Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission
We report results of one-day simultaneous multiwavelength observations of CygnusX-2 using XMM, Chandra, the European VLBI Network and the XMM Optical Monitor. During the observations, the source did not exhibit Z-track movement, but remained in the vicinity of the soft apex. It was in a radio quiesc...
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| Veröffentlicht in: | Astronomy and astrophysics (Berlin) 2011-06, Vol.530, p.A102 |
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| container_title | Astronomy and astrophysics (Berlin) |
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| creator | Bałucińska-Church, M. Schulz, N. S. Wilms, J. Gibiec, A. Hanke, M. Spencer, R. E. Rushton, A. Church, M. J. |
| description | We report results of one-day simultaneous multiwavelength observations of CygnusX-2 using XMM, Chandra, the European VLBI Network and the XMM Optical Monitor. During the observations, the source did not exhibit Z-track movement, but remained in the vicinity of the soft apex. It was in a radio quiescent/quiet state of 60° these structures can still cover large parts of the extended ADC, without absorbing emission from the central neutral star. |
| doi_str_mv | 10.1051/0004-6361/201015931 |
| format | Article |
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S. ; Wilms, J. ; Gibiec, A. ; Hanke, M. ; Spencer, R. E. ; Rushton, A. ; Church, M. J.</creator><creatorcontrib>Bałucińska-Church, M. ; Schulz, N. S. ; Wilms, J. ; Gibiec, A. ; Hanke, M. ; Spencer, R. E. ; Rushton, A. ; Church, M. J.</creatorcontrib><description>We report results of one-day simultaneous multiwavelength observations of CygnusX-2 using XMM, Chandra, the European VLBI Network and the XMM Optical Monitor. During the observations, the source did not exhibit Z-track movement, but remained in the vicinity of the soft apex. It was in a radio quiescent/quiet state of <150 μJy. Strong dip events were seen as 25% reductions in X-ray intensity. The use of broadband CCD spectra in combination with narrow-band grating spectra has now demonstrated for the first time that these dipping events in CygnusX-2 are caused by absorption in cool material in quite a unique way. In the band 0.2 − 10 keV, dipping appears to be due to progressive covering of the Comptonized emission of an extended accretion disk corona, the covering factor rising to 40% in deep dipping with an associated column density of 3 × 1023 atom cm-2. Remarkably, the blackbody emission of the neutron star is not affected by these dips, in strong contrast with observations of typical low mass X-ray binary dipping sources. The Chandra and XMM gratings directly measure the optical depths in absorption edges such as Ne K, Fe L, and O K and a comparison of the optical depths in the edges of non-dip and dip data reveals no increase of optical depth during dipping even though the continuum emission sharply decreases. Based on these findings, at orbital phase 0.35, we propose that dipping in this observation is caused by absorption in the outer disk by structures located opposite to the impact bulge of the accretion stream. With an inclination angle >60° these structures can still cover large parts of the extended ADC, without absorbing emission from the central neutral star.</description><identifier>ISSN: 0004-6361</identifier><identifier>EISSN: 1432-0746</identifier><identifier>DOI: 10.1051/0004-6361/201015931</identifier><language>eng</language><publisher>EDP Sciences</publisher><subject>acceleration of particles ; accretion ; accretion disks ; radio continuum: general ; stars: neutron ; X-rays: binaries ; X-rays: individuals: CygX-2</subject><ispartof>Astronomy and astrophysics (Berlin), 2011-06, Vol.530, p.A102</ispartof><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c2471-44c6bf162de391928ecdb4dc619cfb77147c8bd41500d7c08ff6505f1753f95e3</citedby><cites>FETCH-LOGICAL-c2471-44c6bf162de391928ecdb4dc619cfb77147c8bd41500d7c08ff6505f1753f95e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,3725,27923,27924</link.rule.ids></links><search><creatorcontrib>Bałucińska-Church, M.</creatorcontrib><creatorcontrib>Schulz, N. S.</creatorcontrib><creatorcontrib>Wilms, J.</creatorcontrib><creatorcontrib>Gibiec, A.</creatorcontrib><creatorcontrib>Hanke, M.</creatorcontrib><creatorcontrib>Spencer, R. E.</creatorcontrib><creatorcontrib>Rushton, A.</creatorcontrib><creatorcontrib>Church, M. J.</creatorcontrib><title>Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission</title><title>Astronomy and astrophysics (Berlin)</title><description>We report results of one-day simultaneous multiwavelength observations of CygnusX-2 using XMM, Chandra, the European VLBI Network and the XMM Optical Monitor. During the observations, the source did not exhibit Z-track movement, but remained in the vicinity of the soft apex. It was in a radio quiescent/quiet state of <150 μJy. Strong dip events were seen as 25% reductions in X-ray intensity. The use of broadband CCD spectra in combination with narrow-band grating spectra has now demonstrated for the first time that these dipping events in CygnusX-2 are caused by absorption in cool material in quite a unique way. In the band 0.2 − 10 keV, dipping appears to be due to progressive covering of the Comptonized emission of an extended accretion disk corona, the covering factor rising to 40% in deep dipping with an associated column density of 3 × 1023 atom cm-2. Remarkably, the blackbody emission of the neutron star is not affected by these dips, in strong contrast with observations of typical low mass X-ray binary dipping sources. The Chandra and XMM gratings directly measure the optical depths in absorption edges such as Ne K, Fe L, and O K and a comparison of the optical depths in the edges of non-dip and dip data reveals no increase of optical depth during dipping even though the continuum emission sharply decreases. Based on these findings, at orbital phase 0.35, we propose that dipping in this observation is caused by absorption in the outer disk by structures located opposite to the impact bulge of the accretion stream. With an inclination angle >60° these structures can still cover large parts of the extended ADC, without absorbing emission from the central neutral star.