NGC 6445

NGC 6445, also known as the Little Gem Nebula or Box Nebula, is a planetary nebula in the constellation Sagittarius. It was discovered by William Herschel on May 28, 1786.[6] The distance of NGC 6445 is estimated to be slightly more than 1,000 parsecs based on the parallax measured by Gaia, which was measured at 0.9740±0.3151 mas.[7]

NGC 6445
Emission nebula
Planetary nebula
NGC 6445 by PanSTARRS
Observation data: J2000 epoch
Right ascension 17h 49m 15s[1]
Declination−20° 00′ 35″ [1]
Distance4.5 Kly (1.38 Kpc)[2] ly
Apparent magnitude (V)11.2[3]
Apparent dimensions (V)0′.53 × 0′.53[1]
ConstellationSagittarius
DesignationsPK 008+03 1, Little Gem Nebula,[1] Box Nebula[4][5]

Characteristics

NGC 6445 has been classified as a bipolar planetary nebula.[8][9] Its He/H and N/O abundance ratios are consistent with the Type I definition.[10] In optical images, NGC 6445 features a bright, central ring-shaped morphology and open bipolar lobes[11]; the outer envelope emission of NGC 6445 is [N ii]-dominant.[12]

Structures in the halo of NGC 6445. Left: residual H2 image of NGC 6445 created by subtracting the scaled Brγ image from the H2 image. Right: color-composite image of NGC 6445 created with the [N ii] (red) and the residual H2 (green) images.[13]

Wide-field optical images obtained by the Nordic Optical Telescope (NOT) Andalucía Faint Object Spectrograph and Camera (ALFOSC) show that NGC 6445 has an irregularly shaped central region with a size of ~40" × 50", where the [O iii] emission dominates, while the [N ii] emission is much more extended and defines an overall bipolar morphology. The bipolar lobes are along the east–west (EW) direction with position angle ~ 80°, stretching to about 1'.6 from the center. There are also many filamentary structures across the nebula, which hint at a more complex morphology of NGC 6445. The breadths of the EW lobes reach ~1'.8 at both ends.[13] This means given the distance of NGC 6445 that the nebula is 4 light years across and is among the largest known.[14] NGC 6445 has a faint halo, seen in residual H2 emission images, which show filamentary features well outside the central region along the north–south (NS) direction. These filaments are located ~1'.3 – 1'.6 from the center. The southern filaments are more extended along the EW direction. There are also rays of faint emission coming from the central region.[13]

A close comparison of the residual H2 image against the Spitzer IRAC 8.0 μm and the NOT ALFOSC [N ii] images shows that along NS direction the H2 emission generally delineates the outer boundary of a broad region where the 8.0 μm emission dominates, while the [N ii] emission is more extended along the EW direction, consistent with the bipolar morphology, and is confined within the 8.0 μm-emitting region along the north-south direction. Along this direction, the H2 emission appears to be slightly farther out than the [N ii] emission.[13] This reinforces the notion that the optical emission may be significantly affected by the illumination of UV photons and cannot represent the intrinsic matter distribution of PNe.[15] The [N ii] image mainly traces the bipolar lobes, while the H2 image reveals the limb-brightened gas extended along the equatorial direction.[13]

The northern and the southern H2-emitting filaments, ~1'.4 – 1'.6 from the center of NGC 6445, might be the outer boundaries of an edge-on-viewed torus of this PN. This torus was ejected in the AGB phase, when the projenitor star was a red giant, and is now being disrupted by interaction with the fast stellar wind that was developed later. The south region of the torus seems to be much more disrupted than its north counterpart. Within the EW bipolar lobes, there seem to be two arcs in the H2 emission, as shown in the residual image: a northeast (NE) arc and a southwest (SW) one, both ~1'.0 from the nebular center. The SW arc seems to be disrupted but matches the position of a giant arc in [N ii]. These two H2 arcs might define another pair of bipolar lobes, which have a PA ~ 56°. This PA generally agrees with that of the [O iii]-right inner nebular region of NGC 6445, suggesting that the smaller bipolar bubbles are of relatively higher excitation and thus might have developed recently.[13]

Observation

NGC 6445 lies 2.1 degrees southwest from the open cluster Messier 23. NGC 6445 can be located by star hopping from Messier 23, by firstly locating an arc of 7th and 8th magnitude stars one degree southwest of M23, with the nebula lying 5 arcminutes west of an 8th magnitude star that lies 40 arcminutes west of the southernmost star of the arc. The globular cluster NGC 6440 lies 23 arcminutes to the south and both ojects can be seen in a wide field eyepiece. In low magnification the nebula appears like a fuzzy star and higher magnifications reveal its rectangular disk.[14][16] The planetary nebula is included in the Herschel 400 Catalogue.

