The variable radio counterpart and possible large-scale jet of the new Z source XTE J1701−462
Identifieur interne : 000B12 ( Istex/Corpus ); précédent : 000B11; suivant : 000B13The variable radio counterpart and possible large-scale jet of the new Z source XTE J1701−462
Auteurs : R. P. Fender ; M. Dahlem ; J. Homan ; S. Corbel ; R. Sault ; T. M. BelloniSource :
- Monthly Notices of the Royal Astronomical Society: Letters [ 1745-3925 ] ; 2007-09.
Abstract
We report radio observations, made with the Australia Telescope Compact Array, of the X-ray transient XTE J1701−462. This system has been classified as a new ‘Z’ source, displaying characteristic patterns of behaviour probably associated with accretion on to a low magnetic field neutron star at close to the Eddington limit. The radio counterpart is highly variable, and was detected in six of 16 observations over the period 2006 January–April. The coupling of radio emission to X-ray state, despite limited sampling, appears to be similar to that of other ‘Z’ sources, in that there is no radio emission on the flaring branch. The mean radio and X-ray luminosities are consistent with the other Z sources for a distance of 5–15 kpc. The radio spectrum is unusually flat, or even inverted, in contrast to the related sources, Sco X-1 and Cir X-1, which usually display an optically thin radio spectrum. Deep wide-field observations indicate an extended structure 3 arcmin to the south which is aligned with the X-ray binary. This seems to represent a significant overdensity of radio sources for the field and so, although a background source remains a strong possibility, we consider it plausible that this is a large-scale jet associated with XTE J1701−462.
Url:
DOI: 10.1111/j.1745-3933.2007.00350.x
Links to Exploration step
ISTEX:3B723459C00807DB77E08578A576EC5D9DCDCEE8Le document en format XML
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Belloni</name><affiliation><mods:affiliation>INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy</mods:affiliation></affiliation></author></analytic><monogr></monogr><series><title level="j">Monthly Notices of the Royal Astronomical Society: Letters</title><title level="j" type="abbrev">MNRAS</title><idno type="ISSN">1745-3925</idno><idno type="eISSN">1745-3933</idno><imprint><publisher>Blackwell Science Ltd</publisher><pubPlace>Oxford, UK</pubPlace><date type="published" when="2007-09">2007-09</date><biblScope unit="volume">380</biblScope><biblScope unit="issue">1</biblScope><biblScope unit="page" from="L25">L25</biblScope><biblScope unit="page" to="L29">L29</biblScope></imprint><idno type="ISSN">1745-3925</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">1745-3925</idno></seriesStmt></fileDesc><profileDesc><textClass></textClass></profileDesc></teiHeader><front><div type="abstract">We report radio observations, made with the Australia Telescope Compact Array, of the X-ray transient XTE J1701−462. This system has been classified as a new ‘Z’ source, displaying characteristic patterns of behaviour probably associated with accretion on to a low magnetic field neutron star at close to the Eddington limit. The radio counterpart is highly variable, and was detected in six of 16 observations over the period 2006 January–April. The coupling of radio emission to X-ray state, despite limited sampling, appears to be similar to that of other ‘Z’ sources, in that there is no radio emission on the flaring branch. The mean radio and X-ray luminosities are consistent with the other Z sources for a distance of 5–15 kpc. The radio spectrum is unusually flat, or even inverted, in contrast to the related sources, Sco X-1 and Cir X-1, which usually display an optically thin radio spectrum. Deep wide-field observations indicate an extended structure 3 arcmin to the south which is aligned with the X-ray binary. This seems to represent a significant overdensity of radio sources for the field and so, although a background source remains a strong possibility, we consider it plausible that this is a large-scale jet associated with XTE J1701−462.</div></front></TEI><istex><corpusName>oup</corpusName><author><json:item><name>R. P. Fender</name><affiliations><json:string>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</json:string><json:string>E-mail: rpf@phys.soton.ac.uk</json:string><json:null></json:null><json:string>E-mail: rpf@phys.soton.ac.uk</json:string></affiliations></json:item><json:item><name>M. Dahlem</name><affiliations><json:string>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</json:string></affiliations></json:item><json:item><name>J. 