Absolute Magnitudes of Turnoff Stars in Globular Clusters Palomar
... in astronomy because the intrinsic brightness can be compared with the observed brightness (apparent magnitude) to get the distance using the inverse square law. FTO stars are not traditionally chosen for distance calculations because they span a range of 1.5 magnitudes or more in brightness. When o ...
... in astronomy because the intrinsic brightness can be compared with the observed brightness (apparent magnitude) to get the distance using the inverse square law. FTO stars are not traditionally chosen for distance calculations because they span a range of 1.5 magnitudes or more in brightness. When o ...
GOODS: Great Observatories Origins Deep Survey
... Diffuse source, 0.5” diameter Add ~ 0.9 mag for stellar sources ...
... Diffuse source, 0.5” diameter Add ~ 0.9 mag for stellar sources ...
S282_2 Introduction to active galaxies
... radiation, and this is most apparent from the spectra. Active galaxies come in a variety of types, including Seyfert galaxies, quasars, radio galaxies and blazars. These types were discovered separately and at first seemed quite different, but they all have some form of spectral peculiarity. There i ...
... radiation, and this is most apparent from the spectra. Active galaxies come in a variety of types, including Seyfert galaxies, quasars, radio galaxies and blazars. These types were discovered separately and at first seemed quite different, but they all have some form of spectral peculiarity. There i ...
Here
... One of the many important advances in our knowledge of the distant, early Universe during the past decade has come from observations of spectral line emission from interstellar molecular gas, the raw material from which stars form, in high-redshift (z > 2) galaxies. For convenience, we call these ob ...
... One of the many important advances in our knowledge of the distant, early Universe during the past decade has come from observations of spectral line emission from interstellar molecular gas, the raw material from which stars form, in high-redshift (z > 2) galaxies. For convenience, we call these ob ...
The dark matter crisis: falsification of the current standard model of
... be unphysical. Therefore, a more general definition of a galaxy needs to be used. Throughout this text it is implicitly assumed that a self-gravitating object which consists of stars and perhaps gas is a galaxy if its Newtonian median twobody relaxation time is longer than the Hubble time, trel > τH ...
... be unphysical. Therefore, a more general definition of a galaxy needs to be used. Throughout this text it is implicitly assumed that a self-gravitating object which consists of stars and perhaps gas is a galaxy if its Newtonian median twobody relaxation time is longer than the Hubble time, trel > τH ...
MUFASA: The assembly of the red sequence
... that EAGLE also employs such a re-calibration; Trayford et al. 2015). Finally, Gabor & Davé (2015) showed that such a model can simultaneously produce the trends of satellite (environmental) and central (mass) quenching in accord with observations by e.g. Peng et al. (2010). These results indicate ...
... that EAGLE also employs such a re-calibration; Trayford et al. 2015). Finally, Gabor & Davé (2015) showed that such a model can simultaneously produce the trends of satellite (environmental) and central (mass) quenching in accord with observations by e.g. Peng et al. (2010). These results indicate ...
The Formation and Survival of Discs in a Lambda
... gas, cooling and feedback, focusing on the formation of discs. Our simulations follow eight isolated haloes similar in mass to the Milky Way and extracted from a large cosmological simulation without restriction on spin parameter or merger history. This allows us to investigate how the final propert ...
... gas, cooling and feedback, focusing on the formation of discs. Our simulations follow eight isolated haloes similar in mass to the Milky Way and extracted from a large cosmological simulation without restriction on spin parameter or merger history. This allows us to investigate how the final propert ...
THE UV-OPTICAL GALAXY COLOR-MAGNITUDE DIAGRAM. III
... an extinction-corrected Hess function in order to determine the number density of transition galaxies. We do not use the method of Johnson et al. (2007a, 2007b) because we use the combination of Dn (4000) and NUV r later as a transition rate metric. Kauffmann et al. (2003) measured dust extinction ...
... an extinction-corrected Hess function in order to determine the number density of transition galaxies. We do not use the method of Johnson et al. (2007a, 2007b) because we use the combination of Dn (4000) and NUV r later as a transition rate metric. Kauffmann et al. (2003) measured dust extinction ...
grav1to11 (102 slides)
... escape velocity Vesc(0)=300km/s, • Show M0 has the meaning of total mass – Potential at large r is like that of a point mass M0 – Integrate the density from r=0 to inifnity also gives M0 AS4021 Gravitational Dynamics ...
... escape velocity Vesc(0)=300km/s, • Show M0 has the meaning of total mass – Potential at large r is like that of a point mass M0 – Integrate the density from r=0 to inifnity also gives M0 AS4021 Gravitational Dynamics ...
The effect of helium sedimentation on galaxy cluster masses and
... Sunyaev-Zel’dovich effect (SZE) may be used to infer the helium abundance in the ICM (Markevitch 2007); however, the limited resolution and sensitivity of current SZE interferometers have so far not enabled the measurement of the distribution of helium, even in the cluster cores where the sedimentati ...
... Sunyaev-Zel’dovich effect (SZE) may be used to infer the helium abundance in the ICM (Markevitch 2007); however, the limited resolution and sensitivity of current SZE interferometers have so far not enabled the measurement of the distribution of helium, even in the cluster cores where the sedimentati ...
Discovery of a Dwarf Poststarburst Galaxy near a High Column
... 70 kpc across the sky (Dinshaw et al. 1997). However, the coincidence of line pairs in velocity (v 150 km s1) in QSO spectra can be interpreted either as a physically ‘‘contiguous’’ structure or as a series of ‘‘correlated’’ structures stretching across these sight lines, e.g., metal-enriched ga ...
... 70 kpc across the sky (Dinshaw et al. 1997). However, the coincidence of line pairs in velocity (v 150 km s1) in QSO spectra can be interpreted either as a physically ‘‘contiguous’’ structure or as a series of ‘‘correlated’’ structures stretching across these sight lines, e.g., metal-enriched ga ...
Slide 1
... Can’t draw any robust conclusions! • Results depend on which method is used and which group gets them ...
... Can’t draw any robust conclusions! • Results depend on which method is used and which group gets them ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.