Methanol masers in NGC 253 with ALCHEMI
Artikel i vetenskaplig tidskrift, 2022

Context. Methanol masers of Class I (collisionally pumped) and Class II (radiatively pumped) have been studied in great detail in our Galaxy in a variety of astrophysical environments such as shocks and star-forming regions and are they are helpful to analyze the properties of the dense interstellar medium. However, the study of methanol masers in external galaxies is still in its infancy.
Aims. Our main goal is to search for methanol masers in the central molecular zone (CMZ; inner 500 pc) of the nearby starburst galaxy NGC253. Methods. Covering a frequency range between 84 and 373 GHz (λ = 3.6-0.8 mm) at high angular (1."6 ∼ 27 pc) and spectral (∼8-9 km s-1) resolution with ALCHEMI (ALMA Comprehensive High-resolution Extragalactic Molecular Inventory), we have probed dierent regions across the CMZ of NGC253. In order to look for methanol maser candidates, we employed the rotation diagram method and a set of radiative transfer models. Results.We detect for the first time masers above 84 GHz in NGC253, covering an ample portion of the J-1 (J-1)0-E line series (at 84, 132, 229, and 278 GHz) and the J0 (J-1)1 A series (at 95, 146, and 198 GHz). This confirms the presence of the Class I maser line at 84 GHz, which was already reported, but now being detected in more than one location. For the J-1 (J-1)0-E line series, we observe a lack of Class I maser candidates in the central star-forming disk.
Conclusions. The physical conditions for maser excitation in the J-1 (J-1)0-E line series can be weak shocks and cloud-cloud collisions as suggested by shock tracers (SiO and HNCO) in bi-symmetric shock regions located in the outskirts of the CMZ. On the other hand, the presence of photodissociation regions due to a high star-formation rate would be needed to explain the lack of Class I masers in the very central regions.

Galaxies: Starburst

Masers

Submillimeter: Galaxies

Radio lines: Galaxies

Galaxies: Spiral

Författare

Pedro Humire

Max-Planck-Gesellschaft

C. Henkel

Max-Planck-Gesellschaft

Chinese Academy of Sciences

King Abdulaziz University

A. Hernández-Gómez

Max-Planck-Gesellschaft

S. Martin

European Southern Observatory Santiago

Atacama Large Millimeter-submillimeter Array (ALMA)

J. G. Mangum

National Radio Astronomy Observatory

N. Harada

The Graduate University for Advanced Studies (SOKENDAI)

National Astronomical Observatory of Japan

Academia Sinica

Sebastien Muller

Chalmers, Rymd-, geo- och miljövetenskap, Onsala rymdobservatorium

K. Sakamoto

Academia Sinica

Kunihiko Tanaka

Keio University

Y. Yoshimura

University of Tokyo

Kouichiro Nakanishi

National Astronomical Observatory of Japan

The Graduate University for Advanced Studies (SOKENDAI)

S. Muhle

Universität Bonn

R. Herrero-Illana

European Southern Observatory Santiago

Institut de Ciències de l'Espai (ICE) - CSIC

D. S. Meier

New Mexico Institute of Mining and Technology

National Radio Astronomy Observatory Socorro

E. Caux

Universite Paul Sabatier Toulouse III

Rebeca Aladro

Max-Planck-Gesellschaft

R. Mauersberger

Max-Planck-Gesellschaft

Serena Viti

University College London (UCL)

Universiteit Leiden

L. Colzi

Centro de Astrobiologia (CAB)

Víctor M. Rivilla

Centro de Astrobiologia (CAB)

Mark Gorski

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik

K. Menten

Max-Planck-Gesellschaft

K. Y. Huang

Universiteit Leiden

Susanne Aalto

Chalmers, Rymd-, geo- och miljövetenskap, Astronomi och plasmafysik

P. van der Werf

Universiteit Leiden

K.L. Emig

National Radio Astronomy Observatory

Astronomy and Astrophysics

0004-6361 (ISSN) 1432-0746 (eISSN)

Vol. 663 A33

Ämneskategorier

Meteorologi och atmosfärforskning

Astronomi, astrofysik och kosmologi

Atom- och molekylfysik och optik

DOI

10.1051/0004-6361/202243384

Mer information

Senast uppdaterat

2022-07-26