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| Eridanus superbubble | |
|---|---|
| Name | Eridanus superbubble |
| Type | Superbubble |
| Constellation | Eridanus |
| Distance | ~200–1,000 pc |
| Radius | ~50–300 pc |
| Discovery | Mid-20th century (radio, optical surveys) |
| Notable features | Extended H I shell, soft X-ray emission, Hα filaments |
Eridanus superbubble is a large, multiwavelength cavity in the interstellar medium located toward the constellation Eridanus (constellation), spanning parts of the local sky and intersecting sightlines toward Orion Arm (Milky Way), Taurus Molecular Cloud, and the Gould Belt. First recognized through combined radio, optical, and X-ray surveys, the structure links to surveys conducted by observatories such as Harvard College Observatory, Palomar Observatory, ROSAT, and IRAS and figures in studies involving the Local Bubble and the Perseus Arm.
The initial identification of the feature arose from H I 21-cm line mapping projects led by teams at National Radio Astronomy Observatory and Jodrell Bank Observatory, optical Hα work by groups at Mount Wilson Observatory and Kitt Peak National Observatory, and soft X-ray detections by the UHURU and ROSAT missions, with follow-up contributed by European Space Agency archives. Historical investigations linked filamentary Hα structures to catalogs compiled at Smithsonian Astrophysical Observatory, with later synthesis appearing in reviews by researchers from Harvard-Smithsonian Center for Astrophysics, Max Planck Institute for Astronomy, and University of Chicago. Cross-identifications involved surveys by Two Micron All Sky Survey teams, Planck (spacecraft) dust maps, and early ultraviolet work from Copernicus (satellite).
The region exhibits an extended H I shell visible in observations from instruments operated by National Radio Astronomy Observatory and Arecibo Observatory, ionized Hα filaments mapped by Wisconsin H-Alpha Mapper and Southern H-Alpha Sky Survey Atlas teams, and diffuse soft X-ray emission cataloged by ROSAT and later probed by XMM-Newton and Chandra X-ray Observatory programs. Estimates of distance and size vary between analyses from researchers at University of California, Berkeley, University of Michigan, and University of Toronto, with radii reported from ~50 pc in localized interpretations to several hundred parsecs in synthesis papers by groups at California Institute of Technology and Princeton University. The bubble contains warm ionized medium traced by emission lines studied by the Sloan Digital Sky Survey and cold neutral medium components detected in molecular surveys led by the Institut de Radioastronomie Millimétrique and Nobeyama Radio Observatory.
Proposed origins invoke sequential supernovae from OB associations linked to catalogs maintained by Blaauw and subsequent kinematic work by Blaauw's colleagues at Leiden Observatory and University of Groningen, combined with stellar-wind input from massive stars cataloged in HIPPARCOS and Gaia (spacecraft) data releases. Models developed by theoreticians at Princeton University, University of Colorado Boulder, and the Max Planck Institute for Astrophysics attribute the cavity to clustered feedback from associations related to Orion OB1 association and possibly earlier episodes associated with Scorpius–Centaurus association, invoking mechanisms analyzed in seminars at Institute for Advanced Study and conferences organized by International Astronomical Union. Kinematic ages have been compared to supernova remnant catalogs from Green's Catalogue and to pulsar population studies by teams at Jodrell Bank Observatory.
The object overlaps and interacts with neighboring cavities cataloged by groups studying the Local Interstellar Medium such as teams at Ohio State University, University of Wisconsin–Madison, and University of Delaware, and has been compared directly to the Local Bubble, Loop I (radio loop), and the GSH 238+00+109 complex in analyses presented at meetings of the American Astronomical Society and the International Astronomical Union. Distance constraints from Gaia (spacecraft) parallaxes and interstellar absorption studies from Hubble Space Telescope ultraviolet spectrographs have been used to assess whether the structure is contiguous with the Local Bubble or represents a distinct, overlapping superbubble influenced by the Orion-Eridanus superbubble region debated in literature from researchers at University of Texas at Austin and University of Sydney.
Surveys across radio, optical, infrared, ultraviolet, and X-ray bands have involved instruments and missions including Very Large Array, Arecibo Observatory, Wisconsin H-Alpha Mapper, IRAS, Planck (spacecraft), Spitzer Space Telescope, GALEX, ROSAT, XMM-Newton, and Chandra X-ray Observatory, with ancillary data from HIPPARCOS and Gaia (spacecraft)]. Spectral-line work by teams at Institut de Radioastronomie Millimétrique and Atacama Large Millimeter/submillimeter Array investigators targeted CO and other molecular tracers to probe shell interfaces, while ultraviolet absorption-line studies using instruments from Hubble Space Telescope and data analysis by groups at Space Telescope Science Institute constrained ionization states. Large-scale mapping efforts published by researchers at Max Planck Institute for Solar System Research and Leiden Observatory provided morphology comparisons with radio loops cataloged by Berkhuijsen.
Feedback effects hypothesized in papers from University of Cambridge, Imperial College London, and University of Heidelberg posit that shell compression could trigger secondary star formation in adjacent molecular clouds cataloged by Taurus Molecular Cloud surveys and by teams at Max Planck Institute for Astronomy. Observational campaigns by groups at National Astronomical Observatory of Japan and European Southern Observatory examined young stellar object populations via infrared excesses reported by Spitzer Space Telescope and WISE teams, and compared them to triggering scenarios discussed at conferences organized by Royal Astronomical Society and American Physical Society. The superbubble’s role in driving hot gas into the halo has been assessed in context with galactic fountain models developed at University of Wisconsin–Madison and Harvard-Smithsonian Center for Astrophysics.
Hydrodynamic and magnetohydrodynamic simulations addressing the structure employ codes and collaborations from Princeton University, Max Planck Institute for Astrophysics, University of Chicago, and University of California, Berkeley, using supernova-input prescriptions calibrated against catalogs from Green's Catalogue and stellar-population inputs from Gaia (spacecraft). Numerical studies presented at workshops sponsored by the Simons Foundation and the Kavli Institute for Theoretical Physics explore shell evolution, Rayleigh–Taylor instabilities, and blowout into galactic halo environments described in work by teams at University of Oxford and California Institute of Technology. Comparative model-data efforts leverage archival products from ROSAT, Planck (spacecraft), and WISE to test scenarios of sequential supernova driving and large-scale ISM porosity.
Category:Superbubbles