Masses of the local group and of the M81 group estimated from distortions in the local velocity field

Abstract. For a general dark-energy equation of state, we estimate the maximum possible radius of massive structures that are not destabilized by the acceleration of the cosmological expansion. A comparison with known stable structures constrains the equation of state. The robustness of the constraint can be enhanced through the accumulation of additional astrophysical data and a better understanding of the dynamics of bound cosmic structures.

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“…[18] and the mass estimate M = (1.2 − 2) × 10 12 M ⊙ from ref. [20], which is derived via the virial theorem and from orbital motions.…”

Section: Observational Constraint On the Equation Of Statementioning

confidence: 97%

“…[18]. The mass estimate of [18] is deduced from this radius and cannot be used as a constraint within our approach. For this reason, we employ the kinematic estimate M = (3.17 ± 0.57) × 10 12 M ⊙ of ref.…”

Section: Observational Constraint On the Equation Of Statementioning

confidence: 99%

Constraining dark energy through the stability of cosmic structures

Pavlidou¹,

Tetradis²,

Tomaras³

2014

J. Cosmol. Astropart. Phys.

113

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“…Although we did not detect VHE gamma rays right after the explosion, using the known distance of M82 (d M82 = 3.6 Mpc Karachentsev & Kashibadze 2006) and assuming, as before, a spectral index of 2.6, one can convert the measured flux UL into an UL on the power emitted into VHE gamma rays. Therefore, given the integral UL for energies greater than 300 GeV, 1.3 × 10 −12 photons cm −2 s −1 , the resulting UL on the power emitted is of the order of 10 39 erg s −1 .…”

Section: Discussionmentioning

confidence: 84%

“…SN 2014J was detected on January 21 2014 (MJD 56678) by the UCL Observatory (Fossey et al 2014) and classified as a Type Ia SN with the Dual Imaging Spectrograph on the ARC 3.5 m telescope (January 22;. It is located in the starburst galaxy M82 at a distance of 3.6 Mpc (Karachentsev & Kashibadze 2006). Its proximity has granted it the title of the nearest Type Ia SN in the past 42 years and motivated large multiwavelength follow-up observations from radio to very-highenergy (VHE; E ≥ 100 GeV) gamma rays.…”

Section: Introductionmentioning

confidence: 99%

Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes

Ahnen

Ansoldi

Antonelli

et al. 2017

A&A

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Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. Aims. We probe the possibility of very-high-energy (VHE; E ≥ 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions. Methods. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of ∼ 5.5 hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed. Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE ∝ E −Γ , with a spectral index of Γ = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 × 10 −12 and 4.1 × 10 −13 photons cm −2 s −1 , respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first ∼ 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10 −6 of the total available energy budget (∼ 10 51 erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.

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“…ation the average density of But the corresponding data are not accessible and I use the average density of the Local Group which can be taken from references [32,34] 2) In the Hubble regime one obtains the negative area (low part of the da -dotted curve of igure 17). It c responds to the self-consistent for a ing ong the expansion of the local flow.…”

Section: Hubble Expansion and The Problem Of Dark Energymentioning

confidence: 99%

To the Theory of Galaxies Rotation and the Hubble Expansion in the Frame of Non-Local Physics

Alexeev¹

2012

JMP

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The unified generalized non-local theory is applied for mathematical modeling of cosmic objects. For the case of galaxies the theory leads to the flat rotation curves known from observations. The transformation of Kepler's regime into the flat rotation curves for different solitons is shown. The Hubble expansion with acceleration is explained as result of mathematical modeling based on the principles of non-local physics. Peculiar features of the rotational speeds of galaxies and effects of the Hubble expansion need not in the introduction of new essence like dark matter and dark energy. The origin of difficulties consists in the total Oversimplification following from the principles of local physics.

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Masses of the local group and of the M81 group estimated from distortions in the local velocity field

Cited by 98 publications

References 14 publications

Constraining dark energy through the stability of cosmic structures

Constraining dark energy through the stability of cosmic structures

Very-high-energy gamma-ray observations of the Type Ia Supernova SN 2014J with the MAGIC telescopes

To the Theory of Galaxies Rotation and the Hubble Expansion in the Frame of Non-Local Physics

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