The ultraluminous X-ray source bubble in NGC 5585
Some ultraluminous X-ray sources (ULXs) are surrounded by collisionally ionized bubbles, larger and more energetic than supernova remnants: they are evidence of the powerful outflows associated with super-Eddington X-ray sources. We illustrate the most recent addition to this class: a huge (350 pc ×...
| Main Authors: | , , , , , , |
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| Format: | Journal Article |
| Language: | English |
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OXFORD UNIV PRESS
2021
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| Online Access: | http://hdl.handle.net/20.500.11937/97229 |
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| author | Soria, Roberto Pakull, M.W. Motch, C. Miller-Jones, James Schwope, A.D. Urquhart, R.T. Ryan, M.S. |
| author_facet | Soria, Roberto Pakull, M.W. Motch, C. Miller-Jones, James Schwope, A.D. Urquhart, R.T. Ryan, M.S. |
| author_sort | Soria, Roberto |
| building | Curtin Institutional Repository |
| collection | Online Access |
| description | Some ultraluminous X-ray sources (ULXs) are surrounded by collisionally ionized bubbles, larger and more energetic than supernova remnants: they are evidence of the powerful outflows associated with super-Eddington X-ray sources. We illustrate the most recent addition to this class: a huge (350 pc × 220 pc in diameter) bubble around a ULX in NGC 5585. We modelled the X-ray properties of the ULX (a broadened-disc source with LX ≈ 2-4 × 1039 erg s-1) from Chandra and XMM-Newton, and identified its likely optical counterpart in Hubble Space Telescope images. We used the Large Binocular Telescope to study the optical emission from the ionized bubble. We show that the line emission spectrum is indicative of collisional ionization. We refine the method for inferring the shock velocity from the width of the optical lines. We derive an average shock velocity ≈125 km s-1, which corresponds to a dynamical age of ∼600 000 yr for the bubble, and an average mechanical power Pw ∼1040 erg s-1; thus, the mechanical power is a few times higher than the current photon luminosity. With Very Large Array observations, we discovered and resolved a powerful radio bubble with the same size as the optical bubble, and a 1.4-GHz luminosity ∼1035 erg s-1, at the upper end of the luminosity range for this type of source. We explain why ULX bubbles tend to become more radio luminous as they expand while radio supernova remnants tend to fade. |
| first_indexed | 2025-11-14T11:48:03Z |
| format | Journal Article |
| id | curtin-20.500.11937-97229 |
| institution | Curtin University Malaysia |
| institution_category | Local University |
| language | English |
| last_indexed | 2025-11-14T11:48:03Z |
| publishDate | 2021 |
| publisher | OXFORD UNIV PRESS |
| recordtype | eprints |
| repository_type | Digital Repository |
| spelling | curtin-20.500.11937-972292025-04-30T01:20:27Z The ultraluminous X-ray source bubble in NGC 5585 Soria, Roberto Pakull, M.W. Motch, C. Miller-Jones, James Schwope, A.D. Urquhart, R.T. Ryan, M.S. Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs stars: black holes ISM: bubbles ISM: jets and outflows X-rays: binaries NEARBY SPIRAL GALAXIES BLACK-HOLE CANDIDATE SUPERNOVA-REMNANTS ACCRETION DISK SPECTRAL SIGNATURES RADIO-SOURCES FAST SHOCKS JET-POWER EMISSION STELLAR Some ultraluminous X-ray sources (ULXs) are surrounded by collisionally ionized bubbles, larger and more energetic than supernova remnants: they are evidence of the powerful outflows associated with super-Eddington X-ray sources. We illustrate the most recent addition to this class: a huge (350 pc × 220 pc in diameter) bubble around a ULX in NGC 5585. We modelled the X-ray properties of the ULX (a broadened-disc source with LX ≈ 2-4 × 1039 erg s-1) from Chandra and XMM-Newton, and identified its likely optical counterpart in Hubble Space Telescope images. We used the Large Binocular Telescope to study the optical emission from the ionized bubble. We show that the line emission spectrum is indicative of collisional ionization. We refine the method for inferring the shock velocity from the width of the optical lines. We derive an average shock velocity ≈125 km s-1, which corresponds to a dynamical age of ∼600 000 yr for the bubble, and an average mechanical power Pw ∼1040 erg s-1; thus, the mechanical power is a few times higher than the current photon luminosity. With Very Large Array observations, we discovered and resolved a powerful radio bubble with the same size as the optical bubble, and a 1.4-GHz luminosity ∼1035 erg s-1, at the upper end of the luminosity range for this type of source. We explain why ULX bubbles tend to become more radio luminous as they expand while radio supernova remnants tend to fade. 2021 Journal Article http://hdl.handle.net/20.500.11937/97229 10.1093/mnras/staa3784 English OXFORD UNIV PRESS restricted |
| spellingShingle | Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs stars: black holes ISM: bubbles ISM: jets and outflows X-rays: binaries NEARBY SPIRAL GALAXIES BLACK-HOLE CANDIDATE SUPERNOVA-REMNANTS ACCRETION DISK SPECTRAL SIGNATURES RADIO-SOURCES FAST SHOCKS JET-POWER EMISSION STELLAR Soria, Roberto Pakull, M.W. Motch, C. Miller-Jones, James Schwope, A.D. Urquhart, R.T. Ryan, M.S. The ultraluminous X-ray source bubble in NGC 5585 |
| title | The ultraluminous X-ray source bubble in NGC 5585 |
| title_full | The ultraluminous X-ray source bubble in NGC 5585 |
| title_fullStr | The ultraluminous X-ray source bubble in NGC 5585 |
| title_full_unstemmed | The ultraluminous X-ray source bubble in NGC 5585 |
| title_short | The ultraluminous X-ray source bubble in NGC 5585 |
| title_sort | ultraluminous x-ray source bubble in ngc 5585 |
| topic | Science & Technology Physical Sciences Astronomy & Astrophysics accretion, accretion discs stars: black holes ISM: bubbles ISM: jets and outflows X-rays: binaries NEARBY SPIRAL GALAXIES BLACK-HOLE CANDIDATE SUPERNOVA-REMNANTS ACCRETION DISK SPECTRAL SIGNATURES RADIO-SOURCES FAST SHOCKS JET-POWER EMISSION STELLAR |
| url | http://hdl.handle.net/20.500.11937/97229 |