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The radio counterpart is highly variable, and was detected in six of 16 observations over the period 2006 January–April. The coupling of radio emission to X-ray state, despite limited sampling, appears to be similar to that of other ‘Z’ sources, in that there is no radio emission on the flaring branch. The mean radio and X-ray luminosities are consistent with the other Z sources for a distance of 5–15 kpc. The radio spectrum is unusually flat, or even inverted, in contrast to the related sources, Sco X-1 and Cir X-1, which usually display an optically thin radio spectrum. Deep wide-field observations indicate an extended structure 3 arcmin to the south which is aligned with the X-ray binary. 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(2007)</json:string><json:string>Philips et al. 2007</json:string><json:string>Homan et al. 2007</json:string><json:string>Corbel et al. 2002</json:string><json:string>Penninx et al. (1988)</json:string><json:string>van der Klis 2006</json:string><json:string>Maitra & Bailyn 2006</json:string><json:string>R. P. Fender et al.</json:string><json:string>Remillard et al. 2006</json:string><json:string>Tudose et al. 2006</json:string><json:string>Krauss et al. 2006</json:string><json:string>Fender et al. 2004</json:string><json:string>Stewart et al. 1991</json:string><json:string>Homan & Belloni 2005</json:string><json:string>Mc Hardy et al. 2006</json:string><json:string>Sault, Teuben & Wright 1995</json:string><json:string>Fender (2006)</json:string><json:string>Migliari et al. 2005</json:string><json:string>Fender et al. 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P.</forename><surname>Fender</surname></persName><email>rpf@phys.soton.ac.uk</email><email>rpf@phys.soton.ac.uk</email><affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation><affiliation></affiliation></author><author xml:id="author-0001"><persName><forename type="first">M.</forename><surname>Dahlem</surname></persName><affiliation>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</affiliation></author><author xml:id="author-0002"><persName><forename type="first">J.</forename><surname>Homan</surname></persName><affiliation>Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA</affiliation></author><author xml:id="author-0003"><persName><forename type="first">S.</forename><surname>Corbel</surname></persName><affiliation>AIM–Unité Mixte de Recherche CEA–CNRS, Université Paris VII, UMR 7158, CEA Saclay, Service d'Astrophysique, F-91191 Gif-sur-Yvette, France</affiliation></author><author xml:id="author-0004"><persName><forename type="first">R.</forename><surname>Sault</surname></persName><affiliation>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</affiliation></author><author xml:id="author-0005"><persName><forename type="first">T. 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This seems to represent a significant overdensity of radio sources for the field and so, although a background source remains a strong possibility, we consider it plausible that this is a large-scale jet associated with XTE J1701−462.</p></abstract><textClass><keywords scheme="keyword"><list><head>Keywords</head><item><term>binaries: close</term></item><item><term>stars: individual: XTE J1701−462</term></item><item><term>ISM: jets and outflows</term></item><item><term>radio continuum: stars</term></item></list></keywords></textClass></profileDesc><revisionDesc><change when="2007-09">Published</change></revisionDesc></teiHeader></istex:fulltextTEI><json:item><extension>txt</extension><original>false</original><mimetype>text/plain</mimetype><uri>https://api.istex.fr/document/3B723459C00807DB77E08578A576EC5D9DCDCEE8/fulltext/txt</uri></json:item></fulltext><metadata><istex:metadataXml wicri:clean="corpus oup, element #text not found" wicri:toSee="no header"><istex:xmlDeclaration>version="1.0"</istex:xmlDeclaration><istex:docType PUBLIC="-//NLM//DTD Journal Publishing DTD v2.3 20070202//EN" URI="journalpublishing.dtd" name="istex:docType"></istex:docType><istex:document><article article-type="research-article">
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<contrib contrib-type="author" corresp="yes">
<name><surname>Fender</surname><given-names>R. P.</given-names></name><xref ref-type="aff" rid="aff1"><sup>1</sup></xref><xref ref-type="corresp" rid="cor1"><sup>⋆</sup></xref>
</contrib>
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<name><surname>Dahlem</surname><given-names>M.</given-names></name><xref ref-type="aff" rid="aff2"><sup>2</sup></xref>
</contrib>
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<name><surname>Homan</surname><given-names>J.</given-names></name><xref ref-type="aff" rid="aff3"><sup>3</sup></xref>
</contrib>
<contrib contrib-type="author">
<name><surname>Corbel</surname><given-names>S.</given-names></name><xref ref-type="aff" rid="aff4"><sup>4</sup></xref>
</contrib>
