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  • Aalto, Susanne,1964Chalmers tekniska högskola,Chalmers University of Technology (författare)

ALMA resolves the remarkable molecular jet and rotating wind in the extremely radio-quiet galaxy NGC 1377

  • Artikel/kapitelEngelska2020

Förlag, utgivningsår, omfång ...

  • 2020-08-21
  • EDP Sciences,2020
  • electronicrdacarrier

Nummerbeteckningar

  • LIBRIS-ID:oai:research.chalmers.se:ca667122-4498-43a7-afb4-533c565fe40c
  • https://research.chalmers.se/publication/519178URI
  • https://doi.org/10.1051/0004-6361/202038282DOI
  • https://research.chalmers.se/publication/519637URI

Kompletterande språkuppgifter

  • Språk:engelska
  • Sammanfattning på:engelska

Ingår i deldatabas

Klassifikation

  • Ämneskategori:art swepub-publicationtype
  • Ämneskategori:ref swepub-contenttype

Anmärkningar

  • Submillimetre and millimetre line and continuum observations are important in probing the morphology, column density, and dynamics of the molecular gas and dust around obscured active galactic nuclei (AGNs) and their mechanical feedback. With very high-resolution (0.'' 02x0.'' 03 (2x3 pc)) ALMA 345 GHz observations of CO 3-2, HCO+ 4-3, vibrationally excited HCN 4-3 nu (2)=1f, and continuum we have studied the remarkable, extremely radio-quiet, molecular jet and wind of the lenticular galaxy NGC 1377. The outflow structure is resolved, revealing a 150 pc long, clumpy, high-velocity (similar to 600 km s(-1)), collimated molecular jet where the molecular emission is emerging from the spine of the jet with an average diameter of 3-7 pc. The jet widens to 10-15 pc about 25 pc from the centre, which is possibly due to jet-wind interactions. A narrow-angle (50 degrees -70 degrees), misaligned and rotating molecular wind surrounds the jet, and both are enveloped by a larger-scale CO-emitting structure at near-systemic velocity. The jet and narrow wind have steep radial gas excitation gradients and appear turbulent with high gas dispersion (sigma> 40 km s(-1)). The jet shows velocity reversals that we propose are caused by precession, or more episodic directional changes. We discuss the mechanisms powering the outflow, and we find that an important process for the molecular jet and narrow wind is likely magneto-centrifugal driving. In contrast, the large-scale CO-envelope may be a slow wind, or cocoon that stems from jet-wind interactions. An asymmetric, nuclear r similar to 2 pc dust structure with a high inferred molecular column density N(H-2) similar or equal to 1.8x10(24) cm(-2) is detected in continuum and also shows compact emission from vibrationally excited HCN. The nuclear dust emission is hot (T-d> 180 K) and its luminosity is likely powered by a buried AGN. The lopsided structure appears to be a warped disk, which is responsible for a significant part of the nuclear obscuration and possibly formed as a result of uneven gas inflows. The dynamical mass inside r=1.4 pc is estimated to 9(-3)(+2) x 10(6)M(circle dot) 9 - 3 + 2 x 10 6 M circle dot , implying that the supermassive black hole (SMBH) has a high mass with respect to the stellar velocity dispersion of NGC 1377. We suggest that the SMBH of NGC 1377 is currently in a state of moderate growth, at the end of a more intense phase of accretion and also evolving from a state of more extreme nuclear obscuration. The nuclear growth may be fuelled by low-angular momentum gas inflowing from the gas ejected in the molecular jet and wind. Such a feedback-loop of cyclic outflows and central accretion could explain why there is still a significant reservoir of molecular gas in this ageing, lenticular galaxy. A feedback-loop would be an effective process in growing the nuclear SMBH and thus would constitute an important phase in the evolution of NGC 1377. This also invites new questions as to SMBH growth processes in obscured, dusty galaxies.

Ämnesord och genrebeteckningar

Biuppslag (personer, institutioner, konferenser, titlar ...)

  • Falstad, Niklas,1987Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)falstad (författare)
  • Muller, Sebastien,1976Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)mullers (författare)
  • Wada, K.Kagoshima University (författare)
  • Gallagher, J. S.University of Wisconsin Madison (författare)
  • König, Sabine,1983Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)ksabine (författare)
  • Sakamoto, K.Academia Sinica Taiwan (författare)
  • Vlemmings, Wouter,1974Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)wouterv (författare)
  • Ceccobello, Chiara,1984Chalmers tekniska högskola,Chalmers University of Technology(Swepub:cth)chiarac (författare)
  • Dasyra, K.University of Athens (författare)
  • Combes, F.Sorbonne Université,Sorbonne University (författare)
  • Garcia-Burillo, S.Observatorio Astronómico Nacional (OAN),Spanish National Observatory (OAN) (författare)
  • Oya, Y.University of Tokyo, Japan (författare)
  • Martin, S.Atacama Large Millimeter-submillimeter Array (ALMA),European Southern Observatory Santiago (författare)
  • van der Werf, P.Universiteit Leiden (UL),Leiden University (UL) (författare)
  • Evans, A. S.University of Virginia,National Radio Astronomy Observatory (författare)
  • Kotilainen, J.Turun Yliopisto,University of Turku (författare)
  • Chalmers tekniska högskolaKagoshima University (creator_code:org_t)

Sammanhörande titlar

  • Ingår i:Astronomy and Astrophysics: EDP Sciences6400004-63611432-0746

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