archive / Reference ↗
  2. SIMBAD Astronomical Database (CDS) (2026-10 release) — Wenger, M., et al. 2000, A&AS, 143, 9 (The SIMBAD astronomical database). Archive / Reference ↗

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