Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure

Diemand, Juerg; Kuhlen, M.; Madau, Piero

doi:10.1086/520573

Cited by 578 publications

(792 citation statements)

References 62 publications

(119 reference statements)

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“…Second, we can ground our estimate in recent theoretical works that study the population of dwarfs as satellites of the Milky Way (Reed et al, 2005;Diemand et al, 2007;Springel et al, 2008). These simulations suggest that the number of satellites per halo has the following form:…”

Section: Massive Black Holes In Low-mass and Dwarf Galaxiesmentioning

confidence: 72%

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Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

758

707

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Evidence shows that massive black holes reside in most local galaxies. Studies have also established a number of relations between the MBH mass and properties of the host galaxy such as bulge mass and velocity dispersion. These results suggest that central MBHs, while much less massive than the host (∼ 0.1%), are linked to the evolution of galactic structure. In hierarchical cosmologies, a single big galaxy today can be traced back to the stage when it was split up in hundreds of smaller components. Did MBH seeds form with the same efficiency in small proto-galaxies, or did their formation had to await the buildup of substantial galaxies with deeper potential wells? I briefly review here some of the physical processes that are conducive to the evolution of the massive black hole population. I will discuss black hole formation processes for 'seed' black holes that are likely to place at early cosmic epochs, and possible observational tests of these scenarios.

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Section: Massive Black Holes In Low-mass and Dwarf Galaxiesmentioning

confidence: 72%

“…According to Diemand et al (2007), N * = 0.021 and α = −3, while Springel et al (2008) find N * = 0.052 and α = −3.15. If we extrapolate the M BH − σ correlation to MBH masses (10 2 -10 3 M ), and assume an isothermal galaxy, then v sat ∼ 10-20 km s −1 .…”

Section: Massive Black Holes In Low-mass and Dwarf Galaxiesmentioning

confidence: 99%

Formation of supermassive black holes

Volonteri

2010

Astron Astrophys Rev

758

707

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“…Such pseudo-evolution of dark matter halos has been investigated by several groups, and a consistent finding in numerical simulations is that most halos of M h < ∼ 10 12 M completed matter accretion by z ∼ 1 with little/no net growth in mass over the last seven billion years (e.g. Prada et al 2006;Diemand et al 2007;Diemer et al 2013). Therefore, applying an R h normalization may impose a pseudo-evolution in the properties of galaxies residing in these low-mass halos.…”

Section: Uncertainties Due To Pseudo-evolution Of Halomentioning

confidence: 85%

Mining circumgalactic baryons in the low-redshift universe

Liang

Chen

2014

Monthly Notices of the Royal Astronomical Society

140

229

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This paper presents an absorption-line study of the multiphase circumgalactic medium (CGM) based on observations of Lyα, C II, C IV, Si II, Si III, and Si IV absorption transitions in the vicinities of 195 galaxies at redshift z < 0.176. The galaxy sample is established based on a cross-comparison between public galaxy and QSO survey data and is characterized by a median redshift of z = 0.041, a median projected distance of d = 362 kpc to the sightline of the background QSO, and a median stellar mass of log (M star /M ) = 9.7 ± 1.1. Comparing the absorber features identified in the QSO spectra with known galaxy properties has led to strong constraints for the CGM absorption properties at z < ∼ 0.176. First, abundant hydrogen gas is observed out to d ∼ 500 kpc, well beyond the dark matter halo radius R h of individual galaxies, with a mean covering fraction of ≈ 60%. In contrast, no heavy elements are detected at d > ∼ 0.7 R h from either low-mass dwarfs or high-mass galaxies. The lack of detected heavy elements in low-and high-ionization states suggests that either there exists a chemical enrichment edge at d ≈ 0.7 R h or gaseous clumps giving rise to the observed absorption lines cannot survive at these large distances. Considering all galaxies at d > R h leads to a strict upper limit for the covering fraction of heavy elements of ≈ 3% (at a 95% confidence level) over d = (1 − 9) R h . At d < R h , differential covering fraction between low-and high-ionization gas is observed, suggesting that the CGM becomes progressively more ionized from d < 0.3 R h to larger distances. Comparing CGM absorption observations at low and high redshifts shows that at a fixed-fraction of R h the CGM exhibits stronger mean absorption at z = 2.2 than at z ∼ 0 and that the distinction is most pronounced in low-ionization species traced by C II and Si II absorption lines. We discuss possible pseudo-evolution of the CGM as a result of misrepresentation of halo radius, and present a brief discussion on the implications of these findings.

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“…Computing the marginalized evidence involved integrating over the multidimensional parameter space within predefined priors. In particular, we assumed that the substructure was equally likely to be located at any point in the lens plane and to have a mass between 4.0 × 10 6 M ⊙ and 4.0 × 10 9 M ⊙ , the mass range where comparison with simulations was possible 13,14 . See Supplementary Information for further details on the Bayesian evidence.…”

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confidence: 99%

Gravitational detection of a low-mass dark satellite galaxy at cosmological distance

Vegetti

Lagattuta

McKean

et al. 2012

Nature

358

392

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The mass-function of dwarf satellite galaxies that are observed around Local Group galaxies substantially differs from simulations 1-5 based on cold dark matter: the simulations predict many more dwarf galaxies than are seen. The Local Group, however, may be anomalous in this regard 6, 7 . A massive dark satellite in an early-type lens galaxy at z = 0.222 was recently found 8 using a new method based on gravitational lensing 9, 10 , suggesting that the mass fraction contained in substructure could be higher than is predicted from simulations. The lack of very low mass detections, however, prohibited any constraint on their mass function. Here we report the presence of a 1.9 ± 0.1 × 10 8 M ⊙ dark satellite in the Einstein-ring system JVAS B1938+666 (ref. 11) at z = 0.881, where M ⊙ denotes solar mass. This satellite galaxy has a mass similar to the Sagittarius 12 galaxy, which is a satellite of the Milky Way. We determine the logarithmic slope of the mass function for substructure beyond the local Universe to be α = 1.1 +0.6 −0.4 , with an average mass-fraction of f = 3.3 +3.6 −1.8 %, by combining data on both of these recently discovered galaxies. Our results are consistent with the predictions from cold dark matter simulations 13-15 at the 95 per cent confidence level,and therefore agree with the view that galaxies formed hierarchically in a Universe composed of cold dark matter.The gravitational lens system JVAS B1938+666 (ref. 11) has a bright infrared background galaxy at redshift 2.059 (ref. 16), which is gravitationally lensed into an almost complete Einstein ring of diameter ∼ 0.9 arcseconds by a massive elliptical galaxy at redshift 0. 881 (ref. 17). The bright, highly-magnified Einstein ring made this system an excellent candidate in which to to search for surface brightness anomalies caused by very low mass (dark matter) substructure in the halo around the high redshift elliptical lens galaxy. The presence of a low-mass substructure (e.g. a luminous or dark satellite galaxy; also denoted as substructure hereafter) in the lens galaxy 1

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Formation and Evolution of Galaxy Dark Matter Halos and Their Substructure

Cited by 578 publications

References 62 publications

Formation of supermassive black holes

Formation of supermassive black holes

Mining circumgalactic baryons in the low-redshift universe

Gravitational detection of a low-mass dark satellite galaxy at cosmological distance

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