Diffuse Infrared Background Experiment (DIRBE) Optics Module Breadboard Alignment Methods And Results

Magner, Thomas J.

doi:10.1117/12.7974060

Cited by 15 publications

(2 citation statements)

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“…During these 10 months, the sky was observed in 10 bands, from 1.25 µm to 240 µm. The DIRBE instrument was designed to make accurate absolute sky-brightness measurements, with a stray light rejection of less than 1 nWm −2 sr −1 (Magner 1987) and an absolute gain calibration uncertainty of 3.1% at 1.25 and 2.2 µm (Hauser et al 1998). Consequently, the all-sky maps at IR wavelengths were created with ∼ 0.7 • beam size.…”

Section: Data; Dirbementioning

confidence: 99%

DERIVATION OF A LARGE ISOTOPIC DIFFUSE SKY EMISSION COMPONENT AT 1.25 AND 2.2μm FROM THECOBE/DIRBE DATA

Sano

Kawara

Matsuura

et al. 2015

ApJ

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Using all-sky maps obtained with COBE/DIRBE, we reanalyzed the diffuse sky brightness at 1.25 and 2.2 m, m which consists of zodiacal light, diffuse Galactic light (DGL), integrated starlight (ISL), and isotropic emission including the extragalactic background light. Our new analysis including an improved estimate of the DGL and the ISL with the 2MASS data showed that deviations of the isotropic emission from isotropy were less than 10% in the entire sky at high Galactic latitude ( b 35 | | > ). We derived the DGL to 100 μm brightness ratios of ∼4.79 and ∼1.49 n W m −2 MJy −1 at 1.25 and 2.2 μm, respectively. The result of our analysis revealed a significantly large isotropic component at 1.25 and 2.2 m m with intensities of 60.15 ± 16.14 and 27.68 6.21 n W m sr ,respectively. This intensity is larger than the integrated galaxy light, upper limits from γ-ray observation, and potential contribution from exotic sources (i.e., Population III stars, intrahalo light, direct collapse black holes, and dark stars). We therefore conclude that the excess light may originate from the local universe: the Milky Way and/ or the solar system.

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Section: Data; Dirbementioning

confidence: 99%

DERIVATION OF A LARGE ISOTOPIC DIFFUSE SKY EMISSION COMPONENT AT 1.25 AND 2.2μm FROM THECOBE/DIRBE DATA

Sano

Kawara

Matsuura

et al. 2015

ApJ

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“…25, 2.2, 3.5, 4.9, 12, 25, 60, 100, 160, and 240 µm. The DIRBE instrument was designed to conduct accurate absolute measurements of the sky brightness, with a stray light rejection of less than 1 nWm −2 sr −1 (Magner 1987) and an absolute gain calibration uncertainty of 3.1% and 3.0% at 3.5 and 4.9 µm, respectively (Hauser et al 1998). Consequently, the all-sky maps at IR wavelengths were created with a beam size of ∼ 0.7 • × 0.7 • .…”

Section: Motivation Of the Present Studymentioning

confidence: 99%

Measurements of Diffuse Sky Emission Components in High Galactic Latitudes at 3.5 and 4.9 um Using DIRBE and WISE Data

Sano,

Kawara,

Matsuura

et al. 2015

Preprint

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Using all-sky maps obtained from COBE/DIRBE at 3.5 and 4.9 µm, we present a reanalysis of diffuse sky emissions such as zodiacal light (ZL), diffuse Galactic light (DGL), integrated starlight (ISL), and isotropic residual emission including the extragalactic background light (EBL). Our new analysis, which includes an improved estimate of ISL using the Wide-field Infrared Survey Explorer (WISE) data, enabled us to find the DGL signal in a direct linear correlation between diffuse near-infrared and 100 µm emission at high Galactic latitudes (|b| > 35 • ). At 3.5 µm, the high-latitude DGL result is comparable to the low-latitude value derived from the previous DIRBE analysis. In comparison with models of the DGL spectrum assuming a size distribution of dust grains composed of amorphous silicate, graphite, and polycyclic aromatic hydrocarbon (PAH), the measured DGL values at 3.5 and 4.9 µm constrain the mass fraction of PAH particles in the total dust species to be more than ∼ 2%. This was consistent with the results of Spitzer/IRAC toward the lower Galactic latitude regions. The derived residual emission of 8.9 ± 3.4 nWm −2 sr −1 at 3.5 µm is marginally consistent with the level of integrated galaxy light and the EBL constraints from the γ-ray observations. The residual emission at 4.9 µm is not significantly detected due to the large uncertainty in the ZL subtraction, same as previous studies. Combined with our reanalysis of the DIRBE data at 1.25 and 2.2 µm, the residual emission in the near-infrared exhibits the Rayleigh-Jeans spectrum.

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The Interstellar Medium as Observed by COBE

Mather

1996

New Extragalactic Perspectives in the New South Africa

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Diffuse Infrared Background Experiment (DIRBE) Optics Module Breadboard Alignment Methods And Results

Cited by 15 publications

References 0 publications

DERIVATION OF A LARGE ISOTOPIC DIFFUSE SKY EMISSION COMPONENT AT 1.25 AND 2.2μm FROM THECOBE/DIRBE DATA

DERIVATION OF A LARGE ISOTOPIC DIFFUSE SKY EMISSION COMPONENT AT 1.25 AND 2.2μm FROM THECOBE/DIRBE DATA

Measurements of Diffuse Sky Emission Components in High Galactic Latitudes at 3.5 and 4.9 um Using DIRBE and WISE Data

The Interstellar Medium as Observed by COBE

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