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References
  1. "NGC 6445". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 28 December 2018.
  2. Stanghellini, Letizia; Shaw, Richard A.; Villaver, Eva (10 December 2008). "The Magellanic Cloud Calibration of the Galactic Planetary Nebula Distance Scale". The Astrophysical Journal. 689 (1): 194–202. arXiv:0807.1129. Bibcode:2008ApJ...689..194S. doi:10.1086/592395.
  3. "Revised NGC Data for NGC 6445". spider.seds.org.
  4. Michael E. Bakich (June 11, 2015). "Open cluster IC 4665, the Box Nebula (NGC 6445), and globular cluster". Astronomy.com. Retrieved 27 December 2018.
  5. "Best of AOP: NGC 6445: The Box Nebula". www.noao.edu. National Optical Astronomy Observatory. Retrieved 27 December 2018.
  6. Seligman, Courtney. "NGC 6445 (= P-K 008+03.1 = "PGC 3517785"), the Little Gem Nebula". Celestial Atlas. Retrieved 19 November 2018.
  7. Kimeswenger, S.; Barría, D. (14 August 2018). "Planetary nebula distances in Gaia DR2". Astronomy & Astrophysics. 616: L2. arXiv:1807.06368. Bibcode:2018A&A...616L...2K. doi:10.1051/0004-6361/201833647.
  8. Aller, L. H.; Czyzak, S. J.; Craine, E.; Kaler, J. B. (June 1973). "Spectrophotometric studies 22 irregular ring nebulae NGC 6445". The Astrophysical Journal. 182: 509. doi:10.1086/152158.
  9. Perinotto, M. (June 1991). "Chemical abundances in planetary nebulae - Basic data and correlations between elements". The Astrophysical Journal Supplement Series. 76: 687. Bibcode:1991ApJS...76..687P. doi:10.1086/191578.
  10. Peimbert, M.; Torres-Peimbert, S. (1983). "Type I planetary nebulae". Planetary Nebulae. 103: 233–241. Bibcode:1983IAUS..103..233P.
  11. van Hoof, Peter A. M.; Van de Steene, Griet C.; Beintema, Douwe A.; Martin, P. G.; Pottasch, Stuart R.; Ferland, Gary J. (20 March 2000). "Properties of Dust Grains in Planetary Nebulae. I. The Ionized Region of NGC 6445". The Astrophysical Journal. 532 (1): 384–399. arXiv:astro-ph/9910400. Bibcode:2000ApJ...532..384V. doi:10.1086/308536.
  12. Phillips, J. P.; Ramos-Larios, G. (April 2010). "Spitzer mid-infrared observations of seven bipolar planetary nebulae". Monthly Notices of the Royal Astronomical Society. 405 (4): 2179. arXiv:1004.0038. Bibcode:2010MNRAS.405.2179P. doi:10.1111/j.1365-2966.2010.16617.x.
  13. Fang, Xuan; Zhang, Yong; Kwok, Sun; Hsia, Chih-Hao; Chau, Wayne; Ramos-Larios, Gerardo; Guerrero, Martín A. (29 May 2018). "Extended Structures of Planetary Nebulae Detected in H2 Emission". The Astrophysical Journal. 859 (2): 92. arXiv:1804.08840. doi:10.3847/1538-4357/aac01e. This article contains quotations from this source, which is available under the Creative Commons Attribution 3.0 Unported (CC BY 3.0) license.
  14. Harrington, Philip S. (2010). Cosmic Challenge: The Ultimate Observing List for Amateurs. Cambridge University Press. ISBN 9781139493680.
  15. Zhang, Yong; Kwok, Sun; Ko, Chung-Ming (30 August 2012). "A study of the effect of ionization and illumination on morphologies of planetary nebulae". Proceedings of the International Astronomical Union. 7 (S283): 530–531. Bibcode:2012IAUS..283..530Z. doi:10.1017/S1743921312012276.
  16. Thompson, Robert; Thompson, Barbara (2007). Illustrated Guide to Astronomical Wonders: From Novice to Master Observer. O'Reilly Media, Inc. p. 409. ISBN 9780596526856.


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