Show simple item record

dc.contributor.authorWu, Yu-Ting
dc.contributor.authorTrejo, Alfonso
dc.contributor.authorEspada Fernández, Daniel 
dc.contributor.authorMiyamoto, Yusuke
dc.identifier.citationYu-Ting Wu... [et al.]. Morphological and kinematical analysis of the double-barred galaxy NGC 3504 using ALMA CO (2–1) data, Monthly Notices of the Royal Astronomical Society, Volume 504, Issue 3, July 2021, Pages 3111–3127, []es_ES
dc.descriptionThis paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00650.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic ofKorea), in cooperationwith theRepublic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. The authors are grateful to Krajnovi ' c et al. for the Kinemetry code. The authors thank the referee, Prof. JeffreyKenney, for valuable comments and suggestions that improved this paper. The authors also thank the support of the Astronomical Data Center of the National Astronomical Observatory of Japan, and Anthony Moraghan for assistance on the computational facilities and resources at Academia Sinica Institute of Astronomy and Astrophysics (ASIAA). DE acknowledges support from a Beatriz Galindo senior fellowship (BG20/00224) from the SpanishMinistry of Science and Innovation. YTW wishes to thank Dr. Yu-Nung Su and Dr. Sheng-Yuan Liu for hosting her visit at ASIAA in 2020.es_ES
dc.description.abstractWe present results obtained from ALMA CO (2–1) data of the double-barred galaxy NGC3504.With three times higher angular resolution (∼0. 8) than previous studies, our observations reveal an inner molecular gas bar, a nuclear ring, and four inner spiral arm-like structures in the central 1-kpc region. Furthermore, the CO emission is clearly aligned with the two dust lanes in the outer bar region, with differences in shape and intensity between them. The total molecular gas mass in the observed region (50 arcsec×57 arcsec) is estimated to be∼3.1 × 109M , which is 17 per cent of the stellarmass.We used the Kinemetry package to fit the velocity field and found that circular motion strongly dominates at R = 0.3–0.8 kpc, but radial motion becomes important at R < 0.3 kpc and R = 1.0–2.5 kpc, which is expected due to the presence of the inner and outer bars. Finally, assuming that the gas moves along the dust lanes in the bar rotating frame, we derived the pattern speed of the outer bar to be 18 ± 5 kms−1 kpc−1, the average streaming velocities on each of the two dust lanes to be 165 and 221 km s−1, and the total mass inflow rate along the dust lanes to be 12M yr−1. Our results give a new example of an inner gas bar within a gas-rich double-barred galaxy and suggest that the formation of double-barred galaxies could be associated with the existence of such gas structures.es_ES
dc.description.sponsorshipSpanish Government BG20/00224es_ES
dc.publisherOxford University Presses_ES
dc.rightsAtribución-NoComercial-SinDerivadas 3.0 España*
dc.subjectMethods: observationales_ES
dc.subjectGalaxies: kinematics and dynamicses_ES
dc.subjectGalaxies: structurees_ES
dc.subjectRadio lines: galaxieses_ES
dc.titleMorphological and kinematical analysis of the double-barred galaxy NGC3504 using ALMA CO (2–1) dataes_ES

Files in this item


This item appears in the following Collection(s)

Show simple item record

Atribución-NoComercial-SinDerivadas 3.0 España
Except where otherwise noted, this item's license is described as Atribución-NoComercial-SinDerivadas 3.0 España