Unusual displacement of H <scp>i</scp> due to tidal interaction in Arp 181

Sengupta, Chandreyee; Dwarakanath, K. S.; Saikia, D. J.; Scott, T. C.

doi:10.1093/mnrasl/sls039

Cited by 14 publications

(18 citation statements)

References 23 publications

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“…Accepting the limitations of claims that can be made using the currently available data, we find that the Arp 305 Bridge TDG differs from our previous TDG H i detections in Arp 202 and Arp 181 (Sengupta et al 2014(Sengupta et al , 2013 in having Spitzer 3.6 µm and 4.5 µm counterparts, indicative of an old stellar component. Additionally, Arp 305 TDG has strong UV emission indicating recent SF.…”

Section: Arp 305 Bridge Tdg Candidatecontrasting

confidence: 81%

HI, star formation and tidal dwarf candidate in the Arp 305 system

Sengupta,

Scott,

Paudel

et al. 2017

Preprint

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We present results from our Giant Metrewave Radio Telescope (GMRT) H i observations of the Arp 305 system. The system consists of two interacting spiral galaxies NGC 4016 and NGC 4017, a large amount of resultant tidal debris and a prominent tidal dwarf galaxy (TDG) candidate projected within the tidal bridge between the two principal galaxies. Our higher resolution GMRT H i mapping, compared to previous observations, allowed detailed study of smaller scale features. Our H i analysis supports the conclusion in Hancock et al. (2009) that the most recent encounter between the pair occurred ∼ 4 × 10 8 yrs ago. The GMRT observations also show H i features near NGC 4017 which may be remnants of an earlier encounter between the two galaxies. The H i properties of the Bridge TDG candidate include: M HI ∼ 6.6 × 10 8 M ⊙ and V HI = 3500± 7km s −1 , which is in good agreement with the velocities of the parent galaxies. Additionally the TDG's H i linewidth of 30 km s −1 and modest velocity gradient together with its SFR of 0.2 M ⊙ yr −1 add to the evidence favouring the bridge candidate being a genuine TDG. The Bridge TDG's Spitzer 3.6 µm and 4.5 µm counterparts with a [3.6]-[4.5] colour ∼ -0.2 mag suggests stellar debris may have seeded its formation. Future spectroscopic observations could confirm this formation scenario and provide the metallicity which is a key criteria for the validation for TDG candidates.

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Section: Arp 305 Bridge Tdg Candidatecontrasting

confidence: 81%

HI, star formation and tidal dwarf candidate in the Arp 305 system

Sengupta,

Scott,

Paudel

et al. 2017

Preprint

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“…Arp 65 belongs to a small number of galaxy pairs where the highest density H i is observed beyond the optical disks of the pair following an interaction (e.g. Hibbard & van Gorkom 1996;Sengupta et al 2013). We found that NGC 90 has extended on-going star formation in the outer optical disk, most likely triggered by interaction.…”

Section: Star Formation In the Tidal Debrismentioning

confidence: 68%

“…Some other examples are NGC 3921 (Hibbard & van Gorkom 1996), Arp 105 (Duc et al 1997) and Arp 181 (Sengupta et al 2013). • and inclination = 34.5…”

Section: Evidence Of An Interaction Between Ngc 90 and Ngc 93mentioning

confidence: 99%

Arp 65 interaction debris: massive H I displacement and star formation

Sengupta

Scott

Paudel

et al. 2015

A&A

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Context. Pre-merger tidal interactions between pairs of galaxies are known to induce significant changes in the morphologies and kinematics of the stellar and interstellar medium components. Large amounts of gas and stars are often found to be disturbed or displaced as tidal debris. This debris then evolves, sometimes forming stars and occasionally forming tidal dwarf galaxies. Here we present results from our H i study of Arp 65, an interacting pair hosting extended H i tidal debris.Aims. In an effort to understand the evolution of tidal debris produced by interacting pairs of galaxies, including in situ star and tidal dwarf galaxy formation, we are mapping H i in a sample of interacting galaxy pairs. The Arp 65 pair is the latest member of this sample to be mapped. Methods.Our resolved H i 21 cm line survey is being carried out using the Giant Metrewave Radio Telescope. We used our H i survey data as well as available SDSS optical, Spitzer infra-red and GALEX UV data to study the evolution of the tidal debris and the correlation of H i with the star-forming regions within it.Results. In Arp 65 we see a high impact pre-merger tidal interaction involving a pair of massive galaxies (NGC 90 and NGC 93) that have a stellar mass ratio of ∼1:3. The interaction, which probably occurred ∼1.0-2.5 × 10 8 yr ago, appears to have displaced a large fraction of the H i in NGC 90 (including the highest column density H i) beyond its optical disk. We also find extended on-going star formation in the outer disk of NGC 90. In the major star-forming regions, we find the H i column densities to be ∼4.7 × 10 20 cm −2 or lower. But no signature of star formation was found in the highest column density H i debris SE of NGC 90. This indicates conditions within the highest density H i debris remain hostile to star formation and it reaffirms that high H i column densities may be a necessary but not sufficient criterion for star formation.

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“…Other details are per Figure A1. large fractions of an interacting pair's H i beyond their optical disks (Sengupta et al 2013(Sengupta et al , 2015, but in this case the companion is much less massive and the ∼800 km s −1 velocity separation (Consolandi et al 2017) suggests a high velocity low impact encounter.…”

Section: Discussionmentioning

confidence: 96%

Abell 1367: a high fraction of late-type galaxies displaying H i morphological and kinematic perturbations

Scott

Brinks

Cortese

et al. 2018

Monthly Notices of the Royal Astronomical Society

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To investigate the effects the cluster environment has on Late-Type Galaxies (LTGs) we studied HI perturbation signatures for all Abell 1367 LTGs with HI detections. We used new VLA H i observations combined with AGES single dish blind survey data. Our study indicates that the asymmetry between the high-and low-velocity wings of the characteristic double-horn integrated H i spectrum as measured by the asymmetry parameter, A flux , can be a useful diagnostic for ongoing and/or recent HI stripping. 26% of A1367 LTGs have an A flux ratio, more asymmetrical than 3 times the 1σ spread in the A flux ratio distribution of an undisturbed sample of isolated galaxies (2%) and samples from other denser environments (10% to 20%). Over half of the A 1367 LTGs, which are members of groups or pairs, have an A flux ratio larger than twice the 1 σ spread found in the isolated sample. This suggests inter-group/pair interactions could be making a significant contribution to the LTGs displaying such A flux ratios. The study also demonstrates that the definition of the H i offset from the optical centre of LTGs is resolution dependent, suggesting that unresolved AGES H i offsets that are significantly larger than the pointing uncertainties (> 2 σ) reflect interactions which have asymmetrically displaced significant masses of lower density H i, while having minimal impact on the location of the highest density HI in resolved maps. The distribution of A flux from a comparable sample of Virgo galaxies provides a clear indication that the frequency of H i profile perturbations is lower than in A 1367.

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Unusual displacement of H i due to tidal interaction in Arp 181

Cited by 14 publications

References 23 publications

HI, star formation and tidal dwarf candidate in the Arp 305 system

HI, star formation and tidal dwarf candidate in the Arp 305 system

Arp 65 interaction debris: massive H I displacement and star formation

Abell 1367: a high fraction of late-type galaxies displaying H i morphological and kinematic perturbations

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