<contrib contrib-type="author">
<name><surname>Sault</surname><given-names>R.</given-names></name><xref ref-type="aff" rid="aff2"><sup>2</sup></xref>
</contrib>
<contrib contrib-type="author">
<name><surname>Belloni</surname><given-names>T. M.</given-names></name><xref ref-type="aff" rid="aff5"><sup>5</sup></xref>
</contrib>
<aff id="aff1"><label>1</label>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</aff>
<aff id="aff2"><label>2</label>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</aff>
<aff id="aff3"><label>3</label>Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA</aff>
<aff id="aff4"><label>4</label>AIM–Unité Mixte de Recherche CEA–CNRS, Université Paris VII, UMR 7158, CEA Saclay, Service d'Astrophysique, F-91191 Gif-sur-Yvette, France</aff>
<aff id="aff5"><label>5</label>INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy</aff>
</contrib-group>
<author-notes>
<corresp id="cor1"><label>⋆</label>E-mail: <email>rpf@phys.soton.ac.uk</email></corresp>
</author-notes>
<pub-date pub-type="ppub">
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<year>2007</year>
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<month>5</month>
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<copyright-year>2007</copyright-year>
<abstract>
<p>We report radio observations, made with the Australia Telescope Compact Array, of the X-ray transient XTE J1701−462. This system has been classified as a new ‘Z’ source, displaying characteristic patterns of behaviour probably associated with accretion on to a low magnetic field neutron star at close to the Eddington limit. The radio counterpart is highly variable, and was detected in six of 16 observations over the period 2006 January–April. The coupling of radio emission to X-ray state, despite limited sampling, appears to be similar to that of other ‘Z’ sources, in that there is no radio emission on the flaring branch. The mean radio and X-ray luminosities are consistent with the other Z sources for a distance of 5–15 kpc. The radio spectrum is unusually flat, or even inverted, in contrast to the related sources, Sco X-1 and Cir X-1, which usually display an optically thin radio spectrum. Deep wide-field observations indicate an extended structure 3 arcmin to the south which is aligned with the X-ray binary. This seems to represent a significant overdensity of radio sources for the field and so, although a background source remains a strong possibility, we consider it plausible that this is a large-scale jet associated with XTE J1701−462.</p>
</abstract>
<kwd-group>
<title>Keywords</title>
<kwd>binaries: close</kwd>
<kwd>stars: individual: XTE J1701−462</kwd>
<kwd>ISM: jets and outflows</kwd>
<kwd>radio continuum: stars</kwd>
</kwd-group>
</article-meta>
</front>
<body>
<sec id="ss1" sec-type="intro">
<label>1</label>
<title>Introduction</title>
<p>The relation between accretion and outflow is a key topic in modern high-energy astrophysics, and offers us a unique opportunity to understand the physics of distant, supermassive black holes in active galactic nuclei (AGN) by studying nearby, rapidly varying objects such as X-ray binaries (XRBs). Much of the focus in recent years has been on black holes and how accretion scales between those of mass ∼10 M<sub>⊙</sub> in XRBs and those of mass ≥10<sup>5</sup> M<sub>⊙</sub> in AGN (<xref ref-type="bibr" rid="b24">Merloni, Heinz & di Matteo 2003</xref>; <xref ref-type="bibr" rid="b3">Falcke, Körding & Markoff 2004</xref>; see also <xref ref-type="bibr" rid="b20">Maccarone, Gallo & Fender 2003</xref>; <xref ref-type="bibr" rid="b17">Körding, Falcke & Corbel 2006a</xref>; <xref ref-type="bibr" rid="b37">Wang, Wu & Kong 2006</xref>; <xref ref-type="bibr" rid="b21">MHardy et al. 2006</xref>).</p>
<p>However, the neutron star XRBs represent an extremely valuable ‘control sample’. These systems also produce dramatic jets (e.g. <xref ref-type="bibr" rid="b9">Fomalont, Geldzahler & Bradshaw 2001</xref>; <xref ref-type="bibr" rid="b7">Fender et al. 2004</xref>) over a wide range of accretion rates (<xref ref-type="bibr" rid="b25">Migliari & Fender 2006</xref>). By comparing the two classes of object we can test the necessity of black hole-specific physics, such as event horizons and static limits, for the observed phenomena of accretion and jet production (e.g. <xref ref-type="bibr" rid="b18">Körding, Fender & Migliari 2006b</xref>).</p>
