Balloon Measurements of the Far-Infrared Background Radiation

1973 ◽  
Vol 7 (2) ◽  
pp. 326-344 ◽  
Author(s):  
Dirk Muehlner ◽  
Rainer Weiss
Keyword(s):  
Background Radiation ◽  
Far Infrared ◽  
Infrared Background ◽  
Balloon Measurements

scholarly journals Measurement and Implications of the Cosmic Microwave Background Spectrum

1996 ◽  
Vol 168 ◽  
pp. 17-29
Author(s):  
John C. Mather
Keyword(s):  
Background Radiation ◽  
Far Infrared ◽  
Big Bang ◽  
Scale Invariant ◽  
Background Spectrum ◽  
Nasa Goddard Space ◽  
Wide Range ◽  
Infrared Background ◽  
Microwave Radiometers ◽  
The Big Bang

The Cosmic Background Explorer (COBE) was developed by NASA Goddard Space Flight Center to measure the diffuse infrared and microwave radiation from the early universe. It also measured emission from nearby sources such as the stars, dust, molecules, atoms, ions, and electrons in the Milky Way, and dust and comets in the Solar System. It was launched 18 November 1989 on a Delta rocket, carrying one microwave instrument and two cryogenically cooled infrared instruments. The Far Infrared Absolute Spectrophotometer (FIRAS) mapped the sky at wavelengths from 0.01 to 1 cm, and compared the CMBR to a precise blackbody. The spectrum of the CMBR differs from a blackbody by less than 0.03%. The Differential Microwave Radiometers (DMR) measured the fluctuations in the CMBR originating in the Big Bang, with a total amplitude of 11 parts per million on a 10° scale. These fluctuations are consistent with scale-invariant primordial fluctuations. The Diffuse Infrared Background Experiment (DIRBE) spanned the wavelength range from 1.2 to 240 μm and mapped the sky at a wide range of solar elongation angles to distinguish foreground sources from a possible extragalactic Cosmic Infrared Background Radiation (CIBR). In this paper we summarize the COBE mission and describe the results from the FIRAS instrument. The results from the DMR and DIRBE were described by Smoot and Hauser at this Symposium.

scholarly journals Constraints on Far-Infrared Source Counts in the Lockman Hole using a Power Spectrum Analysis

2001 ◽  
Vol 204 ◽  
pp. 301-301
Author(s):  
H. Matsuhara ◽  
K. Kawara ◽  
Y. Sofue ◽  
Y. Taniguchi ◽  
Y. Sato ◽  
...  
Keyword(s):  
Background Radiation ◽  
Power Spectra ◽  
Far Infrared ◽  
Infrared Space Observatory ◽  
Infrared Source ◽  
Star Forming ◽  
The Galaxy ◽  
Galaxy Count ◽  
Infrared Background ◽  
Lockman Hole

We present the characteristics of far-infrared (FIR) brightness fluctuations at 90 μm and 170 μm in the Lockman Hole, which were surveyed with the ISOPHOT instrument aboard the Infrared Space Observatory (ISO), and give constraints on the galaxy number counts down to 30 mJy at 90 μm and 50 mJy at 170 μm. The fluctuation power spectra of the FIR images are not dominated by IR cirrus, and are instead most likely due to star-forming galaxies. This analysis indicates the existence of strong evolution in the counts. Especially at 90 μm, the source density is much larger than that expected from the currently available galaxy count models. The galaxies responsible for the fluctuations also significantly contribute to the cosmic infrared background radiation recently derived from an analysis of the COBE data.

scholarly journals X-rays from Centaurus A and the Far-Infrared Background Radiation

Science ◽  
1971 ◽  
Vol 171 (3970) ◽  
pp. 500-501 ◽  
Author(s):  
R. Ramaty ◽  
E. T. Byram ◽  
T. A. Chubb ◽  
H. Friedman
Keyword(s):  
Background Radiation ◽  
Far Infrared ◽  
X Rays ◽  
Infrared Background ◽  
Centaurus A

scholarly journals The Impact of Galaxy Formation on the Diffuse Background Radiation

