CROSS-CORRELATION OF NEAR- AND FAR-INFRARED BACKGROUND ANISOTROPIES AS TRACED BY<i>SPITZER</i>AND<i>HERSCHEL</i>

Thacker, Cameron; Gong, Yan; Cooray, Asantha; Bernardis, Francesco De; Smidt, Joseph; Mitchell-Wynne, Ketron

doi:10.1088/0004-637x/811/2/125

Cited by 25 publications

(47 citation statements)

References 56 publications

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“…This has been demonstrated in multi-wavelength cross-correlation studies that provide further constraints for theoretical models of both low-z and highz sources (e.g. Cappelluti et al 2013;Thacker et al 2014). Additional information on the physics and evolution at early times would come by looking for correlations between the CIB and 21 cm maps (Fernandez et al 2014;Mao 2014).…”

Section: Summary and Discussionmentioning

confidence: 86%

On the physical requirements for a pre-reionization origin of the unresolved near-infrared background

Helgason

Ricotti

Kashlinsky

2015

Monthly Notices of the Royal Astronomical Society

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The study of the Cosmic Near-Infrared Background (CIB) light after subtraction of resolved sources can push the limits of current observations and yield information on galaxies and quasars in the early universe. Spatial fluctuations of the CIB exhibit a clustering excess at angular scales ∼1• whose origin has not been conclusively identified, but disentangling the relative contribution from low-and high-redshift sources is not trivial. We explore the likelihood that this signal is dominated by emission from galaxies and accreting black holes in the early Universe. We find that, the measured fluctuation signal is too large to be produced by galaxies at redshifts z>8, which only contribute ∼0.01−0.05 nWm −2 sr −1 to the CIB. Additionally, if the first small mass galaxies have a normal IMF, the light of their ageing stars (fossils) integrated over cosmic time contributes a comparable amount to the CIB as their pre-reionization progenitors. In order to produce the observed level of CIB fluctuation without violating constraints from galaxy counts and the electron optical depth of the IGM, minihalos at z>12 must form preferably top-heavy stars with efficiency f ⋆ 0.1 and at the same time maintain a very low escape fraction of ionizing radiation, f esc <0.1%. If instead the CIB fluctuations are produced by high-z black holes, one requires vigorous accretion in the early universe reaching ρ acc 10 5 M ⊙ Mpc −3 by z≃10. This growth must stop by z∼6 and be significantly obscured not to overproduce the soft cosmic X-ray background (CXB) and its observed coherence with the CIB. We therefore find the range of suitable high-z explanations to be narrow, but could possibly be widened by including additional physics and evolution at those epochs.

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Section: Summary and Discussionmentioning

confidence: 86%

On the physical requirements for a pre-reionization origin of the unresolved near-infrared background

Helgason

Ricotti

Kashlinsky

2015

Monthly Notices of the Royal Astronomical Society

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“…Matsumoto et al (2011) find no correlations of the AKARI source-subtracted diffuse maps with the AKARI far-IR data at 100 µm. Thacker et al (2015) claimed a cross-correlation of Spitzer data with diffuse maps from Herschel at 250, 350 and 500 µm. The Spitzer data at 3.6 µm, with a 0.1 hr net integration depth, was repixelized at the common resolution of 6 ′′ , leading to both significantly larger removed sky and greater shotnoise (i.e.…”