<p>The ‘Z sources’ are the six (or seven, if you include Cir X-1) most luminous neutron star XRBs in our Galaxy, persistently accreting at close to the Eddington limit (within a factor of a few). Their name comes from the characteristic pattern traced out in X-ray colour–colour diagrams (CDs) (<xref ref-type="bibr" rid="b10">Hasinger & van der Klis 1989</xref>; <xref ref-type="bibr" rid="b36">van der Klis 2006</xref>, and references therein). All Z sources are detected in the radio band with approximately the same radio luminosity (<xref ref-type="bibr" rid="b28">Penninx 1989</xref>; <xref ref-type="bibr" rid="b5">Fender & Hendry 2000</xref>). <xref ref-type="bibr" rid="b29">Penninx et al. (1988)</xref> discovered a relation between the three branches of the ‘Z’ in the CD and the strength of the radio emission [see <xref ref-type="bibr" rid="b25">Migliari & Fender (2006)</xref> for further discussion and references]. The two Z/Z-like sources in which the radio emission has been spatially resolved, Sco X-1 and Cir X-1, are both found to be associated with highly relativistic flows energizing more slowly moving radio-emitting components (<xref ref-type="bibr" rid="b9">Fomalont et al. 2001</xref>; <xref ref-type="bibr" rid="b7">Fender et al. 2004</xref>). In particular, the most relativistic flow yet identified in our Galaxy is associated with the neutron star jet source Cir X-1 (<xref ref-type="bibr" rid="b7">Fender et al. 2004</xref>) which sometimes displays X-ray spectral and timing characteristics similar to that of the Z sources. SS 433 may also display this characteristic of an unseen, fast flow energizing more slowly moving knots (<xref ref-type="bibr" rid="b26">Migliari et al. 2005</xref>), which is not something that has been observed in any bona fide black hole candidate.</p>
<sec id="ss1-1">
<label>1.1</label>
<title>XTE J70−462: a new, transient, Z source</title>
<p>XTE J1701−462 was discovered by the <italic>RXTE</italic> satellite as a bright new X-ray transient on 2006 January 18 (<xref ref-type="bibr" rid="b32">Remillard et al. 2006</xref>). X-ray observations soon indicated that it was likely to be a ‘new’ Z source (<xref ref-type="bibr" rid="b12">Homan et al. 2006a,b</xref>). An infrared counterpart was reported (<xref ref-type="bibr" rid="b23">Maitra et al. 2006</xref>; <xref ref-type="bibr" rid="b22">Maitra & Bailyn 2006</xref>), which was found to be coincident with a radio source (<xref ref-type="bibr" rid="b8">Fender, Sault & Dahlem 2006</xref>), although formally inconsistent with a localization from the <italic>Swift X-ray Telescope</italic> (<xref ref-type="bibr" rid="b16">Kennea et al. 2006</xref>). Subsequent localization to better than 1 arcsec with <italic>Chandra</italic> confirmed the association with the optical/infrared/radio counterparts (<xref ref-type="bibr" rid="b19">Krauss et al. 2006</xref>).</p>
<p><xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref> recently reported the first two months' of <italic>RXTE</italic> observations of the source, summarizing the evidence for its classification as a new Z source. CDs and hardness–intensity diagrams (HIDs) are commonly used to identify patterns of X-ray behaviour in accreting X-ray sources within our Galaxy (e.g. <xref ref-type="bibr" rid="b11">Homan & Belloni 2005</xref>; <xref ref-type="bibr" rid="b36">van der Klis 2006</xref>). In <xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref> it was noted that the pattern traced out by XTE J1701−462 in the CD/HID changed significantly on at least nine occasions in the first 70 d of the outburst. In particular, it was noted that for the first ∼25 d of the outburst (i.e. up to around 2006 February 16/MJD 53782) the source was ‘Cyg-like’, and subsequently most ‘Sco-like’, these labels referring to apparent subgroups within the Z sources [see <xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref> for more details].</p>
</sec>
</sec>
<sec id="ss2">
<label>2</label>
<title>Observations</title>
<p>XTE J1701−462 was observed at 16 epochs with the Australia Telescope Compact Array (ATCA) between 2006 January 22 and April 23. All observations were made simultaneously at 4.8 and 8.6 GHz. A log of these observations is presented in <xref ref-type="fig" rid="tbl1">Table 1</xref>, and <xref ref-type="fig" rid="fig1">Fig. 1</xref> indicates the observation epochs on a light curve of the X-ray emission. Many of the observations were very short (nine of the 16 were less than 1.5 h on-source) which resulted in some difficulties in mapping the source. Six of the observations (A, B, F, K, M and N) resulted in unambiguous detections.</p>
<fig id="tbl1" position="float">
<label>Table 1</label>
<caption>
