<i>AKARI</i>OBSERVATION OF THE FLUCTUATION OF THE NEAR-INFRARED BACKGROUND

Matsumoto, Toshio; Seo, Hyunjong; Jeong, Wooju; Lee, Hyung Mok; Matsuura, Shuji; Matsuhara, Hideo; Oyabu, Shinki; Pyo, Jeonghyun; Wada, Takehiko

doi:10.1088/0004-637x/742/2/124

Cited by 90 publications

(154 citation statements)

References 44 publications

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“…Collaboration 2013; Biteau & Williams 2015). (Kashlinsky et al , 2007aCooray et al 2012b), HST/NICMOS (Thompson et al 2007a,b) and AKARI/IRC (Matsumoto et al 2011;Seo et al 2015), confirm a mutually consistent isotropic signal above the noise extending out to ∼1…”

Section: Introductionmentioning

confidence: 82%

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: Introductionmentioning

confidence: 82%

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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“…Such measurements are difficult due to the presence of the strong interplanetary zodaical light but seem to indicate a flux level of νI ν ∼ 10 nW m −2 sr −1 above what is expected from the known galaxy population. Measurements of the fluctuation power spectrum at different wavelengths appear to be much less affected by zodaical light and yield fluctuation levels of ≈ 0.1 nW m −2 sr −1 (Kashlinsky et al 2005(Kashlinsky et al , 2012.8 µm with Spitzer; Matsumoto et al 2011 at 2.4, 3.1 µm with AKARI; Thompson et al 2007 at 1.1 and 1.6 µm with NICMSOS/HST). Theoretically, the most exciting interpretation of the NIRB is that it originates from the many small and faint galaxies at z > 6, some of which could still have massive metal-free (PopIII) stars (see e.g.…”

Section: -Near Infrared Backgroundmentioning

confidence: 96%

Reionization and the Cosmic Dawn with the Square Kilometre Array

et al. 2013

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The Square Kilometre Array (SKA) will have a low frequency component (SKA-low) which has as one of its main science goals the study of the redshifted 21cm line from the earliest phases of star and galaxy formation in the Universe. This 21cm signal provides a new and unique window both on the time of the formation of the first stars and accreting black holes and the subsequent period of substantial ionization of the intergalactic medium. The signal will teach us fundamental new things about the earliest phases of structure formation, cosmology and even has the potential to lead to the discovery of new physical phenomena. Here we present a white paper with an Executive SummaryThe Square Kilometre Array (SKA) will have a low frequency component (AA-low/SKA-low 1 ) which has as one of its main science goals the study of the redshifted 21cm line from the earliest phases of star and galaxy formation in the Universe (see SKA Memo 125). It is during this phase that the first building blocks of the galaxies that we see around us today, including our own Milky Way, were formed. It is a crucial period for understanding the history of the Universe and one for which we have currently very little observational data.We divide the period into two different phases based on the physical processes which affect the Intergalactic Medium. The first period, which we call the Cosmic Dawn, saw the formation of the first stars and accreting black holes, which changed the quantum state of the still neutral Intergalactic Medium. The second period, known as the Epoch of Reionization, is the one during which large areas between the galaxies were photo-ionized by the radiation produced in galaxies and which ended when the Intergalactic Medium had become completely ionized.Observations of the redshifted 21-cm line with SKA will provide a new and unique window on the entire period of Cosmic Dawn and Reionization. The signal is sensitive to the emergence of the first stellar populations, radiation from growing massive black holes and the formation of larger groups of galaxies and bright quasars. At the same time it maps the distribution of most of the baryonic matter in the Universe. The study of the redshifted 21cm line will teach us fundamental new things about the earliest phases of structure formation and cosmology. It even has the potential to lead to the discovery of new physical phenomena. Here we present an overview of the science questions that SKA-low can address, how we plan to tackle these questions and what this implies for the basic design of the telescope.The redshifted 21cm signal will be analyzed with different techniques, which each come with their own requirements for the SKA: (i) Tomography, (ii) power-spectra and higher-order statistics, (iii) hydrogen absorption, (iv) global/total-intensity signal. Whereas all precursors/pathfinders aim to study the signal statistically through its power spectrum, SKA will be able to image the neutral hydrogen distribution directly and its focus will therefore be more on tomograph...

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“…Previous measurements of the EBL have been of two types: direct measurements (e.g., Puget et al 1996;Fixsen et al 1998;Hauser et al 1998;Lagache et al 1999;Cambrésy et al 2001;Bernstein et al 2002;Matsumoto et al 2005Matsumoto et al , 2011Dole et al 2006;Bernstein 2007) and integrated galaxy counts (e.g., Madau & Pozzetti 2000;Totani et al 2001;Xu et al 2005;Dole et al 2006;Hopwood et al 2010;Keenan et al 2010;Berta et al 2011;Béthermin et al 2012). These two methods should converge if the EBL is predominantly derived from galaxies (including any AGN component) and if the photometric data used to detect these galaxies are sufficiently deep.…”

Section: Introductionmentioning

confidence: 99%

Measurements of Extragalactic Background Light From the Far Uv to the Far Ir From Deep Ground- And Space-Based Galaxy Counts

Driver

Andrews

Davies

et al. 2016

ApJ

141

232

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We combine wide and deep galaxy number-count data from theGalaxy And Mass Assembly, COSMOS/G10, Hubble Space Telescope (HST) Early Release Science, HST UVUDF, and various near-, mid-, and far-IR data sets from ESO, Spitzer, and Herschel. The combined data range from the far UV (0.15 μm) to far-IR (500 μm), and in all cases the contribution to the integrated galaxy light (IGL) of successively fainter galaxies converges. Using a simple spline fit, we derive the IGL and the extrapolated IGL in all bands. We argue that undetected low-surfacebrightness galaxies and intracluster/group light are modest, and that our extrapolated-IGL measurements are an accurate representation of the extragalactic background light (EBL). Our data agree with most earlier IGL estimates and with direct measurements in the far IR, but disagree strongly with direct estimates in the optical. Close agreement between our results and recent very high-energy experiments (H.E.S.S. and MAGIC) suggests that there may be an additional foreground affecting the direct estimates. The most likely culprit could be the adopted model of zodiacal light. Finally we use a modified version of the two-component model to integrate the EBL and obtain measurements of the cosmic optical background (COB) and cosmic infrared background of -+ 24 4 4 nW m −2 sr −1 and -+ 26 5 5 nW m −2 sr −1 respectively (48%:52%). Over the next decade, upcoming space missions such as Euclid and the Wide Field Infrared Space Telescope will have the capacity to reduce the COB error to <1%, at which point comparisons to the very high-energy data could have the potential to provide a direct detection and measurement of the reionization field.

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AKARIOBSERVATION OF THE FLUCTUATION OF THE NEAR-INFRARED BACKGROUND

Cited by 90 publications

References 44 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

Reionization and the Cosmic Dawn with the Square Kilometre Array

Measurements of Extragalactic Background Light From the Far Uv to the Far Ir From Deep Ground- And Space-Based Galaxy Counts

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