Photometric vs. Spectroscopic Analysis
| Feature | Photometry | Spectroscopy |
|---|---|---|
| Definition | Measures the intensity or brightness of light integrated over a broad wavelength range. | Analyzes the distribution of light intensity as a function of wavelength (spectrum). |
| Data Output | Light curves, total flux, and magnitudes. | Spectral lines, detailed wavelength-dependent data. |
| Resolution | Low resolution; provides broad-band information. | High resolution; captures fine details of light across wavelengths. |
| Applications | Identifying variability in stars, measuring brightness, and estimating distances. | Determining chemical composition, velocity, temperature, and redshift. |
| Advantages | Faster, simpler, and cheaper; effective for large surveys and basic measurements. | Provides detailed physical and chemical properties of objects. |
| Limitations | Lacks detailed spectral information; subject to contamination in broad filters. | More complex, time-consuming, and requires advanced instrumentation. |
| Instrumentation | Uses photometers or CCD cameras with broad-band filters. | Requires spectrographs or diffraction grating for wavelength separation. |
| Typical Use Cases | Measuring exoplanet transits, supernova searches, and galaxy surveys. | Studying stellar atmospheres, galaxy kinematics, and interstellar medium. |
| Precision | Lower precision for detailed properties. | Higher precision for detailed analysis. |
Both techniques are complementary in astrophysics and are often used together to maximize the understanding of celestial objects.