Interacting binary galaxies. 7: Kinematic data for 12 disturbed ellipticals

Borne, K. D.; Balcells, M.; Hoessel, John G.; McMaster, Matthew

doi:10.1086/174796

Cited by 15 publications

(9 citation statements)

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“…There is an uncertainty in the absolute wavelength calibration of the HST spectrum. Since we do not assume that the central HST LOSVD is symmetric, we must determine the velocity zeropoint of this profile relative to the rest frame of the galaxy (920 ± 10 km s −1 , Borne et al 1994). Unfortunately, our original observing strategy did not include an accurate wavelength calibration, since we were concerned mainly with the central dispersion, and thus did not obtain the necessary flanking arc-lamp spectra.…”

Section: Model Fitsmentioning

confidence: 99%

Axisymmetric, Three-Integral Models of Galaxies: A Massive Black Hole in NGC 3379

Gebhardt

Richstone

Kormendy

et al. 2000

The Astronomical Journal

236

230

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We fit axisymmetric 3-integral dynamical models to NGC 3379 using the line-of-sight velocity distribution obtained from HST/FOS spectra of the galaxy center and ground-based long-slit spectroscopy along four position angles, with the light distribution constrained by WFPC2 and ground-based images. We have fitted models with inclinations from 29 • (intrinsic galaxy type E5) to 90 • (intrinsic E1) and black hole masses from 0 to 10 9 M ⊙ .The best-fit black hole masses range from 6 × 10 7 − 2 × 10 8 M ⊙ , depending on inclination. The preferred inclination is 90 • (edge-on); however, the constraints on allowed inclination are not very strong due to our assumption of constant M/L V . The velocity ellipsoid of the best model is not consistent with either isotropy or a two-integral distribution function. Along the major axis, the velocity ellipsoid becomes tangential at the innermost bin, radial in the mid-range radii, and tangential again at the outermost bins. The rotation rises quickly at small radii due to the presence of the black hole. For the acceptable models, the radial to tangential ((σ 2 θ + σ 2 φ )/2) dispersion in the mid-range radii ranges from 1.1 < σ r /σ t < 1.7, with the smaller black holes requiring larger radial anisotropy. Compared with these 3-integral models, 2-integral isotropic models overestimate the black hole mass since they cannot provide adequate radial motion. However, the models presented in this paper still contain restrictive assumptions-namely assumptions of constant M/L V and spheroidal symmetry-requiring yet more models to study black hole properties in complete generality.

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Section: Model Fitsmentioning

confidence: 99%

Axisymmetric, Three-Integral Models of Galaxies: A Massive Black Hole in NGC 3379

Gebhardt

Richstone

Kormendy

et al. 2000

The Astronomical Journal

236

230

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“…Por outro lado, ESO 505-IG 031 já oferece um perfil diferenciado, reportado na literatura como U-shaped rotation profile, descrito em estudos envolvendo sistemas gravitacionalmente perturbados [55][56][57][58][59][60]. Este tipo de perfilé comum em galáxias elípticas fortemente interagentes, cuja interpretação física, dada por [61], revela um acoplamento de maré entre aórbita da companheira e as estrelas em rotação prógrada ressonante na galáxia cinematicamente distorcida [56,62,63]. O código de síntese espectral STARLIGHT [64,65]é um programa que modela o representativo da contribuição estelar do espectro observado e fornece um espectro sintetizado que melhor representa os espectros estudados em termos das populações estelares de diferentes idades e metalicidades (uma combinação linear de populações estelares simples, SSPs).…”

Section: Curva De Rotaçãounclassified

Estudo Espectroscópico do Par de Galáxias Interagentes ESO 505-IG 030 e ESO 505-IG 031

Sales¹,

Martin²,

Poppe³

et al. 2020

Sitientibus-Fisica

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Este trabalho apresenta os resultados das observações espectroscópicas de fenda longa realizadas para o par de galáxias peculiares interagentes ESO 505-IG 030 e ESO 505-IG 031. Os dados foram obtidos com o espectrógrafo Cassegrain acoplado ao telescópio Perkin-Elmer (1,60m) do Observatório do Pico dos Dias/Laboratório Nacional de Astrofísica (OPD-LNA/MCTI). Trata-se de um par interagente no Universo local (z $\approx$ 0,03957) classificadas como espirais do tipo morfológico Sc. Curvas de rotação, síntese espectral e alguns parâmetros físicos e geométricos são apresentados e discutidos para cada um dos objetos estudados.

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“…This shape appears on interacting binary-disturbed elliptical galaxies (see Borne 1990;Borne & Hoessel 1985, 1988Bender et al 1991;Madejsky 1991;Madejsky et al 1991). The physical interpretation of Borne et al (1994) is that there is a tidal coupling between the orbit of the companion and the resonant prograde rotating stars in the kinematically disturbed galaxy (Borne 1988;Borne & Hoessel 1988;Bacells et al 1989). This U-shape profile in NED01 is thus direct observational evidence of tidal coupling, hence a direct observational signature of tidal friction in action in this pair of galaxies.…”

Section: Ned01mentioning

confidence: 99%

FM 047-02: a collisional pair of galaxies with a ring

Faúndez-Abans

Oliveira-Abans

Krabbe

et al. 2013

A&A

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Aims. We investigate the nature of the galaxy pair FM 047-02, which has been proposed as an archetype of the Solitaire types of peculiar (collisional) ring galaxies. Methods. The study is based on long-slit spectrophotometric data in the range of 3500-9500 Å obtained with the Gemini Multi-Object Spectrograph at Gemini South (GMOS-S). The absorption spectra were used to determine the radial velocity. The stellar population synthesis code STARLIGHT was used to investigate the star formation history of the galaxy pair FM 047-02. Results. During the whole long-slit signal, the spectra of both galaxies resemble those of an early-type galaxy. Both objects are dominated by an old stellar population of 2 × 10 9 < t ≤ 13 × 10 9 yr and a small, but a non-negligible fraction (about 13%) of young stars of t ≤ 5 × 10 7 yr are estimated to contribute to the optical flux for NED02. Both observed small radial-velocity differences, and the structures around NED01 suggest an ongoing tidal interaction of both galaxies. Conclusions. The spectroscopic results and the morphological peculiarities of NED01 can be adequately interpreted as continuing off-center stage of interaction with the companion galaxy NED02. The core of NED01 and NED02 are in counter-rotating motion. The visual appearance of NED01, its kinematical properties, the smooth distribution of material in the ring, and its off-centered nucleus, characterize it as a true archetype of a Solitaire-type ring galaxy in an advanced stage of ring formation.

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Interacting binary galaxies. 7: Kinematic data for 12 disturbed ellipticals

Cited by 15 publications

References 0 publications

Axisymmetric, Three-Integral Models of Galaxies: A Massive Black Hole in NGC 3379

Axisymmetric, Three-Integral Models of Galaxies: A Massive Black Hole in NGC 3379

Estudo Espectroscópico do Par de Galáxias Interagentes ESO 505-IG 030 e ESO 505-IG 031

FM 047-02: a collisional pair of galaxies with a ring

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