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

Abstract

The Haze is an excess of microwave intensity emission surrounding the Galactic centre. It is spatially correlated with the $\gamma$-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 re-analysis 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 analyze 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$\le \nu \le$70 GHz is a power-law with spectral index ${\beta }^{\mathrm{H}}=-2.79\pm 0.08$, which is flatter than the Galactic synchrotron in the same region (${\beta }^{\mathrm{S}}=-2.98\pm 0.04$), but steeper than that obtained from previous works (${\beta }^{\mathrm{H}}\sim -2.5$ at 23$\le \nu \le$70 GHz). We also observe an excess of polarized signal in the QUIJOTE-MFI maps in the Haze area. This is a first hint detection of polarized Haze, or a consequence of curvature of the synchrotron spectrum in that area. Finally, we show that the spectrum of polarized structures associated with Galactic centre activity is steep at low frequencies ($\beta \sim -3.2$ at 2.3 $\le \nu \le$ 23 GHz), and becomes flatter above 11 GHz.

arXiv comment31 pages. Accepted for publication in MNRAS

References in corpus (70)

• Array Programming with NumPy
• emcee: The MCMC Hammer
• HEALPix -- a Framework for High Resolution Discretization, and Fast Analysis of Data Distributed on the Sphere
• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results
• Nine-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Final Maps and Results
• Planck 2018 results. I. Overview and the cosmological legacy of Planck
• Giant Gamma-ray Bubbles from Fermi-LAT: AGN Activity or Bipolar Galactic Wind?
• Planck 2013 results. XI. All-sky model of thermal dust emission
• A Full-Sky H-alpha Template for Microwave Foreground Prediction
• Planck 2018 results. IV. Diffuse component separation
• The Spectrum and Morphology of the Fermi Bubbles
• Microwave ISM Emission Observed by WMAP
• Planck intermediate results. LVII. Joint Planck LFI and HFI data processing
• Joint Bayesian component separation and CMB power spectrum estimation
• A review of indirect searches for particle dark matter
• The Fermi Haze: A Gamma-Ray Counterpart to the Microwave Haze
• The Fermi Bubbles: Giant, Multi-Billion-Year-Old Reservoirs of Galactic Center Cosmic Rays
• Detection of large-scale X-ray bubbles in the Milky Way halo
• Towards a free-free template for CMB foregrounds
• Extended Anomalous Foreground Emission in the WMAP 3-Year Data
• Giant Magnetized Outflows from the Centre of the Milky Way
• Power spectrum estimation from high-resolution maps by Gibbs sampling
• The Fermi Bubbles. I. Possible Evidence for Recent AGN Jet Activity in the Galaxy
• Planck early results. XX. New light on anomalous microwave emission from spinning dust grains
• Evidence Of Dark Matter Annihilations In The WMAP Haze
• Xspect, estimation of the angular power spectrum by computing cross-power spectra with analytical error bars
• A novel estimator of the polarization amplitude from normally distributed Stokes parameters
• A Unified Model of the Fermi Bubbles, Microwave Haze, and Polarized Radio Lobes: Reverse Shocks in the Galactic Center's Giant Outflows
• Probing the Fermi Bubbles in Ultraviolet Absorption: A Spectroscopic Signature of the Milky Way's Biconical Nuclear Outflow
• The State-of-Play of Anomalous Microwave Emission (AME) Research
• The S-PASS view of polarized Galactic Synchrotron at 2.3 GHz as a contaminant to CMB observations
• High Energy Positrons and the WMAP Haze from Exciting Dark Matter
• Polarised radio filaments outside the Galactic plane
• Fermi Bubbles in the Milky Way: the closest AGN feedback laboratory courtesy of Sgr A*?
• Non-Thermal Insights on Mass and Energy Flows Through the Galactic Centre and into the Fermi Bubbles
• X-ray bubbles in the circumgalactic medium of TNG50 Milky Way- and M31-like galaxies: signposts of supermassive black hole activity
• The Fermi Bubbles. II. The Potential Roles of Viscosity and Cosmic Ray Diffusion in Jet Models
• S-band Polarization All Sky Survey (S-PASS): survey description and maps
• The Fermi Bubbles as Starburst Wind Termination Shocks
• IMAGINE: A comprehensive view of the interstellar medium, Galactic magnetic fields and cosmic rays
• Fermi and eRosita bubbles as relics of the past activity of the Galactic black hole
• Spatial variations in the spectral index of polarized synchrotron emission in the 9 yr WMAP sky maps
• QUIJOTE Scientific Results. II. Polarisation Measurements of the Microwave Emission in the Galactic molecular complexes W43 and W47 and supernova remnant W44
• Making CMB temperature and polarization maps with Madam
• Synchrotron Spectral Curvature from 22 MHz to 23 GHz
• Polarized galactic synchrotron and dust emission and their correlation
• QUIJOTE scientific results -- IV. A northern sky survey in intensity and polarization at 10-20GHz with the Multi-Frequency Instrument
• Giant Explosion at the Galactic Center and Huge Shocked Shells in the Halo
• Galactic interstellar turbulence in the southern sky seen through spatial gradients of the polarization vector
• New constraints on the Polarization of Anomalous Microwave Emission in nearby molecular clouds
• A Last Look at the Microwave Haze/Bubbles with WMAP
• Simulating the Fermi Bubbles as Forward Shocks Driven by AGN Jets
• The North Polar Spur and Aquila Rift
• The WMAP haze from the Galactic Center region due to massive star explosions and a reduced cosmic ray scale height
• Magnetic substructure in the northern Fermi Bubble revealed by polarized WMAP emission
• Detection of non-thermal hard X-ray emission from the "Fermi bubble" in an external galaxy
• Constraints on the spectral index of polarized synchrotron emission from WMAP and Faraday-corrected S-PASS data
• On the Detection of CMB B-modes from Ground at Low Frequency
• QUIJOTE scientific results -- VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI
• A Supernova-driven, Magnetically-collimated Outflow as the Origin of the Galactic Center Radio Bubbles
• A new polarisation amplitude bias reduction method
• Template fitting of WMAP 7-year data: anomalous dust or flattening synchrotron emission?
• Origin of Galactic Spurs: New Insight from Radio/X-ray All-sky Maps
• Analysis of WMAP 7-year Temperature Data: Astrophysics of the Galactic Haze
• Dark matter implications of the WMAP-Planck Haze
• Can Planck constrain indirect detection of dark matter in our galaxy?
• The spectral index of polarized diffuse Galactic emission between 30 and 44 GHz
• Diverse metallicities of Fermi bubble clouds indicate dual origins in the disk and halo
• The PICASSO map-making code: application to a simulation of the QUIJOTE northern sky survey
• Probing the Halo Gas Distribution in the Inner Galaxy with Fermi Bubble Observations

Cited by in corpus (5)

• QUIJOTE scientific results -- IV. A northern sky survey in intensity and polarization at 10-20GHz with the Multi-Frequency Instrument
• QUIJOTE scientific results -- VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFI
• Morphological Analysis of the Polarized Synchrotron Emission with WMAP and Planck
• QUIJOTE Scientific Results -- XVII. Studying the Anomalous Microwave Emission in the Andromeda Galaxy with QUIJOTE-MFI
• QUIJOTE scientific results -- XVIII. New constraints on the polarization of the Anomalous Microwave Emission in bright Galactic regions: $\rho$\,Ophiuchi, Perseus and W43