A Study of the Merging Dwarf Galaxy VCC322

Galaxy interactions and mergers can enhance or reduce star formation, but a complete understanding of the involved processes is still lacking. The effect of dwarf galaxy mergers is even less clear than their massive counterpart. We present a study on a dwarf merger remnant in the Virgo cluster, VCC3...

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Veröffentlicht in:The Astrophysical journal Jg. 965; H. 1; S. 3 - 12
Hauptverfasser: Zhang, Lan-Yue, Zhao, Yinghe, Zhang, Hong-Xin
Format: Journal Article
Sprache:Englisch
Veröffentlicht: Philadelphia The American Astronomical Society 01.04.2024
IOP Publishing
Schlagworte:
Astronomical models
Astronomy & Astrophysics
Cold gas
Color
Dwarf galaxies
Emission lines
Galaxy evolution
Galaxy mergers
Galaxy mergers & collisions
Galaxy photometry
Galaxy tails
Metallicity
Sky surveys (astronomy)
Star & galaxy formation
Star formation
Stars
Stellar age
Stellar models
Tidal interaction
Virgo galactic cluster
ISSN:0004-637X, 1538-4357
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Zusammenfassung:Galaxy interactions and mergers can enhance or reduce star formation, but a complete understanding of the involved processes is still lacking. The effect of dwarf galaxy mergers is even less clear than their massive counterpart. We present a study on a dwarf merger remnant in the Virgo cluster, VCC322, which might form a triple system with VCC334 and VCC319. We identify a prominent long and straight tail-like substructure that has a size comparable to its host galaxy VCC322. By comparing the color–color ( g − r versus r − H ) distribution with simple stellar population models, we infer that the metallicity and stellar age of this tail are Z ⋆ ∼ 0.02 Z ⊙ and t ⋆ ∼ 10 Gyr, respectively. In VCC319, we find a sign of isophotal twisting. This suggests that VCC319 may be subject to tidal interaction. An analysis of the Sloan Digital Sky Survey optical spectra of VCC322 indicates mass- and light-weighted ages of about 10 9.8 yr and 10 7.5 yr, respectively, indicating an ongoing star formation activity. However, the star formation in VCC322 seems suppressed when compared to other star-forming dwarfs of comparable stellar masses. Our finding of shock excitation of optical emission lines indicates that interaction-induced shock may contribute to the heating of cold gas and suppression of star formation.
Bibliographie:Galaxies and Cosmology
AAS50565
ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 14
USDOE
AC02-05CH11231
None
ISSN:0004-637X
1538-4357
DOI:10.3847/1538-4357/ad2f2d