[PDF] Top 20 The enhancement of rapidly quenched galaxies in distant clusters at 0 5 < z < 1 0
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The enhancement of rapidly quenched galaxies in distant clusters at 0 5 < z < 1 0
... affects galaxies with very high sSFR (SF1), which are quenched rapidly dur- ing infall, giving rise to ...be quenched, causing them to prematurely evolve into SF3 ...all galaxies ... See full document
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The structure of post starburst galaxies at 0 5 < z < 2: evidence for two distinct quenching routes at different epochs
... forming galaxies, as well as the identification of several unusual populations, ...star-forming galaxies; ii) metal poor quiescent dwarf galaxies, and iii) PSBs, which are selected as re- cently and ... See full document
21
The evolution of post starburst galaxies from z=2 to 0 5
... quiescent galaxies out to redshifts of z ∼ 4 or more ...be rapidly quenched following an early forma- tion ...quiescent galaxies are found to be elliptical and highly compact ...the ... See full document
15
The structure of post starburst galaxies at 0 5 < z < 2 : evidence for two distinct quenching routes at different epochs
... > 1) have experienced a major disruptive event that quenched their star formation and led to a ‘compaction’ of the stellar ...be rapidly quenched via feedback from either an AGN or the ... See full document
21
The evolution of post starburst galaxies from z=2 to 0 5
... post-starburst galaxies in the UKIDSS Ultra Deep Survey, with redshifts of 0.5 < z < 2 and stellar masses log (M/M ) ...at z ∼ 2, to <1 per cent by z ∼ ...quiescent ... See full document
13
Disc colours in field and cluster spiral galaxies at 0 5 ≲z≲ 0 8
... the galaxies that lie on the cluster red sequences are also located in the region of the (U−V, V−J) plane where the systems that have stopped forming stars are expected to ...been quenched, shows its HST / ... See full document
13
Matrices and Division by Zero z/0 = 0
... z =∞ denotes the value of the function W = z at the topological point at the infinity in one point compactification by Aleksandrov. The difference of (10) and (11) is very important as we see clearly by the ... See full document
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The faint end of the 250μm luminosity function at z< 0 5
... are found at z < 0.2. Marchetti et al. (2016), however, were un- able to constrain evolution beyond z ∼ 0.2, as only the bright- est galaxies can be individually detected at higher redshifts. De- ... See full document
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The LOFAR window on star forming galaxies and AGNs – curved radio SEDs and IR–radio correlation at 0<z<2 5
... measurement uncertainties can easily alter these observations and produce biased conclusions on curvature. An important bias is the detection level of the central band, which can severely compromise the interpretation of ... See full document
21
The AT LESS CO(1 0) survey of submillimetre galaxies in the Extended Chandra Deep Field South: First results on cold molecular gas in galaxies at z ˜ 2
... respectively, i.e. 115, 16.6 and 4.2 GHz restframe. This is consistent with the thermal fraction found in M82 (Condon 1992) and some z < 0.5 ULIRGs (Galvin et al. 2016). This result is from fitting to only ... See full document
10
The Hα luminosity dependent clustering of star forming galaxies from z ∼ 0 8 to z ∼ 2 2 with HiZELS
... satellite galaxies (Peng et ...massive galaxies, is also attributed to a shut-down of cold gas accre- tion, via shock heating by the hot halo (Dekel & Birnboim 2006), possibly in combination with AGN ... See full document
21
Effect of Cu2+ Doping on Structural and Optical Properties of Synthetic Zn0 5CuxMg0 5 xFe2O4 (x = 0 0, 0 1, 0 2, 0 3, 0 4) Nano Ferrites
... ing the XRD patterns are well indexed using MDI jade 5 and full proof. The crystal structure is found to be cubic with space group Fd3m.The fined peaks are indexed as the following (220), (311), (400), and (511). ... See full document
10
The dynamics and distribution of angular momentum in HiZELS star forming galaxies at z = 0 8–3 3
... star–forming galaxies from 0.8 ≤ z ≤ .... 0. 00 1 obser- vations allow the inner regions of the galaxies to be spatially ...at z∼3.3 via [O iii ] emission. All of the ... See full document
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... [r] ... See full document
66
Tetrakis(acetonitrile)copper(I) hydrogen oxalate–oxalic acid–acetonitrile (1/0 5/0 5)
... powder dissolved in 2 min., forming a white precipitate and a clear, pale blue supernatant. After 15 min. of stirring, a copious amount of white and dark purple solids settled to the bottom of the flask. The dark purple ... See full document
7
<p>Size at birth, infant growth, and age at pubertal development in boys and girls</p>
... at 5 and 12 months of age was routinely measured in the Danish postnatal health exam- ...at 5-month exam- ination was listed as <3 months or >7 months in the registry (n=171) or the age at 12-month ... See full document
11
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11
Electrochemical hydrogen storage characteristics of Mg2 xCxNi (x= 0, 0 1, 0 2, 0 5) alloys prepared by mechanical alloying
... intermetallic were markedly enhanced by nano- crystallization and amorphization [3]; this can be kinetically improved using elemental additives substituting either Mg [4] or Ni [5] lattice sites. Noticeable ... See full document
6
Microstructure and Properties of Rapidly Solidified Cu 0 81Cr 0 12Zr Alloy
... 22.25 at% Cu. Considering that the solid solubility of Cr in Cu is very small at room temperature and it cannot form into compounds with Cu when there is not other element involved, the dark phase should be pure Cr. The ... See full document
5
BCI-1. ) = 0 BCI-2. = 0 BCI-3. = 0 BCI-4. = 0 and = 0 implies that BCI-5. 0= 0, for all
... Suppose 𝑋𝑋 is a bound BCK-algebra and let 𝐼𝐼 be a proper commutative (resp. implicative, positive implicative ) ideal, then there is a maximal commutative (resp. implicative, positive implicative ) ideal containing ... See full document
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