This creates a stable base for weighted exercises. Making learning more fun -- or interesting -- is what makes it more effective. Next, the artist removes the key face from each key cap, making sure the top of the key cap is a flat surface. As the master key will have been erased by the reboot preceding Forenscope’s installation, Forenscope will have no way of recovering the network connections. Key evidence for the existence of obscured (Type 2) quasars comes from synthesis models of the cosmic X-ray background (e.g., Comastri et al., 1995; Gilli et al., 2007a), as well as direct identification of these objects through various observational techniques. A number of studies using mid-IR colors (Lacy et al., 2004; Stern et al., 2005; Rowan-Robinson et al., 2005; Hickox et al., 2007, hereafter H07), SED fitting (Alonso-Herrero et al., 2006; Donley et al., 2007), or selecting objects based on similarities to mid-IR quasar templates (e.g., Polletta et al., 2006) have been successful in identifying large numbers of dust-obscured quasars, indicating that a large fraction, and possibly a majority of rapid black hole growth is obscured by dust. At present there are a number of possible physical scenarios for obscured quasars; in the simplest "unified models", obscuration is attributed to a broadly axisymmetric "torus" of dust that is part of the central engine, so obscuration is entirely an orientation effect (e.g., Antonucci, 1993; Urry & Padovani, 1995). Alternatively, obscuration may not be due to a central "torus" but to larger dust structures such as those predicted during major mergers of galaxies (e.g., Silk & Rees, 1998; Springel et al., 2005; Hopkins et al., 2006a), and obscured quasars may represent an early evolutionary phase when the growing black hole cannot produce a high enough accretion luminosity to expel the surrounding material (e.g., Hopkins et al., 2008; King, 2010). Observations have revealed evidence for obscuration by a "torus" in some cases and by galactic-scale structures in others (e.g., Zakamska et al., 2005; Page et al., 2004; Martнnez-Sansigre et al., 2009), and while there are examples of obscured quasars that show clear signs of radiative feedback on interstellar gas, it is unclear whether they are driving the galaxy-scale outflows invoked in evolutionary models (Greene et al., 2011). Thus the physical nature of obscured quasars remains poorly understood, and analyses with large samples of mid-IR selected quasars will be essential for a more complete understanding of rapidly growing, obscured black holes

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