J. Kormendy - Academia.edu (original) (raw)
Papers by J. Kormendy
Dark Matter: Key Issues.- Dark Matter in the Galactic Disk.- Extreme M Dwarfs and Brown Dwarfs in... more Dark Matter: Key Issues.- Dark Matter in the Galactic Disk.- Extreme M Dwarfs and Brown Dwarfs in A Deep CCD Survey.- Kinematics of the Galactic Inner Spheroid.- Relatively Dark Matter: The Local Mass Density of Stellar Remnants.- The Dynamics of Open Clusters 35.- Seen and Unseen Matter in the Galactic Disc.- Kinematics of Nearby FV Stars.- The Local Galactic Escape Velocity.- Constraints on the Dark Matter from Optical Rotation Curves.- Differences in Mass Distribution for Field and Cluster Spiral Galaxies 66.- HI Rotation Curves of Galaxies.- Kinematics and Warp in NGC 4565.- Mass/Luminosity Ratios from Rotation of HI IN SO Galaxies.- Mass Determinations and Dark Matter at Intermediate Scales.- The Mass of the Binary Galaxies NGC 4038/39 (The "Antennae").- Radial Velocities of Remote Globular Clusters.- The Trouble with Binary Galaxies.- Evidence for Dark Matter in Galactic Systems.- Galaxy Luminosity Functions, M/L Ratios, and Closure of the Universe.- About the Coma C...
We present a set of structural parameters for the central parts of 57 early-type galaxies observe... more We present a set of structural parameters for the central parts of 57 early-type galaxies observed with the Planetary Camera of the Hubble Space Telescope. These parameters are based on a new empirical law that successfully characterizes the centers of early type galaxies. This empirical law assumes that the surface brightness profile is a combination of two power laws with different slopes gamma and beta for the inner and outer regions. Conventional structural parameters such as core radius and central surface brightness are replaced by break radius r_b, where the transition between power-law slopes takes place, and surface brightness mu_b at that radius. An additional parameter alpha describes the sharpness of the break. The structural parameters are derived using a chi-squared minimization process applied to the mean surface brightness profiles. The resulting model profiles generally give very good agreement to the observed profiles out to the radius of 10 arcseconds imaged by th...
Symposium - International Astronomical Union, 1996
This report has two major purposes. First, we summarize here work by our team on the determinatio... more This report has two major purposes. First, we summarize here work by our team on the determination of the density of stars near the centers of a large sample of galaxies observed with the Hubble Space Telescope. There appear to be two varieties of elliptical galaxies (and bulges). The stellar densities near the centers of small elliptical galaxies exceed those of globular clusters and the density of the universe at the recombination epoch. The radial dependence of density and implied gravitational force seems inconsistent (at least in the case of the smaller elliptical galaxies) with a long-lived triaxial configuration. It therefore seems likely that the central regions of less luminous elliptical galaxies are axisymmetric. For the more luminous ellipticals, the central densities are far more modest and the presence of a distinct core (defined below) is generally well established. Even in these cases, however, we find few if any galaxies with analytic (Taylor expandable) stellar den...
Proceedings of SPIE - The International Society for Optical Engineering
ABSTRACT
Virtually all massive galaxies, including our own, host central black holes ranging in mass from ... more Virtually all massive galaxies, including our own, host central black holes ranging in mass from millions to billions of solar masses. The growth of these black holes releases vast amounts of energy that powers quasars and other weaker active galactic nuclei. A tiny fraction of this energy, if absorbed by the host galaxy, could halt star formation by heating and ejecting ambient gas. A central question in galaxy evolution is the degree to which this process has caused the decline of star formation in large elliptical galaxies, which typically have little cold gas and few young stars, unlike spiral galaxies.
Black holes, an extreme consequence of the mathematics of General Relativity, have long been susp... more Black holes, an extreme consequence of the mathematics of General Relativity, have long been suspected of being the prime movers of quasars, which emit more energy than any other objects in the Universe. Recent evidence indicates that supermassive black holes, which are probably quasar remnants, reside at the centers of most galaxies. As our knowledge of the demographics of these relics of a violent earlier Universe improve, we see tantalizing clues that they participated intimately in the formation of galaxies and have strongly influenced their present–day structure.
