KUG 0200-096: Dwarf Antennae Hosting a Tidal Dwarf Galaxy

Paudel, Sanjaya; Sengupta, Chandreyee; Yoon, Suk-Jin

doi:10.3847/1538-3881/aadb8d

Cited by 5 publications

(4 citation statements)

References 57 publications

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“…Pearson et al (2016) further showed that gas-rich dwarf pairs have more extended atomic gas distribution than unpaired analogues. In addition, case studies of several more star-forming dwarf pairs have been carried out recently (Annibali et al 2016;Privon et al 2017;Paudel & Sengupta 2017b;Paudel et al 2018b;Makarova et al 2018;Johnston et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf–Dwarf Merging

Zhang

Paudel

Smith

et al. 2020

ApJL

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It has long been speculated that many starburst or compact dwarf galaxies are resulted from dwarfdwarf galaxy merging, but unequivocal evidence for this possibility has rarely been reported in the literature. We present the first study of deep optical broadband images of a gas-dominated blue compact dwarf galaxy (BCD) VCC848 (M 2×10 8 M ) which hosts extended stellar shells and thus is confirmed to be a dwarf-dwarf merger. VCC848 is located in the outskirts of the Virgo Cluster. By analyzing the stellar light distribution, we found that VCC848 is the result of a merging between two dwarf galaxies with a primary-to-secondary mass ratio 5 for the stellar components and 2 for the presumed dark matter halos. The secondary progenitor galaxy has been almost entirely disrupted. The age-mass distribution of photometrically selected star cluster candidates in VCC848 implies that the cluster formation rate (CFR, ∝ star formation rate) was enhanced by a factor of ∼ 7 − 10 during the past ∼ 1 Gyr. The merging-induced enhancement of CFR peaked near the galactic center a few hundred Myr ago and has started declining in the last few tens of Myr. The current star formation activities, as traced by the youngest clusters, mainly occur at large galactocentric distances ( 1 kpc). The fact that VCC848 is still (atomic) gas-dominated after the period of most violent collision suggests that gas-rich dwarf galaxy merging can result in BCD-like remnants with extended atomic gas distribution surrounding a blue compact center, in general agreement with previous numerical simulations.

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Section: Introductionmentioning

confidence: 99%

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf–Dwarf Merging

Zhang

Paudel

Smith

et al. 2020

ApJL

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“…sjyoon0691@yonsei.ac.kr (SJY) Massive galaxy mergers have been studied in great detail in both observation and numerical simulations (Barnes 1992;Naab & Ostriker 2009;Duc et al 2011). The dwarf-dwarf interactions, on the other hand, are only starting to be explored as a population (Stierwalt et al 2015;Pearson et al 2016;Besla et al 2018;Paudel et al 2018a). This is partly because such systems are possibly not common in the local universe or they are fainter, which makes them harder to detect.…”

Section: Introductionmentioning

confidence: 99%

“…While dwarf-dwarf mergers were expected to be more common in early universe (Klimentowski et al 2010;Fitts et al 2018), recent observations have shown that they are also present in current epoch. The interaction between dwarf galaxies in isolated environments are frequently reported, however they are rare around massive host (Stierwalt et al 2015;Paudel et al 2018a;Kado-Fong et al 2019).…”

Section: Introductionmentioning

confidence: 99%

MCG+07-20-052: Interacting Dwarf Pair in a Group Environment

Paudel

Sengupta

Yoon³

et al. 2020

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We present an observational study of the interacting pair of dwarf galaxies, MCG+07-20-052 , in the vicinity of Milky Way mass spiral galaxy NGC 2998. MCG+07-20-052 is located at a sky-projected distance of 105 kpc from NGC 2998 and the two have a relative line-of-sight velocity of 60 km s −1 . We observed tidal tail-like extensions on both members (D1 and D2) of the interacting pair MCG+07-20-052 . The interacting dwarf galaxies, D1 and D2, have B-band absolute magnitudes of −17.17 and −17.14 mag, respectively, and D2 is significantly bluer than D1. We obtained HI 21 cm line data of the NGC 2998 system using the Giant Metrewave Radio Telescope (GMRT) to get a more detailed view of the neutral hydrogen (HI) emission in the interacting dwarf galaxies and in the galaxy members of the NGC 2998 group. Evidence of a merger between the dwarf galaxies in the MCG+07-20-052 is also present in the HI kinematics and morphology where we find that the HI is mostly concentrated around D2, which also shows a higher level of star-forming activity and bluer g − r color index compared to D1. In addition, we detect extended tenuous HI emission around another member galaxy, NGC 3006, located close to the MCG+07-20-052 -pair at a sky-projected distance of 41 kpc. We compare here our results from the MCG+07-20-052 pair-NGC 2998 system with other known LMC-SMC-Milky Way type systems and discuss the possible origin of the dwarf-dwarf interaction.

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“…Kado-Fong et al (2020) found that 15%-20% of nearby dwarf galaxies with extreme starburst activities show signs of tidal debris. In addition to the above relatively systematic studies, a few more case studies of gas-rich dwarf pairs have also been carried out (Annibali et al 2016;Privon et al 2017;Paudel & Sengupta 2017b;Paudel et al 2018b;Makarova et al 2018;Johnston et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf-Dwarf Merging: HI Gas, Star Formation and Numerical Simulations

Zhang,

Smith,

et al. 2020

Preprint

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A clear link between a dwarf-dwarf merger event and enhanced star formation (SF) in the recent past was recently identified in the gas-dominated merger remnant VCC 848, offering by far the clearest view of a gas-rich late-stage dwarf-dwarf merger. We present a joint analysis of JVLA H i emission-line mapping, optical imaging and numerical simulations of VCC 848, in order to examine the impact of the merger on the stellar and gaseous distributions. VCC 848 has less than 30% of its H i gas concentrated within the central high-surface-brightness star-forming region, while the remaining H i is entrained in outlying tidal features. Particularly, a well-defined tidal arm reaches N (H i) comparable to the galaxy center but lacks SF. The molecular gas mass inferred from the current SF rate (SFR) dominates over the atomic gas mass in the central ∼ 1.5 kpc. VCC 848 is consistent with being a main-sequence starforming galaxy for its current stellar mass and SFR. The H ii region luminosity distribution largely agrees with that of normal dwarf irregulars with similar luminosities, except that the brightest H ii region is extraordinarily luminous. Our N -body/hydrodynamical simulations imply that VCC 848 is a merger between a gas-dominated primary progenitor and a gas-bearing star-dominated secondary. The progenitors had their first passage on a near-radial non-coplanar orbit more than 1 Gyr ago. The merger did not build up a core as compact as typical compact dwarfs with centralized starburst, which may be partly ascribed to the star-dominated nature of the secondary, and in a general sense, a negative stellar feedback following intense starbursts triggered at early stages of the merger.

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KUG 0200-096: Dwarf Antennae Hosting a Tidal Dwarf Galaxy

Cited by 5 publications

References 57 publications

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf–Dwarf Merging

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf–Dwarf Merging

MCG+07-20-052: Interacting Dwarf Pair in a Group Environment

The Blue Compact Dwarf Galaxy VCC 848 Formed by Dwarf-Dwarf Merging: HI Gas, Star Formation and Numerical Simulations

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