Interacting galaxy NGC4656 and its unusual dwarf companion

Засов, А. В.; Saburova, Anna S.; Egorov, Oleg V.; Уклеин, Р. И.

doi:10.1093/mnras/stx1158

Cited by 11 publications

(18 citation statements)

References 28 publications

(37 reference statements)

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“…This paper continues the series of spectral observations of tidal debris in the interacting galaxies (Arp 270, Arp 194, NGC 4656, see Zasov et al 2015Zasov et al , 2016Zasov et al , 2017. Here we present the results of optical long-slit spectral observations of NGC4017 and TDG carried out at the 6m telescope BTA at the SAO RAS observatory.…”

Section: Introductionmentioning

confidence: 63%

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Young stellar clumps in the interacting system Arp 305

Засов

Saburova

Egorov

et al. 2018

Monthly Notices of the Royal Astronomical Society

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We present the results of optical long-slit spectral observations of interacting system Arp305 carried out at the 6m telescope BTA at the SAO RAS: the radial variation of gas kinematics and oxygen abundance. This study continues the series of spectral observations of tidal debris in the interacting galaxies. Here we pay special attention to the star-forming region between the interacting galaxies -a tidal dwarf galaxy (TDG) candidate. This star-forming system appears to be gravitationally bound or close to this condition. We show that TDG is metal poor in comparison to the parental galaxy. It can indicate that either the origin of star-forming gas of TDG was very far from the centre of parent galaxy or its gas has been diluted by the accretion of metal poor intergalactic gas. Nevertheless the region of the brightest emission clump in TDG where a current star formation takes place reveals a noticeable colour excess evidencing a local gas concentration. We pay attention that TDG is situated in the region of intersection of two gas flows and is in a process of formation probably caused by the collision of these flows. Low velocity difference between TDG, NGC 4017 and the gaseous bridge between them evidences that the lifetime of TDG is restricted by the time of its fall back onto the parent galaxy.

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Section: Introductionmentioning

confidence: 63%

“…We performed the data reduction in a similar way as in the previous papers Zasov et al (2015Zasov et al ( , 2016Zasov et al ( , 2017. Here we utilized the based spectral data reduction pipeline.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Young stellar clumps in the interacting system Arp 305

Засов

Saburova

Egorov

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…In this paper we continue to describe the results of spectral observations at the 6m telescope BTA of Special Astrophysical Observatory of disturbed galaxies with local regions of star formation in the periphery of discs or in the intergalactic space which we started in Zasov et al (2015Zasov et al ( , 2016Zasov et al ( , 2017Zasov et al ( , 2018. Here we focus on the three Arp systems Arp 42, Arp 82, and Arp 58.…”

Section: Introductionmentioning

confidence: 98%

Spectral observations of the systems with the disturbed spiral arms: Arp 42, Arp 82, and Arp 58

Засов

Saburova

Egorov

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We study three Arp' systems of peculiar galaxies: Arp 42 (NGC 5829), Arp 82 (NGC 2535/36) and Arp 58 (UGC 4457), using the long-slit spectral observations carried out at the 6m telescope BTA of Special Astrophysical Observatory. Arp 82 and Arp 58 are the M51-type systems. In the third system -Arp 42, there are two extremely luminous kpc-sized clumps observed at the ends of the bifurcated spiral arm, however the source of perturbations remains unknown. From the emission line measurements we analyzed the distribution of gas line-ofsight (LOS) velocity, velocity dispersion and gas-phase metallicity along the slits estimated by different methods. A special attention is paid to the young regions of star formation at the peripheries of the galaxies and in tidal debris, their connection with gas kinematics and abundance. All three systems show the signs of velocity disturbances and the presence of regions of locally enhanced gas velocity dispersion, as well as the regions of diffuse ionized gas. A distribution of oxygen reveals shallow radial abundance gradients, typical for interacting systems. A faint spiral-like branches of tidal bridges which are observed in NGC 2535 and UGC 4457 may represent the remnants of pre-existing "old" mode of spiral waves.

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“…The dIrr companion of the spiral galaxy NGC 4656 with MB = −16.6 mag and the coordinates J124415.7+321700. Internal motions in this galaxy were studied by Zasov et al (2017).…”

mentioning

confidence: 99%

Local Volume Late-Type Galaxies with an Extreme Ratio of $Hα$-to-$FUV$ Star-Formation Rates

Karachentsev,

Kaisina,

Kaisin

2021

Preprint

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Using a currently most representative sample of 477 late-type galaxies within 11 Mpc of the Milky Way with measured star-formation rates (SF Rs) from the far ultraviolet (F U V ) and Hα emission line fluxes, we select galaxies with the extreme ratios: SF R(Hα)/SF R(F U V ) > 2 and SF R(Hα)/SF R(F U V ) < 1/20. Each subsample amounts to ∼ 5% of the total number and consists of dwarf galaxies with the stellar masses M * /M ⊙ = (5.5 − 9.5) dex. In spite of a huge difference in their SF R(Hα) activity on a scale of ∼ 10 Myr, the temporarily "excited" and temporarily "quiescent" galaxies follow one and the same relation between SF R(F U V ) and M * on a scale of ∼ 100 Myr. Their average specific star-formation rate log[SF R(F U V )/M * ] = −10.1 ± 0.1 (yr −1 ) coinsides with the Hubble parameter log(H 0 ) = −10.14 (yr −1 ). On a scale of t ∼ 10 Myr, variations of SF R have a moderate flash amplitude of less than 1 order above the main-sequence and a fading amplitude to 2 orders below the average level. In general, both temporarily excited and temporarily quiescent galaxies have almost similar gas fractions as normal main-sequence galaxies, being able to maintain the current rate of star-formation on another Hubble time scale. Ranging the galaxies according to the density contrast produced by the nearest massive neighbor exhibits only a low average excess of SF R caused by tidal interactions.

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Interacting galaxy NGC4656 and its unusual dwarf companion

Cited by 11 publications

References 28 publications

Young stellar clumps in the interacting system Arp 305

Young stellar clumps in the interacting system Arp 305

Spectral observations of the systems with the disturbed spiral arms: Arp 42, Arp 82, and Arp 58

Local Volume Late-Type Galaxies with an Extreme Ratio of $Hα$-to-$FUV$ Star-Formation Rates

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