A ∼ 6 Mpc overdensity at z ≅ 2.7 detected along a pair of quasar sight lines: Filament or protocluster?

Abstract

Simulations predict that gas in the intergalactic medium (IGM) is distributed in filamentary structures that connect dense galaxy clusters and form the cosmic web. These structures of predominantly ionized hydrogen are difficult to observe directly due to their lack of emitting regions. We serendipitously detected an overdensity of log N(H? i) > 18.0 absorbers at z ≅ 2.69 along the lines of sight toward a pair of background quasars. Three main absorption regions spanning ∼ 2000 km s-1 (corresponding to 6.4 h70-1 Mpc proper) are coincident in the two lines of sight, which are separated by ∼ 90 h70-1 kpc transverse proper distance. Two regions have [Fe/H]