Near Infrared Extragalactic Background

Matsumoto, Toshio; Cohen, Martin; Freund, Minoru M.; Kawada, Manabu; Lim, Mark D.; Matsuura, Shuji; Murakami, Hiroshi; Noda, Minoru; Tanaka, M.

doi:10.1007/3-540-45553-1_13

Cited by 9 publications

(8 citation statements)

References 18 publications

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“…Using their argument that the fluctuations are 5-10% of the CIB, we have multiplied their fluctuation limits at these wavelengths by 15 to obtain the implied upper limits on the CIB shown in Table 2, results entirely consistent with those explicitly stated by Kashlinsky et al (1996b). Matsumoto et al (2000) studied sky brightness fluctuations in the IRTS data. After removing the discernible stars and large-scale features, they found a fluctuation spectrum which was dominated by read-out noise at wavelengths longer than 2.6 µm.…”

Section: Fluctuation Analysissupporting

confidence: 61%

“…He interpreted the largest standard deviation in his four fields as an upper limit on CIB fluctuations, since there were potential non-cosmic contributions to the fluctuations which he ignored. Wright's 1.25 µm upper limit is somewhat lower than the 92% confidence interval for the detection of Kashlinsky & Odenwald (2000) and well below the data of Matsumoto et al (2000) ( Table 2). His 2.2 µm limit is below the detections reported by Matsumoto et al and Kashlinsky & Odenwald, though within the 92% confidence interval of Kashlinsky & Odenwald.…”

Section: Fluctuation Analysismentioning

confidence: 59%

“…The preliminary report by Matsumoto et al (2000) does not provide detail regarding systematic uncertainties in their results. For example, information such as the zero point uncertainty, limits on stray light, and uncertainty due to a shutter light leak (Noda et al 1996), would be valuable.…”

Section: Background Measurements From Irtsmentioning

confidence: 98%

“…Though consistently calibrated reference stars were used for gain calibration of the two instruments, the relative surface brightness photometry can be discrepant due to systematic errors in determination of the beam shape and spectral response for each instrument, as well as random errors in the measurements of the response of each instrument to the standard reference stars. Matsumoto et al (2000) noted that there is some evidence of calibration inconsistency in that the correlation between the star-subtracted brightness of the NIRS maps and the DIRBE IPD model brightness did not have unity slope at all wavelengths. It will be very valuable to have a more detailed account of the NIRS analysis and its uncertainties.…”

Section: Background Measurements From Irtsmentioning

confidence: 99%

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The Cosmic Infrared Background: Measurements and Implications

Hauser

Dwek

2001

Annu. Rev. Astron. Astrophys.

806

817

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ABSTRACT:The cosmic infrared background records much of the radiant energy released by processes of structure formation that have occurred since the decoupling of matter and radiation following the Big Bang. In the past few years, data from the Cosmic Background Explorer (COBE) mission provided the first measurements of this background, with additional constraints coming from studies of the attenuation of TeV γ-rays. At the same time there has been rapid progress in resolving a significant fraction of this background with the deep galaxy counts at infrared wavelengths from the Infrared Space Observatory (ISO) instruments and at submillimeter wavelengths from the Submillimeter Common User Bolometer Array (SCUBA) instrument. This article reviews the measurements of the infrared background and sources contributing to it, and discusses the implications for past and present cosmic processes.

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Section: Fluctuation Analysissupporting

confidence: 61%

Section: Fluctuation Analysismentioning

confidence: 59%

Section: Background Measurements From Irtsmentioning

confidence: 98%

Section: Background Measurements From Irtsmentioning

confidence: 99%

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The Cosmic Infrared Background: Measurements and Implications

Hauser

Dwek

2001

Annu. Rev. Astron. Astrophys.

806

817

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“…Measurements based upon COBE data are as shown in Figure 1 (see Table 1 for references) . The recently reported ClB measurement from the IRTS mission (Matsumoto et al 2000) is shown as a curve from 1.4-4.0 usu. The detections at UV-optical wavelengths are from the recent report by Bernstein (1999) (vl v == 12, 15, and 18 nW m-2 sr-I at 0.3, 0.55 and 0.8 ust: respectively).…”

Section: Summary and Implicationsmentioning

confidence: 99%

The Far Infrared and Submillimeter Diffuse Extragalactic Background

Hauser

2001

Symp. - Int. Astron. Union

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Abstract. The cosmic infrared background (CIB) radiation was a longsought fossil of energetic processes associated with structure formation and chemical evolution since the Big Bang. The COBE Diffuse Infrared Background Experiment (DIRBE) and Far Infrared Absolute Spectrophotometer (FIRAS) were specifically designed to search for this background from 1.25 J-Lm to millimeter wavelengths. These two instruments provided high quality, absolutely calibrated all-sky maps which have enabled the first detections of the CIB, initially at far infrared and submillimeter wavelengths, and more recently in the near infrared as well. The aim of this paper is to review the status of determinations of the CIB based upon COBE measurements. The results show that the energy in the CIB from far infrared to millimeter wavelengths is comparable to that in the integrated light of galaxies from UV to near infrared wavelengths: the universe had a luminous but dusty past. On the assumption that nucleosynthesis in stars is the energy source for most of this light, the results also imply that 1-8% of cosmic baryons has been converted to helium and heavier elements in stars. The integrated background light from UV to millimeter wavelengths, 60-120 nW m-2 sr-1 , is about 10% of that in the cosmic microwave background. Current knowledge of the CIB provides significant new constraints on models of the history of star formation and galaxy evolution.

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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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Near Infrared Extragalactic Background

Cited by 9 publications

References 18 publications

The Cosmic Infrared Background: Measurements and Implications

The Cosmic Infrared Background: Measurements and Implications

The Far Infrared and Submillimeter Diffuse Extragalactic Background

Reionization and the Cosmic Dawn with the Square Kilometre Array

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