The Observatory

The observatory's end-to-end workflow, from planning to final analysis, is supported by a selected ecosystem of specialized software and data services. This infrastructure is critical for ensuring efficient operation and scientifically accurate results.

Planning and Acquisition

Observational sessions are planned using planetarium applications and other online services. The subsequent automated control of all instrumentation and the execution of imaging sequences are managed by Sequence Generator Pro (SGP), which serves as the primary data acquisition platform. For specialized tasks such as rapid "on-the-fly" captures, SharpCap Pro is also utilized.

Data Processing and Analysis

Once acquired, raw data enters a rigorous processing and analysis pipeline.

• Astrometry: Precision position measurements are performed using Tycho Tracker and Astrometrica.

• Photometry: The measurement of celestial object brightness and its subsequent analysis are carried out using MPO Canopus with its associated data reduction utility MPO Photored, and Tycho Tracker.

Supporting Data Infrastructure

Accurate analysis relies on a robust foundation of reference data. To ensure the level of precision required, all astrometric and photometric measurements are calibrated against the most current, high-accuracy stellar catalogs produced by major international astronomical surveys. Furthermore, for the study of Solar System objects, the observatory retrieves the latest orbital elements and generates precise ephemerides using the official online services maintained by the leading international bodies responsible for planetary science.

Sequence Generator Pro, developed by Main Sequence Software, is the nerve center here at HOB. Sequence Generator Pro is an automation software that allows for the sequencing and coordination of all observatory equipment from a single interface: CCD, CMOS, filter wheel, focuser, mount, camera rotator, and even the dome, weather stations, and more.

Any amateur astronomer knows how difficult it can be to reconcile their passion with "real life," family, and work. It is essential to prevent the long nights of observation, however fulfilling, from eventually negatively impacting other aspects of life. Automation software brilliantly solves this problem by performing all equipment control functions autonomously—from controlling the telescope to acquiring images, pointing the instrument at targets of interest, recognizing the field of view, and imaging them with the correct exposure and the appropriate filter.

This is how the right balance is achieved: the observing session is programmed, routine checks are performed, and then one can serenely attend to other things while the software takes care of everything. The images, automatically acquired during the night, are ready to be analyzed later.

The observatory is situated on an elevated terrace, a location that provides a wide, 180-degree view of the western celestial hemisphere. Conversely, the eastern horizon is completely obstructed by local topography and structures.

These site characteristics define the operational sky coverage, which is constrained to an azimuth range of 198° (South) to 018° (North), and an elevation between 25° and 62°.

Due to the significant impact of atmospheric extinction and local light pollution at low altitudes, a practical observing limit of 30° elevation is typically enforced. This policy helps to maintain a high standard of data quality, which is especially critical for precision photometric studies.

The observatory is located on the outskirts of Capraia Fiorentina, a municipality approximately 20 km west of Florence, Italy. The sky quality at the site is influenced by its proximity to urban centers.

Sky Brightness and Transparency

The site is subject to significant light pollution, characteristic of a Bortle Class 6 to 7 (suburban/urban transition) sky. Under typical conditions, the zenithal visual limiting magnitude (VLM) is approximately 4.5. On nights of exceptional atmospheric transparency, this may improve to a VLM of 5.0.

Atmospheric Seeing

Atmospheric seeing is a critical parameter monitored at the site. The median seeing value is approximately 3.5 arcseconds, measured as the Full Width at Half Maximum of stellar profiles. While conditions can occasionally degrade to values approaching 4.0 arcseconds, periods of better seeing, with FWHM values slightly below 3.0 arcseconds, are also recorded. The best seeing documented at the observatory to date is 2.9 arcseconds.