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Figure 12. Visible light image of M31. Figure 11. Combined bandpass GALEX image of M31 The second goal of the GALEX mission is to use the UV imaging survey data to determine the cosmic star formation history over the red-shift range 0 < z < 1.5 (i.e. over the past 9 Gyrs!), and to determine its dependence on environment, mass, morphology, merging and star formation modality. These data will then be compared with similar galaxy survey data being obtained at longer wavelengths (e.g. in the infra-red by the Spitzer Observatory) which is relevant for the rest wavelengths of UV-bright galaxies at redshifts 1.5 < z < 20 (i.e. the first 4 Gyrs). Finally the third science goal of the GALEX mission is to obtain large statistical samples and detailed studies of nearby galaxies (such as Andromeda) to obtain predictive models of star formation rates in the Local Group. Serendipitously GALEX will also observe a large variety of foreground galactic stellar (UV bright) sources ranging from hot white dwarf stars in the galactic halo to late-type flare stars located within 20pc of the Sun.

Figure 12 Visible light image of M31. Figure 11. Combined bandpass GALEX image of M31 The second goal of the GALEX mission is to use the UV imaging survey data to determine the cosmic star formation history over the red-shift range 0 < z < 1.5 (i.e. over the past 9 Gyrs!), and to determine its dependence on environment, mass, morphology, merging and star formation modality. These data will then be compared with similar galaxy survey data being obtained at longer wavelengths (e.g. in the infra-red by the Spitzer Observatory) which is relevant for the rest wavelengths of UV-bright galaxies at redshifts 1.5 < z < 20 (i.e. the first 4 Gyrs). Finally the third science goal of the GALEX mission is to obtain large statistical samples and detailed studies of nearby galaxies (such as Andromeda) to obtain predictive models of star formation rates in the Local Group. Serendipitously GALEX will also observe a large variety of foreground galactic stellar (UV bright) sources ranging from hot white dwarf stars in the galactic halo to late-type flare stars located within 20pc of the Sun.

Related Figures (14)

Figure 1. GALEX instrument layout showing all major components.
Figure 1. GALEX instrument layout showing all major components.
Figure 2. GALEX instrument and solar panels
Figure 2. GALEX instrument and solar panels
Figure 3. GALEX NUV sealed tube detector. Figure 4. Portion of the GALEX cross delay line anode. passed to the instrument. The x & Y positions are determined on the ground from the counter and fine position value data. The TDC’s, low voltage power supplies, high voltage power supplies and interface electronics are co-located (Figure 1) as a Front End Electronics (FEE) stack close to the detectors.
Figure 3. GALEX NUV sealed tube detector. Figure 4. Portion of the GALEX cross delay line anode. passed to the instrument. The x & Y positions are determined on the ground from the counter and fine position value data. The TDC’s, low voltage power supplies, high voltage power supplies and interface electronics are co-located (Figure 1) as a Front End Electronics (FEE) stack close to the detectors.
Figure 6. NUV flat field image taken at 5200 volts. Figure 5. Pre delivery background image of the NUV tube at 5200 volts. events/sec/spot and 420 events/sec/spot for the FUV and NUV detectors respectively. Again it is possible to compensate for the event losses by employing a dead time correction calibration.
Figure 6. NUV flat field image taken at 5200 volts. Figure 5. Pre delivery background image of the NUV tube at 5200 volts. events/sec/spot and 420 events/sec/spot for the FUV and NUV detectors respectively. Again it is possible to compensate for the event losses by employing a dead time correction calibration.
Figure 7. Image used for FUV linearity assessment. Figure 8. FUV resolution prior to window seal measured with a mask in contact with the top MCP.
Figure 7. Image used for FUV linearity assessment. Figure 8. FUV resolution prior to window seal measured with a mask in contact with the top MCP.
Figure 9. Quantum efficiency of the FUV tube + window, CsI photocathode on MCP. Figure 10. Quantum efficiency of the NUV tube, + window, Cs2Te photocathode on window.
Figure 9. Quantum efficiency of the FUV tube + window, CsI photocathode on MCP. Figure 10. Quantum efficiency of the NUV tube, + window, Cs2Te photocathode on window.
Figure 13. Comparison of GALEX image of M101 with visible light and near IR images
Figure 13. Comparison of GALEX image of M101 with visible light and near IR images
Figure 14. Arcs and loops of filamentary gas ejecta surrounding the dwarf nova-type star Z Cam classical stellar novae, and subsequent analysis of the ejected material surrounding Z Cam should reveal signs of thermo- nuclear processing.
Figure 14. Arcs and loops of filamentary gas ejecta surrounding the dwarf nova-type star Z Cam classical stellar novae, and subsequent analysis of the ejected material surrounding Z Cam should reveal signs of thermo- nuclear processing.
Figure 15. GALEX FUV and NUV light curves for the ROTSE RR Lyrae star, together with corresponding visible ligh curves. Note the far larger magnitude variation in the UV wavelength domain.
Figure 15. GALEX FUV and NUV light curves for the ROTSE RR Lyrae star, together with corresponding visible ligh curves. Note the far larger magnitude variation in the UV wavelength domain.
Figure 16: GALEX wide-field slit-less spectroscopic Observations of the ELAISS-1 field.
Figure 16: GALEX wide-field slit-less spectroscopic Observations of the ELAISS-1 field.
Figure 17: GALEX UV spectrum of a z= 0.5 quasar
Figure 17: GALEX UV spectrum of a z= 0.5 quasar
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EngineeringPhysicsStar FormationGalactic AstronomyGalaxy evolutionOrbital Dynamics
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