<p>Summary of radio observations of XTE J1701−462. Column 1 gives the epoch label, which is used in the discussion in the main text, and also in <xref ref-type="fig" rid="fig1">Fig. 1</xref>. Column 2 indicates whether or not there was a detection of the radio source; only for those unambiguous detections, where yes is indicated, do we provide flux densities. Columns 3–5 give start and stop times and total hours on‐source. Columns 6 and 7 give detections or upper limits at 4.8 and 8.6 GHz respectively (note that in some cases we have indicated detections that appear to be less than three times the error – this is due to uncertainties in the flux calibration for short observations, and does not indicate the reliability of the detection; this particularly applies to epochs A and K). All measurements are based upon naturally weighted maps, and all upper limits are three times the rms noise in the area of the source. Column 8 indicates whether or not the observation was strictly simultaneous with an observation by <italic>RXTE</italic>, and Column 9 indicates our best estimate of the branch or branches of the Z occupied by the source at, or close to, the time of the radio observation.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-tbl001.tif"></graphic>
</fig>
<fig id="fig1" position="float">
<label>Figure 1</label>
<caption>
<p><italic>RXTE</italic> Proportional Counter Array monitoring of XTE J1701−462 over the period 2006 January–April, the first 100 d of the outburst. The epochs of the 16 ATCA radio observations in this period are indicated – only at epochs marked by filled symbols are there unambiguous radio detections of the XRB.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-fig001.gif"></graphic>
</fig>
<p>No polarized signal was detected at any time, with an upper limit on the linear and circular polarization of ≤6 per cent for epoch M, when the source was brightest.</p>
<p>Data reduction was performed with the <sc>miriad</sc> package (<xref ref-type="bibr" rid="b33">Sault, Teuben & Wright 1995</xref>). In most cases naturally weighted, cleaned maps were used for image analysis. We were able to produce a combined map from all the data using visibilities calibrated individually at each epoch. The radio counterpart of XTE J1701−462 is clearly detected at RA (J2000) 17<sup>h</sup>00<sup>m</sup>58<sup>s</sup>.43, Dec. -46° 11′08<sup>s</sup>.44, with an uncertainty of about 0.3 arcsec in each coordinate.</p>
</sec>
<sec id="ss3" sec-type="discussion">
<label>3</label>
<title>Discussion</title>
<sec id="ss3-1">
<label>3.1</label>
<title>Coupling between radio and X-ray emission</title>
<p>In order to compare the radio and X-ray properties of XTE J1701−462, we have made an estimate of which part of the ‘Z’ the source was on at or close to the time of each radio observation. XTE J1701−462 was observed 97 times with <italic>RXTE</italic> between 2006 January 22 and March 20, and once on 2006 April 23, providing simultaneous X-ray coverage for three of our radio observations and X-ray coverage within a few hours for the others. The <italic>RXTE</italic> observations before March 20 were all classified according to their timing properties and position in X-ray CDs by <xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref>, and a separate analysis of the 2006 April 23 <italic>RXTE</italic> observation was done for the current Letter. The location along the Z tracks was estimated for the <italic>RXTE</italic> observations that were closest in time to our radio observations, by determining their position (upper/middle/lower) along the branches of full Z tracks that were traced out in various time intervals (see fig. 3 in <xref ref-type="bibr" rid="b14">Homan et al. 2007</xref>). These estimates are indicated in <xref ref-type="fig" rid="tbl1">Table 1</xref>. The radio detections and upper limits are also indicated as a function of branch of the Z in <xref ref-type="fig" rid="fig2">Fig. 2</xref>.</p>
<fig id="fig2" position="float">
<label>Figure 2</label>
<caption>
<p>Radio detections (filled circles) and upper limits (open triangles) as a function of our estimate of the branch/branches of the Z that the source was on at/close to the time of the radio observations (see <xref ref-type="fig" rid="tbl1">Table 1</xref>). The results are consistent with, but do not independently establish, the relation claimed for the Z source GX 17+2, in which radio emission is strongest on the HB/NB, and suppressed on the FB.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-fig002.gif"></graphic>
</fig>
<p>Our observations appear to indicate that XTE J1701−462 is most likely to be detected as a radio source when on the horizontal or normal branch (HB, NB) of the Z. There are no detections on the flaring branch (FB), including the most stringent upper limit (observation P). This is consistent with the behaviour noted first noted for GX 17+2 by <xref ref-type="bibr" rid="b29">Penninx et al. (1988)</xref> and possibly universal for all Z sources (<xref ref-type="bibr" rid="b28">Penninx 1989</xref>). These periods of relatively strong radio emission almost certainly correspond to the formation of jet-like outflows and/or their interaction with the surrounding medium (as directly observed in the Z/Z-like sources Sco X-1 and Cir X-1: <xref ref-type="bibr" rid="b9">Fomalont et al. 2001</xref>; <xref ref-type="bibr" rid="b7">Fender et al. 2004</xref>). In particular, based primarily on results for Sco X-1, <xref ref-type="bibr" rid="b25">Migliari & Fender (2006)</xref> suggest that the HB/NB vertex may correspond to the point at which the most powerful ejection events occur, and that the jet is suppressed on the FB.</p>
