Surprised in Translation

Scott, Clive

doi:10.1093/fs/knm346

Cited by 4 publications

(6 citation statements)

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“…We have shown that the luminosity gap, M 12 , between the first‐ranked galaxy and the second‐ranked in fields containing at least one LRG is large and this is inconsistent with these brightest members being the statistical extreme of the local galaxy luminosity function within the model of Scott (1957). This dominance of the brightest members changes little over the redshift range of 0.12 < z < 0.38 and is more prominent in the poorer group‐like LRG fields than the richer cluster‐like fields.…”

Section: Discussionmentioning

confidence: 78%

“…The test hinges on two key assumptions about the nature of the galaxy luminosity distribution in clusters. The first is the model of Scott (1957) for the luminosity function, which postulates that, for a given luminosity distribution, overlapping magnitude intervals are statistically independent. If ψ is the integrated luminosity function then the probability of finding ν galaxies in the magnitude interval [ m a , m b ] is The number, ν, of galaxies (within a single isolated cluster) is a Poisson variate with mean and variance ψ( m b ) −ψ( m a ).…”

Section: Statistical Tests Of the Luminosity Function Tailmentioning

confidence: 99%

“…This work complements older studies using samples selected by galaxy overdensities (Tremaine & Richstone 1977; Geller & Postman 1983; Bhavsar & Barrow 1985) and can test the dominance–overdensity hypothesis. It also has a potentially cleaner interpretation, as overdensity‐selected samples are often subjected to bias from projection effects and by the so‐called selection effect (Scott 1957) when comparing samples over a range of redshifts.…”

Section: Introductionmentioning

confidence: 99%

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The bright end of the luminosity function of red sequence galaxies

Loh

Strauss

2006

Monthly Notices of the Royal Astronomical Society

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We study the bright end of the luminosity distribution of galaxies in fields with luminous red galaxies (LRG) from the Sloan Digital Sky Survey (SDSS). Using 2099 deg2 of SDSS imaging data, we search for luminous (≳L*) early‐type galaxies within 1.0 h−1 Mpc of a volume‐limited sample of 12 608 spectroscopic LRG in the redshift range 0.12 < z < 0.38. Most of these objects lie in rich environments, with the LRG being the brightest object within 1.0 h−1 Mpc. The luminosity gap, M12, between the first‐ and second‐ranked galaxies within 1.0 h−1 Mpc is large (∼0.8 mag), substantially larger than can be explained with an exponentially decaying luminosity function of galaxies. The brightest member is less luminous (by 0.1–0.2 mag) and shows a larger gap in LRG selected groups than in cluster‐like environments. The large luminosity gap shows little evolution with redshift to z= 0.4, ruling out the scenario that these LRG selected brightest cluster or group galaxies grow by recent cannibalism of cluster members.

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Section: Discussionmentioning

confidence: 78%

Section: Statistical Tests Of the Luminosity Function Tailmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The bright end of the luminosity function of red sequence galaxies

Loh

Strauss

2006

Monthly Notices of the Royal Astronomical Society

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“…The quaternary 4-arylamino-1,2,3-benzotriazines 2 exhibit a local anaesthetic effect [6] as well as anti-arrhythmic activity. [7] Furthermore, the successful antitumour drug temozolomide (3) also features the triazine ring system. [8][9][10] The first synthesis of temozolomide (3) used methyl isocyanate (MIC) as a reagent, which afforded both high purity and excellent yields.…”

Section: Introductionmentioning

confidence: 99%

Synthesis of Benzotriazine and Aryltriazene Derivatives Starting from 2‐Azidobenzonitrile Derivatives

et al. 2010

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Abstract3‐Substituted 3,4‐dihydro‐4‐imino‐1,2,3‐benzotriazine derivatives 7 were formed from 2‐azidobenzonitriles 4 as starting materials on treatment with Grignard or lithium organic reagents. In some cases these procedures gave aryltriazenes 10 and 11 as products. All compounds were identified by NMR spectroscopy and the structures of three products, namely 7a, 10a and 11i, were corroborated by X‐ray crystallography.

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“…However, it is debatable which observable should be used as a proxy for mass. If luminosity is a good proxy, then the brightest cluster galaxies (BCGs) should be the most massive galaxies; this has led to considerable interest in their properties (Scott 1957; Sandage 1976; Thuan & Romanishin 1981; Malumuth & Kirshner 1981; Hoessel, Oegerle & Schneider 1987; Schombert 1987, 1988; Oegerle & Hoessel 1991; Postman & Lauer 1995; Crawford et al 1999; Laine et al 2003; Bernardi et al 2007a; Lauer et al 2007).…”

Section: Introductionmentioning

confidence: 99%

A search for the most massive galaxies - II. Structure, environment and formation

Bernardi

Hyde

Fritz

et al. 2008

Monthly Notices of the Royal Astronomical Society

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We study a sample of 43 early-type galaxies, selected from the Sloan Digital Sky Survey (SDSS) because they appeared to have velocity dispersions of σ ≥ 350 km s −1 . High-resolution photometry in the SDSS i passband using the High-Resolution Channel of the Advanced Camera for Surveys on board the Hubble Space Telescope shows that just less than half of the sample is made up of superpositions of two or three galaxies, so the reported velocity dispersion is incorrect. The other half of the sample is made up of single objects with genuinely large velocity dispersions. None of these objects has σ larger than 426 ± 30 km s −1 . These objects define rather different size-, mass-and density-luminosity relations than the bulk of the early-type galaxy population; for their luminosities, they are the smallest, most massive and densest galaxies in the Universe. Although the slopes of the scaling relations they define are rather different from those of the bulk of the population, they lie approximately parallel to those of the bulk at fixed σ . This suggests that these objects are simply the large-σ extremes of the early-type population; they are not otherwise unusual. These objects appear to be of two distinct types. The less luminous (M r > −23) objects are rather flattened, and their properties suggest some amount of rotational support. While this may complicate interpretation of the SDSS velocity dispersion estimate, and hence estimates of their dynamical mass and density, we argue that these objects are extremely dense for their luminosities, suggesting merger histories with abnormally large amounts of gaseous dissipation. The more luminous objects (M r < −23) tend to be round and to lie in or at the centres of clusters. Their circular isophotes, large velocity dispersions and environments are consistent with the hypothesis that they are brightest cluster galaxies (BCGs). Models in which BCGs form from predominantly radial mergers having little angular momentum predict that they should be prolate. If viewed along the major axis, such objects would appear to have abnormally large velocity dispersions for their sizes, and to be abnormally round for their luminosities. This is true of the objects in our sample, once we account for the fact that the most luminous galaxies (M r < −23.5), and BCGs, become slightly less round with increasing luminosity. Thus, the shapes of the most luminous galaxies suggest that they formed from radial mergers, and the shapes of the most luminous objects in our large-σ sample suggest that they are the densest of these objects, viewed along the major axis.

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Surprised in Translation

Cited by 4 publications

References 0 publications

The bright end of the luminosity function of red sequence galaxies

The bright end of the luminosity function of red sequence galaxies

Synthesis of Benzotriazine and Aryltriazene Derivatives Starting from 2‐Azidobenzonitrile Derivatives

A search for the most massive galaxies - II. Structure, environment and formation

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