Publications

Here is full list of my publications along with the abstracts and citations for the ten most recent papers. For more information see the CV page or my arXiv and Inspire HEP pages. You can also read my PhD thesis here. 

Publication List

First author:

Co-author:

Other: 

Recent Abstracts

1. Interacting Dark Sector (ETHOS n = 0): Cosmological Constraints from SPT Cluster Abundance with DES and HST and Weak Lensing Data

arXiv:2411.19911

SPT and DES Collaborations, A. Mazoun et al., 2024

Abstract:

We use galaxy cluster abundance measurements from the South Pole Telescope (SPT) enhanced by Multi-Component Matched Filter (MCMF) confirmation and complemented with mass information obtained using weak-lensing data from Dark Energy Survey Year 3 (DES Y3) and targeted Hubble Space Telescope (HST) observations for probing deviations from the cold dark matter paradigm. Concretely, we consider a class of dark sector models featuring interactions between dark matter (DM) and a dark radiation (DR) component within the framework of the Effective Theory of Structure Formation (ETHOS). We focus on scenarios that lead to power suppression over a wide range of scales, and thus can be tested with data sensitive to large scales, as realized for example for DM−DR interactions following from an unbroken non-Abelian SU(N) gauge theory (interaction rate with power-law index n=0 within the ETHOS parameterization). Cluster abundance measurements are mostly sensitive to the amount of DR interacting with DM, parameterized by the ratio of DR temperature to the cosmic microwave background (CMB) temperature, ξDR=TDR/TCMB. We find an upper limit ξDR < 17% at 95% credibility. When the cluster data are combined with Planck 2018 CMB data along with baryon acoustic oscillation (BAO) measurements we find ξDR < 10%, corresponding to a limit on the abundance of interacting DR that is around three times tighter than that from CMB+BAO data alone. We also discuss the complementarity of weak lensing informed cluster abundance studies with probes sensitive to smaller scales, explore the impact on our analysis of massive neutrinos, and comment on a slight preference for the presence of a non-zero interacting DR abundance, which enables a physical solution to the S8 tension.

Cite it: 


@ARTICLE{2024arXiv241119911M,

       author = {{Mazoun}, Asmaa and {Bocquet}, Sebastian and {Mohr}, Joseph J. and {Garny}, Mathias and {Rubira}, Henrique and {Klein}, Matthias and {Bleem}, Lindsey and {Grandis}, Sebastian and {Schrabback}, Tim},

        title = "{Interacting Dark Sector (ETHOS $n=0$): Cosmological Constraints from SPT Cluster Abundance with DES and HST Weak Lensing Data}",

      journal = {arXiv e-prints},

     keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},

         year = 2024,

        month = nov,

          eid = {arXiv:2411.19911},

        pages = {arXiv:2411.19911},

          doi = {10.48550/arXiv.2411.19911},

archivePrefix = {arXiv},

       eprint = {2411.19911},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024arXiv241119911M},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

2. Cosmic topology. Part Ic. Limits on lens spaces from circle searches

arXiv:2409.02226

COMPACT Collaboration, S. Saha et al., 2024

Abstract:

The Cosmic microwave background (CMB) temperature and polarization observations indicate that in the best-fit Λ Cold Dark Matter model of the Universe, the local geometry is consistent with at most a small amount of positive or negative curvature, i.e., |ΩK|≪1. However, whether the geometry is flat (E3), positively curved (S3) or negatively curved (H3), there are many possible topologies. Among the topologies of S3 geometry, the lens spaces L(p,q), where p and q (p>1 and 0<q<p) are positive integers, are quotients of the covering space of S3 (the three-sphere) by ℤp, the cyclic group of order p. We use the absence of any pair of circles on the CMB sky with matching patterns of temperature fluctuations to establish constraints on p and q as a function of the curvature scale that are considerably stronger than those previously asserted for most values of p and q. The smaller the value of |ΩK|, i.e., the larger the curvature radius, the larger the maximum allowed value of p. For example, if |ΩK|≃0.05 then p≤9, while if |ΩK|≃0.02, p can be as high as 24. Future work will extend these constraints to a wider set of S3 topologies.  

