Parametric Intelligent Design System of Manipulator of 4 DOF

Li, Jing; Zou, Xiangjun; Chen, Yin Le; Sun, Qi; Chen, Yan; Wang, Hong Jun

doi:10.4028/www.scientific.net/kem.455.499

Cited by 2 publications

(2 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This may also explain the difference in clustering between the two types of AGNs. Recently, Lim et al (2016) used the mass ratio of the central galaxy to its host halo as an observable proxy of halo assembly time and found it is correlated with many properties of the galaxies it hosts. Moreover, halo assembly history and substructure fraction are found to depend on large scale structures (e.g.…”

Section: Summary and Discussionmentioning

confidence: 99%

DIFFERENCES IN HALO-SCALE ENVIRONMENTS BETWEEN TYPE 1 AND TYPE 2 AGNs AT LOW REDSHIFT

Jiang

Wang

et al. 2016

ApJ

View full text Add to dashboard Cite

Using low-redshift (z < 0.09) samples of AGNs, normal galaxies and groups of galaxies selected from the Sloan Digital Sky Survey (SDSS), we study the environments of type 1 and type 2 AGNs both on small and large scales. Comparisons are made for galaxy samples matched in redshift, r-band luminosity, [O III] luminosity, and also the position in groups (central or satellite). We find that type 2 AGNs and normal galaxies reside in similar environments. Type 1 and type 2 AGNs have similar clustering properties on large scales ( 1 h −1 Mpc), but at scales smaller than 100 h −1 kpc, type 2s have significant more neighbors than type 1s (3.09 ± 0.69 times more for central AGNs at 30 h −1 kpc). These results suggest that type 1 and type 2 AGNs are hosted by halos of similar masses, as is also seen directly from the mass distributions of their host groups (∼ 10 12 h −1 M ⊙ for centrals and ∼ 10 13 h −1 M ⊙ for satellites). Type 2s have significantly more satellites around them, and the distribution of their satellites is also more centrally concentrated. The host galaxies of both types of AGNs have similar optical properties, but their infrared colors are significantly different. Our results suggest that the simple unified model based solely on torus orientation is not sufficient, but that galaxy interactions in dark matter halos must have played an important role in the formation of the dust structure that obscures AGNs.

show abstract

Section: Summary and Discussionmentioning

confidence: 99%

DIFFERENCES IN HALO-SCALE ENVIRONMENTS BETWEEN TYPE 1 AND TYPE 2 AGNs AT LOW REDSHIFT

Jiang

Wang

et al. 2016

ApJ

View full text Add to dashboard Cite

show abstract

“…For example, such large-scale effects may be produced by the dependence of star formation on halo assembly history (see e.g. Hearin, Watson, & van den Bosch 2015;Lim et al 2016;Tinker et al 2016;Zentner et al 2016), combined with halo assembly bias that links halo formation with large-scale structure (e.g. Gao, Springel, & White 2005;Wechsler et al 2006;Jing, Suto & Mo 2007), or may be produced by the preheating of the intergalactic gas owing to the formation of large scale structure (e.g.…”

Section: Introductionmentioning

confidence: 99%

ELUCID. IV. Galaxy Quenching and its Relation to Halo Mass, Environment, and Assembly Bias

Wang

Chen

et al. 2018

ApJ

View full text Add to dashboard Cite

We examine the quenched fraction of central and satellite galaxies as a function of galaxy stellar mass, halo mass, and the matter density of their large scale environment. Matter densities are inferred from our ELUCID simulation, a constrained simulation of local Universe sampled by SDSS, while halo masses and central/satellite classification are taken from the galaxy group catalog of Yang et al. The quenched fraction for the total population increases systematically with the three quantities. We find that the 'environmental quenching efficiency', which quantifies the quenched fraction as function of halo mass, is independent of stellar mass. And this independence is the origin of the stellar massindependence of density-based quenching efficiency, found in previous studies. Considering centrals and satellites separately, we find that the two populations follow similar correlations of quenching efficiency with halo mass and stellar mass, suggesting that they have experienced similar quenching processes in their host halo. We demonstrate that satellite quenching alone cannot account for the environmental quenching efficiency of the total galaxy population and the difference between the two populations found previously mainly arises from the fact that centrals and satellites of the same stellar mass reside, on average, in halos of different mass. After removing these halo-mass and stellar-mass effects, there remains a weak, but significant, residual dependence on environmental density, which is eliminated when halo assembly bias is taken into account. Our results therefore indicate that halo mass is the prime environmental parameter that regulates the quenching of both centrals and satellites. Subject headings: dark matter -large-scale structure of the universe -galaxies: halos -methods: statistical

show abstract

Parametric Intelligent Design System of Manipulator of 4 DOF

Cited by 2 publications

References 1 publication

DIFFERENCES IN HALO-SCALE ENVIRONMENTS BETWEEN TYPE 1 AND TYPE 2 AGNs AT LOW REDSHIFT

DIFFERENCES IN HALO-SCALE ENVIRONMENTS BETWEEN TYPE 1 AND TYPE 2 AGNs AT LOW REDSHIFT

ELUCID. IV. Galaxy Quenching and its Relation to Halo Mass, Environment, and Assembly Bias

Contact Info

Product

Resources

About