Diffuse Galactic Light in the Field of the Translucent High Galactic Latitude Cloud Mbm32

Abstract

We have conducted B-, g-, V-, and R-band imaging in a 45 × 40 field containing part of the high Galactic latitude translucent cloud MBM32, and correlated the intensity of diffuse optical light S ν (λ) with that of 100 μm emission S ν (100 μm). A χ 2 minimum analysis is applied to fit a linear function to the measured correlation and derive the slope parameter b(λ) = ΔS ν (λ)/ΔS ν (100 μm) of the best-fit linear function. Compiling a sample by combining our b(λ) and published ones, we show that the b(λ) strength varies from cloud to cloud by a factor of four. Finding that b(λ) decreases as S ν (100 μm) increases in the sample, we suggest that a nonlinear correlation including a quadratic term of S ν (100 μm) 2 should be fitted to the measured correlation. The variation of optical depth, which is A V = 0.16-2.0 in the sample, can change b(λ) by a factor of 2-3. There would be some contribution to the large b(λ) variation from the forward-scattering characteristic of dust grains which is coupled to the non-isotropic interstellar radiation field (ISRF). Models of the scattering of diffuse Galactic light (DGL) underestimate the b(λ) values by a factor of two. This could be reconciled by deficiency in UV photons in the ISRF or by a moderate increase in dust albedo. Our b(λ) spectrum favors a contribution from extended red emission (ERE) to the diffuse optical light; b(λ) rises from B to V faster than the models, seems to peak around 6000 Å and decreases toward long wavelengths. Such a characteristic is expected from the models in which the DGL is combined with ERE.

On the origin of near-infrared extragalactic background light anisotropy

“…The maps are scaled from 100 μm intensity in MJy sr −1 to near-infrared intensity in nW m −2 sr −1 using the empirical correlation determined from an analysis of the CIBER low resolution spectrometer (LRS; paper in preparation), which yields scalings of 15 nW m −2 sr −1 (MJy sr −1 ) −1 and 8 nW m −2 sr −1 (MJy sr −1 ) −1 at 1.1 μm and 1.6 μm, respectively. Our near-to far-infrared conversion factor is consistent with the upper range of conversion factors in previous measurements (19,(45)(46)(47)(48) which produces a conservative estimate for the DGL foreground. We assume a constant scaling, appropriate for optically thin dust in these high Galactic latitude fields.…”

The Burrell Schmidt Deep Virgo Survey: Tidal Debris, Galaxy Halos, and Diffuse Intracluster Light in the Virgo Cluster

“…dust clouds (Witt et al 2008, Ienaka et al 2013) show a linear relationship between the optical flux and the IRAS 100µ emission. If such a model holds for the features in our deep optical imaging, we can attempt to remove the cirrus from our image by subtracting a suitably scaled version of the 250µ map from our V -band mosaic.…”

Probing interstellar turbulence in cirrus with deep optical imaging: no sign of energy dissipation at 0.01 pc scale

“…Following the detection of the infrared emission at high Galactic latitude with IRAS (Low et al 1984), there have been several studies showing the good spatial correlation between the optical DGL and the infrared emission, especially at 100 µm (de Vries & Le Poole 1985;Laureijs et al 1987;Guhathakurta & Tyson 1989;Paley et al 1991;Zagury et al 1999;Ienaka et al 2013). The strong spatial correlation with the infrared and the spectral energy distribution of the DGL 1 confirmed that it is caused by scattering by large dust grains (Brandt & Draine 2012).…”