Annual Review of Astronomy and Astrophysics, 1995
Arxiv preprint astro-ph/ …, 2004
Proceedings of the International Astronomical Union
The oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier sp... more The oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier speakers at this Symposium worried that selection effects bias the derivation of black hole scaling relations. I therefore added – and this proceedings paper emphasizes – a discussion of why we can be confident that selection effects do not bias the observed correlations between BH mass M• and the luminosity, stellar mass, and velocity dispersion of host ellipticals and classical bulges. These are the only galaxy components that show tight BH-host correlations. The scatter plots of M• with host properties for pseudobulges and disks are upper envelopes of scatter that does extend to lower BH masses. BH correlations are most consistent with a picture in which BHs coevolve only with classical bulges and ellipticals. Four physical regimes of coevolution (or not) are suggested by Kormendy & Ho 2013 and are summarized here.
International Astronomical Union Colloquium
Nous présentons une méthode de mesure des distances des galaxies elliptiques basée sur une relati... more Nous présentons une méthode de mesure des distances des galaxies elliptiques basée sur une relation entre la brillance superficielle et un rayon déduit de la distribution spatiale de l’intensité de lumière émise. Nous confrontons ensuite les distances calculées à partir de la vitesse pour 11 galaxies de l’amas de la Vierge, avec celles de 8 objets de plus grand décalage spectral pour la plupart. Ceci implique que l’amas de la Vierge est à une distance plus faible que celle donnée par sa vitesse:, résultat négatif confirmant la conclusion de Sandage et Tammann (1974, 1975), à savoir la non existence d’une vitesse particulière de l’amas de la Vierge.
AIP Conference Proceedings, 1992
Astron J, 1998
This paper is a study of the mass distribution in the central 35&... more This paper is a study of the mass distribution in the central 35" ~= 1.7 kpc of the E5 galaxy NGC 3377. Stellar rotation velocity and velocity dispersion profiles (seeing sigma_* = 0.20"-0.56") and V-band surface photometry (sigma_* = 0.20"-0.26") have been obtained with the Canada-France-Hawaii Telescope. NGC 3377 is kinematically similar to M32: the central kinematic gradients are steep.
Bulletin of the American Astronomical Society, May 1, 2000
Vizier Online Data Catalog, Nov 1, 2009
Dark Matter: Key Issues.- Dark Matter in the Galactic Disk.- Extreme M Dwarfs and Brown Dwarfs in... more Dark Matter: Key Issues.- Dark Matter in the Galactic Disk.- Extreme M Dwarfs and Brown Dwarfs in A Deep CCD Survey.- Kinematics of the Galactic Inner Spheroid.- Relatively Dark Matter: The Local Mass Density of Stellar Remnants.- The Dynamics of Open Clusters 35.- Seen and Unseen Matter in the Galactic Disc.- Kinematics of Nearby FV Stars.- The Local Galactic Escape Velocity.- Constraints on the Dark Matter from Optical Rotation Curves.- Differences in Mass Distribution for Field and Cluster Spiral Galaxies 66.- HI Rotation Curves of Galaxies.- Kinematics and Warp in NGC 4565.- Mass/Luminosity Ratios from Rotation of HI IN SO Galaxies.- Mass Determinations and Dark Matter at Intermediate Scales.- The Mass of the Binary Galaxies NGC 4038/39 (The "Antennae").- Radial Velocities of Remote Globular Clusters.- The Trouble with Binary Galaxies.- Evidence for Dark Matter in Galactic Systems.- Galaxy Luminosity Functions, M/L Ratios, and Closure of the Universe.- About the Coma C...
We present a set of structural parameters for the central parts of 57 early-type galaxies observe... more We present a set of structural parameters for the central parts of 57 early-type galaxies observed with the Planetary Camera of the Hubble Space Telescope. These parameters are based on a new empirical law that successfully characterizes the centers of early type galaxies. This empirical law assumes that the surface brightness profile is a combination of two power laws with different slopes gamma and beta for the inner and outer regions. Conventional structural parameters such as core radius and central surface brightness are replaced by break radius r_b, where the transition between power-law slopes takes place, and surface brightness mu_b at that radius. An additional parameter alpha describes the sharpness of the break. The structural parameters are derived using a chi-squared minimization process applied to the mean surface brightness profiles. The resulting model profiles generally give very good agreement to the observed profiles out to the radius of 10 arcseconds imaged by th...
