Searching for anomalous microwave emission in nearby galaxies K-band observations with the Sardinia Radio Telescope

被引：5
作者：
Bianchi, S. [1 ]
Murgia, M. [2 ]
Melis, A. [2 ]
Casasola, V [3 ]
Galliano, F. [4 ]
Govoni, F. [2 ]
Jones, A. P. [5 ]
Madden, S. C. [4 ]
Paladino, R. [3 ]
Salvestrini, F. [1 ]
Xilouris, E. M. [6 ]
Ysard, N. [5 ]
机构：
[1] INAF Osservatorio Astrofis Arcetri, LE Fermi 50, I-50125 Florence, Italy
[2] INAF Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy
[3] INAF Ist Radioastron, Via P Gobetti 101, I-40129 Bologna, Italy
[4] Univ Paris Saclay, Univ Paris Diderot, Sorbonne Paris Cite, AIM,CEA,CNRS, F-91191 Gif Sur Yvette, France
[5] Univ Paris Saclay, CNRS, Inst Astrophys Spatiale, F-91405 Orsay, France
[6] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote Sen, Ioannou Metaxa & Vasileos Pavlou, Athens 15236, Greece
来源：
ASTRONOMY & ASTROPHYSICS | 2022年 / 658卷
关键词：
radio continuum: galaxies; galaxies: ISM; galaxies: photometry; dust; extinction; SPINNING DUST EMISSION; INTERSTELLAR DUST; PLANCK; ORIGIN; MODEL; I;
D O I：
10.1051/0004-6361/202142684
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Aims. We observed four nearby spiral galaxies (NGC 3627, NGC 4254, NGC 4736, and NGC 5055) in the K band with the 64-m Sardinia Radio Telescope, with the aim of detecting anomalous microwave emission (AME), a radiation component presumably due to spinning dust grains, which has been observed thus far in the Milky Way and only in a handful of other galaxies (most notably, M 31). Methods. We mapped the galaxies at 18.6 and 24.6 GHz and studied their global photometry together with other radio-continuum data from the literature in order to find AME as emission in excess of the synchrotron and thermal components. Results. We only found upper limits for AME. These nondetections, and other upper limits in the literature, are nevertheless consistent with the average AME emissivity from a few detections: it is epsilon(AME )(30GH)(z)= 2.4 +/- 0.4 x 10(-2) MJy sr(-1) (M-circle dot pc(-2))(-1) in units of dust surface density (equivalently, 1.4 +/- 0.2 x 10(-18) Jy sr(-1) (H cm(-2) )(-1) in units of H column density). We finally suggest searching for AME in quiescent spirals with relatively low radio luminosity, such as M 31.
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