3-D crossing shock wave-turbulent boundary layer interaction

Gnedin, Marianna; Knight, Doyle; Zheltovodov, A. A.; Maksimov, A. I.; Shevchenko, A. M.; Vorontsov, S. S.

doi:10.2514/6.1996-2001

Cited by 7 publications

(4 citation statements)

References 9 publications

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“…In practice, the halo of ESO325-G004 may deviate from the assumptions of this model, especially in the innermost regions, where the dark matter distribution may contract in response to the dominant baryonic component. Simulations by different groups differ in their estimates of the strength of this ef- Gnedin et al 2011). Reviewing comparisons of hydrodynamic simulations against dissipationless control simulations, we note the following: Gnedin et al (2011) find enhancements in the the inner dark-matter mass (enclosed within 1 per cent of the halo virial radius) by factors of 2-4.…”

Section: Constraints On the Imfmentioning

confidence: 93%

“…Simulations by different groups differ in their estimates of the strength of this ef- Gnedin et al 2011). Reviewing comparisons of hydrodynamic simulations against dissipationless control simulations, we note the following: Gnedin et al (2011) find enhancements in the the inner dark-matter mass (enclosed within 1 per cent of the halo virial radius) by factors of 2-4. Johansson, Naab & Ostriker (2012) find the central dark-matter mass (enclosed within 2 kpc) is enhanced by a factor of 2.3 (their halo A2).…”

Section: Constraints On the Imfmentioning

confidence: 93%

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A giant elliptical galaxy with a lightweight initial mass function★†

Smith¹,

Lucey²

2013

Monthly Notices of the Royal Astronomical Society

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We present new observations of the closest-known strong-lensing galaxy, the σ ≈ 330 km s −1 giant elliptical ESO325-G004, made with the ESO Very Large Telescope. The low redshift of the lens (z l = 0.035) results in arcs being formed at a small fraction of the effective radius, (R Ein = 2.85 arcsec ≈ R eff /4). At such small radii, stars dominate the lensing mass, so that lensing provides a direct probe of the stellar mass-to-light ratio, with only small corrections needed for dark matter. However, the redshift of the galaxy lensed by ESO325-G004 was unknown until now, so the lensing mass was not securely determined. Using X-SHOOTER, we have detected multiple spectral lines, from two bright parts of the arc system, and measured a source redshift of z s = 2.141. Combined with lens modelling constraints, this yields a total mass inside the Einstein radius of 1.50±0.06×10 11 M ⊙ . We estimate the range of possible contribution of dark matter to the lensing mass, using halo profile statistics from cosmological N-body simulations. Subtracting this component yields a stellar mass-to-light ratio for the lens of M * /L F814W = 3.14 +0.24 −0.42 (M/L) ⊙,F814W . Using VIMOS, we have also obtained very high signal-to-noise spectroscopy for the lens galaxy. Fitting models to this spectrum confirms that ESO325-G004 has a very old stellar population. For a Milky-Waylike (Kroupa) IMF, the stellar population fit yields a predicted stellar mass-to-light ratio of Υ MW = 3.01±0.25(M/L) ⊙,F814W . Hence the mass attributable to stars with a Kroupa IMF is consistent with the lensing estimate. By contrast, a Salpeter (or heavier) IMF is disfavoured at the 99.8 per cent confidence level. A "heavyweight" IMF, with a mass twice as large as the Kroupa case, is firmly excluded for this galaxy. Such an IMF has been proposed for more distant elliptical lenses, and also to explain strong dwarf-star sensitive spectral features, in particular the Na I 8200Å doublet. A FORS2 far-red spectrum shows that this feature is as strong in ESO325-G004 as it is in other high-σ ellipticals, suggesting tension between dwarf-star indicators and lensing-mass constraints for this galaxy.

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Section: Constraints On the Imfmentioning

confidence: 93%

Section: Constraints On the Imfmentioning

confidence: 93%

A giant elliptical galaxy with a lightweight initial mass function★†

Smith¹,

Lucey²

2013

Monthly Notices of the Royal Astronomical Society

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“…Knowing the virial mass and concentration of each halo, we can reconstruct the NFW density profile; however, it is likely that this profile is altered in some way by the formation of galaxies at the halo centres. One possibility is for the dark matter to contract adiabatically (Blumenthal et al 1986;Gnedin et al 2004Gnedin et al , 2011), but it is also possible for baryons to transfer energy to the halo and cause it to expand instead (e.g. Macciò et al 2012;Di Cintio et al 2014;Pontzen & Governato 2014).…”

Section: Modelmentioning

confidence: 99%

“…Macciò et al 2012;Di Cintio et al 2014;Pontzen & Governato 2014). We employ here the same parametrization of these effects as in DW15: a free, continuous parameter ν interpolates between the adiabatic contraction prescription of Gnedin et al (2011) (ν = 1), and an expansion of the same magnitude (ν = −1). 8 ν = 0 corresponds to no effect of disc formation, in which case haloes retain their NFW form.…”

Section: Modelmentioning

confidence: 99%

The Faber–Jackson relation and Fundamental Plane from halo abundance matching

Desmond

2016

Mon. Not. R. Astron. Soc.

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The Fundamental Plane (FP) describes the relation between the stellar mass, size, and velocity dispersion of elliptical galaxies; the Faber-Jackson relation (FJR) is its projection onto {mass, velocity} space. In this work we redeploy and expand the framework of Desmond & Wechsler (2015) to ask whether abundance matching-based ΛCDM models that have shown success in matching the spatial distribution of galaxies are also capable of explaining key properties of the FJR and FP, including their scatter. Within our framework, agreement with the normalisation of the FJR requires haloes to expand in response to disc formation. We find that the tilt of the FP may be explained by a combination of the observed non-homology in galaxy structure and the variation in mass-to-light ratio produced by abundance matching with a universal initial mass function (IMF), provided that the anisotropy of stellar motions is taken into account. However, the predicted scatter around the FP is considerably increased by situating galaxies in cosmologically-motivated haloes due to variations in halo properties at fixed stellar mass, and appears to exceed that of the data. This implies that additional correlations between galaxy and halo variables may be required to fully reconcile these models with elliptical galaxy scaling relations.

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Simulation of Shock Wave-Turbulent Boundary Layer Interactions Using the Reynolds-Averaged Navier-Stokes Equations

Knight

1999

ICASE/LaRC Interdisciplinary Series in Science and Engineering

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3-D crossing shock wave-turbulent boundary layer interaction

Cited by 7 publications

References 9 publications

A giant elliptical galaxy with a lightweight initial mass function★†

A giant elliptical galaxy with a lightweight initial mass function★†

The Faber–Jackson relation and Fundamental Plane from halo abundance matching

Simulation of Shock Wave-Turbulent Boundary Layer Interactions Using the Reynolds-Averaged Navier-Stokes Equations

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