History of the mass ejection in K4-37: from the AGB to the evolved planetary nebula phase

• DOI: 10.1093/mnras/stw3245
• Publication Date: 2016-12-12T15:32:35Z
• Authors: L. F. Miranda; P. F. Guillén; L. Olguín; R. Vázquez
• Keywords: ISM: jets and outflows; Astrophysics - Solar and Stellar Astrophysics; jets and outflows [ISM]; 0103 physical sciences; individual: K4-37 [Planetary nebulae]; FOS: Physical sciences; Circumstellar matter; 01 natural sciences; Solar and Stellar Astrophysics (astro-ph.SR); Planetary nebulae: individual: K4-37

We present narrow-, broad-band, and WISE archive images, and high- and intermediate-resolution long-slit spectra of K 4-37, a planetary nebula that has never been analyzed in detail. Although K 4-37 appears bipolar, the morphokinematical analysis discloses the existence of three distinct axes and additional particular directions in the object, indicating that K 4-37 is a multi-axis planetary nebula that has probably been shaped by several bipolar outflows at different directions. A 4-6 M$_{\odot}$ main-sequence progenitor is estimated from the derived high nebular He and N abundances, and very high N/O abundance ratio ($\sim$2.32). The general properties are compatible with K 4-37 being a highly evolved planetary nebula located at $\sim$14 kpc. The WISE image at 22 $��$m reveals K 4-37 to be surrounded by a large ($\sim$13$\times$8 pc$^2$) elliptical detached shell probably related to material ejected from the AGB progenitor. The observed elliptical morphology suggests deformation of an originally spherical AGB shell by the ISM magnetic field or by the influence of a companion. We compare K 4-37 and NGC 6309 and found remarkable similarities in their physical structure but noticeably different chemical abundances that indicate very different progenitor mass. This strongly suggests that, irrespective of the initial mass, their (presumably binary) central stars have shared a very similar mass ejection history.<br/>Accepted in MNRAS, 11 pages, 6 figures<br/>