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Sarah E I on Muck Rack

Sarah E I

As seen in: arXiv, Oxford Academic, Oxford University Press (OUP), Caltech
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Articles by Sarah E I

Astrophysics > Astrophysics of Galaxies

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By Sarah E I
| arXiv
arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website. Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them. Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.
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Astrophysics > Astrophysics of Galaxies

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By Hiddo S B, Sarah E I
| arXiv
arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website. Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them. Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.
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Astrophysics > Astrophysics of Galaxies

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By Emanuele Paolo, Larry Lindsey, Sarah E I
| arXiv
arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website. Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them. Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.
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A z ∼ 6.2 Quasar on the Local M_BH–σ* Relation Quenching Its Host Galaxy from the Aether Survey

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By Emanuele Paolo, Sarah E I, Fabrizio Arrigoni
| Caltech
Acknowledgement WL thanks John Silverman for his constructive suggestions. W.L. acknowledges support from NASA through STScI grants JWST-Survey-3428 and HST-GO-17758. R.D. acknowledges support from the PRORIS 2025 “CosmoWebb” and the INAF minigrant 2024: “The interstellar medium at high redshift.” M.O. is supported by the Japan Society for the Promotion of Science (JSPS) KAKENHI grant No. 24K22894 and 26K07155.
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Astrophysics > Astrophysics of Galaxies

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By Sarah E I, Sarah E. I. Bosman
| arXiv
arXivLabs is a framework that allows collaborators to develop and share new arXiv features directly on our website. Both individuals and organizations that work with arXivLabs have embraced and accepted our values of openness, community, excellence, and user data privacy. arXiv is committed to these values and only works with partners that adhere to them. Have an idea for a project that will add value for arXiv's community? Learn more about arXivLabs.
Open in Who Shared View Duplicates (690) Issue with article?

Deep learning the intergalactic medium using Lyman-alpha forest at 4 ≤ z ≤ 5

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By Max-Planck-Institut für Astronomie, Sarah E I
| Oxford Academic Verified
Accurately understanding the thermal history of the intergalactic medium (IGM) stands as a fundamental goal in astronomy, as it offers crucial insights into the timing and duration of the H i and He ii reionization epochs. One of the most robust methods for probing this thermal history is through the examination of Lyα absorption, commonly known as the Ly forest, observed in the spectra of quasars (Becker, Bolton & Lidz 2015).
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E-XQR-30: The evolution of Mg ii, C ii, and O i across 2 < z < 6

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By Alma Maria, Blackford Hill, Piazza Dei Cavalieri, Sarah E I
| Oxford University Press (OUP)
The Epoch of Reionization (EoR) marks a major transition in the evolutionary history of the Universe when cosmic neutral hydrogen was (re)ionized by ultraviolet (UV) radiation from the first light sources and thereby marked an end to the Dark Ages. Studying reionization involves the understanding of the nature, formation and evolution of the first generation of stars and galaxies, quasars and the nature of the ionizing radiation.
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E-XQR-30: The evolution of Mg ii, C ii and O i across 2 < z < 6

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By Alma Maria, Blackford Hill, Sarah E I, P.zzadei Cavalieri
| Oxford University Press (OUP)
Intervening metal absorbers in quasar spectra at z > 6 can be used as probes to study the chemical enrichment of the Universe during the Epoch of Reionization (EoR).
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Measuring the photo-ionization rate, neutral fraction and mean free path of H i ionizing photons at 4.9 ≤ z ≤ 6.0 from a large sample of XShooter and ESI spectra | Monthly Notices of the Royal Astronomical Society | Oxford Academic

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By Max-Planck-Institut für Astronomie, Madingley Road, Homi Bhabha Road, Sarah E I
| Oxford University Press (OUP)
We measure the mean free path (⁠|$\lambda _{\rm mfp,H\, \small {I}}$|⁠), photo-ionization rate (⁠|$\langle \Gamma _{\rm H\, \small {I}} \rangle$|⁠) and neutral fraction (⁠|$\langle f_{\rm H\, \small {I}} \rangle$|⁠) of hydrogen in 12 redshift bins at 4.85 < z < 6.05 from a large sample of moderate resolution XShooter and ESI QSO absorption spectra.
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