</description><subject>acceleration of particles</subject><subject>accretion</subject><subject>accretion disks</subject><subject>radio continuum: general</subject><subject>stars: neutron</subject><subject>X-rays: binaries</subject><subject>X-rays: individuals: CygX-2</subject><issn>0004-6361</issn><issn>1432-0746</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2011</creationdate><recordtype>article</recordtype><recordid>eNo9kMlOwzAURS0EEqXwBWz8A6Z-8ZQsSwoFUQkJMa2wHMcOhmZQnEL797Qq6urp6t1zFwehS6BXQAVMKKWcSCZhklCgIDIGR2gEnCWEKi6P0ejQOEVnMX5tYwIpG6GPWei60FQ4NDjfVM0qvpNkFwyuV8shkF_z45auqYZPbE3dmVA1uFw5PLTYFLHtuyG0DW49duvBNaUr8XSWY1eHGLePc3TizTK6i_87Ri-3N8_5HVk8zu_z6YLYhCsgnFtZeJBJ6VgGWZI6Wxa8tBIy6wulgCubFiUHQWmpLE29l4IKD0ownwnHxojtd23fxtg7r7s-1KbfaKB6p0jvBOidAH1QtKXIngpxcOsDYvpvLRVTQqf0Tc8eruF1_nSrGfsDKWpn2g</recordid><startdate>201106</startdate><enddate>201106</enddate><creator>Bałucińska-Church, M.</creator><creator>Schulz, N. 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J.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c2471-44c6bf162de391928ecdb4dc619cfb77147c8bd41500d7c08ff6505f1753f95e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2011</creationdate><topic>acceleration of particles</topic><topic>accretion</topic><topic>accretion disks</topic><topic>radio continuum: general</topic><topic>stars: neutron</topic><topic>X-rays: binaries</topic><topic>X-rays: individuals: CygX-2</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Bałucińska-Church, M.</creatorcontrib><creatorcontrib>Schulz, N. S.</creatorcontrib><creatorcontrib>Wilms, J.</creatorcontrib><creatorcontrib>Gibiec, A.</creatorcontrib><creatorcontrib>Hanke, M.</creatorcontrib><creatorcontrib>Spencer, R. E.</creatorcontrib><creatorcontrib>Rushton, A.</creatorcontrib><creatorcontrib>Church, M. J.</creatorcontrib><collection>Istex</collection><collection>CrossRef</collection><jtitle>Astronomy and astrophysics (Berlin)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Bałucińska-Church, M.</au><au>Schulz, N. S.</au><au>Wilms, J.</au><au>Gibiec, A.</au><au>Hanke, M.</au><au>Spencer, R. E.</au><au>Rushton, A.</au><au>Church, M. J.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission</atitle><jtitle>Astronomy and astrophysics (Berlin)</jtitle><date>2011-06</date><risdate>2011</risdate><volume>530</volume><spage>A102</spage><pages>A102-</pages><issn>0004-6361</issn><eissn>1432-0746</eissn><abstract>We report results of one-day simultaneous multiwavelength observations of CygnusX-2 using XMM, Chandra, the European VLBI Network and the XMM Optical Monitor. During the observations, the source did not exhibit Z-track movement, but remained in the vicinity of the soft apex. It was in a radio quiescent/quiet state of <150 μJy. Strong dip events were seen as 25% reductions in X-ray intensity. The use of broadband CCD spectra in combination with narrow-band grating spectra has now demonstrated for the first time that these dipping events in CygnusX-2 are caused by absorption in cool material in quite a unique way. In the band 0.2 − 10 keV, dipping appears to be due to progressive covering of the Comptonized emission of an extended accretion disk corona, the covering factor rising to 40% in deep dipping with an associated column density of 3 × 1023 atom cm-2. Remarkably, the blackbody emission of the neutron star is not affected by these dips, in strong contrast with observations of typical low mass X-ray binary dipping sources. The Chandra and XMM gratings directly measure the optical depths in absorption edges such as Ne K, Fe L, and O K and a comparison of the optical depths in the edges of non-dip and dip data reveals no increase of optical depth during dipping even though the continuum emission sharply decreases. Based on these findings, at orbital phase 0.35, we propose that dipping in this observation is caused by absorption in the outer disk by structures located opposite to the impact bulge of the accretion stream. With an inclination angle >60° these structures can still cover large parts of the extended ADC, without absorbing emission from the central neutral star.</abstract><pub>EDP Sciences</pub><doi>10.1051/0004-6361/201015931</doi><oa>free_for_read</oa></addata></record> |
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| ispartof | Astronomy and astrophysics (Berlin), 2011-06, Vol.530, p.A102 |
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| source | Bacon EDP Sciences France Licence nationale-ISTEX-PS-Journals-PFISTEX; Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals; EDP Sciences |
| subjects | acceleration of particles accretion accretion disks radio continuum: general stars: neutron X-rays: binaries X-rays: individuals: CygX-2 |
| title | Dipping in CygnusX-2 in a multi-wavelength campaign due to absorption of extended ADC emission |
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