Masses of the Planetary Nebula Central Stars in the Galactic Globular Cluster System from HST Imaging and Spectroscopy

Journal Article · Fri Feb 10 04:00:00 EST 2017 · Astrophysical Journal

DOI:https://doi.org/10.3847/1538-4357/836/1/93· OSTI ID:22663831

Jacoby, George H. ^[1]; Marco, Orsola De ^[2]; Davies, James ^[3]; Lotarevich, I. ^[4]; Bond, Howard E. ^[5]; Harrington, J. Patrick ^[6]; Lanz, Thierry ^[7]

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1. Lowell Observatory, Flagstaff, AZ 86001 (United States)
2. Department of Physics and Astronomy, Macquarie University, Sydney, NSW 2109 (Australia)
3. Space Telescope Science Institute, Baltimore MD 21218 (United States)
4. American Museum of Natural History, New York, NY (United States)
5. Department of Astronomy and Astrophysics, Pennsylvania State University, University Park, PA 16802 (United States)
6. University of Maryland, College Park, MD (United States)
7. Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, F-06304 Nice (France)

The globular cluster (GC) system of our Galaxy contains four planetary nebulae (PNe): K 648 (or Ps 1) in M15, IRAS 18333-2357 in M22, JaFu 1 in Pal 6, and JaFu 2 in NGC 6441. Because single-star evolution at the low stellar mass of present-epoch GCs was considered incapable of producing visible PNe, their origin presented a puzzle. We imaged the PN JaFu 1 with the Hubble Space Telescope (HST) to obtain photometry of its central star (CS) and high-resolution morphological information. We imaged IRAS 18333-2357 with better depth and resolution, and we analyzed its archival HST spectra to constrain its CS temperature and luminosity. All PNe in Galactic GCs now have quality HST data, allowing us to improve CS mass estimates. We find reasonably consistent masses between 0.53 and 0.58 M {sub ⊙} for all four objects, though estimates vary when adopting different stellar evolutionary calculations. The CS mass of IRAS 18333-2357, though, depends strongly on its temperature, which remains elusive due to reddening uncertainties. For all four objects, we consider their CS and nebula masses, their morphologies, and other incongruities to assess the likelihood that these objects formed from binary stars. Although generally limited by uncertainties (∼0.02 M {sub ⊙}) in post-AGB tracks and core mass versus luminosity relations, the high-mass CS in K 648 indicates a binary origin. The CS of JaFu 1 exhibits compact, bright [O iii] and H α emission, like EGB 6, suggesting a binary companion or disk. Evidence is weaker for a binary origin of JaFu 2.

• OSTI ID: 22663831
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 836; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
BINARY STARS
EMISSION
GALAXIES
IMAGES
LUMINOSITY
MASS
PHOTOMETRY
PLANETARY NEBULAE
RESOLUTION
SPACE
SPECTRA
SPECTROSCOPY
STAR EVOLUTION
TELESCOPES