[PDF] Top 20 On the UV compactness and morphologies of typical Lyman α emitters from z ∼ 2 to z ∼ 6
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On the UV compactness and morphologies of typical Lyman α emitters from z ∼ 2 to z ∼ 6
... for UV-selected star-forming galaxies from the literature (in light blue): large diamond (van der Wel et ...at z ∼ 0 and of the same size as LAEs at z ∼ ...redshifts, typical SFGs start ... See full document
17
Resolved Lyman α properties of a luminous Lyman break galaxy in a large ionised bubble at z = 6 53
... high-ionisation UV lines as NV, CIV or HeII are detected (Matthee et ...other UV-luminous galaxies at z ∼ 7 ...rest-frame UV emission is resolved into two components with effective radii ... See full document
15
Lyman α emitters gone missing: evidence for late reionization?
... metagalactic UV-background model, which incorporates a wide range of recent observational ...Ly α transmissivity due to the increasingly neutral, inhomogeneously reionized intervening IGM, but we also ... See full document
17
Resolved Lyman α properties of a luminous Lyman break galaxy in a large ionised bubble at z = 6 53
... suffer from such intrinsic line pro- file ...the UV continuum emission and resembles the Lyα ...at z = ...the UV components; Carniani et ...velocity from the regions where [CII] and the ... See full document
14
VLT/FORS2 view at z ~ 6: Lyman α emitter fraction and galaxy physical properties at the edge of the epoch of cosmic reionization
... of Lyman-α emitters (LAEs) among the galaxy population has been found to increase from z ∼ 0 to z ∼ 6 and drop dramatically at z > ...a Lyman continuum ... See full document
13
The Lyman alpha luminosity function at z=5 7 6 6 and the steep drop of the faint end:implications for reionization
... LF from z ∼ 6 to z ∼ 7, with a significant decrease ...at z > 6 caused by reioniza- tion not being ...brightest emitters would not suffer from such a decline ... See full document
16
Lyman Continuum and Lyman α Emission from Galaxies at High Redshift
... of UV radiation responsible for the ionization of hydrogen in the IGM is one of the crucial steps required for further understanding of galaxy formation and ...observing Lyman Continuum (LyC, hν > ...7 ... See full document
174
Spectroscopic properties of luminous Lyman α emitters at $z \approx 6 7$ and comparison to the Lyman break population
... Lyα emitters can be used to study the neutral fraction of the inter-galactic medium (IGM) in the epoch of reionization ...at z > 6.5: at fixed UV luminosity, the fraction of typical ... See full document
17
The clustering of typical Ly$α$ emitters from $z \sim 2 5 6$: host halo masses depend on Ly$α$ and UV luminosities
... ( z ) ...( z ) nor- malized line luminosity similar to previous narrowband works for Hα-, [O ii ]-, and [O iii ]-selected emission line galaxies (Sobral et ... See full document
21
(Z) 2 Nitroethenamine
... CÐN distances range from 1.303 to 1.335 AÊ (Gate et al., 1985; Hazell & Mukhopadhyay, 1980; DiaÂnez et al., 1985; Schlueter & Cook, 1989) and the nitro CÐN distances range from 1.378 to 1.395 AÊ. ... See full document
7
Methyl (Z,Z) α (methoxyimino) 2 [({1 [3 (trifluoromethyl)phenyl]ethylidene}amino)oxymethyl]benzeneacetate
... C17 0.081 (4) 0.132 (4) 0.090 (4) −0.005 (3) 0.017 (3) −0.013 (3) C18 0.0561 (17) 0.0618 (17) 0.0609 (18) 0.0098 (14) 0.0048 (13) −0.0023 (14) C19 0.0782 (19) 0.0797 (18) 0.094 (2) 0.0228 (15) 0.0098 (15) 0.0182 ... See full document
8
Uniqueness of meromorphic solutions of the difference equation \(R {1}(z)f(z+1)+R {2}(z)f(z)=R {3}(z)\)
... Throughout the whole paper, for a meromorphic function f (z), we use standard notations of the Nevanlinna theory (see, e.g., [2, 8, 14]) such as T(r, f ), m(r, f ), and N(r, f ) and define respectively the ... See full document
11
The production and escape of Lyman Continuum radiation from star forming galaxies at z~2 and their redshift evolution
... and UV data are similar to that of Rutkowski et al. (2016), but our typical galaxy has an order of magnitude higher star formation rate ...selected from wide-field surveys and the typical SFR ... See full document
19
On Z 2 x Z 2 - Cordial Graphs
... 2 0 , 1 is the residue classes modulo 2, where 0 denote the set of all even integers and 1 denote the set of all odd integers and consequently 2 2 0 , 0 , 1 , ... See full document
5
Local analogues to z ~ 5 Lyman break galaxies
... According to the standard cosmological model, the ΛCDM model in which the Uni- verse contains both a cosmological constant (Λ) and cold dark matter (abbreviated CDM), the first stars in the Universe formed some tens to ... See full document
227
(Z) α Chloromethyl 3,3′,4,4′ tetramethoxystilbene
... and (II) it is possible to conclude that the isomer denoted `1. Form' by Gellerstedt et al. (1976) is (IIIb) (the methylene group signal is located at 4.46) and that the isomer denoted `2. Form' by these authors ... See full document
12
An Isomorphism Problem in Z^2
... Note also that Euler’s characterization implies that if a pair of integers x, y are each representable as the sum of two integer squares, then their product xy is also representable as a sum of two integer squares. A ... See full document
9
A Flat Photoionization Rate at 2 ≤ z ≤ 4.2: Evidence for a Stellar-Dominated UV Background and against a Decline of Cosmic Star Formation beyond z ~ 3
... 2 ≤ z ≤ 4.2. Note, however, that the absolute nor- malization of Γ depends on the cosmology, the thermal history of the IGM, as well as on the gas density dis- tribution (e.g., Bolton et al. 2005), and that ... See full document
6
Discovery of a single faint AGN in a large sample of z > 5 Lyman break galaxies
... interloping z ∼ 1 galaxies (which can have similar optical colours) and many cool stellar (or substel- lar) objects that can contaminate LBG ...using 2-arcsec apertures centred on the I-band po- sition and ... See full document
7
(Z) 2 (2 Chloro 3,3,3 trifluoroprop 1 enyl) 6 methoxyphenyl acetate
... The title compound was synthesized by a modified literature procedure (Fujita & Hiyama, 1986). Zinc powder (3.25 g, 50 mmol) and acetic anhydride (3.06 g, 30 mmol) were added into a solution of ... See full document
7
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