Gamma-ray burst investigation via polarimetry and spectroscopy
... explore rather directly the universe in the epoch where first stars formed. 2.1.1 When did the first stars form? High-redshift GRBs GRB afterglows are bright enough to be used as pathfinders to the very early universe. Since long-duration GRBs are related to the death of massive stars, it is likely ...
... explore rather directly the universe in the epoch where first stars formed. 2.1.1 When did the first stars form? High-redshift GRBs GRB afterglows are bright enough to be used as pathfinders to the very early universe. Since long-duration GRBs are related to the death of massive stars, it is likely ...
sdssv15 - Sloan Digital Sky Survey
... Local census of the galaxy population: How did galaxies form? Find the most distant objects in the Universe: What are the highest quasar redshifts? ...
... Local census of the galaxy population: How did galaxies form? Find the most distant objects in the Universe: What are the highest quasar redshifts? ...
Revisiting the Hubble sequence in the SDSS DR7
... approach, since the classified sample contains lots of galaxies fainter than the limiting magnitude of the training sample. Therefore, it is very important to check that these faint galaxies are not systematically misclassified just because they are not represented in the training. As a first check, ...
... approach, since the classified sample contains lots of galaxies fainter than the limiting magnitude of the training sample. Therefore, it is very important to check that these faint galaxies are not systematically misclassified just because they are not represented in the training. As a first check, ...
astro-ph/9505110 PDF
... square is the Orion Nebula from Walter, Dufour & Hester (1992); stars are solar neighborhood B stars from Gies & Lambert (1992) and Cunha & Lambert (1994); solar value is from Grevesse & Noels (1993). Right: C/N vs. O/H; symbols are the same as for the left panel. on the massive star yields of Woosl ...
... square is the Orion Nebula from Walter, Dufour & Hester (1992); stars are solar neighborhood B stars from Gies & Lambert (1992) and Cunha & Lambert (1994); solar value is from Grevesse & Noels (1993). Right: C/N vs. O/H; symbols are the same as for the left panel. on the massive star yields of Woosl ...
pptx - LSST
... • Members have access to DESC communication tools, internal website, and documents • Full members have access to DESC computing resources and all DESC data products. Full membership requires a description of the work you plan to undertake and a commitment of time to the collaboration • Tools availab ...
... • Members have access to DESC communication tools, internal website, and documents • Full members have access to DESC computing resources and all DESC data products. Full membership requires a description of the work you plan to undertake and a commitment of time to the collaboration • Tools availab ...
Constraining the Warm Dark Matter Particle Mass through Ultra
... assume a correction factor ≈ 4 to account for the number of dwarfs being missed by current surveys, and lower correction factors would appreciably weaken the constraints. Given the potential systematic problems with known astrophysical WDM constraints, and the present lack of experimental determinat ...
... assume a correction factor ≈ 4 to account for the number of dwarfs being missed by current surveys, and lower correction factors would appreciably weaken the constraints. Given the potential systematic problems with known astrophysical WDM constraints, and the present lack of experimental determinat ...
sdssv13 - Sloan Digital Sky Survey
... Local census of the galaxy population: How did galaxies form? Find the most distant objects in the Universe: What are the highest quasar redshifts? ...
... Local census of the galaxy population: How did galaxies form? Find the most distant objects in the Universe: What are the highest quasar redshifts? ...
Summary - X-ray Astronomy Group at ISAS
... the important science problems and “Forget the technology” I will not give specific numbers (e.g. energy resolution, spatial resolution, sensitivity) this has been well covered in the talks on specific missions I personally believe that we have the technology to make major steps forward As Suzaku ha ...
... the important science problems and “Forget the technology” I will not give specific numbers (e.g. energy resolution, spatial resolution, sensitivity) this has been well covered in the talks on specific missions I personally believe that we have the technology to make major steps forward As Suzaku ha ...
A Wide-Field Study of the z~ 0.8 Cluster RX J0152. 7
... Luminosity-limited samples selected in the rest-frame UV include many bright, low mass, star forming galaxies as a result of the large scatter in their mass-to-light ratios at a fixed galaxy stellar mass. Selecting by stellar mass thus provides a more well-defined and homogeneous sample. In this pap ...
... Luminosity-limited samples selected in the rest-frame UV include many bright, low mass, star forming galaxies as a result of the large scatter in their mass-to-light ratios at a fixed galaxy stellar mass. Selecting by stellar mass thus provides a more well-defined and homogeneous sample. In this pap ...
Article PDF - IOPscience
... galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation ...
... galaxies, as seen through their stellar light distributions, contain enough physical information to offer this classification. We argue through the use of 240 images of nearby galaxies that three model-independent parameters measured on a single galaxy image reveal its major ongoing and past formation ...
The star formation history of galaxies in 3D: CALIFA perspective
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
... 2.1. Hubble sequence: stellar population properties of galaxies in the tuning-fork diagram One step to understand how galaxies form and evolve is classifying galaxies and studying their properties. Most of the massive galaxies in the near Universe are E, S0 and spirals (Blanton & Moustakas 2009), fo ...
Redshift
In physics, redshift happens when light or other electromagnetic radiation from an object is increased in wavelength, or shifted to the red end of the spectrum. In general, whether or not the radiation is within the visible spectrum, ""redder"" means an increase in wavelength – equivalent to a lower frequency and a lower photon energy, in accordance with, respectively, the wave and quantum theories of light.Some redshifts are an example of the Doppler effect, familiar in the change of apparent pitches of sirens and frequency of the sound waves emitted by speeding vehicles. A redshift occurs whenever a light source moves away from an observer. Another kind of redshift is cosmological redshift, which is due to the expansion of the universe, and sufficiently distant light sources (generally more than a few million light years away) show redshift corresponding to the rate of increase in their distance from Earth. Finally, gravitational redshift is a relativistic effect observed in electromagnetic radiation moving out of gravitational fields. Conversely, a decrease in wavelength is called blueshift and is generally seen when a light-emitting object moves toward an observer or when electromagnetic radiation moves into a gravitational field. However, redshift is a more common term and sometimes blueshift is referred to as negative redshift.Knowledge of redshifts and blueshifts has been applied to develop several terrestrial technologies such as Doppler radar and radar guns. Redshifts are also seen in the spectroscopic observations of astronomical objects. Its value is represented by the letter z.A special relativistic redshift formula (and its classical approximation) can be used to calculate the redshift of a nearby object when spacetime is flat. However, in many contexts, such as black holes and Big Bang cosmology, redshifts must be calculated using general relativity. Special relativistic, gravitational, and cosmological redshifts can be understood under the umbrella of frame transformation laws. There exist other physical processes that can lead to a shift in the frequency of electromagnetic radiation, including scattering and optical effects; however, the resulting changes are distinguishable from true redshift and are not generally referred to as such (see section on physical optics and radiative transfer).