Cite it: 


@ARTICLE{2024arXiv240902226S,

       author = {{Saha}, Samanta and {Copi}, Craig J. and {Starkman}, Glenn D. and {Anselmi}, Stefano and {Carr{\'o}n Duque}, Javier and {Barandiaran}, Mikel Martin and {Akrami}, Yashar and {Cornet-Gomez}, Fernando and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Mihaylov}, Deyan P. and {Pereira}, Thiago S. and {Samandar}, Amirhossein and {Tamosiunas}, Andrius},

        title = "{Cosmic topology. Part Ic. Limits on lens spaces from circle searches}",

      journal = {arXiv e-prints},

     keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory},

         year = 2024,

        month = sep,

          eid = {arXiv:2409.02226},

        pages = {arXiv:2409.02226},

          doi = {10.48550/arXiv.2409.02226},

archivePrefix = {arXiv},

       eprint = {2409.02226},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240902226S},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

3. Cosmic topology. Part IIIa. Microwave background parity violation without parity-violating microphysics

arXiv:2407.09400

COMPACT Collaboration, A. Samandar et al., 2024

Abstract:

The standard cosmological model, which assumes statistical isotropy and parity invariance, predicts the absence of correlations between even-parity and odd-parity observables of the cosmic microwave background (CMB). Contrary to these predictions, large-angle CMB temperature anomalies generically involve correlations between even-ℓ and odd-ℓ angular power spectrum  Cℓ, while recent analyses of CMB polarization have revealed non-zero equal-ℓ EB correlations. These findings challenge the conventional understanding, suggesting deviations from statistical isotropy, violations of parity, or both. Cosmic topology, which involves changing only the boundary conditions of space relative to standard cosmology, offers a compelling framework to potentially account for such parity-violating observations. Topology inherently breaks statistical isotropy, and can also break homogeneity and parity, providing a natural paradigm for explaining observations of parity-breaking observables without the need to add parity violation to the underlying microphysics. Our investigation delves into the harmonic space implications of topology for CMB correlations, using as an illustrative example EB correlations generated by tensor perturbations under both parity-preserving and parity-violating scenarios. Consequently, these findings not only challenge the foundational assumptions of the standard cosmological model but also open new avenues for exploring the topological structure of the Universe through CMB observations.

Cite it: 


@ARTICLE{2024arXiv240709400S,

       author = {{Samandar}, Amirhossein and {Carr{\'o}n Duque}, Javier and {Copi}, Craig J. and {Barandiaran}, Mikel Martin and {Mihaylov}, Deyan P. and {Pereira}, Thiago S. and {Starkman}, Glenn D. and {Akrami}, Yashar and {Anselmi}, Stefano and {Cornet-Gomez}, Fernando and {Eskilt}, Johannes R. and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Tamosiunas}, Andrius},

        title = "{Cosmic topology. Part IIIa. Microwave background parity violation without parity-violating microphysics}",

      journal = {arXiv e-prints},

     keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory},

         year = 2024,

        month = jul,

          eid = {arXiv:2407.09400},

        pages = {arXiv:2407.09400},

archivePrefix = {arXiv},

       eprint = {2407.09400},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240709400S},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

4. Cosmic topology. Part IVa. Classification of manifolds using machine learning: a case study with small toroidal universes

arXiv:2404.01236

COMPACT Collaboration, A. Tamosiunas et al., 2024

Abstract:

