We present measurements of the auto- and cross-frequency power spectra of the cosmic infrared background (CIB) at 250, 350, and 500 μm (1200, 860, and 600 GHz) from observations totaling ~70 deg2 made with the SPIRE instrument aboard the Herschel Space Observatory. We measure a fractional anisotropy δI/I = 14% ± 4%, detecting signatures arising

A series of 33 different polycyclic aromatic hydrocarbons (PAHs) were studied by far infrared spectroscopy (terahertz spectroscopy) in the spectral range comprised between 600 and 50 cm(-1). In addition to common PAHs like naphthalene, anthracene, phenanthrene, fluoranthene, picene, pyrene, benzo[α]pyrene, and perylene, also quite unusual PAHs were

We studied the evolution of the Fundamental Plane in B- and g-bands, for two samples of early-type galaxies at 0.2 z 0.35 and 0.35 z 1.2. We found a difference in the intercept that can be interpreted as galaxies at z > ~0.7 being 0.68 and 0.52 mag brighter in the B- and g-band respectively, than their local counterparts. From the study of the

The wealth of exoplanets and the architectures of planetary systems that continue to emerge, is astounding and raises questions about the general picture of planet formation and evolution. To achieve such a stage of understanding, continuing studies of planetary systems in various stellar environments are essential. At present, of about 900 known

Dust around active galactic nuclei (AGNs) is distributed over a wide range of spatial scales and can be observed in the infrared (IR). It is generally assumed that the distribution on parsec scales forms a geometrically and optically thick entity in the equatorial plane around the accretion disk and broad-line region—dubbed "dust torus"—that emits

Context. Temperature, surface gravity, and metallicitity are basic stellar atmospheric parameters necessary to characterize a star. There are several methods to derive these parameters and a comparison of their results often shows considerable discrepancies, even in the restricted group of solar-type FGK dwarfs. Aims: We want to check the