QUIJOTE scientific results - VI. The Haze as seen by QUIJOTE

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

Monthly Notices of the Royal Astronomical Society

Advertised on:
3
2023
Number of authors
25
IAC number of authors
13
Citations
4
Refereed citations
4
Description
The Haze is an excess of microwave intensity emission surrounding the Galactic Centre. It is spatially correlated with the γ-ray Fermi bubbles, and with the S-PASS radio polarization plumes, suggesting a possible common provenance. The models proposed to explain the origin of the Haze, including energetic events at the Galactic Centre and dark matter decay in the Galactic halo, do not yet provide a clear physical interpretation. In this paper, we present a reanalysis of the Haze including new observations from the Multi-Frequency Instrument (MFI) of the Q-U-I Joint TEnerife (QUIJOTE) experiment, at 11 and 13 GHz. We analyse the Haze in intensity and polarization, characterizing its spectrum. We detect an excess of diffuse intensity signal ascribed to the Haze. The spectrum at frequencies 11 GHz $\, \le \nu \le \,$ 70 GHz is a power law with spectral index βH = -2.79 ± 0.08, which is flatter than the Galactic synchrotron in the same region (βS = -2.98 ± 0.04), but steeper than that obtained from previous works (βH ~ -2.5 at 23 GHz $\, \le \, \nu \le \,$ 70 GHz). We also observe an excess of polarized signal in the QUIJOTE-MFI maps in the Haze area. This is a first hint detection of polarized Haze, or a consequence of curvature of the synchrotron spectrum in that area. Finally, we show that the spectrum of polarized structures associated with Galactic Centre activity is steep at low frequencies (β ~ -3.2 at 2.3 GHz ≤ ν ≤ 23 GHz), and becomes flatter above 11 GHz.
Related projects
The QUIJOTE experiment at the Teide Observatory
QUIJOTE CMB Experiment (Q-U-I JOint TEnerife CMB Experiment)
QUIJOTE es un programa de dos telescopios y su batería de instrumentos, instalados en el Observatorio del Teide, dedicados fundamentalmente a la caracterización de la polarización del Fondo Cósmico de Microondas, en el rango de frecuencias de 10-42 GHz.
José Alberto
Rubiño Martín
Full-sky map showing the spatial distribution of the primary anisotropies of the Cosmic Microwave Background (generated 380,000 years after the Big Bang) derived from observations of the Planck satellite
Anisotropy of the Cosmic Microwave Background
The general goal of this project is to determine and characterize the spatial and spectral variations in the temperature and polarisation of the Cosmic Microwave Background in angular scales from several arcminutes to several degrees. The primordial matter density fluctuations which originated the structure in the matter distribution of the present
Rafael
Rebolo López