On the existence of (l,m,n)-spreads

Bernardi, Marco Paolo; Schiavi, Emilio

doi:10.1007/bf01229248

Cited by 10 publications

(17 citation statements)

References 3 publications

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“…The weighted average of those five determinations is (m − M ) 0 = 31.22 ± 0.25 mag. Of the remaining three values, two fall comfortably within the 1σ uncertainties following homogenization: (m − M ) 0 = 31.21 ± 0.13 mag (Bernardi et al 2002) and (m − M ) 0 = 31.20 ± 0.33 mag (Allen & Shanks 2004). The third value, (m − M ) 0 = 31.45 ± 0.14 mag (Masters et al 2006), is larger although still consistent with the bulk of our values.…”

Section: Fornaxmentioning

confidence: 70%

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? VII. A Distance Framework out to 100 Mpc

Grijs

Bono

2020

ApJS

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We consider the body of published distance moduli to the Fornax and Coma galaxy clusters, with specific emphasis on the period since 1990. We have carefully homogenized our final catalogs of distance moduli onto the distance scale established in the previous papers in this series. We assessed systematic differences associated with the use of specific tracers, and consequently discarded results based on application of the Tully-Fisher relation and of globular cluster and planetary nebula luminosity functions. We recommend 'best' weighted relative distance moduli for the Fornax and Coma clusters with respect to the Virgo cluster benchmark of ∆(m − M ) Fornax−Virgo 0

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Section: Fornaxmentioning

confidence: 70%

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? VII. A Distance Framework out to 100 Mpc

Grijs

Bono

2020

ApJS

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“…Therefore, some authors have claimed that the emission in the GeV -TeV energy range may have origin in different physical processes (Brown & Adams 2011;Georganopoulos et al 2005). The radio galaxy IC310, also called B0313+411 and J0316+4119, located in the Perseus Cluster at a redshift of z=0.00189 (Bernardi et al 2002) is one of brightest objects of the Perseus cluster of galaxies in the radio and X-ray bands. Due to its kiloparsec-scale radio morphology, it has been classified as a head-tail or, more specifically, narrow-angle tail radio galaxy (Feretti et al 1998;Sijbring & de Bruyn 1998).…”

Section: Introductionmentioning

confidence: 99%

Modeling the spectral energy distribution of the radio galaxy IC310

Fraija

Marinelli

Galván-Gaméz

et al. 2017

Astroparticle Physics

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The radio galaxy IC310 located in the Perseus Cluster is one of the brightest objects in the radio and X-ray bands, and one of the closest active galactic nuclei observed in very-high energies. In GeV -TeV γ-rays, IC310 was detected in low and high flux states by the MAGIC telescopes from October 2009 to February 2010. Taking into account that the spectral energy distribution (SED) up to a few GeV seems to exhibit a double-peak feature and that a single-zone synchrotron self-Compton (SSC) model can explain all of the multiwavelength emission except for the non-simultaneous MAGIC emission, we interpret, in this work, the multifrequency data set of the radio galaxy IC310 in the context of homogeneous hadronic and leptonic models. In the leptonic framework, we present a multi-zone SSC model with two electron populations to explain the whole SED whereas for the hadronic model, we propose that a single-zone SSC model describes the SED up to a few GeVs and neutral pion decay products resulting from pγ interactions could describe the TeV -GeV γ-ray spectra. These interactions occur when Fermi-accelerated protons interact with the seed photons around the SSC peaks. We show that, in the leptonic model the minimum Lorentz factor of second electron population is exceedingly high γ e ∼ 10 5 disfavoring this model, and in the hadronic model the required proton luminosity is not extremely high ∼ 10 44 erg/s, provided that charge neutrality between the number of electrons and protons is given. Correlating the TeV γ-ray and neutrino spectra through photo-hadronic interactions, we find that the contribution of the emitting region of IC310 to the observed neutrino and ultra-high-energy cosmic ray fluxes are negligible.

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“…IC 310 is located on the outskirts of the Perseus galaxy cluster with a redshift of z = 0.0189 (Bernardi et al 2002). Originally, this object was classified as a head-tail radio galaxy (Ryle & Windram 1968;Miley 1980;Sijbring & de Bruyn 1998).…”

Section: Introductionmentioning

confidence: 99%

First multi-wavelength campaign on the gamma-ray-loud active galaxy IC 310

Ahnen

Ansoldi

Antonelli

et al. 2017

A&A

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Context. The extragalactic very-high-energy gamma-ray sky is rich in blazars. These are jetted active galactic nuclei that are viewed at a small angle to the line-of-sight. Only a handful of objects viewed at a larger angle are known so far to emit above 100 GeV. Multi-wavelength studies of such objects up to the highest energies provide new insights into the particle and radiation processes of active galactic nuclei. Aims. We report the results from the first multi-wavelength campaign observing the TeV detected nucleus of the active galaxy IC 310, whose jet is observed at a moderate viewing angle of 10• − 20• . Methods. The multi-instrument campaign was conducted between 2012 November and 2013 January, and involved observations with MAGIC, Fermi, INTEGRAL, Swift, OVRO, MOJAVE and EVN. These observations were complemented with archival data from the AllWISE and 2MASS catalogs. A one-zone synchrotron self-Compton model was applied to describe the broad-band spectral energy distribution. Results. IC 310 showed an extraordinary TeV flare at the beginning of the campaign, followed by a low, but still detectable TeV flux. Compared to previous measurements in this energy range, the spectral shape was found to be steeper during the low emission state. Simultaneous observations in the soft X-ray band showed an enhanced energy flux state and a harder-when-brighter spectral shape behaviour. No strong correlated flux variability was found in other frequency regimes. The broad-band spectral energy distribution obtained from these observations supports the hypothesis of a double-hump structure. Conclusions. The harder-when-brighter trend in the X-ray and VHE emission, observed for the first time during this campaign, is consistent with the behaviour expected from a synchrotron self-Compton scenario. The contemporaneous broad-band spectral energy distribution is well described with a one-zone synchrotron self-Compton model using parameters that are comparable to those found for other gamma-ray-emitting misaligned blazars.

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On the existence of (l,m,n)-spreads

Cited by 10 publications

References 3 publications

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? VII. A Distance Framework out to 100 Mpc

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? VII. A Distance Framework out to 100 Mpc

Modeling the spectral energy distribution of the radio galaxy IC310

First multi-wavelength campaign on the gamma-ray-loud active galaxy IC 310

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