Ground-based variability surveys towards Centaurus A: worthwhile
... Context. Difference imaging has proven to be a powerful technique for detecting and monitoring the variability of unresolved stellar sources in M 31. Using this technique in surveys of galaxies outside the Local Group could have many interesting applications. Aims. The goal of this paper is to test d ...
... Context. Difference imaging has proven to be a powerful technique for detecting and monitoring the variability of unresolved stellar sources in M 31. Using this technique in surveys of galaxies outside the Local Group could have many interesting applications. Aims. The goal of this paper is to test d ...
Dark baryonic matter
... cannot be distinguished : addition of images = amplification • But : amplification effect varies with time as lens passes in front of source - period T • Efficient for observation of e.g. faint stars ...
... cannot be distinguished : addition of images = amplification • But : amplification effect varies with time as lens passes in front of source - period T • Efficient for observation of e.g. faint stars ...
The Void Probability Function and Related Statistics
... Constraining the HOD parameters Berlind and Weinberg 2002, Tinker, Weinberg & Warren 2006 Void statistics expected to be sensitive to HOD at low halo masses BW02:M =(M/M1)a with a lower cutoff Mmin
Strong correlation between the minimum mass scale Mmin / size of voids
TWW06: M = M +
... Constraining the HOD parameters Berlind and Weinberg 2002, Tinker, Weinberg & Warren 2006 Void statistics expected to be sensitive to HOD at low halo masses BW02:
The Physical Nature of Cosmic Accretion of Baryons and Dark Matter
... our assumed mass profile inside the halo. For example, using an isothermal profile instead of NFW gives results that are consistent at the ∼ 10% level. Figure 2 shows the predicted values of the enclosed overdensity. Throughout this paper, we define overdensities relative to the mean matter density, ...
... our assumed mass profile inside the halo. For example, using an isothermal profile instead of NFW gives results that are consistent at the ∼ 10% level. Figure 2 shows the predicted values of the enclosed overdensity. Throughout this paper, we define overdensities relative to the mean matter density, ...
Coevolution of SMBHs and host galaxies at high z
... • If the AGN fraction is larger in the protocluster simply due to the presence of more massive SMBHs, then an average protocluster AGN would be more luminous than an average field AGN by the same factor • For this to be the case, the SMBHs would have to be ≈3−10 times more massive in the protocluste ...
... • If the AGN fraction is larger in the protocluster simply due to the presence of more massive SMBHs, then an average protocluster AGN would be more luminous than an average field AGN by the same factor • For this to be the case, the SMBHs would have to be ≈3−10 times more massive in the protocluste ...
OLIMPO
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
... • We have selected 40 nearby rich clusters to be measured in a single long duration flight. • For all these clusters high quality data are available from XMM/Chandra ...
Slides
... The gravitational potential determines where the galaxies form and where the ISW fluctuations are created! Thus the galaxies and the CMB should be correlated, though its not a direct template. Most of the cross correlation arises on large or intermediate angular scales (>1degree). The CMB is well de ...
... The gravitational potential determines where the galaxies form and where the ISW fluctuations are created! Thus the galaxies and the CMB should be correlated, though its not a direct template. Most of the cross correlation arises on large or intermediate angular scales (>1degree). The CMB is well de ...
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.