Contributing to science through astronomy can be an extremely rewarding experience, but it comes with its challenges: unpredictable weather, learning new techniques, and figuring out what to observe in the first place. While we cannot control the weather, we can help with the other two. Our training materials will guide you through the basics, and the objects listed on this page will help you decide what to observe during your first sessions.
Visual Stellar Photometry
Visual observing has been at the heart of the AAVSO for over a century, and it remains one of our favorite ways to engage with the night sky. WIth just your eyes, binoculars, or a small telescope, you can track how stars change in brightness and submit your data to the AAVSO International Database.
For first time observers, we recommend observing radially pulsating stars and eclipsing binaries. The radially pulsating stars we recommend below are delta Cepheids (DCEP), and W Virginis stars (CW). These stars repeat the same changes time after time, so you can easily compare your observations against past data. We’ve also included eclipsing binaries of the Algol type (EA) which have straightforward light curves and of the beta Lyrae type (EB) which continually vary throughout their cycles.
Northern Objects
| Object | Type | Season (North) | V Mag Range | Period |
| bet Lyr | EB | Summer | 3.30 – 4.35 | 12.9 d |
| bet Per | EA | Winter | 2.09 – 3.30 | 2.8 d |
| del Cep | DCEP | Anytime | 3.49 – 4.36 | 5.3 d |
| eta Aql | DCEP | Summer | 3.49 – 4.30 | 7.17 d |
Southern Objects
| Object | Type | Season (South) | V Mag Range | Period |
| W Sgr | DCEP | Fall, Winter | 4.28 – 5.10 | 7.59 d |
| eta Aql | DCEP | Winter | 3.49 – 4.30 | 7.17 d |
| kap Pav | CW | Winter | 3.91 – 4.78 | 9.08 d |
| bet Dor | DCEP | Spring, Summer | 3.41 – 4.08 | 9.84 d |
| V Puppis | EB | Summer | 4.35 – 4.92 | 1.45 d |
Digital Stellar Photometry
If you’re beginning your journey with a smart telescope, DSLR camera, or dedicated CCD/CMOS sensor, one of the best first objects to observe is a High Amplitude Delta Scuti (HADS) star. These radially pulsating variables change in brightness by a few tenths of a magnitude in just 45–200 minutes!
This rapid variability means you can capture an entire light curve in only a few hours of observing. We think this is an ideal way to learn the fundamentals of image calibration, photometry, and light curve analysis without waiting weeks or months to see results. HADS stars are also bright and well studied, making them reliable, rewarding, and scientifically valuable targets for your first digital observations.
As a bonus, HADS stars are excellent objects to share at star parties. Because their pulsations unfold on such short timescales, you can actually watch stellar variability in action, bringing the science of the stars to life in real time.
Northern Objects
| Object | Type | Season (North) | V Mag Range | Period |
| GP And | HADS | Spring | 10.4 – 11.0 | 113 m |
| V0572 Cam | HADS | Anytime | 11.5 – 11.9 | 124 m |
Southern Hemisphere
| Object | Type | Season (South) | V Mag Range | Period |
| ZZ Mic | HADS | Fall | 9.27 – 9.59 | 97 m |
| V1338 Cen | HADS | Spring | 10.18 – 10.68 | 187 m |
Stellar Spectroscopy
Spectroscopy splits light into its component colors and allows us to determine a star’s temperature, composition, velocity, and other physical processes that photometry alone cannot. Whether you’re using a simple slitless grating or a high-resolution spectrograph, every spectrum you record captures unique information about how stars live and change.
The AAVSO collects and discriminates spectra of pulsating stars, eclipsing binaries, Be stars, novae, and many other types of variables. No matter your experience level of requirement, there’s a place for you in stellar spectroscopy.
TK
Exoplanet Photometry
Exoplanet transits are among the most exciting targets for digital observers using smart telescopes, DSLR cameras, or dedicated CCD/CMOS sensors. When a planet passes in front of its host star, it causes a small but measurable dip in brightness—what astronomers call a transit. By carefully recording these dips, you can directly detect the presence of a world orbiting another star.
For your first exoplanet projects, it’s best to start with bright stars that have relatively large eclipse depths of at least 15 millimagnitudes (mmag, or parts per thousand). These deeper, easier-to-detect transits will help you build confidence in your techniques and equipment while ensuring your results are scientifically valuable. The objects listed above are some of the best choices for beginners.
Exoplanet observing requires precise planning: not only must your computer clock be accurate, but you also need to observe before, during, and after the transit to establish a proper baseline. To make this easier, we recommend using the Swarthmore Transit Finder, which provides predicted transit times for your location and helps you select events with good visibility and strong eclipse depths.
Exoplanet observing requires patience—most transits take several hours—but the payoff is extraordinary. With the right setup, you can record the passage of a planet across its star and contribute data that professional astronomers use to refine orbital parameters and improve transit predictions. Few projects connect amateur astronomers so directly with cutting-edge science: every exoplanet light curve you produce helps expand our understanding of distant worlds.
Northern Objects
| Object | Season (North) | V Mag | Depth (mmag) | Period |
| Qatar-6 | Spring | 11.50 | 23 | 3.50 d |
| WASP-107 | Fall | 11.59 | 23 | 5.72 d |
| KELT-23 | Summer | 10.25 | 20 | 2.25 d |
| TOI-1516 | Anytime | 10.81 | 18 | 2.05 d |
| V0376 Peg | Spring | 7.65 | 18 | 3.52 d |
| WASP-77 A | Spring | 10.12 | 17 | 1.36 d |
Southern Hemisphere
| Object | Season (South) | V Mag | Depth (mmag) | Period |
| WASP-107 | Spring | 11.59 | 23 | 5.72 d |
| WASP-46 | Fall | 12.90 | 22 | 1.43 d |
| WASP-77 A | Fall | 10.12 | 17 | 1.36 d |
| WASP-121 | Winter | 10.51 | 17 | 1.27 d |
| WASP-164 | Anytime | 12.60 | 17 | 1.77 d |
Sunspot Counting
The Sun! Be sure to observe safely—never look at the Sun directly without a special solar filter (not sunglasses or photographic film negative).