<p>The Z sources are likely to be accreting persistently (in most cases) at close to the Eddington limit. It may be useful to compare them to black hole XRBs accreting at comparably high Eddington ratios, such as GRS 1915+105. Both classes of object make dramatic and rapid state transitions and are associated with episodic production of powerful relativistic jets. Such objects may, in turn, be our best ‘local’ equivalents of quasars accreting at very high rates at redshifts of <italic>z</italic>≥ 1. Therefore careful comparison of objects such as XTE J1701−462 with black holes accreting at high rates may provide our best test of the effects of e.g. event horizons, static limits on accretion and jet formation.</p>
</sec>
<sec id="ss3-2">
<label>3.2</label>
<title>Spectral index</title>
<p>The two-point radio spectra of these detections are plotted in <xref ref-type="fig" rid="fig3">Fig. 3</xref>. It is interesting to note that for the majority of the radio detections of XTE J1701−462 the source radio spectrum is flat/inverted (spectral index α≥ 0, where S<sub>ν</sub>∝ν<sup>α</sup>). This seems to be in contrast to most emission associated with transient outbursts from XRBs which generally has an optically thin spectrum (α≤−0.6). Optically thin emission is also observed in Cir X-1 (<xref ref-type="bibr" rid="b6">Fender et al. 1998, 2004</xref>) and Sco X-1 (<xref ref-type="bibr" rid="b9">Fomalont et al. 2001</xref>), although in both sources episodes of flat-spectrum core emission have been seen. The flat/inverted radio spectrum is in fact more reminiscent of the steady, flat-spectrum radio emission observed from black holes in hard X-ray states (<xref ref-type="bibr" rid="b4">Fender 2001</xref>), although <xref ref-type="bibr" rid="b25">Migliari & Fender (2006)</xref> do suggest that it should also be observed in hard-state neutron stars. Such flat-spectrum emission is believed to arise in a partially self-absorbed jet (<xref ref-type="bibr" rid="b1">Blandford & Königl 1979</xref>; <xref ref-type="bibr" rid="b15">Kaiser 2006</xref>). Given the rather poor coverage and weak source in most cases, there remains some uncertainty in these spectral index measurements. If the spectrum is genuinely flat or inverted it implies the ongoing production of a compact jet and not, for example, shocks in diffuse regions well separated from the binary. The limits on the polarization (≤6 per cent in Stokes <italic>Q</italic>, <italic>U</italic>, <italic>V</italic>) are consistent with the self-absorbed jet model – measured linear polarizations for flat-spectrum jets in black hole XRBs are at the few per cent level (<xref ref-type="bibr" rid="b4">Fender 2001</xref>, and references therein).</p>
<fig id="fig3" position="float">
<label>Figure 3</label>
<caption>
<p>Two-point radio spectra for XTE J1701−462 for the six unambiguous detections. The spectra are generally flat or inverted, in contrast to the optically thin emission usually associated with transients. If real, this indicates that when the radio emission is detected the jet is currently being generated in regions with significant synchrotron self-absorption (i.e. the base of the jet close to the neutron star).</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-fig003.gif"></graphic>
</fig>
</sec>
<sec id="ss3-3">
<label>3.3</label>
<title>Luminosity and distance</title>
<p>As noted above, it is a defining characteristic of Z sources that they are accreting at near to (sometimes in excess of) the Eddington limit for a 1.4 -M<sub>⊙</sub>, neutron star, and that they are relatively strong radio sources. <xref ref-type="bibr" rid="b25">Migliari & Fender (2006)</xref> plotted the radio luminosity as a function of X-ray luminosity for all neutron star XRBs with radio counterparts, and indeed found the Z sources to be the most luminous in both bands. In <xref ref-type="fig" rid="fig4">Fig. 4</xref> we plot the same sample with a point representing XTE J1701−462 at each of three distances: 5, 10 and 15 kpc. The point is based upon the estimated flux of ∼10<sup>−8</sup> erg s<sup>−1</sup> cm<sup>−2</sup> for observation phase G in <xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref>, which is close in time to our observation M. We have chosen a mean flux density for this period of ∼0.5 mJy. We note that while this estimate of the mean radio flux does not take into account non-detections, nor did the estimates of <xref ref-type="bibr" rid="b5">Fender & Hendry (2000)</xref> on which the points for the other Z sources are based. Based solely on this rough comparison, it seems reasonable to conclude that XTE J1701−462 lies at a distance of ∼10 kpc, with an error of a factor of 2. Compare this to a different approach in <xref ref-type="bibr" rid="b14">Homan et al. (2007)</xref>, where a distance of ∼15 kpc was derived.</p>
