Finite thin disc models of four galaxies in the Ursa Major cluster: NGC 3877, NGC 3917, NGC 3949 and NGC 4010

González, Guillermo; Plata-Plata, Sandra M.; Ramos-Caro, Javier

doi:10.1111/j.1365-2966.2010.16303.x

Cited by 12 publications

(15 citation statements)

References 12 publications

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“…Pedraza, Ramos-Caro & González (2008) study a family of axisymmetric flat models of generalized Kalnajs type which give satisfactory behavior of the rotational curves without the assumption of a dark matter halo. González, Plata & Ramos-Caro (2010) start from the observational data of four galaxies and construct models with the corresponding densities and potentials. The effects of relativistic corrections are studied in (Ramos-Caro, Agn & Pedraza 2012, Nguyen & Lingam 2013, and a model motivated by renormalization group corrections is investigated in (Rodrigues, Letelier & Shapiro 2010).…”

Section: Introductionmentioning

confidence: 99%

On the rotation curves for axially symmetric disc solutions of the Vlasov–Poisson system

Andréasson¹,

Rein²

2014

Monthly Notices of the Royal Astronomical Society

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A large class of flat axially symmetric solutions to the VlasovPoisson system is constructed with the property that the corresponding rotation curves are approximately flat, slightly decreasing or slightly increasing. The rotation curves are compared with measurements from real galaxies and satisfactory agreement is obtained. These facts raise the question whether the observed rotation curves for disk galaxies may be explained without introducing dark matter. Furthermore, it is shown that for the ansatz we consider stars on circular orbits do not exist in the neighborhood of the boundary of the steady state.

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Section: Introductionmentioning

confidence: 99%

On the rotation curves for axially symmetric disc solutions of the Vlasov–Poisson system

Andréasson¹,

Rein²

2014

Monthly Notices of the Royal Astronomical Society

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“…By means of the nonlinear least square fitting, the analytical velocity curves were adjusted to the observed ones of three specific spiral galaxies: NGC 3726, NGC 3877 and NGC 4010. The resulting analytical models were used to determine the mass-density distributions and the vertical and epicyclic frequencies, showing that unlike the results presented in González et al (2010) for NGC 3877 and NGC 4010, our models satisfy the stability conditions for radial and vertical perturbations. Even though the set of models presented here should be considered as a rough approximation, the circular velocities were shown to fit very accurately to the observed rotation curves and in the three cases the stability conditions were fully satisfied.…”

Section: Discussionmentioning

confidence: 72%

“…The observational data were taken from Verheijen & Sancisi (2001) for three specific galaxies in the Ursa Major cluster: NGC 3726, NGC 3877 and NGC 4010. Following the procedure outlined in González et al (2010), we take the galaxy radius R d as the given by the largest tabulated value of the data. Thus, (6), we get the well-known Miyamoto-Nagai Potential (Miyamoto & Nagai, 1975).…”

Section: Rotation Curves Fittingmentioning

confidence: 99%

Orbital dynamics in realistic galaxy models: NGC 3726, NGC 3877 and NGC 4010

Dubeibe

Martínez-Sicachá

González

2019

Rev. Acad. Colomb. Cienc. Ex. Fis. Nat.

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In the present paper, using a generalization of the Miyamoto and Nagai potential we adjusted the observed rotation curves of three specific spiral galaxies to the analytical circular velocities. The observational data have been taken from a 21 cm-line synthesis imaging survey using the Westerbork Synthesis Radio Telescope, for three particular galaxies in the Ursa Major cluster: NGC 3726, NGC 3877 and NGC 4010. Accordingly, the dynamics of the system is analyzed in terms of the Poincaré sections method, finding that for larger values of the angular momentum of the test particle or lower values its total energy the dynamics is mainly regular, while on the opposite cases, the dynamics is mainly chaotic. Our toy model opens the possibility to find chaotic bounded orbits for stars in those particular galaxies.Dinámica orbital en modelos realistas de galáxias: NGC 3726, NGC 3877 y NGC 4010 ResumenEn el presente trabajo, utilizando una generalización del potencial de Miyamoto-Nagai, se ajustan las curvas de rotación observadas de tres galaxias espirales a las velocidades circulares analíticas. Los datos observacionales se tomaron de un conjunto de imágenes de línea de 21 centímetros (o línea HI) obtenidos con el Westerbork Synthesis Radio Telescope (WSRT), para tres galaxias particulares en el grupo de la Ursa Major: NGC 3726, NGC 3877 y NGC 4010. Seguidamente, se analiza la dinámica del sistema en términos del método de secciones de Poincaré, encontrando que para valores grandes del momento angular de la partícula de prueba o valores bajos su energía total, la dinámica es principalmente regular, mientras que en los casos opuestos, la dinámica es principalmente caótica. Nuestro modelo abre la posibilidad de encontrarórbitas caóticas acotadas para estrellas presentes en esas galaxias particulares.Palabras clave: Dinámica estelar, Galaxias: cinemática y dinámica, Dinámica no lineal y caos.

