Molecular line emission in NGC 4945, imaged with ALMA

C. Henkel, S. Mühle, G. Bendo, G. I.G. Józsa, Y. Gong, S. Viti, S. Aalto, F. Combes, S. García-Burillo, L. K. Hunt, J. Mangum, S. Martín, S. Muller, J. Ott, P. Van Der Werf, A. A. Malawi, H. Ismail, E. Alkhuja, H. M. Asiri, R. AladroF. Alves, Y. Ao, W. A. Baan, F. Costagliola, G. Fuller, J. Greene, C. M.V. Impellizzeri, F. Kamali, R. S. Klessen, R. Mauersberger, X. D. Tang, K. Tristram, M. Wang, J. S. Zhang

Research output: Contribution to journalArticle

9 Scopus citations

Abstract

NGC 4945 is one of the nearest (D ≈ 3.8 Mpc; 100 ≈ 19 pc) starburst galaxies. To investigate the structure, dynamics, and composition of the dense nuclear gas of this galaxy, ALMA band 3 (λ ≈ 3−4 mm) observations were carried out with ≈200 resolution. Three HCN and two HC+ isotopologues, CS, C3H2, SiO, HCO, and CH3C2H were measured. Spectral line imaging demonstrates the presence of a rotating nuclear disk of projected size 1000 × 200 reaching out to a galactocentric radius of r ≈ 100 pc with position angle PA = 45 ± 2, inclination i = 75 ± 2 and an unresolved bright central core of size<200. The continuum source, representing mostly free-free radiation from star forming regions, is more compact than the nuclear disk by a linear factor of two but shows the same position angle and is centered 000 . 39 ± 000 . 14 northeast of the nuclear accretion disk defined by H2O maser emission. Near the systemic velocity but outside the nuclear disk, both HCN J = 1 → 0 and CS J = 2 → 1 delineate molecular arms of length>1500 (>285 pc) on opposite sides of the dynamical center. These are connected by a (deprojected) ≈ 0.6 kpc sized molecular bridge, likely a dense gaseous bar seen almost ends-on, shifting gas from the front and back side into the nuclear disk. Modeling this nuclear disk located farther inside (r<100 pc) with tilted rings provides a good fit by inferring a coplanar outflow reaching a characteristic deprojected velocity of ≈50 km s−1. All our molecular lines, with the notable exception of CH3C2H, show significant absorption near the systemic velocity (≈571 km s−1), within the range ≈500-660 km s−1. Apparently, only molecular transitions with low critical H2 density (ncrit< 104 cm−3) do not show absorption. The velocity field of the nuclear disk, derived from CH3C2H, provides evidence for rigid rotation in the inner few arcseconds and a dynamical mass of Mtot = (2.1 ± 0.2) × 108 M inside a galactocentric radius of 200 . 45 (≈45 pc), with a significantly flattened rotation curve farther out. Velocity integrated line intensity maps with most pronounced absorption show molecular peak positions up to ≈100 . 5 (≈30 pc) southwest of the continuum peak, presumably due to absorption, which appears to be most severe slightly northeast of the nuclear maser disk. A nitrogen isotope ratio of14N/15N ≈ 200-450 is estimated. This range of values is much higher then previously reported on a tentative basis. Therefore, because15N is less abundant than expected, the question for strong15N enrichment by massive star ejecta in starbursts still remains to be settled.

Original languageEnglish (US)
Article numberA155
JournalAstronomy and Astrophysics
Volume615
DOIs
StatePublished - 2018

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Keywords

  • Abundances
  • Galaxies: ISM
  • Galaxies: individual: NGC4945
  • Galaxies: starburst
  • Galaxies: structure
  • Nuclear reactions
  • Nucleosynthesis
  • Radio lines: ISM

Fingerprint Dive into the research topics of 'Molecular line emission in NGC 4945, imaged with ALMA'. Together they form a unique fingerprint.

  • Cite this

    Henkel, C., Mühle, S., Bendo, G., Józsa, G. I. G., Gong, Y., Viti, S., Aalto, S., Combes, F., García-Burillo, S., Hunt, L. K., Mangum, J., Martín, S., Muller, S., Ott, J., Van Der Werf, P., Malawi, A. A., Ismail, H., Alkhuja, E., Asiri, H. M., ... Zhang, J. S. (2018). Molecular line emission in NGC 4945, imaged with ALMA. Astronomy and Astrophysics, 615, [A155]. https://doi.org/10.1051/0004-6361/201732174