QUIJOTE Scientific Results – XVII. Studying the anomalous microwave emission in the Andromeda Galaxy with QUIJOTE-MFI

Fernández-Torreiro, M; Génova-Santos, R T; Rubiño-Martín, J A; López-Caraballo, C H; Peel, M W; Arce-Tord, C; Rebolo, R; Artal, E; Ashdown, M; Barreiro, R B; Casas, F J; de la Hoz, E; Guidi, F; Herranz, D; Hoyland, R; Lasenby, A; Martínez-Gonzalez, E; Piccirillo, L; Poidevin, F; Ruiz-Granados, B; Tramonte, D; Vansyngel, F; Vielva, P; Watson, R A

doi:10.1093/mnras/stad3145

Cited by 3 publications

(1 citation statement)

References 76 publications

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“…A recent study by Harper et al (2023) reported the marginal detection of AME in M31, suggesting that it may not be uniformly distributed throughout the entire galaxy. Conversely, the study by Fernández-Torreiro et al (2024) presented a contrasting view, strongly advocating for the presence of AME in M31. In addition, Tibbs et al (2018) reported an AME-like source in a small spiral galaxy in the Local Group, M33, in its global spectral energy distribution (SED).…”

Section: Introductionmentioning

confidence: 97%

Detection of Extragalactic Anomalous Microwave Emission in NGC 2903 Using KVN Single-dish Observations

Poojon,

Chung,

Hoang

et al. 2024

ApJ

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We present the results of the single-dish observations using the Korean VLBI Network to search for anomalous microwave emission (AME) in nearby galaxies. The targets were selected from ‘Mapping the dense molecular gas in the strongest star-forming galaxies' (MALATANG), a legacy survey project of the James Clerk Maxwell Telescope. The MALATANG galaxies are good representatives of local galaxies with enhanced nuclear activity associated with star formation and/or active galactic nuclei (AGNs), providing IR-bright galaxy samples; thus, they are good candidates for AME hosts. Combining with ancillary data, we investigated the radio–IR spectral energy distribution (SED), while searching for AME signals in five galaxies. The AME in NGC 2903 was well detected at a significant confidence level, whereas that in NGC 2146 and M82 was marginal. NGC 1068 and Arp 299 indicated no significant hints, and we provide upper limits for the AME. The best-fit SED exhibited local peaks of the AME components at higher frequencies and with stronger peak fluxes than those in previous studies. This suggested that AME originates from denser environments such as molecular clouds or photodissociation regions rather than warm neutral/ionized medium as commonly suggested by previous studies. Further, our AME-detected targets were observed to exhibit higher specific star formation rates than the other extragalactic AME hosts. Furthermore, AME favored starburst galaxies among our sample rather than AGN hosts. Consequently, this might imply that AGNs are excessively harsh environments for tiny dust to survive.

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Section: Introductionmentioning

confidence: 97%

Detection of Extragalactic Anomalous Microwave Emission in NGC 2903 Using KVN Single-dish Observations

Poojon,

Chung,

Hoang

et al. 2024

ApJ

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COMAP Galactic science I: observations of spinning dust emission at 30 GHz in dark clouds surrounding the λ-Orionis H ii region

Harper,

Dickinson,

Cleary

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Anomalous Microwave Emission (AME) is a major component of Galactic emission in the frequency band 10–60 GHz and is commonly modelled as rapidly rotating spinning dust grains. The photodissociation region (PDR) at the boundary of the λ-Orionis H ii region has been identified by several recent analyses as one of the brightest spinning dust-emitting sources in the sky. We investigate the Barnard 30 dark cloud, a dark cloud embedded within the λ-Orionis PDR. We use total-power observations of Barnard 30 from the CO Mapping Array Project (COMAP) pathfinder instrument at 26–34GHz with a resolution of 4.′5 alongside existing data from Planck, WISE, IRAS, ACT, and the 1.447 GHz GALFACTS survey. We use aperture photometry and template fitting to measure the spectral energy distribution of Barnard 30. We find that the spinning dust is the dominant emission component in the 26–34GHz range at the 6 σ level (S30GHz = 3.35 ± 0.56 Jy). From correlating COMAP data with dust templates we find no evidence that polycyclic aromatic hydrocarbons are the preferred carrier for the spinning dust emission, suggesting that the spinning dust carriers are due to a mixed population of very small grains. Finally, we find evidence for variations in spinning dust emissivity and peak frequency within Barnard 30, and that these variations are possibly driven by changes in dust grain population and the total radiation field. Confirming the origin of the variations in the spinning dust spectrum will require both future COMAP observations at 15 GHz combined with spectroscopic mid-infrared data of Barnard 30.

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Radio-to-submillimetre spectral energy distributions of NGC 1365

Chen,

Bendo,

Fuller

et al. 2024

Monthly Notices of the Royal Astronomical Society

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We analyse the radio-to-submillimetre spectral energy distribution (SED) for the central pseudobulge of NGC 1365 using archival data from the Atacama Large Millimeter/submillimeter Array (ALMA) and the Very Large Array (VLA). This analysis shows that free-free emission dominates the continuum emission at 50–120 GHz and produces about 75 per cent of the 103 GHz continuum emission. However, the fraction of 103 GHz continuum emission originating from free-free emission varies significantly among different subregions in the pseudobulge, particularly for an outflow from the AGN on the eastern pseudobulge where the synchrotron emission produces half of the 103 GHz continuum emission. Free-free emission also dominates at 103 GHz within the central 400 pc diameter region, but this emission is associated with the AGN rather than star formation. The star formation rate (SFR) within the pseudobulge derived from the ALMA free-free emission is 8.9 ± 1.1 M⊙ yr−1. This is comparable to the SFR from the mid-infrared emission but higher than the SFR from the extinction-corrected Hα line emission, mainly because the pseudobulge is heavily dust obscured. The 1.5 GHz emission yields a comparable SFR for the pseudobulge but may have lower SFRs within subregions of the pseudobulge because of the diffusion outside of these regions of the electrons producing the synchrotron radiation. We propose that applying a correction factor of 75 per cent to the 80–110 GHz continuum emission could provide valuable estimates of the free-free emission without performing any SED decomposition, which could derive extinction-free SFRs within 20 per cent accuracy.

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QUIJOTE Scientific Results – XVII. Studying the anomalous microwave emission in the Andromeda Galaxy with QUIJOTE-MFI

Cited by 3 publications

References 76 publications

Detection of Extragalactic Anomalous Microwave Emission in NGC 2903 Using KVN Single-dish Observations

Detection of Extragalactic Anomalous Microwave Emission in NGC 2903 Using KVN Single-dish Observations

COMAP Galactic science I: observations of spinning dust emission at 30 GHz in dark clouds surrounding the λ-Orionis H ii region

Radio-to-submillimetre spectral energy distributions of NGC 1365

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