Not exact matches
The BICEP2 instrument can not distinguish the cosmic contribution from other sources directly, so, measurements of
galactic dust collected by other sources, such
as the Planck satellites were used.
Other effects, such
as light scattering from cosmic
dust and the synchrotron radiation generated by electrons moving around
galactic magnetic fields within our own galaxy, can also produce these polarisation twists.
Our black hole's violent meeting with G2 began last year, and
as it continues, it should give astronomers a chance to peer inside the
galactic center — the neighborhood around the black hole — rather than just simulate the swirling disc of gas and
dust surrounding it.
For tens of millions of years, most have been far from the
galactic disc where
dust and gas resides, so heavy elements such
as calcium should have sunk beyond detection long before.
But teasing out this primordial signal is difficult,
as swirls in the CMB could also be caused by
galactic dust, and confidence had started to wane by the official publication of the BICEP2 results in June.
Dust grains in the Galaxy could imprint a similar polarization pattern in the CMB
as gravitational waves can, but based on several different predictions of the
galactic contribution the researchers concluded that their data was more likely to originate from primordial gravitational waves.
A popular theory known
as the «unified theory» suggests that differences in the brightness of active
galactic nuclei,
as seen from here on Earth, are due to the placement of this donut of obscuring
dust relative to our angle of observation.
The bright center band in the above image represents heated interstellar
dust as seen along the
galactic plane of the Milky Way.
Many active
galactic nuclei are surrounded by large, dark, donut - shaped clouds of gas and
dust,
as seen in this artist's rendering.
«Detecting the Rayleigh signal is challenging because the frequency range where Rayleigh scattering has the biggest effect is contaminated by «noise» and foregrounds, such
as galactic dust,» lead author Elham Alipour said.
As a result, many specific structural features of the spiral arms are not well known, especially when compared with other spirals observed outside the Milky Way such as Andromeda (which is located a few million ly above the galactic plane of obscuring dust in the Milky Way's dis
As a result, many specific structural features of the spiral arms are not well known, especially when compared with other spirals observed outside the Milky Way such
as Andromeda (which is located a few million ly above the galactic plane of obscuring dust in the Milky Way's dis
as Andromeda (which is located a few million ly above the
galactic plane of obscuring
dust in the Milky Way's disk.
As for NGC2976, an extended
dust component is observed along the minor axis, which shows a distribution somewhat asymmetrical to the
galactic disk; this might be associated with the HI bridge in the M81 / M82 group that NGC2976 belongs to.