Non-trivial spatial topology of the Universe may give rise to potentially measurable signatures in the cosmic microwave background. We explore different machine learning approaches to classify harmonic-space realizations of the microwave background in the test case of Euclidean E1 topology (the 3-torus) with a cubic fundamental domain of a size scale significantly smaller than the diameter of the last scattering surface. Different machine learning approaches are capable of classifying the harmonic-space realizations with accuracy greater than 99% if the topology scale is half of the diameter of the last scattering surface and orientation of the topology is known. For distinguishing random rotations of these sky realizations from realizations of the covering space, the extreme gradient boosting classifier algorithm performs best with an accuracy of 88%. Slightly lower accuracies of 83% to 87% are obtained with the random forest classifier along with one- and two-dimensional convolutional neural networks. The techniques presented here can also accurately classify non-rotated cubic E1 topology realizations with a topology scale slightly larger than the diameter of the last-scattering surface, if provided enough training data. This work identifies the prospects and the main challenges for developing machine learning techniques that are capable of accurately classifying observationally viable topologies.

Cite it: 


@ARTICLE{2024arXiv240401236T,

       author = {{Tamosiunas}, Andrius and {Cornet-Gomez}, Fernando and {Akrami}, Yashar and {Anselmi}, Stefano and {Carr{\'o}n Duque}, Javier and {Copi}, Craig J. and {Eskilt}, Johannes R. and {G{\"u}ng{\"o}r}, {\"O}zen{\c{c}} and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Barandiaran}, Mikel Martin and {Mertens}, James B. and {Mihaylov}, Deyan P. and {Pereira}, Thiago S. and {Saha}, Samanta and {Samandar}, Amirhossein and {Starkman}, Glenn D. and {Taylor}, Quinn and {Vardanyan}, Valeri},

        title = "{Cosmic topology. Part IVa. Classification of manifolds using machine learning: a case study with small toroidal universes}",

      journal = {arXiv e-prints},

     keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Theory},

         year = 2024,

        month = apr,

          eid = {arXiv:2404.01236},

        pages = {arXiv:2404.01236},

          doi = {10.48550/arXiv.2404.01236},

archivePrefix = {arXiv},

       eprint = {2404.01236},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024arXiv240401236T},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

5. Using machine learning to optimise chameleon fifth force experiments

arXiv:2308.00844 | JCAP

Chad Briddon, Clare Burrage, Adam Moss, Andrius Tamosiunas, 2024

Abstract:


The chameleon is a theorised scalar field that couples to matter and possess a screening mechanism, which weakens observational constraints from experiments performed in regions of higher matter density. One consequence of this screening mechanism is that the force induced by the field is dependent on the shape of the source mass (a property that distinguishes it from gravity). Therefore an optimal shape must exist for which the chameleon force is maximised. Such a shape would allow experiments to improve their sensitivity by simply changing the shape of the source mass. In this work we use a combination of genetic algorithms and the chameleon solving software SELCIE to find shapes that optimise the force at a single point in an idealised experimental environment. We note that the method we used is easily customised, and so could be used to optimise a more realistic experiment involving particle trajectories or the force acting on an extended body. We find the shapes outputted by the genetic algorithm possess common characteristics, such as a preference for smaller source masses, and that the largest fifth forces are produced by small `umbrella'-like shapes with a thickness such that the source is unscreened but the field reaches its minimum inside the source. This remains the optimal shape even as we change the chameleon potential, and the distance from the source, and across a wide range of chameleon parameters. We find that by optimising the shape in this way the fifth force can be increased by 2.45 times when compared to a sphere, centred at the origin, of the same volume and mass.


Cite it:


@ARTICLE{2024JCAP...02..011B,

       author = {{Briddon}, Chad and {Burrage}, Clare and {Moss}, Adam and {Tamosiunas}, Andrius},

        title = "{Using machine learning to optimise chameleon fifth force experiments}",

      journal = {\jcap},

     keywords = {dark energy theory, Machine learning, modified gravity, General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics},

         year = 2024,

        month = feb,

       volume = {2024},

       number = {2},

          eid = {011},

        pages = {011},

          doi = {10.1088/1475-7516/2024/02/011},

archivePrefix = {arXiv},

       eprint = {2308.00844},

 primaryClass = {gr-qc},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024JCAP...02..011B},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

