Spatial structure of the WMAP-Planck haze

Rubtsov, G.; Zhezher, Y.

doi:10.48550/arxiv.1812.05228

Cited by 2 publications

(2 citation statements)

References 27 publications

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“…It resembles a jet structure that emanates from the center of our galaxy, extending nearly 8 kpc perpendicular to the galactic plane, in what could be the result of past accretion process in the galactic center black hole (Ko et al 2019). This structure has well-defined edges in coincidence with X-ray signatures seen by the ROSAT mission in the 1990s (Ponti et al 2019), and a microwave excess in the same region known as "WMAP haze" (Finkbeiner 2004;Rubtsov & Zhezher 2018).…”

Section: The Galactic Gamma-ray Contentmentioning

confidence: 68%

Extreme and high synchrotron peak blazars beyond 4FGL: The 2BIGB γ-ray catalogue

Arsioli

Chang

Musiimenta

2020

Monthly Notices of the Royal Astronomical Society

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We present the results of a γ-ray likelihood analysis over all the extreme and high synchrotron peak blazars (EHSP & HSP) from the 3HSP sample. We investigate 2013 multifrequency seed positions under the eyes of Fermi Large Area Telescope, considering 11 years of observations. We report on 1160 γ-ray signatures detected down to the 3 σ threshold in the energy range between 500 MeV to 500 GeV. The detections include 235 additional sources concerning 4FGL, all confirmed via high-energy TS maps, and represent an improvement of ∼25% for the number of EHSP & HSP currently described in γ-rays. We build the γray spectral energy distribution for all the 1160 sources, delivering to the very high-energy community a dedicated spectral description of the entire 3HSP population. We plot the γray logN-logS for the 3HSP sample, and also for the EHSP & HSP subsamples. We measure the total contribution of HSP+EHSP to the extragalactic gamma-ray background, which reaches up to ∼33% at 100 GeV. Also, we show how does the γ-ray detectability improves according to the synchrotron peak flux as represented by the Figure of Merit (FOM) parameter. We highlight that the search for TeV peaked blazars may benefit from considering HSP and EHSP as a whole, instead of EHSPs only. We entitle this γ-ray sample as Second Brazil-ICRANet Gamma-ray Blazar catalog, with the acronym 2BIGB. All information will be available on public data repositories (Brazilian Science Data Center-BSDC, OpenUniverse, GitHub https://github.com/BrunoArsioli), including the broadband models and the spectral energy distribution data points.2 TeVcat:http://tevcat.uchicago.edu/ is a regularly updated list of TeV detected astrophysical sources. From there we count 81 extragalactic TeV sources, which includes 72 blazars, 3 Starbursts, 1 Globular Cluster, 2 AGNs of unknown type and 3 gamma-ray bursts.

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Section: The Galactic Gamma-ray Contentmentioning

confidence: 68%

Extreme and high synchrotron peak blazars beyond 4FGL: The 2BIGB γ-ray catalogue

Arsioli

Chang

Musiimenta

2020

Monthly Notices of the Royal Astronomical Society

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“…A common origin has been proposed for the two phenomena, the WMAP-Planck haze and high-energy bubbles, and the spatial dimensions and locations of the haze in the microwave and Fermi bubbles are indeed compatible within the limits of the experimental error (Rubtsov & Zhezher 2018).…”

Section: Introductionmentioning

confidence: 68%

Broadband Radio Study of the North Polar Spur: Origin of the Spectral Turnover with Insights into the X-Ray and Gamma-Ray Spectra

Iwashita,

Kataoka,

Sofue

2023

ApJ

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The North Polar Spur (NPS) is a giant structure that is clearly visible in both radio and X-ray all-sky maps. We analyzed broadband radio observations covering a range between 22 MHz and 70 GHz to systematically analyze the thermal/nonthermal emissions associated with the NPS. We demonstrate that the radio emission of the NPS comprises synchrotron, free–free, and dust emission; however, synchrotron emissions dominate over other emissions, especially at high Galactic latitudes. Moreover, the synchrotron spectra exhibit a power-law behavior with N(γ) ∝ γ −s (s ≃ 1.8–2.4) up to a few GHz moderated by a turnover at ν brk ≃ 1 GHz, above which the spectral index s decreases by one. Assuming that the turnover is due to the electrons being cooled by synchrotron radiation before escaping (or advecting) from the emission region, the magnetic field strength can be estimated to be B ∼ 8 μG if the NPS is a distant structure that is near the Galactic center (GC). However, an unreasonably strong B ∼ 114 μG is required if the NPS is near the local supernova remnant (SNR). The corresponding nonthermal energy stored in the NPS is E n/th ≃ 4.4 × 1055 erg in the GC scenario, whereas E n/th ≃ 4.1 × 1052 erg is difficult to explain with a single local SNR. We also estimated the gamma-ray emission associated with the NPS through inverse Comptonization of the cosmic microwave background, which peaks at 100–1000 keV with a flux of ν F ν ∼ 10−9 erg cm−2 s−1 sr−1 in the GC model, and may be a good candidate for detection by future X-ray/gamma-ray observatories.

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Spatial structure of the WMAP-Planck haze

Cited by 2 publications

References 27 publications

Extreme and high synchrotron peak blazars beyond 4FGL: The 2BIGB γ-ray catalogue

Extreme and high synchrotron peak blazars beyond 4FGL: The 2BIGB γ-ray catalogue

Broadband Radio Study of the North Polar Spur: Origin of the Spectral Turnover with Insights into the X-Ray and Gamma-Ray Spectra

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