Reconstructing the fraction of baryons in the intergalactic medium with fast radio bursts via Gaussian processes

Qiang, Da-Chun; Hao, Wei

doi:10.1088/1475-7516/2020/04/023

Cited by 15 publications

(16 citation statements)

References 136 publications

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“…The total baryon density of the Universe, Ω baryons =0.0455, is well constrained from measurements of Cosmic Microwave Background (CMB) anisotropies (Aghanim et al 2016), light element abundances coupled with Big Bang nucleosynthesis (Cooke & Fumagalli 2018) and, in the near future, from observations of dispersion measures (DM) of Fast Radio Bursts (FRBs) (e.g. Qiang & Wei 2020;Macquart et al 2020). We note that results from these different experiments involving vastly different physical processes and observation techniques agree remarkably well.…”

Section: Introductionmentioning

confidence: 82%

Tracing the 10$^7$K Warm-Hot Intergalactic Medium with UV absorption lines

Fresco,

Péroux,

Merloni

et al. 2020

Preprint

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Today, the majority of the cosmic baryons in the Universe are not observed directly, leading to an issue of "missing baryons" at low redshift. Cosmological hydrodynamical simulations have indicated that a significant portion of them will be converted into the so-called Warm-Hot Intergalactic Medium (WHIM), with gas temperature ranging between 10 5 -10 7 K. While the cooler phase of this gas has been observed using O VI and Ne VIII absorbers at UV wavelengths, the hotter fraction detection relies mostly on observations of O VII and O VIII at X-ray wavelengths. Here, we target the forbidden line of [Fe XXI] λ 1354Å which traces 10 7 K gas at UV wavelengths, using more than one hundred high-spectral resolution (R∼49,000) and high signal to noise VLT/UVES quasar spectra, corresponding to over 600 hrs of VLT time observations. A stack of these at the position of known DLAs lead to a 5-σ limit of log[N([Fe XXI])] <17.4 (EW r est < 22mÅ), three orders of magnitude higher than the expected column density of the WHIM log[N([Fe XXI])] <14.5. This work proposes an alternative to X-ray detected 10 7 K WHIM tracers, by targeting faint lines at UV wavelengths from the ground benefiting from higher instrumental throughput, enhanced spectral resolution, longer exposure times and increased number of targets. The number of quasar spectra required to reach this theoretical column density with future facilities including 4MOST, ELT/HIRES, MSE and the Spectroscopic Telescope appears challenging at present. Probing the missing baryons is essential to constrain the accretion and feedback processes which are fundamental to galaxy formation.

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Section: Introductionmentioning

confidence: 82%

Tracing the 10$^7$K Warm-Hot Intergalactic Medium with UV absorption lines

Fresco,

Péroux,

Merloni

et al. 2020

Preprint

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“…While it is well known that ∼ 90% of the baryons are locked in the IGM at z 1.5 (Meiksin 2009;McQuinn 2016), the value of f IGM (z) at lower redshift is not yet precisely known, and as such it is the subject of ongoing research (e.g. Li et al 2019Li et al , 2020Qiang & Wei 2020). We show the recent measurement of f IGM (z) from observations of fast radio bursts (FRBs) at z ∼ 0 by Li et al (2020) with the teal circle in Figure A4.…”

Section: A3 Comparison With Observationsmentioning

confidence: 99%

Extended Hernquist–Springel formalism for cosmic star formation

Sorini

Peacock

2021

Monthly Notices of the Royal Astronomical Society

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We present a revised and extended version of the analytic model for cosmic star formation originally given by Hernquist & Springel in 2003. The key assumption of this formalism is that star formation proceeds from cold gas, at a rate that is limited by an internal consumption timescale at early times, or by the rate of generation of gas via cooling at late times. These processes are analysed as a function of the mass of dark matter haloes and integrated over the halo population. We modify this approach in two main ways to make it more general: (1) halo collapse times are included explicitly, so that the behaviour is physically reasonable at late times; (2) allowance is made for a mass-dependent baryon fraction in haloes, which incorporates feedback effects. This model reproduces the main features of the observed baryonic Tully-Fisher relationship, and is consistent with observational estimates of the baryon mass fraction in the intergalactic medium. With minimal adjustment of parameters, our approach reproduces the observed history of cosmic star formation within a factor of two over the redshift range 0 < z < 10. This level of agreement is comparable to that achieved by state-of-the-art cosmological simulations. Our simplified apparatus has pedagogical value in illuminating the results of such detailed calculations, and also serves as a means for rapid approximate exploration of non-standard cosmological models.

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“…While it is well known that ∼ 90% of the baryons are locked in the IGM at 𝑧 1.5 (Meiksin 2009;McQuinn 2016), the value of 𝑓 IGM (𝑧) at lower redshift is not yet precisely known, and as such it is the subject of ongoing research (e.g. Li et al 2019Li et al , 2020Qiang & Wei 2020). We show the recent measurement of 𝑓 IGM (𝑧) from observations of fast radio bursts (FRBs) at 𝑧 ∼ 0 by Li et al (2020) with the teal circle in Figure A4.…”

Section: Data Availabilitymentioning

confidence: 99%

Extended Hernquist-Springel formalism for cosmic star formation

Sorini,

Peacock

2021

Preprint

View full text Add to dashboard Cite

We present a revised and extended version of the analytic model for cosmic star formation originally given by Hernquist & Springel in 2003. The key assumption of this formalism is that star formation proceeds from cold gas, at a rate that is limited by an internal consumption timescale at early times, or by the rate of generation of gas via cooling at late times. These processes are analysed as a function of the mass of dark matter haloes and integrated over the halo population. We modify this approach in two main ways to make it more general: (1) halo collapse times are included explicitly, so that the behaviour is physically reasonable at late times; (2) allowance is made for a mass-dependent baryon fraction in haloes, which incorporates feedback effects. This model reproduces the main features of the observed baryonic Tully-Fisher relationship, and is consistent with observational estimates of the baryon mass fraction in the intergalactic medium. With minimal adjustment of parameters, our approach reproduces the observed history of cosmic star formation within a factor of two over the redshift range 0 < 𝑧 < 10. This level of agreement is comparable to that achieved by state-of-the-art cosmological simulations. Our simplified apparatus has pedagogical value in illuminating the results of such detailed calculations, and also serves as a means for rapid approximate exploration of non-standard cosmological models.

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Reconstructing the fraction of baryons in the intergalactic medium with fast radio bursts via Gaussian processes

Cited by 15 publications

References 136 publications

Tracing the 10$^7$K Warm-Hot Intergalactic Medium with UV absorption lines

Tracing the 10$^7$K Warm-Hot Intergalactic Medium with UV absorption lines

Extended Hernquist–Springel formalism for cosmic star formation

Extended Hernquist-Springel formalism for cosmic star formation

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