A direct measurement of the high-mass end of the velocity dispersion function at z ∼ 0.55 from SDSS-III/BOSS

Montero-Dorta, Antonio D.; Bolton, A.; Shu, Y.

doi:10.1093/mnras/stx321

Cited by 12 publications

(11 citation statements)

References 71 publications

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“…There are also some systematic errors due to the uncertainty of the velocity distribution function of lensing galaxies (equation 21). In this work, we adopt the modified Schechter function with parameters from Choi et al (2007) based on the SDSS DR3 data, while other authors using different data bases obtain somewhat different parameters (see Montero-Dorta et al 2017, for a recent comparison). Also, different strategies for sample selection and function modelling can affect the shape of the velocity distribution function (see e.g.…”

Section: Summary and Discussionmentioning

confidence: 99%

Gravitational lensing of gravitational waves: a statistical perspective

Mao

Zhao

et al. 2018

Monthly Notices of the Royal Astronomical Society

188

200

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In this paper, we study the strong gravitational lensing of gravitational waves (GWs) from a statistical perspective, with particular focus on the high frequency GWs from stellar binary black hole coalescences. These are most promising targets for groundbased detectors such as Advanced Laser Interferometer Gravitational Wave Observatory (aLIGO) and the proposed Einstein Telescope (ET) and can be safely treated under the geometrical optics limit for GW propagation. We perform a thorough calculation of the lensing rate, by taking account of effects caused by the ellipticity of lensing galaxies, lens environments, and magnification bias. We find that in certain GW source rate scenarios, we should be able to observe strongly lensed GW events once per year (∼ 1 yr −1 ) in the aLIGO survey at its design sensitivity; for the proposed ET survey, the rate could be as high as ∼ 80 yr −1 . These results depend on the estimate of GW source abundance, and hence can be correspondingly modified with an improvement in our understanding of the merger rate of stellar binary black holes. We also compute the fraction of four-image lens systems in each survey, predicting it to be ∼ 30 per cent for the aLIGO survey and ∼ 6 per cent for the ET survey. Finally, we evaluate the possibility of missing some images due to the finite survey duration, by presenting the probability distribution of lensing time delays. We predict that this selection bias will be insignificant in future GW surveys, as most of the lens systems (∼ 90 per cent) will have time delays less than ∼ 1 month, which will be far shorter than survey durations.

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Section: Summary and Discussionmentioning

confidence: 99%

Gravitational lensing of gravitational waves: a statistical perspective

Mao

Zhao

et al. 2018

Monthly Notices of the Royal Astronomical Society

188

200

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show abstract

“…Comparison with the Field Velocity Dispersion Function There are several VDF measurements for quiescent (or early-type) galaxies in the field based on SDSS and/or BOSS spectroscopy (Sheth et al 2003;Mitchell et al 2005;Choi et al 2007;Chae 2010;Montero-Dorta et al 2017;Sohn et al 2017b). These field VDFs differ from one another possibly due to differences in sample selection.…”

Section: 2mentioning

confidence: 99%

“…These strong lensing studies underscore the fundamental importance of the central velocity dispersions. The velocity dispersion distribution, i.e., the velocity dispersion function (VDF hereafter), has been measured for general field galaxies based on the SDSS and BOSS galaxy surveys (Sheth et al 2003;Mitchell et al 2005;Choi et al 2007;Bernardi et al 2010;Montero-Dorta et al 2017). These VDFs measured from the general galaxy population, which we refer to as field VDFs, have similar shapes at σ > 150 km s −1 , but they differ substantially for σ ≤ 150 km s −1 .…”

Section: Introductionmentioning

confidence: 99%

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

Sohn

Zahid

Geller

2017

ApJ

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We investigate the distribution of central velocity dispersions for quiescent galaxies in the SDSS at 0.03 ≤ z ≤ 0.10. To construct the field velocity dispersion function (VDF), we construct a velocity dispersion complete sample of quiescent galaxies with D n 4000 > 1.5. The sample consists of galaxies with central velocity dispersion larger than the velocity dispersion completeness limit of the SDSS survey. Our VDF measurement is consistent with previous field VDFs for σ > 200 km s −1 . In contrast with previous results, the VDF does not decline significantly for σ < 200 km s −1 . The field and the similarly constructed cluster VDFs are remarkably flat at low velocity dispersion (σ < 250 km s −1 ). The cluster VDF exceeds the field for σ > 250 km s −1 providing a measure of the relatively larger number of massive subhalos in clusters. The VDF is a probe of the dark matter halo distribution because the measured central velocity dispersion may be directly proportional to the dark matter velocity dispersion. Thus the VDF provides a potentially powerful test of simulations for models of structure formation.

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“…Note that several studies point to the stellar velocity dispersion as the best tracer of halo mass (e.g., Zahid et al 2016Zahid et al , 2019. This motivates the use of the velocity dispersion function (VDF, e.g., Montero-Dorta et al 2017a) in the context of halo-galaxy connection models.…”

Section: The Correlations Between Halo and Galaxy Propertiesmentioning

confidence: 99%

The manifestation of secondary halo bias on the galaxy population from IllustrisTNG300

Montero-Dorta,

Artale,

Abramo

et al. 2020

Preprint

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We use the improved IllustrisTNG300 magneto-hydrodynamical cosmological simulation to revisit the effect that secondary halo bias has on the clustering of the central galaxy population. With a side length of 205 h −1 Mpc and significant improvements on the sub-grid model with respect to the previous Illustris boxes, IllustrisTNG300 allows us to explore the dependencies of galaxy clustering over a large cosmological volume and wide halo-mass range. We show, at high statistical significance, that the halo assembly bias signal (i.e., the secondary dependence of halo bias on halo formation redshift) manifests itself on the clustering of the central galaxy population when this is split by stellar mass, colour, specific star formation rate, and surface density. A significant detection is also obtained for galaxy size: at fixed halo mass, larger central galaxies are more tightly clustered than smaller central galaxies in haloes of mass M vir 10 12.5 h −1 M . This effect, however, seems to be uncorrelated with halo formation time, unlike the rest of the secondary dependencies analysed. We also explore the transmission of the halo spin bias signal, i.e., the secondary dependence of halo bias on halo spin. Although galaxy spin retains little information about the total spin of the halo, the correlation is enough to produce a significant galaxy spin bias signal. We discuss possible ways to probe the spin bias effects with observations.

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A direct measurement of the high-mass end of the velocity dispersion function at z ∼ 0.55 from SDSS-III/BOSS

Cited by 12 publications

References 71 publications

Gravitational lensing of gravitational waves: a statistical perspective

Gravitational lensing of gravitational waves: a statistical perspective

The Velocity Dispersion Function for Quiescent Galaxies in the Local Universe

The manifestation of secondary halo bias on the galaxy population from IllustrisTNG300

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