6. Cosmic topology. Part IIa. Eigenmodes, correlation matrices, and detectability of orientable Euclidean manifolds

arXiv:2306.17112 | JCAP

COMPACT Collaboration, J. R. Eskilt et al., 2024

Abstract:


If the Universe has non-trivial spatial topology, observables depend on both the parameters of the spatial manifold and the position and orientation of the observer. In infinite Euclidean space, most cosmological observables arise from the amplitudes of Fourier modes of primordial scalar curvature perturbations. Topological boundary conditions replace the full set of Fourier modes with specific linear combinations of selected Fourier modes as the eigenmodes of the scalar Laplacian. We present formulas for eigenmodes in orientable Euclidean manifolds with the topologies E1 - E6, E11, E12, E16, and E18 that encompass the full range of manifold parameters and observer positions, generalizing previous treatments. Under the assumption that the amplitudes of primordial scalar curvature eigenmodes are independent random variables, for each topology we obtain the correlation matrices of Fourier-mode amplitudes (of scalar fields linearly related to the scalar curvature) and the correlation matrices of spherical-harmonic coefficients of such fields sampled on a sphere, such as the temperature of the cosmic microwave background (CMB). We evaluate the detectability of these correlations given the cosmic variance of the observed CMB sky. We find that topologies where the distance to our nearest clone is less than about 1.2 times the diameter of the last scattering surface of the CMB give a correlation signal that is larger than cosmic variance noise in the CMB. This implies that if cosmic topology is the explanation of large-angle anomalies in the CMB, then the distance to our nearest clone is not much larger than the diameter of the last scattering surface. We argue that the topological information is likely to be better preserved in three-dimensional data, such as will eventually be available from large-scale structure surveys.


Cite it:


@ARTICLE{2024JCAP...03..036E,

       author = {{Eskilt}, Johannes R. and {Akrami}, Yashar and {Anselmi}, Stefano and {Copi}, Craig J. and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Mihaylov}, Deyan P. and {Starkman}, Glenn D. and {Tamosiunas}, Andrius and {Mertens}, James B. and {Petersen}, Pip and {Saha}, Samanta and {Taylor}, Quinn and {G{\"u}ng{\"o}r}, {\"O}zen{\c{c}} and {The Compact Collaboration}},

        title = "{Cosmic topology. Part IIa. Eigenmodes, correlation matrices, and detectability of orientable Euclidean manifolds}",

      journal = {\jcap},

     keywords = {CMBR theory, cosmological parameters from CMBR, cosmology of theories beyond the SM, physics of the early universe, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory},

         year = 2024,

        month = mar,

       volume = {2024},

       number = {3},

          eid = {036},

        pages = {036},

          doi = {10.1088/1475-7516/2024/03/036},

archivePrefix = {arXiv},

       eprint = {2306.17112},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024JCAP...03..036E},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

7. Cosmic topology. Part I. Limits on orientable Euclidean manifolds from circle searches

arXiv:2211.02603 | JCAP

COMPACT Collaboration, P. Petersen et al., 2023

Abstract:


A key goal The Einstein field equations of general relativity constrain the local curvature at every point in spacetime, but say nothing about the global topology of the Universe. Cosmic microwave background anisotropies have proven to be the most powerful probe of non-trivial topology since, within ΛCDM, these anisotropies have well-characterized statistical properties, the signal is principally from a thin spherical shell centered on the observer (the last scattering surface), and space-based observations nearly cover the full sky. The most generic signature of cosmic topology in the microwave background is pairs of circles with matching temperature and polarization patterns. No such circle pairs have been seen above noise in the WMAP or Planck temperature data, implying that the shortest non-contractible loop around the Universe through our location is longer than 98.5% of the comoving diameter of the last scattering surface. We translate this generic constraint into limits on the parameters that characterize manifolds with each of the nine possible non-trivial orientable Euclidean topologies, and provide a code which computes these constraints. In all but the simplest cases, the shortest non-contractible loop in the space can avoid us, and be shorter than the diameter of the last scattering surface by a factor ranging from 2 to at least 6. This result implies that a broader range of manifolds is observationally allowed than widely appreciated. Probing these manifolds will require more subtle statistical signatures than matched circles, such as off-diagonal correlations of harmonic coefficients.


