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Subtracted map (SN) in terms of surface density in the sky for RC stars

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cma 36

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The phone comes with a decent set of specs for a device costing just 799 Yuan in China (for the 2GB version, which we're testing as well; ...

Now that we've had a chance to play with it for a few hours, we can tell that it doesn't just look good, but is fairly well made as well.

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Distance profile of the Canis Major overdensity. Upper panel: distance distribution of RC stars

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The chin features two sets of holes, one of which are for the speaker audio to let out, and the other, the mic.

Galaxy-S-III-6595.jpg

Figure 3. A star diagonal can give a more comfortable observing position but at the

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Figure 3

Yes it looks big with a 5.3" Super HD AMOLED screen. Almost as good as the retina screen from iPhone 4/4S with Galaxy note ...

Fig. 1. The Wearable Multimodal Monitoring System (WMMS)

NGC6871-R2 BLACK-S.jpg

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PARALLAX OF GALACTIC CEPHEIDS FROM SPATIALLY SCANNING THE WIDE FIELD CAMERA 3 ON THE HUBBLE SPACE TELESCOPE: THE CASE OF SS CANIS MAJORIS - IOPscience

Figure 4

Old open clusters around the main body of CMa.

Volume 1 Astronomy, Earth Atmosphere and Gravity Field, Life Sciences, And Materials Processing | Sun | Astronomy

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Figure 6

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Figure 61: Light curve of galaxy SDSS J132102.26+453223.8 obtained with Gaia [image credit: ESA/Gaia/DPAC/Z. Kostrzewa-Rutkowska (Warsaw University ...

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Figure 3.5

Figure 2. CO J = 5 → 4 spectrum of B1-E5, as

OH 1612-MHz maser emission from IRAS 04553−6825 with the H2O maser velocity

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Figure 5. Marginal 0.683 and 0.95 two-dimensional credibility regions in the ΩM–w plane for

Figure 11.

Comparison of synthetic spectra at selected U − V colours for SNe II-P arising

Average infrared colours versus spectral types for Be stars in this paper. The x-

Left-hand panel: infrared CMD of a 6°× 5° field near

Figure 1

PARALLAX OF GALACTIC CEPHEIDS FROM SPATIALLY SCANNING THE WIDE FIELD CAMERA 3 ON THE HUBBLE SPACE TELESCOPE: THE CASE OF SS CANIS MAJORIS - IOPscience

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Figure 12. Subtracted density map taken from Fig. 5(a) (Northern hemisphere densities rescaled

Figure 5

Difference of mean compressed distance moduli with respect to the compressed data set of B14,

The appearance of the Sgr dSph if it were placed at the distance and position of

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Figure 16. Same as Figure 15, but for previously identified galaxies (left)

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Pairwise comparisons of covariance matrices for compressed distance moduli obtained from various computations. In each

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Figure 23: LISA Pathfinder results (image credit: ESA/LISA Pathfinder Collaboration)

Figure 2.5

Effelsberg (in black, spectral resolution δv of 0.1 km s

Marginal 0.683 and 0.95 contours of the post-compression standardization parameters inferred from the Gaussian

Fig. 13

Figure 5.1

Figure 7. Column densities for H 2 O and CO 2 ices. Red and