Evolution of dispersion in the cosmic deuterium abundance

Dvorkin, Irina; Vangioni, Elisabeth; Silk, Joseph; Petitjean, P.; Olive, Keith A.

doi:10.1093/mnrasl/slw028

Cited by 24 publications

(39 citation statements)

References 42 publications

(72 reference statements)

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“…We however caution that a high-resolution spectrum with high S/N ratio is necessary to better take into account blends with the Ly-α forest and confirm our measurement. 1 We do not take into account astration of the order of 0.1 dex due to the high metallicity and redshift of our system (see Dvorkin et al 2016). …”

Section: +016mentioning

confidence: 99%

Discovery of a Perseus-like cloud in the early Universe

Noterdaeme

Krogager

Balashev

et al. 2017

A&A

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We present the discovery of a molecular cloud at z abs ≈ 2.5255 along the line of sight to the quasar SDSS J 000015.17+004833.3. We use a high-resolution spectrum obtained with the Ultraviolet and Visual Echelle Spectrograph together with a deep multi-wavelength medium-resolution spectrum obtained with X-shooter (both on the Very Large Telescope) to perform a detailed analysis of the absorption lines from ionic, neutral atomic and molecular species in different excitation levels, as well as the broad-band dust extinction.We find that the absorber classifies as a Damped Lyman-α system (DLA) with log N(H i) (cm −2 ) = 20.8 ± 0.1. The DLA has supersolar metallicity (Z ∼ 2.5 Z , albeit to within a factor of two to three) with a depletion pattern typical of cold gas and an overall molecular fraction f = 2N(H 2 )/(2N(H 2 ) + N(H i)) ∼ 50%. This is the highest f -value observed to date in a high-z intervening system. Most of the molecular hydrogen arises from a clearly identified narrow (b ∼ 0.7 km s −1 ), cold component in which carbon monoxide molecules are also found, with log N(CO) ≈ 15. With the help of the spectral synthesis code Cloudy, we study the chemical and physical conditions in the cold gas. We find that the line of sight probes the gas deep after the H i-to-H 2 transition in a ∼4−5 pc-size cloud with volumic density n H ∼ 80 cm −3 and temperature of only 50 K. Our model suggests that the presence of small dust grains (down to about 0.001 µm) and high cosmic ray ionisation rate (ζ H ∼ a few times 10 −15 s −1 ) are needed to explain the observed atomic and molecular abundances. The presence of small grains is also in agreement with the observed steep extinction curve that also features a 2175 Å bump. Interestingly, the chemical and physical properties of this cloud are very similar to what is seen in diffuse molecular regions of the nearby Perseus complex, despite the former being observed when the Universe was only 2.5 Gyr old. The high excitation temperature of CO rotational levels towards J0000+0048 betrays however the higher temperature of the cosmic microwave background. Using the derived physical conditions, we correct for a small contribution (0.3 K) of collisional excitation and obtain T CMB (z = 2.53) ≈ 9.6 K, in perfect agreement with the predicted adiabatic cooling of the Universe.

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Section: +016mentioning

confidence: 99%

Discovery of a Perseus-like cloud in the early Universe

Noterdaeme

Krogager

Balashev

et al. 2017

A&A

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“…In addition, the assumption that D/H=D I/H I is justified in these systems; the ionization correction is expected to be 0.1% (Savin 2002;Cooke & Pettini 2016). Furthermore, galactic chemical evolution models suggest that most of the deuterium atoms in these almost pristine systems are yet to be cycled through many generations of stars; the correction for astration (i.e., the processing of gas through stars) is therefore negligible (see the comprehensive list of references provided by Cyburt et al 2016;Dvorkin et al 2016).…”

Section: Introductionmentioning

confidence: 99%

THE PRIMORDIAL DEUTERIUM ABUNDANCE OF THE MOST METAL-POOR DAMPED Lyα SYSTEM^∗

Cooke

Pettini

Nollett

et al. 2016

ApJ

140

161

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“…We use the complete formulae for the angular power spectrum, derived in Cusin, Pitrou & Uzan (2017), see also , in our analysis. et al (2016a,b); Dvorkin et al (2018), which we summarize below (see the companion article for extensive explanations). For each model, we compute the GW luminosity L G (z, f G , M G ) of a given galaxy as a function of halo mass M G and redshift z as follows.…”

Section: Astrophysical Building Blocksmentioning

confidence: 90%

“…The overall factor β is used to normalize our model with respect to the number of events observed by LIGO/Virgo. Following Dvorkin et al (2018), the birth rate of binaries with component masses (m, m ≤ m) is R bin (m, m ) = R2(m)R2(m )P (m, m ), where P (m, m ) is a normalized distribution describing the association of mass m and m in a BH binary system.…”

Section: Astrophysical Building Blocksmentioning

confidence: 99%

Stochastic gravitational wave background anisotropies in the mHz band: astrophysical dependencies

Cusin

Dvorkin

Pitrou

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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We show that the anisotropies of the astrophysical stochastic gravitational wave background in the mHz band have a strong dependence on the modelling of galactic and sub-galactic physics. We explore a wide range of self-consistent astrophysical models for stellar evolution and for the distribution of orbital parameters, all calibrated such that they predict the same number of resolved mergers to fit the number of detections during LIGO/Virgo O1+O2 observations runs. We show that different physical choices for the process of black hole collapse and cut-off in the black hole mass distribution give fractional differences in the angular power spectrum of anisotropies up to 50% on all angular scales. We also point out that the astrophysical information which can be extracted from anisotropies is complementary to the isotropic background and individual mergers. These results underline the interest in the anisotropies of the stochastic gravitational wave background as a new and potentially rich field of research, at the cross-road between astrophysics and cosmology.

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Evolution of dispersion in the cosmic deuterium abundance

Cited by 24 publications

References 42 publications

Discovery of a Perseus-like cloud in the early Universe

Discovery of a Perseus-like cloud in the early Universe

THE PRIMORDIAL DEUTERIUM ABUNDANCE OF THE MOST METAL-POOR DAMPED Lyα SYSTEM^∗

Stochastic gravitational wave background anisotropies in the mHz band: astrophysical dependencies

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Evolution of dispersion in the cosmic deuterium abundance

Cited by 24 publications

References 42 publications

Discovery of a Perseus-like cloud in the early Universe

Discovery of a Perseus-like cloud in the early Universe

THE PRIMORDIAL DEUTERIUM ABUNDANCE OF THE MOST METAL-POOR DAMPED Lyα SYSTEM∗

Stochastic gravitational wave background anisotropies in the mHz band: astrophysical dependencies

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THE PRIMORDIAL DEUTERIUM ABUNDANCE OF THE MOST METAL-POOR DAMPED Lyα SYSTEM^∗