The 1997 reference of diffuse night sky brightness

Leinert, Ch.; Bowyer, Stuart; Haikala, L. K.; Hanner, M. S.; Hauser, M. G.; Levasseur-Regourd, Anny-Chantal; Mann, Ingrid; Mattila, K.; Reach, W. T.; Schlosser, W.; Staude, H. J.; Toller, G. N.; Weiland, J. L.; Weinberg, J. L.; Witt, A. N.

doi:10.1051/aas:1998105

Cited by 444 publications

(467 citation statements)

References 155 publications

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“…However, as we move to the red the space mission begins to look much more attractive. From the ground, the near-IR sky brightness (relevant for broadband imaging) is dominated by the decay of OH radicals, which are produced in vibrationally excited states at ∼ 90 km altitude in the Earth's upper atmosphere (Leinert et al, 1998). The typical sky brightness rises from 18.5 mag AB arcsec −2 in the Z band through 15.4 mag AB arcsec −2 in the H band.…”

Section: Advantages Of a Space Missionmentioning

confidence: 99%

“…61 In space in the 1-2 µm region the dominant background is instead scattering of sunlight off of interplanetary dust particles (the "zodiacal light"). The typical brightness is ∼ 23 mag AB arcsec −2 near the ecliptic poles and 21.5 mag AB arcsec −2 in the ecliptic plane (Leinert et al, 1998). Thus in the H band the sky brightness is a factor of 300-1000 lower in space, which means that a space telescope with even ∼ 1 m 2 collecting area would outperform the best ground-based telescopes in terms of near-IR imaging survey speed.…”

Section: Advantages Of a Space Missionmentioning

confidence: 99%

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Observational probes of cosmic acceleration

et al. 2013

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The accelerating expansion of the universe is the most surprising cosmological discovery in many decades, implying that the universe is dominated by some form of "dark energy" with exotic physical properties, or that Einstein's theory of gravity breaks down on cosmological scales. The profound implications of cosmic acceleration have inspired ambitious efforts to understand its origin, with experiments that aim to measure the history of expansion and growth of structure with percent-level precision or higher. We review in detail the four most well established methods for making such measurements: Type Ia supernovae, baryon acoustic oscillations (BAO), weak gravitational lensing, and the abundance of galaxy clusters. We pay particular attention to the systematic uncertainties in these techniques and to strategies for controlling them at the level needed to exploit "Stage IV" dark energy facilities such as BigBOSS, LSST, Euclid, and WFIRST. We briefly review a number of other approaches including redshift-space distortions, the Alcock-Paczynski effect, and direct measurements of the Hubble constant H 0 . We present extensive forecasts for constraints on the dark energy equation of state and parameterized deviations from General Relativity, achievable with Stage III and Stage IV experimental programs that incorporate supernovae, BAO, weak lensing, and cosmic microwave background data. We also show the level of precision required for clusters or other methods to provide constraints competitive with those of these fiducial programs. We emphasize the value of a balanced program that employs several of the most powerful methods in combination, both to cross-check systematic uncertainties and to take advantage of complementary information. Surveys to probe cosmic acceleration produce data sets that support a wide range of scientific investigations, and they continue the longstanding astronomical tradition of mapping the universe in ever greater detail over ever larger scales.

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Section: Advantages Of a Space Missionmentioning

confidence: 99%

Section: Advantages Of a Space Missionmentioning

confidence: 99%

Observational probes of cosmic acceleration

et al. 2013

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“…The failure of the models stems from our incomplete understanding of the physical properties and distribution of the dust in the inner heliosphere. Most of what we know comes from coronagraph and eclipse observations from Earth and the in-situ and photometric observations from the Helios mission in the 1970's (Leinert et al 1998).…”

Section: Science Question 8: 'What Is the Dust Environment In The Innmentioning

confidence: 99%

The Wide-Field Imager for Solar Probe Plus (WISPR)

et al. 2015

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mission designed to orbit as close as 7 million km (9.86 solar radii) from Sun center. WISPR employs a 95 • radial by 58 • transverse field of view to image the fine-scale structure of the solar corona, derive the 3D structure of the large-scale corona, and determine whether a dust-free zone exists near the Sun. WISPR is the smallest heliospheric imager to date yet it comprises two nested wide-field telescopes with large-format (2 K × 2 K) APS CMOS detectors to optimize the performance for their respective fields of view and to minimize the risk of dust damage, which may be considerable close to the Sun. The WISPR electronics are very flexible allowing the collection of individual images at cadences up to 1 second at perihelion or the summing of multiple images to increase the signal-to-noise when the spacecraft is further from the Sun. The dependency of the Thomson scattering emission of the corona on the imaging geometry dictates that WISPR will be very sensitive to the emission from plasma close to the spacecraft in contrast to the situation for imaging from Earth orbit. WISPR will be the first 'local' imager providing a crucial link between the large-scale corona and the in-situ measurements.

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“…However, robust detection of the COB has long been hampered by the extremely bright foreground emissions. While expected brightness of the COB is around 1 bgu ≡ 1 × 10 −9 erg s −1 cm −2 sr −1Å−1 , the terrestrial airglow and the zodiacal light (ZL) are a few orders of magnitude brighter than this level at optical wavelengths (Leinert et al 1998). The diffuse Galactic light (DGL), which refers to scattered starlight by the interstellar dust, is another but much fainter component of the diffuse light of the night sky.…”

Section: Introductionmentioning

confidence: 99%

Cosmic Optical Background: the view from Pioneer 10/11

et al. 2011

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Abstract. We present the new constraints on the cosmic optical background (COB) obtained from an analysis of the Pioneer 10/11 Imaging Photopolarimeter (IPP) data. After careful examination of data quality, the usable measurements free from the zodiacal light are integrated into sky maps at the blue (∼0.44 µm) and red (∼0.64 µm) bands. Accurate starlight subtraction is achieved by referring to all-sky star catalogs and a Galactic stellar population synthesis model down to 32.0 mag. We find that the residual light is separated into two components: one component shows a clear correlation with thermal 100 µm brightness, while another betrays a constant level in the lowest 100 µm brightness region. Presence of the second component is significant after all the uncertainties and possible residual light in the Galaxy are taken into account, thus it most likely has the extragalactic origin (i.e., the COB). The derived COB brightness is (1.8 ± 0.9) × 10 −9 and (1.2 ± 0.9) × 10 −9 erg s −1 cm −2 sr −1Å−1 at the blue and red band, respectively, or 7.9 ± 4.0 and 7.7 ± 5.8 nW m −2 sr −1 . Based on a comparison with the integrated brightness of galaxies, we conclude that the bulk of the COB is comprised of normal galaxies which have already been resolved by the current deepest observations. There seems to be little room for contributions of other populations including "first stars" at these wavelengths. On the other hand, the first component of the IPP residual light represents the diffuse Galactic light (DGL)-scattered starlight by the interstellar dust. We derive the mean DGL-to-100 µm brightness ratios of 2.1 × 10 −3 and 4.6 × 10 −3 at the two bands, which are roughly consistent with the previous observations toward denser dust regions. Extended red emission in the diffuse interstellar medium is also confirmed.

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The 1997 reference of diffuse night sky brightness

Cited by 444 publications

References 155 publications

Observational probes of cosmic acceleration

Observational probes of cosmic acceleration

The Wide-Field Imager for Solar Probe Plus (WISPR)

Cosmic Optical Background: the view from Pioneer 10/11

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