120 citations · 433 across the 21 of their papers we have counts for
11 papers · 1 filter
Exploring Compact Symmetric Objects with Complex Morphologies
E. E. Sheldahl, G. B. Taylor, S. E. Tremblay +9
Compact symmetric objects (CSOs) are a unique class of jetted active galactic nuclei (AGN) defined by sub-kpc radio emission, showing radio structure on both sides of the central e…
The first degree-scale starlight-polarization-based tomography map of the magnetized interstellar medium
V. Pelgrims, N. Mandarakas, R. Skalidis +21
We present the first degree-scale tomography map of the dusty magnetized interstellar medium (ISM) from stellar polarimetry and distance measurements. We used the RoboPol polarimet…
A compilation of optical starlight polarization catalogs
G. V. Panopoulou, L. Markopoulioti, F. Bouzelou +7
Polarimetry of stars at optical and near-infrared wavelengths is an invaluable tool for tracing interstellar dust and magnetic fields. Recent studies have demonstrated the power of…
CO enhancement by magnetohydrodynamic waves; Striations in the Polaris Flare
R. Skalidis, K. Gkimisi, K. Tassis +4
The formation of molecular gas in interstellar clouds is a slow process, but is enhanced by gas compression. Magnetohydrodynamic (MHD) waves create compressed quasiperiodic linear…
The Musca molecular cloud: The perfect "filament" is still a sheet
A. Tritsis, F. Bouzelou, R. Skalidis +3
The true 3-dimensional (3D) morphology of the Musca molecular cloud is a topic that has received significant attention lately. Given that Musca does not exhibit intense star-format…
HI-H transition: exploring the role of the magnetic field
R. Skalidis, K. Tassis, G. V. Panopoulou +6
Atomic gas in the diffuse interstellar medium (ISM) is organized in filamentary structures. These structures usually host cold and dense molecular clumps. The Galactic magnetic fie…
Why take the square root? An assessment of interstellar magnetic field strength estimation methods
R. Skalidis, J. Sternberg, J. R. Beattie +2
The magnetic field strength in interstellar clouds can be estimated indirectly by using the spread of dust polarization angles (). The method developed by Davis 1951 and by Cha…
Local Bubble contribution to the 353-GHz dust polarized emission
R. Skalidis, V. Pelgrims
It has not been shown so far whether the diffuse Galactic polarized emission at frequencies relevant for cosmic microwave background (CMB) studies originates from nearby or more di…
Gaia DR2 unravels incompleteness of nearby cluster population: New open clusters in the direction of Perseus
T. Cantat-Gaudin, A. Krone-Martins, N. Sedaghat +13
Open clusters (OCs) are popular tracers of the structure and evolutionary history of the Galactic disk. The OC population is often considered to be complete within 1.8 kpc of the S…
Local measurements of the mean interstellar polarization at high Galactic latitudes
R. Skalidis, G. V. Panopoulou, K. Tassis +4
We conduct a small-scale pathfinding survey designed to identify the average polarization properties of the diffuse ISM locally at the lowest dust content regions. We perform deep…
A closer look at the "characteristic" width of molecular cloud filaments
G. V. Panopoulou, I. Psaradaki, R. Skalidis +2
Filaments in Herschel molecular cloud images are found to exhibit a "characteristic width". This finding is in tension with spatial power spectra of the data, which show no indicat…