Detecting high-<i>z</i>galaxies in the near-infrared background

Yue, Bin; Ferrara, Andrea; Helgason, Kari

doi:10.1093/mnras/stw511

Cited by 7 publications

(6 citation statements)

References 55 publications

(68 reference statements)

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“…The authors argue that the cross-power is of extragalactic origin, although it is not possible to determine if the signal is produced by a single population of sources (accreting BHs) or by different populations in the same area. Indeed, theoretical models show that highly obscured accreting black holes with mass [10 4 − 10 6 ] M at z > 13 provide a natural explanation for the observed signal (Yue et al 2013(Yue et al , 2014, requiring a number density of active BHs of [2.7 − 4] × 10 −5 M Mpc −3 at z ∼ 13 (Yue et al 2016). While a detailed calculation of the cross-correlation between CXB and CIB is beyond the scope of the present analysis, in the right panel of Fig.…”

Section: Resultsmentioning

confidence: 99%

Faint progenitors of luminousz ∼ 6 quasars: Why do not we see them?

Pezzulli

Valiante

Orofino

et al. 2016

Mon. Not. R. Astron. Soc.

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Observational searches for faint active nuclei at z > 6 have been extremely elusive, with a few candidates whose high-z nature is still to be confirmed. Interpreting this lack of detections is crucial to improve our understanding of high-z supermassive black holes (SMBHs) formation and growth. In this work, we present a model for the emission of accreting BHs in the X-ray band, taking into account super-Eddington accretion, which can be very common in gas-rich systems at high-z. We compute the spectral energy distribution for a sample of active galaxies simulated in a cosmological context, which represent the progenitors of a z ∼ 6 SMBH with M BH ∼ 10 9 M . We find an average Compton thick fraction of ∼ 45% and large typical column densities (N H 10 23 cm 2 ). However, faint progenitors are still luminous enough to be detected in the X-ray band of current surveys. Even accounting for a maximum obscuration effect, the number of detectable BHs is reduced at most by a factor 2. In our simulated sample, observations of faint quasars are mainly limited by their very low active fraction ( f act ∼ 1%), which is the result of short, super-critical growth episodes. We suggest that to detect high-z SMBHs progenitors, large area surveys with shallower sensitivities, such as Cosmos Legacy and XMM-LSS+XXL, are to be preferred with respect to deep surveys probing smaller fields, such as CDF-S. 1 Hereafter we adopt a Lambda Cold Dark Matter (ΛCDM) cosmology with parameters Ω M = 0.314, Ω Λ = 0.686, and h = 0.674 (Planck Collaboration et al. 2014).

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Section: Resultsmentioning

confidence: 99%

Faint progenitors of luminousz ∼ 6 quasars: Why do not we see them?

Pezzulli

Valiante

Orofino

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The cross-power was interpreted as imprints from early accreting black holes, e.g. by Direct Collapse Black Holes (DCBH, Yue et al 2013Yue et al , 2016 at z>12 or Primordial LIGOtype Black Holes (PBH, Kashlinsky 2016).…”

Section: Introductionmentioning

confidence: 99%

“…However, these studies of the CIB-CXB cross power are limited to an angular scale within ∼1000 due to the small fields studied, although a larger field is better, given that the power spectra at the larger angular scale are less dominated by the noise and better constrained by the models (Yue et al 2013(Yue et al , 2016(Yue et al , 2017. Moreover, even after stacking of a few fields in C17, no significant cross correlation between CIB and CXB other than the [0.5-2] keV band was found.…”

Section: Introductionmentioning

confidence: 99%

The SPLASH and Chandra COSMOS Legacy Survey: The Cross-power between Near-infrared and X-Ray Background Fluctuations

