MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS
We present observations of the SS 433 jets using the Chandra High Energy Transmission Grating Spectrometer with contemporaneous optical and Very Long Baseline Array observations. The X-ray and optical emission line regions are found to be related but not coincident as the optical line emission persi...
| Main Authors: | , , , , , , , |
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| Format: | Article |
| Language: | en_US |
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IOP Publishing
2014
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| Online Access: | http://hdl.handle.net/1721.1/85885 https://orcid.org/0000-0002-5769-8441 |
| _version_ | 1826201837747830784 |
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| author | Canizares, Claude R. Hillwig, Todd C. Mioduszewski, Amy J. Rupen, Michael Schulz, Norbert S. Heinz, Sebastian Nowak, Michael A. Marshall, Herman |
| author2 | MIT Kavli Institute for Astrophysics and Space Research |
| author_facet | MIT Kavli Institute for Astrophysics and Space Research Canizares, Claude R. Hillwig, Todd C. Mioduszewski, Amy J. Rupen, Michael Schulz, Norbert S. Heinz, Sebastian Nowak, Michael A. Marshall, Herman |
| author_sort | Canizares, Claude R. |
| collection | MIT |
| description | We present observations of the SS 433 jets using the Chandra High Energy Transmission Grating Spectrometer with contemporaneous optical and Very Long Baseline Array observations. The X-ray and optical emission line regions are found to be related but not coincident as the optical line emission persists for days while the X-ray emission lines fade in less than 5000 s. The line Doppler shifts from the optical and X-ray lines match well, indicating that they are less than 3 × 10[superscript 14] cm apart. The jet Doppler shifts show aperiodic variations that could result from shocks in interactions with the local environment. These perturbations are consistent with a change in jet direction but not jet speed. The proper motions of the radio knots match the kinematic model only if the distance to SS 433 is 4.5 ± 0.2 kpc. Observations during eclipse show that the occulted emission is very hard, seen only above 2 keV and rising to comprise >50% of the flux at 8 keV. The soft X-ray emission lines from the jet are not blocked, constraining the jet length to [> over ~]2 × 10[superscript 12] cm. The base jet density is in the range 10[superscript 10-13] cm[superscript –3], in contrast to our previous estimate based on the Si XIII triplet, which is likely to have been affected by UV de-excitation. There is a clear overabundance of Ni by a factor of about 15 relative to the solar value, which may have resulted from an unusual supernova that formed the compact object. |
| first_indexed | 2024-09-23T11:57:59Z |
| format | Article |
| id | mit-1721.1/85885 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T11:57:59Z |
| publishDate | 2014 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/858852022-10-01T07:17:32Z MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS Canizares, Claude R. Hillwig, Todd C. Mioduszewski, Amy J. Rupen, Michael Schulz, Norbert S. Heinz, Sebastian Nowak, Michael A. Marshall, Herman MIT Kavli Institute for Astrophysics and Space Research Marshall, Herman Lee Canizares, Claude R. Schulz, Norbert S. Nowak, Michael A. We present observations of the SS 433 jets using the Chandra High Energy Transmission Grating Spectrometer with contemporaneous optical and Very Long Baseline Array observations. The X-ray and optical emission line regions are found to be related but not coincident as the optical line emission persists for days while the X-ray emission lines fade in less than 5000 s. The line Doppler shifts from the optical and X-ray lines match well, indicating that they are less than 3 × 10[superscript 14] cm apart. The jet Doppler shifts show aperiodic variations that could result from shocks in interactions with the local environment. These perturbations are consistent with a change in jet direction but not jet speed. The proper motions of the radio knots match the kinematic model only if the distance to SS 433 is 4.5 ± 0.2 kpc. Observations during eclipse show that the occulted emission is very hard, seen only above 2 keV and rising to comprise >50% of the flux at 8 keV. The soft X-ray emission lines from the jet are not blocked, constraining the jet length to [> over ~]2 × 10[superscript 12] cm. The base jet density is in the range 10[superscript 10-13] cm[superscript –3], in contrast to our previous estimate based on the Si XIII triplet, which is likely to have been affected by UV de-excitation. There is a clear overabundance of Ni by a factor of about 15 relative to the solar value, which may have resulted from an unusual supernova that formed the compact object. 2014-03-21T18:54:01Z 2014-03-21T18:54:01Z 2013-09 2013-04 Article http://purl.org/eprint/type/JournalArticle 0004-637X 1538-4357 http://hdl.handle.net/1721.1/85885 Marshall, Herman L., Claude R. Canizares, Todd Hillwig, Amy Mioduszewski, Michael Rupen, Norbert S. Schulz, Michael Nowak, and Sebastian Heinz. “MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS.” The Astrophysical Journal 775, no. 1 (September 20, 2013): 75. https://orcid.org/0000-0002-5769-8441 en_US http://dx.doi.org/10.1088/0004-637X/775/1/75 The Astrophysical Journal Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf IOP Publishing arXiv |
| spellingShingle | Canizares, Claude R. Hillwig, Todd C. Mioduszewski, Amy J. Rupen, Michael Schulz, Norbert S. Heinz, Sebastian Nowak, Michael A. Marshall, Herman MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title | MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title_full | MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title_fullStr | MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title_full_unstemmed | MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title_short | MULTIWAVELENGTH OBSERVATIONS OF THE SS 433 JETS |
| title_sort | multiwavelength observations of the ss 433 jets |
| url | http://hdl.handle.net/1721.1/85885 https://orcid.org/0000-0002-5769-8441 |
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