Symposium - International Astronomical Union, 1996
This report has two major purposes. First, we summarize here work by our team on the determinatio... more This report has two major purposes. First, we summarize here work by our team on the determination of the density of stars near the centers of a large sample of galaxies observed with the Hubble Space Telescope. There appear to be two varieties of elliptical galaxies (and bulges). The stellar densities near the centers of small elliptical galaxies exceed those of globular clusters and the density of the universe at the recombination epoch. The radial dependence of density and implied gravitational force seems inconsistent (at least in the case of the smaller elliptical galaxies) with a long-lived triaxial configuration. It therefore seems likely that the central regions of less luminous elliptical galaxies are axisymmetric. For the more luminous ellipticals, the central densities are far more modest and the presence of a distinct core (defined below) is generally well established. Even in these cases, however, we find few if any galaxies with analytic (Taylor expandable) stellar den...
Proceedings of SPIE - The International Society for Optical Engineering
ABSTRACT
Virtually all massive galaxies, including our own, host central black holes ranging in mass from ... more Virtually all massive galaxies, including our own, host central black holes ranging in mass from millions to billions of solar masses. The growth of these black holes releases vast amounts of energy that powers quasars and other weaker active galactic nuclei. A tiny fraction of this energy, if absorbed by the host galaxy, could halt star formation by heating and ejecting ambient gas. A central question in galaxy evolution is the degree to which this process has caused the decline of star formation in large elliptical galaxies, which typically have little cold gas and few young stars, unlike spiral galaxies.
Black holes, an extreme consequence of the mathematics of General Relativity, have long been susp... more Black holes, an extreme consequence of the mathematics of General Relativity, have long been suspected of being the prime movers of quasars, which emit more energy than any other objects in the Universe. Recent evidence indicates that supermassive black holes, which are probably quasar remnants, reside at the centers of most galaxies. As our knowledge of the demographics of these relics of a violent earlier Universe improve, we see tantalizing clues that they participated intimately in the formation of galaxies and have strongly influenced their present–day structure.
Annual Review of Astronomy and Astrophysics, 1995
Arxiv preprint astro-ph/ …, 2004
Proceedings of the International Astronomical Union
The oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier sp... more The oral version of this paper summarized Kormendy & Ho 2013, ARA&A, 51, 511. However, earlier speakers at this Symposium worried that selection effects bias the derivation of black hole scaling relations. I therefore added – and this proceedings paper emphasizes – a discussion of why we can be confident that selection effects do not bias the observed correlations between BH mass M• and the luminosity, stellar mass, and velocity dispersion of host ellipticals and classical bulges. These are the only galaxy components that show tight BH-host correlations. The scatter plots of M• with host properties for pseudobulges and disks are upper envelopes of scatter that does extend to lower BH masses. BH correlations are most consistent with a picture in which BHs coevolve only with classical bulges and ellipticals. Four physical regimes of coevolution (or not) are suggested by Kormendy & Ho 2013 and are summarized here.
International Astronomical Union Colloquium
Nous présentons une méthode de mesure des distances des galaxies elliptiques basée sur une relati... more Nous présentons une méthode de mesure des distances des galaxies elliptiques basée sur une relation entre la brillance superficielle et un rayon déduit de la distribution spatiale de l’intensité de lumière émise. Nous confrontons ensuite les distances calculées à partir de la vitesse pour 11 galaxies de l’amas de la Vierge, avec celles de 8 objets de plus grand décalage spectral pour la plupart. Ceci implique que l’amas de la Vierge est à une distance plus faible que celle donnée par sa vitesse:, résultat négatif confirmant la conclusion de Sandage et Tammann (1974, 1975), à savoir la non existence d’une vitesse particulière de l’amas de la Vierge.
AIP Conference Proceedings, 1992
Astron J, 1998
This paper is a study of the mass distribution in the central 35&... more This paper is a study of the mass distribution in the central 35" ~= 1.7 kpc of the E5 galaxy NGC 3377. Stellar rotation velocity and velocity dispersion profiles (seeing sigma_* = 0.20"-0.56") and V-band surface photometry (sigma_* = 0.20"-0.26") have been obtained with the Canada-France-Hawaii Telescope. NGC 3377 is kinematically similar to M32: the central kinematic gradients are steep.
Bulletin of the American Astronomical Society, May 1, 2000
Vizier Online Data Catalog, Nov 1, 2009