[PDF] Top 20 The clustering and halo occupation distribution of Lyman-break galaxies at z ~ 4
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The clustering and halo occupation distribution of Lyman-break galaxies at z ~ 4
... bright galaxies in the model are more strongly clustered than faint ...of clustering on luminosity is in qualita- tive agreement with the observations, but is weaker than is inferred from clustering ... See full document
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Large-scale structure of Lyman break galaxies around a radio galaxy protocluster at z ∼ 4
... the clustering ampli- tude A ω is significantly larger than its uncertainty ( ≥ 6 σ ), con- firming that there is a non-random clustering signal present in our LBG ... See full document
5
Local analogues to z ~ 5 Lyman break galaxies
... a z ∼ ...and distribution of Lyman break analogue galaxies, this sample of photLBA objects will form the bulk of the analysis presented ...distant Lyman break ... See full document
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The production and escape of Lyman Continuum radiation from star forming galaxies at z~2 and their redshift evolution
... sive galaxies predominantly inhabit denser environments and galaxy clusters, whereas star-forming systems are mostly found in the ...star-forming galaxies is higher in more distant clusters than those in ... See full document
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Lyman Continuum and Lyman α Emission from Galaxies at High Redshift
... matter distribution on the largest scales (> 100 Mpc) in the Universe is for the most part determined by nonbaryonic cold dark matter (CDM) and ...in galaxies as well as the surrounding intergalactic ... See full document
174
The production and escape of Lyman Continuum radiation from star forming galaxies at z~2 and their redshift evolution
... of galaxies as a function of their UV luminosity (lumi- nosity functions) at z > 7 ...at z ∼ 2− 3), and a steepening of the faint-end slope with increasing red- shift (see for example the recent ... See full document
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A Spectroscopic Redshift Measurement for a Luminous Lyman Break Galaxy at z = 7.730 Using Keck/MOSFIRE
... of galaxies showing strong Ly α emission due to an increased neutral fraction in the intergalactic medium ( IGM ) at z > 6 ( Stark et ...the Lyman continuum break are underway using the ... See full document
6
Did Galaxies Reionize the Universe?
... < z < ...for galaxies beyond z ≃ ...beyond z ≃ 6 − 7 remained controversial because of their limited or marginal ...of z ≃ 7 − 8 candidates is more robust than those based on ... See full document
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The production and escape of Lyman-Continuum radiation from star-forming galaxies at z {sim} 2 and their redshift evolution
... By matching our sample of HAEs and LAEs with the public GALEX EM cleaned catalogue (e.g. Zamojski et al. 2007; Conseil et al. 2011), we find that 33 HAEs and 5 LAEs have a detection with N U V < 26 within a separation ... See full document
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First Data Release of the COSMOS Lyα Mapping and Tomography Observations: 3D Lyα Forest Tomography at 2.05 < z < 2.55
... The galaxies are represented by small spheres which all have the same size — in the future, we will aim to incorporate the morphologies and colors of the individual galaxies into the ... See full document
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Three Lyα emitters at z~6 : early GMOS/Gemini data from the GLARE project
... The work of detecting and analyzing objects at very high redshift is a challenging but rapidly advancing field. In recent months, increasing numbers of galaxies have been found at redshifts of z ≈ 6 , as a ... See full document
5
Candidate Massive Galaxies at z~4 in the Dark Energy Survey
... rived ages tend to cluster around the lower age limit set in HyperZ (0.1 Gyr). This is to be expected as - in χ 2 minimi- sation fitting of stellar populations containing young com- ponents - the best-fitting model tend ... See full document
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nIFTy cosmology: the clustering consistency of galaxy formation models
... It is important to notice that the models used have not been recal- ibrated for this particular simulation. The agreement between the models could be improved by calibrating the models in the simu- lation where the ... See full document
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Faint submillimeter galaxies identified through their optical/near infrared colors: 1 Spatial clustering and halo masses
... 27.7, and z ¢ = 26.6, respectively ( 3 σ , 2 diameter apertures ) . Details of the Suprime-Cam survey are provided in Furusawa et al. ( 2008 ) . The mid-infrared IRAC data were obtained by the Spitzer Legacy ... See full document
12
Stellar mass halo mass relation for the brightest central galaxies of X ray clusters since z~0 65
... universe, galaxies form within their cold dark matter ...of galaxies is regulated by the more complex physics of gas cooling, heating, and consumption by star formation as well as merger ... See full document
9
CO(1-0) survey of high-z radio galaxies: alignment of molecular halo gas with distant radio sources
... Fig. 7 shows that the CO(1–0) emission in MRC 0156-252 is located just outside a large reservoir of Ly α emission, with the boundary region between the Lyα and CO(1–0) gas occurring at the edge of the radio hotspot. The ... See full document
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nIFTy cosmology: comparison of galaxy formation models
... from the Millennium simulation have been compared with a special focus on the luminosity function (LF) of galaxy groups – high- lighting differences amongst models, especially for the magnitude gap distribution ... See full document
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The impact of strong gravitational lensing on observed Lyman-break galaxy numbers at 4 ≤ z ≤ 8 in the GOODS and the XDF blank fields
... high-redshift galaxies using the largest samples of LBGs at 4 ≤ z ≤ 8 (Bouwens et ...at z ∼ 4, z ∼ 5, z ∼ 6 and z ∼ 7–8 in order to infer the total expected lensed ... See full document
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Spectroscopic properties of luminous Lyman α emitters at $z \approx 6 7$ and comparison to the Lyman break population
... at z = ...at z = 6.6 and z = ...at z ∼ 2 − 3 ...at z ∼ 7, Santos et al. (2016) undertook a comparable survey at z = ...at z ≈ 6 − 7 play an important role in the ... See full document
17
Radio observations confirm young stellar populations in local analogues to z ~5 Lyman break galaxies
... Interestingly, Tabatabaei et al. (2017) present not only a calibration from total radio continuum to star forma- tion rate, but also its decomposition into thermal and non- thermal components, calibrated against the ... See full document
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