Distinguishing AGN from starbursts as the origin of double-peaked Lyman-alpha emitters in the reionization era

Padmanabhan, Hamsa; Loeb, Abraham

doi:10.1051/0004-6361/202040107

A&A

2021

DOI: 10.1051/0004-6361/202040107

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Distinguishing AGN from starbursts as the origin of double-peaked Lyman-alpha emitters in the reionization era

Hamsa Padmanabhan

Abraham Loeb

Abstract: We discuss the possible origin of the double-peaked profiles recently observed in Lyman-alpha emitters (LAEs) at the epoch of reionization (z ≳ 6.5) from obscured active galactic nuclei (AGN). In combining the extent of the Lyman-α near-zones estimated from the blue peak velocity offset in these galaxies, with the ionizing emissivity of quasars at z ≳ 6, we forecast the intrinsic UV and X-ray luminosities of the AGN needed to give rise to their double-peaked profiles. We also estimate the extent of the obscu… Show more

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Cited by 3 publications

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Wave dark matter and ultra-diffuse galaxies

Pozo

Broadhurst

Martino

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Dark matter as a Bose-Einstein condensate, such as the axionic scalar field particles of String Theory, can explain the coldness of dark matter on large scales. Pioneering simulations in this context predict a rich wave-like structure, with a ground state soliton core in every galaxy surrounded by a halo of excited states that interfere on the de Broglie scale. This de Broglie scale is largest for low mass galaxies as momentum is lower, providing a simple explanation for the wide cores of dwarf spheroidal galaxies. Here we extend these “wave dark matter” (ψDM) predictions to the newly discovered class of “Ultra Diffuse Galaxies” (UDG) that resemble dwarf spheroidal galaxies but with more extended stellar profiles. Currently the best studied example, DF44, has a uniform velocity dispersion of ≃ 33km/s, extending to at least 3 kpc, that we show is reproduced by our ψDM simulations with a soliton radius of ≃ 0.5 kpc. In the ψDM context, we show the relatively flat dispersion profile of DF44 lies between massive galaxies with compact dense solitons, as may be present in the Milky Way on a scale of 100pc and lower mass galaxies where the velocity dispersion declines centrally within a wide, low density soliton, like Antlia II, of radius 3 kpc.

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Wave dark matter and ultra-diffuse galaxies

Pozo

Broadhurst

Martino

et al. 2021

Monthly Notices of the Royal Astronomical Society

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Understanding the ‘feeble giant’ Crater II with tidally stretched wave dark matter

Pozo

Broadhurst

Emami

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The unusually large ‘dwarf’ galaxy Crater II, with its small velocity dispersion, ≃3 km s−1, defies expectations that low-mass galaxies should be small and dense. We combine the latest stellar and velocity dispersion profiles finding Crater II has a prominent dark core of radius $\simeq 0.71^{+0.09}_{-0.08}$ kpc, surrounded by a low density halo, with a transition visible between the core and the halo. We show that this profile matches the distinctive core-halo profile predicted by ‘Wave Dark Matter’ as a Bose-Einstein condensate, ψDM, where the ground state soliton core is surrounded by a tenuous halo of interfering waves, with a marked density transition predicted between the core and halo. Similar core-halo structure is seen in most dwarf spheroidal galaxies (dSphs), but with smaller cores, ≃0.25 kpc and higher velocity dispersions, ≃9 km s−1, and we argue here that Crater II may have been a typical dSph that has lost most of its halo mass to tidal stripping, so its velocity dispersion is lower by a factor of 3 and the soliton is wider by a factor of 3, following the inverse scaling required by the Uncertainty Principle. This tidal solution for Crater II in the context of ψDM is supported by its small pericenter of ≃20 kpc established by Gaia, implying significant tidal stripping of Crater II by the Milky Way is expected.

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Alleviating the Need for Exponential Evolution of JWST Galaxies in 10¹⁰ M _⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum

Padmanabhan

Loeb

2023

ApJL

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We infer the evolution of the UV luminosities of galaxies in haloes of masses 1010–1011 M ⊙ in the redshift range of z ∼ 9–16 from the recent JWST data. Within the standard ΛCDM cosmological model, it is found that the average luminosities in this halo mass range show an exponential evolution with redshift, in excess of that expected from astrophysical considerations including the evolution of UV luminosity from Population III galaxies. We find that an enhancement of power on scales k ∼ 1 Mpc−1, as captured by a cosmological transfer function modified from the ΛCDM form, is able to alleviate this effect and allow for a nonevolving UV luminosity as a function of redshift at z > 10, consistently with the corresponding findings for lower redshifts. We discuss the possible astrophysical and cosmological reasons for such an enhancement.

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Distinguishing AGN from starbursts as the origin of double-peaked Lyman-alpha emitters in the reionization era

Cited by 3 publications

References 62 publications

Wave dark matter and ultra-diffuse galaxies

Wave dark matter and ultra-diffuse galaxies

Understanding the ‘feeble giant’ Crater II with tidally stretched wave dark matter

Alleviating the Need for Exponential Evolution of JWST Galaxies in 10¹⁰ M _⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum

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Product

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About

Distinguishing AGN from starbursts as the origin of double-peaked Lyman-alpha emitters in the reionization era

Cited by 3 publications

References 62 publications

Wave dark matter and ultra-diffuse galaxies

Wave dark matter and ultra-diffuse galaxies

Understanding the ‘feeble giant’ Crater II with tidally stretched wave dark matter

Alleviating the Need for Exponential Evolution of JWST Galaxies in 1010 M ⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum

Contact Info

Product

Resources

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Alleviating the Need for Exponential Evolution of JWST Galaxies in 10¹⁰ M _⊙ Haloes at z > 10 by a Modified ΛCDM Power Spectrum