Cite it:


@ARTICLE{2023JCAP...01..030P,

       author = {{Petersen}, Pip and {Akrami}, Yashar and {Copi}, Craig J. and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Starkman}, Glenn D. and {Tamosiunas}, Andrius and {Eskilt}, Johannes R. and {G{\"u}ng{\"o}r}, {\"O}zen{\c{c}} and {Saha}, Samanta and {Taylor}, Quinn and {Compact Collaboration}},

        title = "{Cosmic topology. Part I. Limits on orientable Euclidean manifolds from circle searches}",

      journal = {\jcap},

     keywords = {CMBR theory, cosmological parameters from CMBR, cosmology of theories beyond the SM, physics of the early universe, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory},

         year = 2023,

        month = jan,

       volume = {2023},

       number = {1},

          eid = {030},

        pages = {030},

          doi = {10.1088/1475-7516/2023/01/030},

archivePrefix = {arXiv},

       eprint = {2211.02603},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2023JCAP...01..030P},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

8. Promise of Future Searches for Cosmic Topology

arXiv:2210.11426 | Phys. Rev. Lett.

COMPACT Collaboration, Y. Akrami et al., 2024

Abstract:


The shortest distance around the Universe through us is unlikely to be much larger than the horizon diameter if microwave background anomalies are due to cosmic topology. We show that observational constraints from the lack of matched temperature circles in the microwave background leave many possibilities for such topologies. We evaluate the detectability of microwave background multipole correlations for sample cases. Searches for topology signatures in observational data over the large space of possible topologies pose a formidable computational challenge. 


Cite it:


@ARTICLE{2024PhRvL.132q1501A,

       author = {{Akrami}, Yashar and {Anselmi}, Stefano and {Copi}, Craig J. and {Eskilt}, Johannes R. and {Jaffe}, Andrew H. and {Kosowsky}, Arthur and {Petersen}, Pip and {Starkman}, Glenn D. and {Gonz{\'a}lez-Quesada}, Kevin and {G{\"u}ng{\"o}r}, {\"O}zen{\c{c}} and {Mihaylov}, Deyan P. and {Saha}, Samanta and {Tamosiunas}, Andrius and {Taylor}, Quinn and {Vardanyan}, Valeri and {Compact Collaboration}},

        title = "{Promise of Future Searches for Cosmic Topology}",

      journal = {\prl},

     keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology, High Energy Physics - Theory},

         year = 2024,

        month = apr,

       volume = {132},

       number = {17},

          eid = {171501},

        pages = {171501},

          doi = {10.1103/PhysRevLett.132.171501},

archivePrefix = {arXiv},

       eprint = {2210.11426},

 primaryClass = {astro-ph.CO},

       adsurl = {https://ui.adsabs.harvard.edu/abs/2024PhRvL.132q1501A},

      adsnote = {Provided by the SAO/NASA Astrophysics Data System}}

9. Chameleon Screening in Cosmic Voids

arXiv:2206.06480 | JCAP

Andrius Tamosiunas, Chad Briddon, Clare Burrage, Alan Cuthforth, Adam Moss, Thomas Vincent, 2022

Abstract:


