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Paper   IPM / Astronomy / 16926
School of Astronomy
  Title:   Exploring the millimetre emission in nearby galaxies: analysis of the edge-on galaxy NGC 891
1.  S. Katsioli
2.  R. Adam
3.  P. Ade
4.  H. Ajeddig
5.  P. Andre
6.  E. Artis
7.  H. Aussel
8.  A. Beelen
9.  A. Benoit
10.  S. Berta
11.  L. Bing
12.  O. Bourrion
13.  M. Calvo
14.  A. Catalano
15.  I. De Looze
16.  M. De Petris
17.  F.-X. Desert
18.  S. Doyle
19.  E. F. C. Driessen
20.  G. Ejlali
21.  M. Galametz
22.  F. Galliano
23.  A. Gomez
24.  J. Goupy
25.  A. P. Jones
26.  A. Hughes
27.  F. Keruzore
28.  C. Kramer
29.  B. Ladjelate
30.  G. Lagache
31.  S. Leclercq
32.  J.-F. Lestrade
33.  J.-F. Macias-Perez
34.  S. C. Madden
35.  A. Maury
36.  P. Mauskopf
37.  F. Mayet
38.  A. Monfardini
39.  M. Munoz-Echeverrla
40.  A. Nersesian
41.  L. Perotto
42.  G. Pisano
43.  N. Ponthieu
44.  V. Reveret
45.  A. J. Rigby
46.  A. Ritacco
47.  C. Romero
48.  H. Roussel
49.  F. Ruppin
50.  K. Schuster
51.  S. Shu
52.  A. Sievers
53.  M. W. L. Smith
54.  F. Tabatabaei
55.  C. Tucker
56.  E. M. Xilouris
57.  R. Zylka
  Status:   Published
  Journal: EPJ
  Vol.:  257
  Year:  2022
  Supported by:            ipm IPM
New observations of the edge-on galaxy NGC 891, at 1.15 and 2 mm obtained with the IRAM 30-m telescope and the NIKA2 camera, within the framework of the IMEGIN (Interpreting the Millimetre Emission of Galaxies with IRAM and NIKA2) Large Program, are presented in this work. By using multiwavelength maps (from the mid-IR to the cm wavelengths) we perform SED fitting in order to extract the physical properties of the galaxy on both global and local (kpc) scales. For the interpretation of the observations we make use of a state-of-the-art SED fitting code, HerBIE (HiERarchical Bayesian Inference for dust Emission). The observations indicate a galaxy morphology, at mm wavelengths, similar to that of the cold dust emission traced by sub-mm observations and to that of the molecular gas. The contribution of the radio emission at the NIKA2 bands is very small (negligible at 1.15 mm and at 2 mm) while it dominates the total energy budget at longer wavelengths (beyond 5 mm). On local scales, the distribution of the free-free emission resembles that of the dust thermal emission while the distribution of the synchrotron emission shows a deficiency along the major axis of the disc of the galaxy.

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