New synthesis models of consistent extragalactic background light over cosmic time

Khaire, Vikram; Srianand, R.

doi:10.1093/mnras/stz174

Cited by 131 publications

(157 citation statements)

References 280 publications

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“…The only massive group in the field with multiple galaxies of L > 0.25L * near the blazar sightline is at z = 0.433, a strong indication that 1ES 1553+113 is a member of this galaxy group. toionization from the blazar (λL λ = 10 46 erg s −1 at 1 Rydberg and UV spectral slope of α = −1.4 based the COS spectrum) and UV background (Khaire & Srianand 2019) as shown in Figure 4. Nicastro et al (2018) demonstrated that the O VII detection and O VI/O VIII non-detections at z = 0.4339 require a gas temperature of T ≈ 10 6 K with little contribution from photoionization.…”

Section: Discovery and Redshift Of The Group Hosting 1es 1553+113mentioning

confidence: 99%

The Physical Origins of the Identified and Still Missing Components of the Warm–Hot Intergalactic Medium: Insights from Deep Surveys in the Field of Blazar 1ES1553+113

Johnson

Mulchaey

Chen

et al. 2019

ApJL

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The relationship between galaxies and the state/chemical enrichment of the warm-hot intergalactic medium (WHIM) expected to dominate the baryon budget at low-z provides sensitive constraints on structure formation and galaxy evolution models. We present a deep redshift survey in the field of 1ES1553+113, a blazar with a unique combination of UV+X-ray spectra for surveys of the circum-/intergalactic medium (CGM/IGM). Nicastro et al. (2018) reported the detection of two O VII WHIM absorbers at z = 0.4339 and 0.3551 in its spectrum, suggesting that the WHIM is metal-rich and sufficient to close the missing baryons problem. Our survey indicates that the blazar is a member of a z = 0.433 group and that the higher-z O VII candidate arises from its intragroup medium. The resulting bias precludes its use in baryon censuses. The z = 0.3551 candidate occurs in an isolated environment 630 kpc from the nearest galaxy (with stellar mass log M * /M ≈ 9.7) which we show is unexpected for the WHIM. Finally, we characterize the galactic environments of broad H I Lyα absorbers (Doppler widths of b = 40 − 80 km s −1 ; T 4 × 10 5 K) which provide metallicity independent WHIM probes. On average, broad Lyα absorbers are ≈2× closer to the nearest luminous (L > 0.25L * ) galaxy (700 kpc) than narrow (b < 30 km s −1 ; T 4 × 10 5 K) ones (1300 kpc) but ≈2× further than O VI absorbers (350 kpc). These observations suggest that gravitational collapse heats portions of the IGM to form the WHIM but with feedback that does not enrich the IGM far beyond galaxy/group halos to levels currently observable in UV/X-ray metal lines.

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Section: Discovery and Redshift Of The Group Hosting 1es 1553+113mentioning

confidence: 99%

The Physical Origins of the Identified and Still Missing Components of the Warm–Hot Intergalactic Medium: Insights from Deep Surveys in the Field of Blazar 1ES1553+113

Johnson

Mulchaey

Chen

et al. 2019

ApJL

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“…Notice, that in this figure measurements byBecker & Bolton (2013) andFaucher-Giguère et al (2008a) are not corrected to the cosmology used in this paper. The solid curve shows a model from(Khaire & Srianand 2019).…”

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confidence: 99%

Thermal State of the Intergalactic Medium at z ∼ 2–4

Telikova

Shternin

Balashev

2019

ApJ

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We present a new method to infer parameters of the temperature-density relation in the intergalactic medium in the post-reionization epoch at z ∼ 2 − 4. This method is based on the analysis of the Lyα absorbers distribution over column densities and Doppler parameters by the model joint probability density function. This approach allows us to measure the power-law index γ of the temperaturedensity relation and a certain combination of the temperature at the mean density T 0 and hydrogen photoionization rate Γ. To estimate T 0 and Γ separately, we employ measurements of the Lyα forest effective opacity and the model gas probability density function. We show that γ tends to be lower than 1.6 and reaches 1.3 at redshift ∼ 3. The inferred temperatures at the mean density are ∼ (2±0.5)×10 4 K in the studied redshift range. Both these estimates favour He ii reionization at z 3. We find that the hydrogen photoionization rate is ∼ 0.6 × 10 −12 s −1 , which is consistent with previous measurements.

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“…Notice that the measurements from [20] are not corrected for the cosmology used in the present paper. The solid curve shows a model from [21]. of the Lyα lines is a sum of two contributions…”

Section: Methodsmentioning

confidence: 99%

Jeans smoothing of the Ly forest absorption lines

Telikova

Balashev

Shternin

2019

J. Phys.: Conf. Ser.

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We investigate a contribution of the Jeans smoothing to the minimal width of Lyα forest lines and discuss how the accounting for this additional broadening affects the inferred parameters of the intergalactic matter equation of state. We estimate a power-law index γ of the equation of state, a temperature at the mean density T0 and a hydrogen photoionization rate Γ within 4 redshift bins. Furthermore, in each bin we obtain an upper limit on the scaleparameter fJ, which sets the relation between the Jeans length and the characteristic physical size of the absorber clouds.

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New synthesis models of consistent extragalactic background light over cosmic time

Cited by 131 publications

References 280 publications

The Physical Origins of the Identified and Still Missing Components of the Warm–Hot Intergalactic Medium: Insights from Deep Surveys in the Field of Blazar 1ES1553+113

The Physical Origins of the Identified and Still Missing Components of the Warm–Hot Intergalactic Medium: Insights from Deep Surveys in the Field of Blazar 1ES1553+113

Thermal State of the Intergalactic Medium at z ∼ 2–4

Jeans smoothing of the Ly forest absorption lines

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