A key goal in cosmology in the upcoming decade will be to form a better understanding of the accelerated expansion of the Universe. Upcoming surveys, such as the Vera C. Rubin Observatory's 10-year Legacy Survey of Space and Time (LSST), Euclid and the Square Killometer Array (SKA) will deliver key datasets required to tackle this and other puzzles in contemporary cosmology. With this data, constraints of unprecedented power will be put on different models of dark energy and modified gravity. In this context it is crucial to understand how screening mechanisms, which hide the deviations of these theories from the predictions of general relativity in local experiments, affect structure formation. In this work we approach this problem by using a combination of analytic and numerical methods to describe chameleon screening in the context of cosmic voids. We apply a finite element method code, SELCIE, to solve the chameleon equation of motion for a number of void profiles derived from observational data and simulations. The obtained results indicate a complex relationship between the properties of cosmic voids and the size of the chameleon acceleration of a test particle. We find that the fifth force on a test particle in a void is primarily related to the depth and the inner density gradient of the void. For realistic void profiles, the obtained chameleon-to-Newtonian acceleration ratios range between aϕ/aNewt ≈ 10-6- 10-5. However, it should be noted that in unusually deep voids with large inner density gradients, the acceleration ratios can be significantly higher. We also discuss the optimal density profiles for detecting the fifth force in the upcoming observational surveys. 


Cite it:


@article{2022arXiv220606480T,

    author = {{Tamosiunas}, Andrius and {Briddon}, Chad and {Burrage}, Clare and {Cutforth}, Alan and {Moss}, Adam and {Vincent}, Thomas},

    title = "{Chameleon Screening in Cosmic Voids}",

    keywords = {General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics},

    year = 2022,

    month = jun,

    eid = {arXiv:2206.06480},

    pages = {arXiv:2206.06480},

  archivePrefix = {arXiv},

    eprint = {2206.06480},

    primaryClass = {gr-qc},

    adsurl = {https://ui.adsabs.harvard.edu/abs/2022arXiv220606480T},

    adsnote = {Provided by the SAO/NASA Astrophysics Data System}}


10. Chameleon Screening Depends on the Shape and Structure of NFW Halos

arXiv:2108.10364 | JCAP

Andrius Tamosiunas, Chad Briddon, Clare Burrage, Weiguang Cui and Adam Moss, 2022

Abstract:


Chameleon gravity is an example of a model that gives rise to interesting phenomenology on cosmological scales while simultaneously possessing a screening mechanism, allowing it to avoid solar system constraints. Such models result in non-linear field equations, which can be solved analytically only in simple highly symmetric systems. In this work we study the equation of motion of a scalar-tensor theory with chameleon screening using the finite element method. More specifically, we solve the field equation for spherical and triaxial NFW cluster-sized halos. This allows a detailed investigation of the relationship between the NFW concentration and the virial mass parameters and the magnitude of the chameleon acceleration, as measured at the virial radius. In addition, we investigate the effects on the chameleon acceleration due to halo triaxiality. We focus on the parameter space regions that are still allowed by the observational constraints. We find that given our dataset, the largest allowed value for the chameleon-to-NFW acceleration ratio at the virial radius is ∼ 10-7. This result strongly indicates that the chameleon models that are still allowed by the observational constraints would not lead to any measurable effects on galaxy cluster scales. Nonetheless, we also find that there is a direct relationship between the NFW potential and the chameleon-to-NFW acceleration ratio at the virial radius. Similarly, there is a direct (yet a much more complicated) relationship between the NFW concentration, the virial mass and the acceleration ratios at the virial radius. Finally, we find that triaxiality introduces extra directional effects on the acceleration measurements. These effects in combination could potentially be used in future observational searches for fifth forces.


Cite it:


@article{Briddon:2021etm,

    author = "Briddon, Chad and Burrage, Clare and Moss, Adam and Tamosiunas, Andrius",

    title = "{SELCIE: a tool for investigating the chameleon field of arbitrary sources}",

    eprint = "2110.11917",

    archivePrefix = "arXiv",

    primaryClass = "gr-qc",

    doi = "10.1088/1475-7516/2021/12/043",

    journal = "JCAP",

    volume = "12",

    number = "12",

    pages = "043",

    year = "2021"}