The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Fuentes-Carrera, I.; Rosado, M.; Amram, P.; Dultzin‐Hacyan, D.; Cruz-González, I.; Salo, H.; Laurikainen, Eija; Bernal, Argelia; Ambrocio-Cruz, P.; Coarer, E. Le

doi:10.1051/0004-6361:20034190

Cited by 34 publications

(51 citation statements)

References 48 publications

(74 reference statements)

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“…Here, we show the potential of this type of observations for revealing details about the interaction process, over complete galaxy disks, using Fabry-Perot spectroscopy giving two-dimensional kinematics across a relatively large field. Fabry-Perot observations of interacting galaxies have been reported previously; Rampazzo et al (2005) studied five such systems, while Fuentes-Carrera et al (2004) presented observations of Arp 271, the subject of this Letter, and the same group have carried out more recent work in this field (see, e.g., Repetto et al 2010). In this Letter, we report the results of observations of Arp 271 (NGC 5426 + NGC 5427) using a Fabry-Perot spectrometer.…”

Section: Introductionmentioning

confidence: 73%

Detection of Infalling Hydrogen in Transfer Between the Interacting Galaxies NGC 5426 and NGC 5427

Font¹,

Beckman²,

Rosado³

et al. 2011

ApJ

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Using velocity tagging we have detected hydrogen from NGC 5426 falling onto its interacting partner NGC 5427. Our observations, with the GHaFaS Fabry-Perot spectrometer, produced maps of the two galaxies in Hα surface brightness and radial velocity. We found emission with the range of velocities associated with NGC 5426 along lines of sight apparently emanating from NGC 5427, superposed on the velocity map of the latter. After excluding instrumental effects we assign the anomalous emission to gas pulled from NGC 5426 during its passage close to NGC 5427. Its distribution, more intense between the arms and just outside the disk of NGC 5427, and weak, or absent, in the arms, suggests that the infalling gas is behind the disk, ionized by Lyman continuum photons escaping from NGC 5427. Modeling this, we estimate the distances of these gas clouds behind the plane: a few hundred parsecs to a few kiloparsecs. We also estimate the mass of the infalling (ionized plus neutral) gas, finding an infall rate of 10 M per year, consistent with the high measured star formation rate across the disk of NGC 5427 and with the detected circumnuclear galactic wind.

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Section: Introductionmentioning

confidence: 73%

Detection of Infalling Hydrogen in Transfer Between the Interacting Galaxies NGC 5426 and NGC 5427

Font¹,

Beckman²,

Rosado³

et al. 2011

ApJ

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“…Error bars give the dispersion of the rotation velocities computed for all the pixels found inside each elliptical ring defined by the successive bins. This approach is described in more detail in Fuentes-Carrera et al (2004) and Garrido et al (2005). • .…”

Section: Rotation Curvesmentioning

confidence: 99%

“…Nevertheless, care must be taken when using kinematic information from interacting galaxies, since they are subject to kinematical perturbations that may affect the correct determination of an RC that actually traces the global mass distribution of the galaxy. For this reason, 3D spectroscopy observations are required to separate circular from noncircular motions in the velocity field of a galaxy and its rotation curve as shown in Fuentes-Carrera et al (2004).…”

Section: Introductionmentioning

confidence: 99%

Kinematics and dynamics of the M 51-type galaxy pair NGC 3893/96 (KPG 302)

Fuentes-Carrera

Rosado

Amram

et al. 2007

A&A

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Aims. We study the kinematics and dynamics of the M 51-type interacting galaxy pair KPG 302 (NGC 3893/96). We analyze the perturbations induced by the encounter on each member of the pair, as well as the distribution of the dark matter (DM) halo of the main galaxy in order to explore possible differences between DM halos of "isolated" galaxies and those of galaxies belonging to a pair. Methods. The velocity field of each galaxy was obtained using scanning Fabry-Perot interferometry. A two-dimensional kinematic and dynamical analysis of each galaxy and the pair as a whole are done emphasizing the contribution of circular and non-circular velocities. Non-circular motions can be traced on the rotation curves of each galaxy allowing us to differentiate between motions associated to particular features and motions that reflect the global mass distribution of the galaxy. For the main galaxy of the pair, NGC 3893, optical kinematic information is complemented with HI observations from the literature to build a multi-wavelength rotation curve. We try to fit this curve with a mass-distribution model using different DM halos. Results. Non-circular motions are detected on the velocity fields of both galaxies. These motions can be associated to perturbations due to the encounter and, in the case of the main galaxy, to the presence of a structure such as spiral arms. The location of the corotation radius of this galaxy is also explored. We find that the multi-wavelength rotation curve of NGC 3893, "cleaned" from the effect of non-circular motions, cannot be fitted whether by a pseudo-isothermal or by a NFW DM halo.

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“…This common HI envelope is elongated from SE to NW, parallel to the line that joins the nuclei of both galaxies. The kinematical 260 M. Rosado, R. Gabbasov & I. Fuentes-Carrera analysis derived from the PUMA Fabry-Perot observations has been already published in Fuentes-Carrera et al (2007).…”

Section: Introductionmentioning

confidence: 99%

Numerical Simulations of KPG 302 (NGC 3893/96)

Rosado¹,

Gabbasov²,

Fuentes-Carrera³

2010

Proc. IAU

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Abstract. We present the results of numerical simulations on the M51-type galaxy pair KPG 302 (NGC 3893/96) taking as boundary conditions for these simulations the results of our observations on the kinematics of this pair. The observations allow us to deduce the different components of each galaxy in the pair (stellar disk and bulge, dark matter halo) as well as the geometry of the encounter at the present time. The numerical simulations were carried out using GADGET2 numerical code including gas. We describe in detail how the numerical simulations are being done. We succeeded to reproduce the actual conditions of the pair, in particular, the granddesign spiral arms of NGC 3893 (the main galaxy of the pair) when the numerical simulations include gas, consider a parabolic direct collision and multiple passages.

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The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Cited by 34 publications

References 48 publications

Detection of Infalling Hydrogen in Transfer Between the Interacting Galaxies NGC 5426 and NGC 5427

Detection of Infalling Hydrogen in Transfer Between the Interacting Galaxies NGC 5426 and NGC 5427

Kinematics and dynamics of the M 51-type galaxy pair NGC 3893/96 (KPG 302)

Numerical Simulations of KPG 302 (NGC 3893/96)

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