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A fundamental metallicity relation for galaxies at z = 0.84–1.47 from
A fundamental metallicity relation for galaxies at z = 0.84–1.47 from

... allows for the placement of up to 400 1.2 arcsec diameter fibres within a 30 arcmin diameter circular field of view and the light ...
Article PDF - IOPscience
Article PDF - IOPscience

FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS
FIELD GALAXIES AND THEIR AGNs: NATURE VERSUS

- Max-Planck-Institut für Astronomie
- Max-Planck-Institut für Astronomie

Summary - X-ray Astronomy Group at ISAS
Summary - X-ray Astronomy Group at ISAS

... • angular resolution • sensitivity XMM/Chandra are ideally suited for • extending previous studies to fainter, higher redshift, higher – and lower luminosity systems • detailed studies of many bright low redshift objects. • critical progress in the temporal/spectral domain Combined with other facili ...
Mark Correlations: Relating Physical Properties to Spatial Distributions
Mark Correlations: Relating Physical Properties to Spatial Distributions

Study properties of dwarf galaxies in and around the nearby Lynx
Study properties of dwarf galaxies in and around the nearby Lynx

SimulationDatabases
SimulationDatabases

A Deeper Look at Faint H $\ alpha $ Emission in Nearby Dwarf
A Deeper Look at Faint H $\ alpha $ Emission in Nearby Dwarf

3 science case - Giant Magellan Telescope Organization
3 science case - Giant Magellan Telescope Organization

astro-ph/9704019 2 Apr 1997 - National Optical Astronomy
astro-ph/9704019 2 Apr 1997 - National Optical Astronomy

HI in Early-type Galaxies
HI in Early-type Galaxies

The Panchromatic STARBurst IRregular Dwarf Survey (STARBIRDS
The Panchromatic STARBurst IRregular Dwarf Survey (STARBIRDS

Chapter 1
Chapter 1

Annual Report 2014 - Max Planck Institute for Astrophysics
Annual Report 2014 - Max Planck Institute for Astrophysics

here  - ISAS/JAXA
here - ISAS/JAXA

SN Ia host galaxy properties and the dust extinction
SN Ia host galaxy properties and the dust extinction

... underlying AV distribution, but rather to explore how the observed distribution relates to host galaxy observables to ascertain which host galaxy property should have priority in future SN Ia surveys. The SDSS-SN fits used in this analysis made use of a particular extinction distribution as a prior, ...
Lyman Break Galaxies at z~ 5: Luminosity Function
Lyman Break Galaxies at z~ 5: Luminosity Function

... well as the rest-frame photometric data points of LBGs at z ∼ 3 in the HDF-N (Papovich et al. 2001). The model spectra reasonably cover the UV colors of the LBGs at z ∼ 3. The adoption of the dust extinction is rather arbitrary to reproduce the redder colors of LBGs. The interpretation is, however, ...
The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS
The galaxy stellar mass function at 3.5 ≤z ≤ 7.5 in the CANDELS

the inclination of the dwarf irregular galaxy
the inclination of the dwarf irregular galaxy

Where stars are born: Javier Blasco-Herrera
Where stars are born: Javier Blasco-Herrera

Wide-field surveys and astronomical discovery space
Wide-field surveys and astronomical discovery space

A re-examination of galactic conformity and a comparison with semi
A re-examination of galactic conformity and a comparison with semi

... of the effect and how it changes as a function of the mass of the central galaxy. Conformity extends over a central galaxy stellar mass range spanning two orders of magnitude. The scale dependence and the precise nature of the effect depend on the mass of the central. In central galaxies with masses ...
Feedback in low-mass galaxies in the early Universe
Feedback in low-mass galaxies in the early Universe

... the evolution of galaxies during the peak epoch of star formation, with a variety of important consequences for the properties of galaxies and the intergalactic medium. These consequences include the shape of the relationship between the heavy-element content of galaxies and their mass; in both loca ...
Star formation in luminous quasar host galaxies at z = 1–2 ⋆
Star formation in luminous quasar host galaxies at z = 1–2 ⋆

< 1 ... 4 5 6 7 8 9 10 11 12 ... 45 >

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.
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