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This H II region includes the reflection and emission nebulae IC 59 and IC 63. Both nebulae have a cometary shape, with IC 63 being the brighter of the two. The difference in appearance between the two nebulae is a consequence of their physical distance from γ Cas. IC 63 displays a well-defined ionization front, while this is lacking in IC 59. The nebulae are the closest photodissociation regions to the Sun.
IC 59
This nebula was discovered by German astronomer Max Wolf on December 30, 1893, then added to J. L. E. Dreyer's Index Catalogue of Nebulae in 1895. It spans an angular size of 10′ and is visible with a small telescope. From the perspective of the Earth, IC 59 is positioned in front of γ Cas, and the closest tip to the star is located at a separation of 13.5 ly (4.15 pc). It is a photodissociation region that is being sculpted by γ Cas. Light from the star is being scattered from the nebula at an angle of 17° toward the Earth.
Although the tip of the nebula has been considered the closest point to γ Cas, the western concave face is where the most intense UV radiation is being received. Hence the tip may actually be further away from the star than the rest of the cloud. The warmer component of this nebula has a mean temperature of 675±49 K, while the cooler component is 150±34 K.
IC 63
IC 63 is sometimes dubbed the Ghost Nebula, or the ghost of Cassiopeia. It was discovered by Max Wolf on the same night as IC 59, and has since been extensively studied. It spans an angular size of 10′ and is visible with a small telescope. From the perspective of the Earth, IC 63 is positioned behind γ Cas, and the closest tip to the star is located at a separation of 7.5 ly (2.3 pc). It is a photodissociation region that is being sculpted by γ Cas. Light from the star is being scattered from the nebula at an angle of 154° toward the Earth.
There is no evidence of triggered star formation in this nebula. The warmer component of this nebula has a mean temperature of 740±47 K, while the cooler component is 207±30 K. The velocity distribution across the nebula varies with the distance from the star, and is consistent with it being driven by the radiation. The atomic hydrogen in the PDR structure has a clumpy organization, while the tip has a ring-like structure. The entire structure seems to be moving apart and it is likely that this nebula will completely disperse within a half million years.
References
^ Dubout-Crillon, R. (July 1976), "H II regions of the northern Milky Way: medium-large-field photographic atlas and catalogue.", Astronomy and Astrophysics, Supplement Series, 25: 25–54, Bibcode:1976A&AS...25...25D.
^ Foster, T.; Brunt, C. M. (November 2015), "A CGPS Look at the Spiral Structure of the Outer Milky Way. I. Distances and Velocities to Star-forming Regions", The Astronomical Journal, 150 (5), id. 147, arXiv:1405.7003, Bibcode:2015AJ....150..147F, doi:10.1088/0004-6256/150/5/147.
^ Karr, J. L.; et al. (February 2005), "A Multiwavelength Study of IC 63 and IC 59", The Astronomical Journal, 129 (2): 954–968, Bibcode:2005AJ....129..954K, doi:10.1086/426912.
^ Eiermann, Jacob M.; et al. (April 2024), "The 3D geometry of reflection nebulae IC 59 and IC 63 with their illuminating star gamma Cas", Monthly Notices of the Royal Astronomical Society, 529 (2): 1680–1687, arXiv:2401.06941, Bibcode:2024MNRAS.529.1680E, doi:10.1093/mnras/stae102.
Dreyer, J. L. E. (1895), "Index Catalogue of Nebulæ found in the years 1888 to 1894, with Notes and Corrections to the New General Catalogue", Memoirs of the Royal Astronomical Society, 51: 185, Bibcode:1895MmRAS..51..185D.
Thi, W. -F.; et al. (December 2009), "ISO observation of molecular hydrogen and fine-structure lines in the photodissociation region IC63", Monthly Notices of the Royal Astronomical Society, 400 (2): 622–628, Bibcode:2009MNRAS.400..622T, doi:10.1111/j.1365-2966.2009.15501.x.
France, K.; et al. (August 2005), "Fluorescent Molecular Hydrogen Emission in IC 63: FUSE, Hopkins Ultraviolet Telescope, and Rocket Observations", The Astrophysical Journal, 628 (2): 750–757, arXiv:astro-ph/0504166, Bibcode:2005ApJ...628..750F, doi:10.1086/430878.
Blouin, D.; et al. (May 1997), "A radio continuum and H i study of IC 63, IC 59, and IRAS 00556+6048: nebulae in the vicinity of gamma CAS", Monthly Notices of the Royal Astronomical Society, 287 (2): 455–471, Bibcode:1997MNRAS.287..455B, doi:10.1093/mnras/287.2.455.
Blouin, D.; et al. (September 1997), "Erratum: A radio continuum and H I study of IC 63, IC 59 and IRAS 00556 + 6048: nebulae in the vicinity of γ Cas", Monthly Notices of the Royal Astronomical Society, 290 (1): 208, doi:10.1093/mnras/290.1.208.
Jansen, David J.; et al. (February 1994), "Physical and chemical structure of the IC 63 nebula. I. Millimeter and far-infrared observations", Astronomy and Astrophysics, 282: 605–620, Bibcode:1994A&A...282..605J.
Jansen, D. J.; et al. (October 1995), "Physical and chemical structure of the IC 63 nebula. II. Chemical models.", Astronomy and Astrophysics, 302: 223, Bibcode:1995A&A...302..223J.
Jansen, D. J.; et al. (May 1996), "Physical and chemical structure of the IC 63 nebula. III. Gas-phase carbon abundance.", Astronomy and Astrophysics, 309: 899–906, Bibcode:1996A&A...309..899J.
The brightest star is Gamma Cassiopeiae. The blue IC 59 nebula is positioned above the star and the redder IC 63 is to the left.
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