<fig id="fig4" position="float">
<label>Figure 4</label>
<caption>
<p>Radio luminosity as a function of X-ray luminosity for neutron star XRBs. The Z sources are the most luminous group of objects in both bands. The locus of XTE J1701−462, around the time of our observation M, is indicated for three different distances.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-fig004.gif"></graphic>
</fig>
</sec>
<sec id="ss3-4">
<label>3.4</label>
<title>An ultrarelativistic jet and a large-scale nebula?</title>
<p>Finally, the similarities with the other Z sources, in terms of the X-ray properties and their relation to the radio emission, suggest that XTE J1701−462 may harbour a relativistic jet like those resolved in Sco X-1 (<xref ref-type="bibr" rid="b9">Fomalont et al. 2001</xref>) and Cir X-1 (<xref ref-type="bibr" rid="b7">Fender et al. 2004</xref>). Future high angular resolution observations with ATCA and Australian e-VLBI (<xref ref-type="bibr" rid="b30">Philips et al. 2007</xref>) may resolve and track the variability of such a jet.</p>
<p>Furthermore, Cir X-1 has an arcmin-scale radio nebula which seems to be powered by the central jet (Stewart et al. 1991; <xref ref-type="bibr" rid="b35">Tudose et al. 2006</xref>), as do a number of black hole XRBs (e.g. <xref ref-type="bibr" rid="b27">Mirabel et al. 1992</xref>; <xref ref-type="bibr" rid="b2">Corbel et al. 2002</xref>). In order to investigate whether XTE J1701−462 may have a similar large-scale radio structure, we created a deep image by summing all of the available data (<xref ref-type="fig" rid="fig5">Fig. 5</xref>). Several fairly strong sources are clearly detected to the south of XTE J1701−462, and are approximately lined up back towards the XRB. Peak fluxes for XTE J1701−462 and the sources A–D are listed in <xref ref-type="fig" rid="tbl2">Table 2</xref>, measured from naturally weighted summed maps at both frequencies. The spectral index is also given, and indicates that sources A–D are all non-thermal in nature, with an apparent trend of steepening spectra with increasing distance to the south (although resolution effects may play a role if the structure also becomes more diffuse to the south).</p>
<fig id="fig5" position="float">
<label>Figure 5</label>
<caption>
<p>Summed radio image from all 16 epochs of ATCA observations (24.1 h on-source). The radio counterpart of XTE J1701−462, unambiguously detected in at least one-third of the observations, is indicated to the north of the figure. This radio source is entirely consistent with the <italic>Chandra</italic> localization reported by <xref ref-type="bibr" rid="b19">Krauss et al. (2006)</xref>. There is clearly a complex of radio sources about 3 arcmin to the south, and aligned towards the XRB. Peak fluxes for XTE J1701−462 and components A–B from this map are given in <xref ref-type="fig" rid="tbl2">Table 2</xref>. The image is at 4.8 GHz and the contours are at (−3, 3, 6, 12, 24) times the rms noise of 28 μJy.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-fig005.gif"></graphic>
</fig>
<fig id="tbl2" position="float">
<label>Table 2</label>
<caption>
<p>Peak fluxes and spectral index of XTE J−462 and sources A–D at 4.8 and 8.6 GHz as measured from the summed, naturally weighted maps.</p>
</caption>
<graphic mimetype="image" xlink:href="380-1-L25-tbl002.tif"></graphic>
</fig>
<p>Note that while variations in the flux of XTE J1701−462 between epochs could cause artefacts in such a combined map, we consider it highly unlikely that they could produce the extended structure seen in <xref ref-type="fig" rid="fig5">Fig. 5</xref>. Furthermore, this structure is visible to a varying degree in longer individual runs (runs B, F, M, N, O and P). The obvious initial interpretation of this structure is that it is an unrelated background radio source, probably extragalactic. However, based on the source counts from the Australia Telescope ESO Slice Project 5-GHz deep survey (<xref ref-type="bibr" rid="b31">Prandoni et al. 2006</xref>), we would only expect ∼0.05 sources in the 1.5–2.5 mJy range in a region the size of the map presented in <xref ref-type="fig" rid="fig5">Fig. 5</xref>. Sources B, C and D are all in this range. In addition, if we consider that sources A–D are a single extended source, for the integrated flux density, ∼5 mJy, the ATESP survery indicates a mean angular size of ≲10 arcsec, much less than the ≳60 arcsec angular extent of the source(s). Furthermore, the SIMBAD<xref ref-type="fn" rid="fn1"><sup>1</sup></xref>> data base lists no catalogued objects at this location. XTE J1701−462 appears to lie in a region of the sky that is overdense in bright, compact, 5-GHz radio sources.</p>
