An international team of astronomers led by members of the Laboratory for Space Research (LSR) and Department of Physics at The University of Hong Kong (HKU) has discovered a rare celestial jewel — a so-called planetary nebula (PN) inside a 500 million-year-old galactic open cluster (OC) called M37 (also known as NGC2099). This is a very rare finding of high astrophysical value. Their findings have just been published in the prestigious open-access paper Astrophysical Journal Letters.
Planetary nebulae are the ejected, glowing shrouds of dying stars that shine with a rich emission line spectrum and display, as a result, their distinct colors and shapes that make them photogenic magnets for the public interest. It was no coincidence that one of the first James Webb Space Telescope (the largest optical telescope in space) images released to the public was a planetary nebula! It, with the rather ungainly name of “IPHASX J055226.2+323724”, is only the 3rd example of an association between a planetary nebula and an OC out of the ~4,000 planetary nebulae known in our Galaxy.
The oldest planetary nebula ever found
It also appears to be the oldest planetary nebula ever found. The small team led by Professor Quentin PARKER, Director of the HKU LSR, has determined some interesting properties for their discovery. The authors found it has a “kinematic age” of 70,000 years. This estimate is based on how fast the nebula is expanding, as determined from its emission lines, and assuming this speed has remained effectively the same since the beginning, and is the time elapsed since the nebular shell was first ejected by the host, a dying star. This compares to typical planetary nebula ages of 5,000-25,000 years. It is truly a grand old dame in planetary nebula terms, but of course a mere “blink of the eye” in terms of the life of the original star itself, which runs to hundreds of millions of years.
Because this “grand old dame” lives in a stellar cluster, this environment enables the team to determine powerful additional parameters not possible for the general galactic planetary nebula population. These include estimating the mass of the planetary nebula’s progenitor star when it turned off the stellar main sequence, as derived from the observed properties of the thousands of stars in the cluster when plotted in a so-called color-magnitude diagram. The team can also estimate the residual mass of the central star that ejected the planetary nebulae via theoretical isochrones and observed properties of the hot, blue central star.
As a result, they figured out how massive the star was that ejected the planetary nebula gaseous shell when it was born and how much mass is now left in its residual, contracting hot core (which is already a so-called ‘White Dwarf’ star). Fresh “Gaia” data for the hot blue, planetary nebula central star also provide a good distance estimate allowing its actual size at this extreme age to be determined as 3.2pc (parsec, an astronomical unit of measure for interstellar space with 1pc equal to 3.26 light-years) in diameter — unsurprisingly perhaps also at the extreme end of known planetary nebula physical sizes. Former HKU Ph.D. student Dr. Vasiliki FRAGKOU, the first author of the study, stated:
“I am so excited to be able to work on these fascinating rare cases of OC-PN associations because they keep turning up important science results, like all three cases we have found are butterfly (bi-polar) PN in terms of shape, all are very faint and highly evolved, and all have Type-I chemistry according to their emission lines, and of course all have intermediate to high progenitor masses.”
Corresponding author Professor Quentin Parker said,
“This is only the third example of a PN found in a Galactic open star cluster, and my group has found all three confirmed examples. They are incredibly rare but also very important as these beautiful objects allow us to independently determine points on the so-called initial to final mass relation (IFMR) for stars — an important astrophysical relation — independent of the traditional method of using white dwarfs in clusters.
“Intriguingly, all our points lie just below the empirical IFMR trend currently established but add to the “kink” in this relation found recently in the 2-3 Solar mass range for the original progenitor mass by Marigo et al in the Nature Astronomy journal. Our OC-PN points fortuitously are found in currently sparsely populated regions of the IFMR, making them even more valuable.”
Co-author Professor Albert ZILJSTRA, Hung Hing Ying Distinguished Visiting Professor in Science and Technology at HKU LSR from the University of Manchester commented on the planetary nebula visibility lifetimes which have previously been much shorter in the general Galaxy:
“This new result implies that the location of a PN in an OC provides an environment suitable for allowing the PNe to expand and fade without disruption by the ambient ISM (which is typically much weaker in an OC) and not as would be the case in the Galaxy.”
Provided by The University of Hong Kong [Note: Materials may be edited for content and length.]
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