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• W2992163907 abstract "The DENIS survey is currently imaging 21334 deg of the mainly southern sky in the IJK and the observations are expected to go on until mid 2000. The expectations for extragalactic and cosmological research are outlined, including a quantitative assessment of the effects of recent star formation on the measured fluxes of galaxies. The galaxy extraction is much improved with the modeling of the PSF across the 12×12 frames and the reliability of star/galaxy separation (currently based upon a combination of classical and neural-network based methods) is measured from visual inspection to be > 90% at I = 16. The I band counts follow the high bright-end normalization and the J differential counts follow N(J) ≃ 11×dex[0.6 (J −14)] deg mag and are expected to be complete, reliable and photometrically accurate (∆m < 0.1) for J ≤ 14. 1 Cosmology and Near-Infrared selection Workers in the Infrared bands know that the Near-Infrared (NIR) is 4 (J) to 10 (K) times less affected by extinction from dust than is the V band [9]. This has two advantages: 1) A nearly-full view of the Universe, even behind the Zone of Avoidance, and 2) A view of external galaxies unaffected by their internal extinction by dust. The second advantage of the Near-Infrared is its smaller bias to recent star formation, in comparison with bluer bands and also to the mid and far IR, whose emission arises from thermal dust created and heated by young stars. The lack of sensitivity to recent star formation can be quantified as follows. Figure 1 shows the evolution of broad-band luminosities, normalized to that of a 13 Gyr old stellar population for different color bands. The evolution is strongest in the B band (and even more so in 1 COSMOLOGY AND NEAR-INFRARED SELECTION 2 Figure 1: Time evolution of broad band luminosities (Johnson BV JHK and Cousins RI) of stellar burst for stellar population with a Rana & Basu [26] IMF, using the PEGASE [14] spectral evolution model including nebular emission (which only affects the luminosities within 10 Myr from the burst). U or far-UV, neither of which are plotted in Figure 1) and weakest in the H and K bands. Nevertheless, there is a burst of emission in H and K roughly 10 Myr after the starburst, when the massive stars evolve off the main-sequence to the giant branch. Table 1 below shows that the enhancement of broad band flux in the B band due to star formation occurring 1 Myr ago, relative to the B flux of an old stellar population of the same mass and IMF, is 40 times greater than the analogous enhancement of the K band flux. Table 1: Broad-band luminosity enhancement relative to old (13 Gyr) population (normalized to the analogous K band relative enhancement) Age B V Rc Ic J H K 1 Myr 40 18 14 3.4 1.8 0.7 1 10 Myr 5.6 2.4 1.7 1.4 1.06 1.05 1 100 Myr 7.8 3.5 2.3 1.6 1.15 1.03 1 1 Gyr 3.7 2.7 2.4 1.9 1.26 1.04 1 2 Gyr 2.1 1.7 1.5 1.4 1.11 1.02 1 One interesting point is that the H band is to within a few percent as insensitive to recent star formation as the K band, and even less sensitive by up to 30% for very recent (< 5Myr) star formation, with the inclusion of nebular emission in the adopted PEGASE [14] spectral evolution model, which is stronger in K because of free-free recombination enhancing the continuum at longer wavelengths. Another interesting point is that the J band at 1.25 μ is almost 2 THE DENIS SURVEY 3 as insensitive to recent star formation as the K band, to within typically 20% or less, except for bursts younger than 8 Myr. The Ic band is considerably more sensitive to recent star formation than J (in Figure 1 and Table 1, Ic is typically three times more distant fromK, logarithmically, than is J from K)." @default.
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• W2992163907 date "1997-01-01" @default.
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• W2992163907 title "Galaxies and Cosmology with DENIS" @default.
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