Cappelluti

Arendt

et al. 2018

ApJ

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We study the source-subtracted near-infrared and X-ray background fluctuations of the COSMOS field using data from the Spitzer SPLASH program (∼1272 hours) and Chandra COSMOS Legacy Survey (4.6 Ms). The new auto power spectra of the cosmic infrared and X-ray background fluctuations reach maximum angular scales of ∼ 3000 and ∼ 5000 , respectively. We measure the cross power spectra between each infrared and X-ray band and calculate the mean power above 20 . We find that the soft X-ray band is correlated with 3.6 and 4.5 µm at ∼ 4 σ significance level. The significance between hard X-ray and the 3.6 µm (4.5 µm) band is ∼ 2.2 σ (∼ 3.8 σ). The combined infrared (3.6 + 4.5 µm) data are correlated with the X-ray data in soft ([0.5-2] keV), hard ([2-7] keV) and broad ([0.5-7] keV) bands at ∼ 5.6 σ, ∼ 4.4 σ and ∼ 6.6 σ level, respectively. We compare the new measurements with existing models for the contributions from known populations at z<7, which are not subtracted. The model predictions are consistent with the measurements but we cannot rule out contributions from other components, such as Direct Collapse Black Holes (DCBH). However, the stacked cross-power spectra, combining other available data, show excess fluctuations about an order of magnitude on average at ∼4σ confidence at scales within ∼300 . By studying the X-ray SED of the cross-power signal, assuming no significant variation from the infrared, we find that its shape is consistent with DCBHs.

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“…Its origin, however, was not further investigated as it was not relevant to the main focus of their work, which was a possible clustering signal of very high redshift (z > 5) AGN via a cross-correlation analysis with the cosmic near-infrared (NIR) background (also see e.g. Yue et al 2013;Yue, Ferrara & Helgason 2016;Helgason et al 2016;Mitchell-Wynne et al 2016).…”

Section: Introductionmentioning

confidence: 99%

Studying the ICM in clusters of galaxies via surface brightness fluctuations of the cosmic X-ray background

Kolodzig

Gilfanov

Hütsi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We study the surface brightness fluctuations of the cosmic X-ray background (CXB) using Chandra data of XBOOTES. After masking out resolved sources we compute the power spectrum of fluctuations of the unresolved CXB for angular scales from ≈ 2 ′′ to ≈ 3• . The nontrivial large-scale structure (LSS) signal dominates over the shot noise of unresolved point sources at all scales above ∼ 1 ′ and is produced mainly by the intracluster medium (ICM) of unresolved clusters and groups of galaxies, as shown in our previous publication.The shot-noise-subtracted power spectrum of CXB fluctuations has a power-law shape with the slope of Γ = 0.96 ± 0.06. Its energy spectrum is well described by the redshifted emission spectrum of optically-thin plasma with the best-fit temperature of T ≈ 1.3 keV and the best-fit redshift of z ≈ 0.40. They are in good agreement with theoretical expectations based on the X-ray luminosity function and scaling relations of clusters. From these values we estimate the typical mass and luminosity of the objects responsible for CXB fluctuations, M 500 ∼ 10 13.6 M ⊙ h −1 and L 0.5−2.0 keV ∼ 10 42.5 erg s −1 . On the other hand, the fluxweighted mean temperature and redshift of resolved clusters are T ≈ 2.4 keV and z ≈ 0.23, confirming that fluctuations of unresolved CXB are caused by cooler (i.e. less massive) and more distant clusters, as expected. We show that the power spectrum shape is sensitive to the ICM structure all the way to the outskirts, out to ∼ few × R 500 . We also look for possible contribution of the warm-hot intergalactic medium (WHIM) to the observed CXB fluctuations.Our results underline the significant diagnostics potential of the CXB fluctuation analysis in studying the ICM structure in clusters.

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Detecting high-zgalaxies in the near-infrared background

Cited by 7 publications

References 55 publications

Faint progenitors of luminousz ∼ 6 quasars: Why do not we see them?

Faint progenitors of luminousz ∼ 6 quasars: Why do not we see them?

The SPLASH and Chandra COSMOS Legacy Survey: The Cross-power between Near-infrared and X-Ray Background Fluctuations

Studying the ICM in clusters of galaxies via surface brightness fluctuations of the cosmic X-ray background

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