Section: Fig 14 Frommentioning

confidence: 99%

Looking at cosmic near-infrared background radiation anisotropies

et al. 2018

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The cosmic infrared background (CIB) contains emissions accumulated over the entire history of the Universe, including from objects inaccessible to individual telescopic studies. The near-IR (∼ 1 − 10 µm) part of the CIB, and its fluctuations, reflects emissions from nucleosynthetic sources and gravitationally accreting black holes (BHs). If known galaxies are removed to sufficient depths the source-subtracted CIB fluctuations at near-IR can reveal sources present in the first-stars-era and possibly new stellar populations at more recent times. This review discusses the recent progress in this newly emerging field which identified, with new data and methodology, significant source-subtracted CIB fluctuations substantially in excess of what can be produced by remaining known galaxies. The CIB fluctuations further appear coherent with unresolved cosmic X-ray background (CXB) indicating a very high fraction of BHs among the new sources producing the CIB fluctuations. These observations have led to intensive theoretical efforts to explain the measurements and their properties. While current experimental configurations have limitations in decisively probing these theories, their potentially remarkable implications will be tested in the upcoming CIB measurements with the ESA's Euclid dark energy mission. We describe the goals and methodologies of LIBRAE (Looking at Infrared Background Radiation with Euclid), a NASA-selected project for CIB science with Euclid, which has the potential for transforming the field into a new area of precision cosmology. * Alexander. Kashlinsky@nasa.gov; Code 665, Observational Cosmology Lab, E. Probing IGM at pre-reionization: CMB-CIB crosspower 48 F. History of emissions from Lyman tomography 49 G. Probing BAOs and dark energy at 10 < z < 16 50 H. LIBRAE summary 51 VIII. Other forthcoming experimental configurations 52 IX. Outlook for the future 53 X. Appendix: acronyms and abbreviations 54 XI. Acknowledgments 54 References 55 4π c I ν /h Planck = 0.63 Iν MJy/sr cm −3 . For comparison the CMB photons are orders-of-magnitude more abundant with n CMB = 413 cm −3 .CMB observations established the flat geometry of the Universe. We will thus adopt the Friedman-Robertson-Walker flat metric for the Universe with the interval given by dsω are the redshift, comoving coordinate distance, cosmic time, and solid angle. Photons move along null geodesics, ds 2 = 0. The Friedman equations with the matter, dark energy (Λ), radiation/relativistic component and curvature density parameters Ω m , Ω Λ , Ω γ , Ω K lead to c(1 + z)dt/dz = R H /E(z), where E(z) ≡ [Ω γ (1 + z) 4 + Ω m (1 + z) 3 + Ω K (1 + z) 2 + Ω Λ f (z)] 1/2 with f (z) describing the evolution of DE and R H ≡ cH −1 0 . The Hubble constant is H(z) = H 0 E(z) and the distance measures become: the coordinate distance x(z) = c (1 + z)dt = R H z 0 dz/E(z), the comoving angular di-Advanced CCD Imaging Spectrometer -imaging arrays AEGIS XD All-wavelength Extended Groth strip International Survey -X-ray, deep AGB Asymptotic giant branch AKARI A Japane...

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“…We also examined the near-IR and far-IR cross correlation using the PolSpice analysis Planck is shown in figure 15. The fluctuation seems to have smooth connection with Herschel 350 µm one (Thacker et al 2015) toward smaller angular scales.…”

Section: Discussionmentioning

confidence: 77%

“…Note that the Spitzer (3.6 µm) spectrum is scaled to the IRTS 2.2 µm under the Rayleigh-Jeans assumption for the comparison. According to the measurements at sub-degree scale by Thacker et al (2015), about half of the near-IR background can be explained by dusty, star forming galaxies, and the residuals can be explained by the IHL.…”

Section: Discussionmentioning

confidence: 99%

Large angular scale fluctuations of near-infrared extragalactic background light based on the IRTS observations

Kim

Matsumoto

Lee

et al. 2019

Publications of the Astronomical Society of Japan

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Abstract We measure the spatial fluctuations of the Near-Infrared Extragalactic Background Light (NIREBL) from 2° to 20° in angular scale at the 1.6 and $2.2\, \mu \mathrm{m}$ using data obtained with Near-Infrared Spectrometer (NIRS) on board the Infrared Telescope in Space (IRTS). The brightness of the NIREBL is estimated by subtracting foreground components such as zodiacal light, diffuse Galactic light, and integrated star light from the observed sky. The foreground components are estimated using well-established models and archive data. The NIREBL fluctuations for the 1.6 and $2.2\, \mu \mathrm{m}$ connect well toward the sub-degree scale measurements from previous studies. Overall, the fluctuations show a wide bump with a center at around 1° and the power decreases toward larger angular scales with nearly a single power-law spectrum (i.e., ${F[\sqrt{l(l+1)C_l/2\pi }]} \sim \theta ^{-1}]$, indicating that the large-scale power is dominated by the random spatial distribution of the sources. After examining several known sources, contributors such as normal galaxies, high-redshift objects, intra-halo light, and far-IR cosmic background, we conclude that the excess fluctuation at around the 1° scale cannot be explained by any of them.

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CROSS-CORRELATION OF NEAR- AND FAR-INFRARED BACKGROUND ANISOTROPIES AS TRACED BYSPITZERANDHERSCHEL

Cited by 25 publications

References 56 publications

On the physical requirements for a pre-reionization origin of the unresolved near-infrared background

On the physical requirements for a pre-reionization origin of the unresolved near-infrared background

Looking at cosmic near-infrared background radiation anisotropies

Large angular scale fluctuations of near-infrared extragalactic background light based on the IRTS observations

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