A Halpha band image of IC5070 pillar showing Herbig-Haro Object 555, stack of 24x900s bin1, calibrated and stacked and processed in Pixinsight.
|Center (RA, Dec):||(312.781, 44.352)|
|Center (RA, hms):||20h 51m 07.381s|
|Center (Dec, dms):||+44° 21' 08.830"|
|Size:||40 x 32 arcmin|
|Pixel scale:||0.873 arcsec/pixel|
|Orientation:||Up is -180 degrees E of N|
Herbig–Haro (HH) objects are small patches of nebulosity associated with newly born stars, and are formed when narrow jets of gas ejected by young stars collide with clouds of gas and dust nearby at speeds of several hundred kilometres per second. Herbig–Haro objects are ubiquitous in star-forming regions, and several are often seen around a single star, aligned with its rotational axis. HH objects are transient phenomena, lasting not more than a few thousand years. They can evolve visibly over quite short astronomical timescales as they move rapidly away from their parent star into the gas clouds of interstellar space (the interstellar medium or ISM). Hubble Space Telescope observations have revealed the complex evolution of HH objects over the period of a few years, as parts of the nebula fade while others brighten as they collide with clumpy material of the interstellar medium. The objects were first observed in the late 19th century by Sherburne Wesley Burnham, but were not recognised as being a distinct type of emission nebula until the 1940s. The first astronomers to study them in detail were George Herbig and Guillermo Haro, after whom they have been named. Herbig and Haro were working independently on studies of star formation when they first analysed the objects, and recognised that they were a by-product of the star formation process. (wikipedia)