Show simple item record

Files in this item


Item metadata

dc.contributor.authorChen, Guangwen
dc.contributor.authorWu, Xufen
dc.contributor.authorKong, Xu
dc.contributor.authorLiu, Wen-Juan
dc.contributor.authorZhao, HongSheng
dc.identifier.citationChen , G , Wu , X , Kong , X , Liu , W-J & Zhao , H 2018 , ' Ring galaxies through off-center minor collisions by tuning bulge-to-disk mass ratio of progenitors ' , Astrophysical Journal , vol. 864 , no. 1 , 72 .
dc.identifier.otherPURE: 256011680
dc.identifier.otherPURE UUID: d7cd884d-47ac-4548-8789-49510976fb51
dc.identifier.otherBibtex: urn:19986f87675fe4aecae4096d766178e9
dc.identifier.otherScopus: 85053156745
dc.identifier.otherWOS: 000443244200023
dc.descriptionThis work is supported by the National Natural Science Foundation of China (NSFC 11503025, 11421303), Anhui Natural Science Foundation under grant 1708085MA20 and "the Fundamental Research Funds for the Central Universities." X.W. thanks the additional support provided by "Hundred Talents Project of Anhui Province." X.K. and G.C. are supported by the National Key R&D Program of China (2015CB857004, 2017YFA0402600), and the National Natural Science Foundation of China (NSFC, Nos. 11320101002, 11421303, and 11433005). G.C. thanks the support from the "Fund for Fostering Talents in Basic Science of the National Natural Science Foundation of China NO.J1310021." W.L. acknowledges the support from the Natural Science Foundation of China grant (NSFC 11703079) and the "Light of West China" Program of Chinese Academy of Sciences (CAS).en
dc.description.abstractCollisional ring galaxies (CRGs) are formed through off-center collisions between a target galaxy and an intruder dwarf galaxy. We study the mass distribution and kinematics of CRGs by tuning the bulge-to-disk mass ratio (B/D) for the progenitor; i.e., the target galaxy. We find that the lifetime of the ring correlates with the initial impact velocity vertical to the disk plane (i.e., vz0). Three orbits for the collisional galaxy pair, on which clear and asymmetric rings form after collisions, are selected to perform the N -body simulations at different values of B/D for the progenitor. It is found that the ring structures are the strongest for CRGs with small values of B/D . The Sérsic index, n , of the central remnant in the target galaxy becomes larger after collision. Moreover, the Sérsic index of a central remnant strongly correlates with the initial value of B/D for the progenitor. A bulge-less progenitor results in a late-type object in the center of the ring galaxy, whereas a bulge-dominated progenitor leads to an early-type central remnant. Progenitors with B/D ∈ [0.1, 0.3] (i.e., minor bulges) leave central remnants with n  ≈ 4. These results provide a possible explanation for the formation of a recently observed CRG with an early-type central nucleus, SDSS J1634+2049. In addition, we find that the radial and azimuthal velocity profiles for a ring galaxy are more sensitive to the B/D than the initial relative velocity of the progenitor.
dc.relation.ispartofAstrophysical Journalen
dc.rights© 2018. The American Astronomical Society. All rights reserved. This work is made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at:
dc.subjectGalaxies: evolutionen
dc.subjectGalaxies: generalen
dc.subjectGalaxies: interactionsen
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleRing galaxies through off-center minor collisions by tuning bulge-to-disk mass ratio of progenitorsen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.description.statusPeer revieweden

This item appears in the following Collection(s)

Show simple item record