Dust attenuation in galaxies up to redshift 2 V. Buat
... formation rate (SFR) in the universe and its evolution with redshift from UV-optical surveys. The search for relations between dust attenuation and observed or commonly measured quantities are very useful in this context. It is also particularly important to study the dependence of dust attenuation ...
... formation rate (SFR) in the universe and its evolution with redshift from UV-optical surveys. The search for relations between dust attenuation and observed or commonly measured quantities are very useful in this context. It is also particularly important to study the dependence of dust attenuation ...
Other Worlds: Analyzing the Light Curves of
... In general, it is extremely difficult to detect planets directly, and it is much more common to detect extrasolar planets indirectly using one of the techniques outlined in this section. Planets are very faint compared to their host stars, and the planet’s light is generally swamped by the much more ...
... In general, it is extremely difficult to detect planets directly, and it is much more common to detect extrasolar planets indirectly using one of the techniques outlined in this section. Planets are very faint compared to their host stars, and the planet’s light is generally swamped by the much more ...
formation of z 6 quasars from hierarchical
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
... 6 Nagoya University, Dept. of Physics, Nagoya, Aichi 464-8602, Japan and 7 Spitzer Fellow Accepted to ApJ ...
The Evolution of the Mass-Size relation to z = 3.5 in the GOODS
... have smaller half-light radii. Their “norm optical sizes are thus perhaps not strong galaxies between 10 < log(M ...
... have smaller half-light radii. Their “norm optical sizes are thus perhaps not strong galaxies between 10 < log(M ...
Astronomy 1010L Lab Manual - The University of Tennessee at
... Earth’s shadow is now labeled. Zoom in enough to separate the Moon from the outline of the Earth’s shadow. Use the +Hour and +Minute Functions on the Date menu to track the position of the Moon relative to the Earth’s shadow. You may have to use the search feature to re‐center the Moon in the scre ...
... Earth’s shadow is now labeled. Zoom in enough to separate the Moon from the outline of the Earth’s shadow. Use the +Hour and +Minute Functions on the Date menu to track the position of the Moon relative to the Earth’s shadow. You may have to use the search feature to re‐center the Moon in the scre ...
The KMOS Redshift One Spectroscopic Survey
... ing the redshifted Hα 6563Å nebular emission line to obtain a measure of their ongoing star formation. The majority of the KROSS galaxies are selected to be those with known spectroscopic redshifts from various surveys, while the remainder (∼ 25%) are known Hα emitters from the HiZELS narrow-band s ...
... ing the redshifted Hα 6563Å nebular emission line to obtain a measure of their ongoing star formation. The majority of the KROSS galaxies are selected to be those with known spectroscopic redshifts from various surveys, while the remainder (∼ 25%) are known Hα emitters from the HiZELS narrow-band s ...
Slide 1
... • Spectral fitting and observations in X-rays/radio provide a strong support for the presence of an IMBH - Mass range = 6000 - 92000 M • Sub-Eddington radiation-pressure dominated accretion disk with a high (~4x10-4 M yr-1) at the outburst peak. • ~1yr recurrence timescale in the outbursts seen in t ...
... • Spectral fitting and observations in X-rays/radio provide a strong support for the presence of an IMBH - Mass range = 6000 - 92000 M • Sub-Eddington radiation-pressure dominated accretion disk with a high (~4x10-4 M yr-1) at the outburst peak. • ~1yr recurrence timescale in the outbursts seen in t ...
The Spitzer/GLIMPSE Surveys - UW-Madison Astronomy
... more detailed picture of their morphologies, especially those with small angular sizes. IRDCs are most easily observed in the 8 μm IRAC band because of the bright PAH emission that permeates the Galactic plane. Because they are seen in silhouette, we generally expect them to lie relatively close to ...
... more detailed picture of their morphologies, especially those with small angular sizes. IRDCs are most easily observed in the 8 μm IRAC band because of the bright PAH emission that permeates the Galactic plane. Because they are seen in silhouette, we generally expect them to lie relatively close to ...
