| Date/Place | 2020-07-20 at Elijah Observatory | |
| Scope | Takahashi FSQ85ED | |
| Camera | QSI583wsg | |
| Integration | Using focal reducer. Mosaic of 4 panels. RGB-Hα-OIII composition Integration time for each panel: RGB: 25 x 600 sec. Hα: 25 x 1200 sec. OIII: 25 x 1800 sec. Link to starless version: Here | |
| Comment | G65.2 + 5.7 is an extensive supernova remnant visible in the constellation Cygnus. It includes some filaments cataloged with the abbreviations Sh2-91, Sh2-94 and Sh2-96. It is located at a distance of about 2600 ly on the inner edge of the Orion Arm at a distance slightly higher than the giant molecular cloud that forms the so-called "Swan's Rift"; the center of the remnant is about 80 parsecs north of the galactic plane. According to the studies carried out on the expansion speed of the super bubble generated by the explosion, the progenitor star would have exploded about 300,000 years ago, while other studies that take into account the X-ray observations conducted by the ROSAT satellite have indicated a much lower age, about 28,000 years old. The pulsar that makes up the rest of the star's core has not yet been identified with certainty. In 1996 the millisecond pulsar PSR J1931 + 30 was identified in the direction of G65.2 + 5.7; However, studies on its dispersion have ruled out a physical link between the pulsar and the supernova remnant, since for the former a distance of about 3000 parsec was derived, that is four times greater than that of G65.2 + 5.7. The southern filament of G65.2 + 5.7 shows a strong polarization, indicating the presence of a strong magnetic field; based on the X-ray data, this supernova remnant has been cataloged as a "thermal composite" remnant. Moreover, with the exception of a few areas, G65.2 + 5.7 seems to have already entered the cooling phase. (Text adapted from wikipedia) |
