Gamma Rays from SN 1987A due to Pseudoscalar Conversion

Grifols, J.A.; Massó, Eduard; Toldrà, Ramon

doi:10.1103/physrevlett.77.2372

Cited by 161 publications

(156 citation statements)

References 23 publications

Supporting

Mentioning

152

Contrasting

Order By: Relevance

“…at 95% confidence level, is a factor of 3 stronger than the upper bound obtained from the analysis of SN987A [8][9][10]. We note that the transfer matrix only depends on the central magnetic field B 0 and g aγ through ∆ γai , and that the transformation B 0 → λB 0 , g aγ → g aγ /λ leaves the conversion probability invariant.…”

Section: Resultsmentioning

confidence: 56%

See 1 more Smart Citation

A new bound on axion-like particles

Marsh

Russell

Fabian

et al. 2017

J. Cosmol. Astropart. Phys.

146

126

View full text Add to dashboard Cite

Axion-like particles (ALPs) and photons can quantum mechanically interconvert when propagating through magnetic fields, and ALP-photon conversion may induce oscillatory features in the spectra of astrophysical sources. We use deep (370 ks), short frame time Chandra observations of the bright nucleus at the centre of the radio galaxy M87 in the Virgo cluster to search for signatures of light ALPs. The absence of substantial irregularities in the X-ray power-law spectrum leads to a new upper limit on the photon-ALP coupling, g aγ : using a very conservative model of the cluster magnetic field consistent with Faraday rotation measurements from M87 and M84, we find g aγ < 2.6 × 10 −12 GeV −1 at 95% confidence level for ALP masses m a ≤ 10 −13 eV. Other consistent magnetic field models lead to stronger limits of g aγ 1.1-1.5 × 10 −12 GeV −1 . These bounds are all stronger than the limit inferred from the absence of a gamma-ray burst from SN1987A, and rule out a substantial fraction of the parameter space accessible to future experiments such as ALPS-II and IAXO.

show abstract

Section: Resultsmentioning

confidence: 56%

“…GeV −1 for light ALPs with m a 4.4 × 10 −10 eV [8][9][10]. For reviews of experimental and astrophysical axion and ALP bounds, see [11][12][13].…”

Section: −12mentioning

confidence: 99%

A new bound on axion-like particles

Marsh

Russell

Fabian

et al. 2017

J. Cosmol. Astropart. Phys.

146

126

View full text Add to dashboard Cite

show abstract

“…For ultra-light ALPs (m a < ∼ 10 −11 eV), the absence of gamma-rays from SN 1987A yields a stringent limit of g 11 1 [21] or even g 11 0.3 [22]. In the range 10 −11 eV ≪ m a ≪ 10 −2 eV, the CAST bound is the most general and stringent.…”

Section: A Reconversion In the Milky Waymentioning

confidence: 99%

Milky Way as a kiloparsec-scale axionscope

2008

View full text Add to dashboard Cite

Very high energy gamma-rays are expected to be absorbed by the extragalactic background light over cosmological distances via the process of electron-positron pair production. Recent observations of cosmologically distant gamma-ray emitters by ground based gamma-ray telescopes have, however, revealed a surprising degree of transparency of the universe to very high energy photons. One possible mechanism to explain this observation is the oscillation between photons and axion-likeparticles (ALPs). Here we explore this possibility further, focusing on photon-ALP conversion in the magnetic fields in and around gamma-ray sources and in the magnetic field of the Milky Way, where some fraction of the ALP flux is converted back into photons. We show that this mechanism can be efficient in allowed regions of the ALP parameter space, as well as in typical configurations of the Galactic Magnetic Field. As case examples, we consider the spectrum observed from two HESS sources: 1ES1101-232 at redshift z = 0.186 and H 2356-309 at z = 0.165. We also discuss features of this scenario which could be used to distinguish it from standard or other exotic models.

show abstract

“…Many experimental efforts are underway to detect and constrain these DM candidates via their direct (e.g. Asztalos et al 2010;Aalseth et al 2011;Aprile et al 2012;Agnese et al 2014;Akerib et al 2014;Angloher et al 2014;Budker et al 2014;Stadnik & Flambaum 2014) or indirect (e.g Brockway, Carlson & Raffelt 1996;Grifols, Masso & Toldra 1996;Ackermann et al 2011;Abbasi et al 2012;Aguilar et al 2013;Friedland, Giannotti & Wise 2013;Blum et al 2014) interactions with the SM, but no definitive evidence has so far emerged. 1 As these experiments designed to directly detect WIMPs and axions continue to report null results (Beringer et al 2012;Akerib et al 2014), with associated shrinkage of allowed parameter space, we are motivated to try to constrain the particle nature of DM via the only interaction it is known to have: gravitation.…”

Section: Introductionmentioning

confidence: 99%

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Bozek¹,

Marsh²,

Silk³

et al. 2015

Monthly Notices of the Royal Astronomical Society

173

208

View full text Add to dashboard Cite

If the dark matter (DM) were composed of axions, then structure formation in the Universe would be suppressed below the axion Jeans scale. Using an analytic model for the halo mass function of a mixed DM model with axions and cold dark matter, combined with the abundance-matching technique, we construct the UV-luminosity function. Axions suppress high-z galaxy formation and the UV-luminosity function is truncated at a faintest limiting magnitude. From the UV-luminosity function, we predict the reionization history of the universe and find that axion DM causes reionization to occur at lower redshift. We search for evidence of axions using the Hubble Ultra Deep Field UV-luminosity function in the redshift range z = 6-10, and the optical depth to reionization, τ , as measured from cosmic microwave background polarization. All probes we consider consistently exclude m a 10 −23 eV from contributing more than half of the DM, with our strongest constraint ruling this model out at more than 8σ significance. In conservative models of reionization a dominant component of DM with m a = 10 −22 eV is in 3σ tension with the measured value of τ , putting pressure on an axion solution to the cusp-core problem. Tension is reduced to 2σ for the axion contributing only half of the DM. A future measurement of the UV-luminosity function in the range z = 10-13 by JWST would provide further evidence for or against m a = 10 −22 eV. Probing still higher masses of m a = 10 −21 eV will be possible using future measurements of the kinetic Sunyaev-Zel'dovich effect by Advanced ACTPol to constrain the time and duration of reionization.

show abstract

Gamma Rays from SN 1987A due to Pseudoscalar Conversion

Cited by 161 publications

References 23 publications

A new bound on axion-like particles

A new bound on axion-like particles

Milky Way as a kiloparsec-scale axionscope

Galaxy UV-luminosity function and reionization constraints on axion dark matter

Contact Info

Product

Resources

About