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“…So, we will adjust these constants in such a way that the circular velocity v 2 c ( R) fits with the data of the rotation curve of some particular galaxy. As expression (33) for the circular velocity only involves derivatives of the Legendre polynomials of even order, it can be written as the rotation law (González, Plata-Plata and Ramos-Caro, 2010)…”

Section: Obtaining Particular Modelsmentioning

confidence: 99%

Analytical potentials for flat galaxies with spheroidal halos

González

Reina

2016

Rev. Acad. Colomb. Cienc. Ex. Fis. Nat.

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A family of analytical potential-density pairs for flat galaxies with spheroidal halos is presented. The potential are obtained by means of the sum of two independent terms: a potential associated with a thin disc and a potential associated with a spheroidal halo, which are expressed as appropriated superpositions of products of Legendre functions, in such a way that the model implies a linear relationship between the masses of the thin disc and the spheroidal halo. By taking a particular case for the halo potential, we found that the circular velocity obtained can be adjusted very accurately to the observed rotation curves of some specific galaxies, so that the models are stable against radial and vertical perturbations. Two particular models for the galaxies NGC4389 and UGC6969 are obtained by adjusting the circular velocity with data of the observed rotation curve of some galaxies of the Ursa Mayor Cluster, as reported in Verheijen and Sancisi (2001). The values of the halo mass and the disc mass for these two galaxies are computed obtaining a very narrow interval of values for these quantities. Furthermore, the values of obtained masses are in perfect agreement with the expected order of magnitude and with the relative order of magnitude between the halo mass and the disc mass. © 2016. Acad. Colomb. Cienc. Ex. Fis. Nat.Key words: Potential Theory; Disk Galaxies; Celestial Mechanics; Galactic Mass. Potenciales analíticos para galaxias planas con halos esferoidales ResumenSe presenta una familia de pares analíticos potencial-densidad para galaxias planas con halos esferoidales. Los potenciales son obtenidos por medio de la suma de dos términos independientes: un potencial asociado al disco delgado y un potencial asociado al halo esferoidal, los cuales son expresados apropiadamente como la superposición de productos de funciones de Legendre, de tal manera que el modelo implica una relación lineal entre las masas del disco delgado y el halo esferoidal. Tomando un caso particular para el potencial del halo, encontramos que la velocidad circular obtenida puede ser ajustada muy precisamente con la curva de rotación de algunas galaxias específicas, de tal manera que los modelos son estables contra perturbaciones radiales y verticales. Dos modelos particulares para las galaxias NGC4389 y UGC6969 son obtenidos ajustando la velocidad circular del modelo con datos de la curva de rotación observada de algunas galaxias del Cluster de la Osa Mayor, reportados en Verheijen and Sancisi (2001). Los valores de la masa del halo y la masa del disco para estas dos galaxias son calculados obteniendo un intervalo muy estrecho de valores para dichas cantidades. Además, los valores de masa aquí obtenidos están en perfecto acuerdo con el orden de magnitud esperado y con el orden de magnitud relativo entre la masa del halo y la masa del disco.

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Finite thin disc models of four galaxies in the Ursa Major cluster: NGC 3877, NGC 3917, NGC 3949 and NGC 4010

Cited by 12 publications

References 12 publications

On the rotation curves for axially symmetric disc solutions of the Vlasov–Poisson system

On the rotation curves for axially symmetric disc solutions of the Vlasov–Poisson system

Orbital dynamics in realistic galaxy models: NGC 3726, NGC 3877 and NGC 4010

Analytical potentials for flat galaxies with spheroidal halos

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