Constraints on Axion-like Particles from X-Ray Observations of NGC1275

Berg, Mark A.; Conlon, Joseph P.; Day, Francesca; Jennings, Nicholas R.; Krippendorf, Sven; Powell, A.; Rummel, Markus

doi:10.3847/1538-4357/aa8b16

Cited by 97 publications

(133 citation statements)

References 60 publications

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“…In general, we find that the photon to ALP conversion probability P γ→a is proportional to B 2 g 2 aγγ , and to the total extent and coherence length of the magnetic field. Consistency with current observations requires g aγγ 5 × 10 −12 GeV −1 [17,18,[25][26][27].…”

Section: Axion-like Particle Phenomenologysupporting

confidence: 76%

“…The effect of low mass ALPs at other wavelengths is often more subtle, and therefore X-ray astronomy has perhaps a crucial role to play in searching for axion-like particles. Existing X-ray data has been used to place world-leading bounds on the ALP-photon interaction by searching for characteristic modulations in the spectra of point sources passing through the magnetic fields of galaxy clusters [17][18][19][20].…”

Section: Introductionmentioning

confidence: 99%

“…These bounds are more constraining than existing bounds on low mass ALPs. For example, Chandra observations of NGC1275 give g aγγ 1.4 × 10 −12 GeV −1 [17].…”

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confidence: 99%

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Searching for Axion-Like Particles with X-ray Polarimeters

Day

Krippendorf

2018

Galaxies

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X-ray telescopes are an exceptional tool for searching for new fundamental physics. In particular, X-ray observations have already placed world-leading bounds on the interaction between photons and axion-like particles (ALPs). ALPs are hypothetical new ultra-light particles motivated by string theory models. They can also act as dark matter and dark energy, and provide a solution to the strong CP problem. In a background magnetic field, ALPs and photons may interconvert. This leads to energy dependent modulations in both the flux and polarisation of the spectra of point sources shining through large magnetic fields. The next generation of polarising X-ray telescopes will offer new detection possibilities for ALPs. Here we present techniques and projected bounds for searching for ALPs with X-ray polarimetry. We demonstrate that upcoming X-ray polarimetry missions have the potential to place world-leading bounds on ALPs.

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Section: Axion-like Particle Phenomenologysupporting

confidence: 76%

Section: Introductionmentioning

confidence: 99%

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Searching for Axion-Like Particles with X-ray Polarimeters

Day

Krippendorf

2018

Galaxies

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“…One can subtract the cluster emission using the spectrum from a region close to the AGN (this was the approach used in [10] and yields very similar results to those presented here). However, it is statistically preferable to model the cluster emission directly, rather than trying to remove it via subtraction.…”

Section: Discussionmentioning

confidence: 79%

Consistency of Hitomi, XMM-Newton, and Chandra 3.5 keV data from Perseus

et al. 2017

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Hitomi observations of Perseus with the Soft X-ray Spectrometer (SXS) provide a high-resolution look at the 3.5 keV feature reported by multiple groups in the Perseus cluster. The Hitomi spectrum -which involves the sum of diffuse cluster emission and the point-like central Active Galactic Nucleus (AGN) -does not show any excess at E ∼ 3.5keV, giving an apparent inconsistency with previous observations of excess diffuse emission. We point out that 2009 Chandra data reveals a strong dip in the AGN spectrum at E = (3.54 ± 0.02)keV (cluster frame) -the identical energy to the diffuse excess observed by XMM-Newton. Scaling this dip to the 2016 AGN luminosity and adding it to the diffuse XMM-Newton excess, this predicts an overall dip in the SXS field of view of (−5.9 ± 4.4) × 10 −6 ph cm −2 s −1 at E = 3.54 keV -a precise match to the Hitomi data when broadened by the dark matter virial velocity. We describe models of Fluorescent Dark Matter that can reproduce this physics, in which dark matter absorbs and then re-emits 3.5 keV photons emitted from the central AGN.The nature of dark matter is a question of fundamental importance in particle physics, astrophysics and cosmology. The X-ray spectra around E = 3.5 keV of galaxy clusters and other objects have been intensely studied following the announcement in [1, 2] of an unidentified emission line around this energy. In this respect, the Perseus cluster has been of special interest. For both XMM-Newton and Chandra data, the signal for Perseus found in [1, 2] was much stronger than that inferred from the stacked sample of distant clusters in [1] (in the much studied scenario where the 3.5 keV line arises from dark matter decay to photons). A similar result was found in [3], and also confirmed with Suzaku studies of the Perseus cluster in [4,5] (although see [6] for a contrary view on Suzaku data).The 3.5 keV line has been discussed at length in the literature. Both astrophysical explanations (such as potassium emission [1,3] or sulphur charge exchange [7]) and more exotic ones such as dark matter have been put forward as its origin. There is currently no consensus opinion on the physics behind the line and an overall review of studies of the 3.5 keV line is contained in [8].The CCD technology present on Chandra, XMMNewton and Suzaku has limited energy resolution. The launch of Hitomi, with the microcalorimeters present on its Soft X-ray Spectrometer (SXS), was expected to offer a decisive test of the 3.5 keV line, both in Perseus and in other clusters. Sadly Hitomi was lost around one month after launch, but prior to its loss it performed a deep groundbreaking observation of the centre of the Perseus cluster.The data from the Hitomi observations around E ∼ 3.5 keV were recently reported in [9]. No excess was seen, and it is stated that this is incompatible at more than 3σ with the strong signal from Perseus observed with other telescopes.In this paper, we show that that there is no incompatibility and that the overall observational picture is consistent. While the XMM-...

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“…This applies not only to the usual parity even operator F µν F µν , but also the parity odd operator, requiring the existence of a coupling L ⊃ − 1 4 g aγγ aF µνF µν (1) in the effective Lagrangian, whereF µν = µνρσ F ρσ ., The pseudoscalar a is an axion-like particle (ALP), which is not necessarily the QCD axion, and it may be a nontrivial linear combination of the hundreds or thousands of ALPs expected from studies of string vacua. Numerous ground-based experiments [1][2][3][4] and satellite observations [5][6][7][8][9][10][11] place constraints on ALP-photon interactions, probing widely different regimes for the axion mass m a and coupling strength g aγγ . Existing limits are already remarkable, within a few orders of magnitude of GUT scale decay constants f aγγ ≡ g −1 aγγ .…”

Section: Introductionmentioning

confidence: 99%

Towards string theory expectations for photon couplings to axionlike particles

et al. 2019

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ALP-photon couplings are modeled in large ensembles of string vacua and random matrix theories. In all cases, the effective coupling increases polynomially in the number of ALPs, of which hundreds or thousands are expected in the string ensembles, many of which are ultralight. The expected value of the couplings gaγγ ≃ 10 −12 GeV −1 − 10 −10 GeV −1 provide viable targets for future x-ray telescopes and axion helioscopes, and in some cases are already in tension with existing data.

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Constraints on Axion-like Particles from X-Ray Observations of NGC1275

Cited by 97 publications

References 60 publications

Searching for Axion-Like Particles with X-ray Polarimeters

Searching for Axion-Like Particles with X-ray Polarimeters

Consistency of Hitomi, XMM-Newton, and Chandra 3.5 keV data from Perseus

Towards string theory expectations for photon couplings to axionlike particles

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