2001 ◽  
Vol 204 ◽  
pp. 423-435
Author(s):  
Joseph Silk ◽  
Julien Devriendt
Keyword(s):  
Star Formation ◽  
Galaxy Formation ◽  
Background Radiation ◽  
Formation Rate ◽  
Far Infrared ◽  
Diffuse Background ◽  
Infrared Background ◽  
Optical Wavelengths ◽  
The Impact ◽  
Formation Phase

The far infrared background is a sink for the hidden aspects of galaxy formation. At optical wavelengths, ellipticals and spheroids are old, even at z ~ 1. Neither the luminous formation phase nor their early evolution is seen in the visible. We infer that ellipticals and, more generally, most spheroids must have formed in dust-shrouded starbursts. In this article, we show how separate tracking of disk and spheroid star formation enables us to infer that disks dominate near the peak in the cosmic star formation rate at z ≲ 2 and in the diffuse ultraviolet/optical/infrared background, whereas spheroid formation dominates the submillimetre background.

scholarly journals Prospects for Future Far-Infrared/Submillimeter Studies of the High-Redshift Universe

2002 ◽  
Vol 12 ◽  
pp. 493-496
Author(s):  
Andrew W. Blain
Keyword(s):  
Background Radiation ◽  
High Redshift ◽  
Wide Band ◽  
Far Infrared ◽  
High Mass ◽  
Background Intensity ◽  
Spectral Structure ◽  
Dusty Galaxies ◽  
Infrared Background ◽  
Balloon Experiments

AbstractObservations made usingCOBE, SCUBA,ISOand MAMBO have provided a reasonable working knowledge of both the intensity of the submm and far-infrared background radiation and the source counts of luminous high-redshift dusty galaxies. However, because there are uncertainties in the background intensity determinations, the samples of detected galaxies are small, and most importantly, their redshift distributions are very incomplete, details of the evolution of dusty galaxies remain unresolved. The next steps forward in the field will be the launches ofSIRTFandASTRO-F, the commissioning of SOFIA and new, more capable ground-based mm/submm-wave cameras - BOLOCAM, SHARC-II and SCUBA-II - the use of ultra-long duration balloon experiments, such as BLAST, the construction of ALMA and the arrival ofFIRST, and ultimately the advent of space-borne far-infrared interferometers, such asSPECS. There are also exciting prospects for direct mm/submm-wave CO-line redshift surveys using wide-band spectrographs. Using these new facilities, the number of high-redshift dusty galaxies known will be increased dramatically. Spectroscopy usingSIRTF, SOFIA andFIRSTwill probe the astrophysical processes within these sources in detail, hopefully addressing the open question of the fraction of the counts and background radiation that is generated by the formation of high-mass stars and by active galactic nuclei (AGNs). The spatial and spectral structure of distant dusty galaxies will finally be resolved in detail using ALMA andSPECS.

Measurement of the Far-Infrared Background Radiation in the Night Sky

1971 ◽  
Vol 27 (17) ◽  
pp. 1154-1157 ◽  
Author(s):  
A. G. Blair ◽  
J. G. Beery ◽  
F. Edeskuty ◽  
R. D. Hiebert ◽  
J. P. Shipley ◽  
...  
Keyword(s):  
Background Radiation ◽  
Far Infrared ◽  
Infrared Background ◽  
Night Sky

scholarly journals Infrared Line Emission by Broadly Distributed Gas

1990 ◽  
Vol 139 ◽  
pp. 149-155
Author(s):  
Martin Harwit
Keyword(s):  
Spectral Line ◽  
Background Radiation ◽  
Line Emission ◽  
Far Infrared ◽  
Spectral Lines ◽  
The Past ◽  
Sufficient Energy ◽  
Infrared Background ◽  
Radiation Measurements

Diffuse infrared background radiation measurements have traditionally been carried out across broad wavelength bands, primarily because there seldom appeared to be sufficient energy available in individual spectral lines to make such observations possible. In the past few years, far-infrared searches for spectral line background radiation have become possible, and considerably greater use of these capabilities will become available in the next few years. The promise of this kind of observation is reviewed.

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