Coevolution of Black Holes and Galaxies

By P. Martini. 2004

209 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/6cc57a9bf56d4a25e865a26204a636e31324b809

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Citations in the corpus

A Concise Reference to (Projected) Sérsic R 1/n Quantities, Including Concentration, Profile Slopes, Petrosian Indices, and Kron Magnitudes (2005, methodology): “Thus, at constant (R/Re), γ is a monotonically increasing function of the Sérsic index n (Graham et al. 2003b).”
STRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES (2008, background): “Therefore, when ellipticals or bulges that satisfy the core parameters correlations merge, this tends to destroy the correlations (Kormendy 1993; Faber et al. 1997).”
A Log-Quadratic Relation for Predicting Supermassive Black Hole Masses from the Host Bulge Sérsic Index (2006, methodology): “A discussion of the original galaxy light-profiles can be found in Erwin et al. (2002), see also Trujillo et al.”
The unresolved hard X-ray background: the missing source population implied by the Chandra and XMM-Newton deep fields (2004, methodology): “We have used a similar calculation to Fabian & Iwasawa (1999) although note that the bolometric correction is ∼10–15 for our lower luminosity objects (Fabian 2004).”
NEW LIMITS ON AN INTERMEDIATE-MASS BLACK HOLE IN OMEGA CENTAURI. I. HUBBLE SPACE TELESCOPE PHOTOMETRY AND PROPER MOTIONS (2009, result): “These results are not surprising, given the long half-mass relaxation time of ∼ 10 years (McLaughlin & van der Marel 2005). Omega Cen has long been known to have multiple stellar populations. The proper-motion catalog we have constructed here has enabled us to look for variations in kinematics betwe”
Massive Black Holes in Star Clusters. II. Realistic Cluster Models (2004, methodology): “If 10% of all globular clusters contain IMBHs, extragalactic globular clusters could be one of the major sources of gravitational wave events for LISA.”
Formation of Massive Black Holes in Dense Star Clusters. I. Mass Segregation and Core Collapse (2003, background): “Our preliminary results from MC simulations including a realistic treatment of stellar collisions (Rasio et al. 2003) indicate that the formation of a very massive star through runaway collisions is a likely outcome.”
A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids (2005, background): “The range spanned in the figure corresponds well to the range of quasar lifetimes implied by the observations above and others (Martini 2004, and references therein), but this figure provides a more direct means to compare with future observations which better constrain the quasar lifetime Given…”
Massive Black Hole Binary Evolution (2004, background): “Weak cusps may be remnants of strong cusps that were destroyed by binary SBHs during galaxy mergers; in fact the structure and kinematics of galactic nuclei are now believed to be fossil relics of the merger process [135].”
Massive star formation: nurture, not nature (2004, background): “Key words: stars: formation – stars: luminosity function, mass function – globular clusters and associations: general.”