Intergalactic filaments spin

Spin Alignment of Dark Matter Haloes in Filaments and Walls

The MMF technique is used to segment the cosmic web as seen in a cosmological N-body simulation into wall-like and filament-like structures. We find that the spins and shapes of dark matter haloes are significantly correlated with each other and with the orientation of their host structures. The shape orientation is such that the halo minor axes tend to lie perpendicular to the host structure, ...

Intergalactic Medium

Constraint on intergalactic dust from thermal history of intergalactic medium

We present a new constraint on the amount of dust in the intergalactic medium (IGM) at high redshift. We derive the thermal history of the IGM by taking account of the photoelectric heating by dust grains, and compare it with the thermal history suggested by observations of Lyman α forests. As a result, if the IGM grain size is & 100 Å, the dust-gas mass ratio of the IGM at z & 2 is . 1/100 Gal...

The Spin Temperature and 21cm Brightness of the Intergalactic Medium in the Pre-reionization Era

We use numerical hydrodynamical simulations of early structure formation in a ΛCDM universe to investigate the spin temperature and 21cm brightness of the diffuse intergalactic medium (IGM) prior to the epoch of cosmic reionization, at z . 20. In the absence of any radiative heating, collisions between neutral hydrogen atoms can efficiently decouple the spin temperature from the CMB only in den...

Intergalactic Star Formation

Star formation in interacting systems may take place in various locations, from the dust–enshrouded core of Ultraluminous Infrared Galaxies to more unusual places such as the debris of colliding galaxies expelled into the intergalactic medium. Determining whether star-formation proceeds in the latter environment, far from the parent galaxies, in a similar way as in spiral disks has motivated th...