<p>The possibility must therefore be considered that the source to the south may be related in some way to the XRB. If so, it appears to take the form of a curved, one-sided radio jet (there is no comparable structure to the north). At an angular separation from the XRB of 3 arcmin and a distance of 5–15 kpc, the physical separation of components A–D from XTE J1701−462 is greater than 10<sup>19</sup> cm, which at face value seems to rule out an association with the 2006 January outburst, as apparent velocities greater than 80<italic>c</italic> would be required [but see <xref ref-type="bibr" rid="b7">Fender et al. (2004)</xref> for the intriguingly similar case of Cir X-1]. Further radio observations to look for variability and more diffuse structure are planned, as are observations at other wavelengths.</p>
</sec>
</sec>
<sec id="ss4" sec-type="conclusions">
<label>4</label>
<title>Conclusions</title>
<p>In 2006 January a new X-ray transient, XTE J1701−462, was discovered, and rapidly established to display the characteristics of a Z-type neutron star XRB. In this Letter we report on the variable radio counterpart to this X-ray source, which demonstrates a coupling between X-ray state (branch of the Z) and radio luminosity similar to that of the other Z sources. By analogy with Sco X-1 and Cir X-1, we interpret this as telling us about the connection between accretion flows and the production of a relativistic jet. Fortunately, since its activation, XTE J1701−462 has remained a bright X-ray source (as of 2007 May), and provides us with a new laboratory in which to study these phenomena. Furthermore, there is some evidence that the source is powering a large-scale radio jet, which hints not only at phases of past activity, but also at the possibility of a nebula which may be used to constrain the integrated jet power and provide a further direct comparison between jets from neutron stars and those from black holes.</p>
</sec>
</body>
<back>
<ack>
<sec id="ss5">
<title>Acknowledgments</title>
<p>RPF thanks Simone Migliari for providing his data for <xref ref-type="fig" rid="fig4">Fig. 4</xref>, and Derek Moss for assistance with radio source counts. We also thank the referee for suggesting, and the Editor for insisting, that we check on the expected source counts. We acknowledge the extreme flexibility of the schedulers and observers at the Australia Telescope Compact Array who supported these observations. The ATCA is run by ATNF for CSIRO.</p>
</sec>
</ack>
<ref-list>
<title>References</title>
<ref id="b1">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Blandford</surname><given-names>R.</given-names></name><name><surname>Königl</surname><given-names>A.</given-names></name></person-group>, <year>1979</year>, <source>ApJ</source>, <volume>232</volume>, <fpage>34</fpage></citation>
</ref>
<ref id="b2">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Corbel</surname><given-names>S.</given-names></name><name><surname>Fender</surname><given-names>R. P.</given-names></name><name><surname>Tzioumis</surname><given-names>A. K.</given-names></name><name><surname>Tomsick</surname><given-names>J. A.</given-names></name><name><surname>Orosz</surname><given-names>J. A.</given-names></name><name><surname>Miller</surname><given-names>J. M.</given-names></name><name><surname>Wijnands</surname><given-names>R.</given-names></name><name><surname>Kaaret</surname><given-names>P.</given-names></name></person-group>, <year>2002</year>, <source>Sci</source>, <volume>298</volume>, <fpage>196</fpage></citation>
</ref>
<ref id="b3">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Falcke</surname><given-names>H.</given-names></name><name><surname>Körding</surname><given-names>E.</given-names></name><name><surname>Markoff</surname><given-names>S.</given-names></name></person-group>, <year>2004</year>, <source>A&A</source>, <volume>414</volume>, <fpage>895</fpage></citation>
</ref>
<ref id="b4">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fender</surname><given-names>R. P.</given-names></name></person-group>, <year>2001</year>, <source>MNRAS</source>, <volume>322</volume>, <fpage>31</fpage></citation>
</ref>
<ref id="b5">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fender</surname><given-names>R. P.</given-names></name><name><surname>Hendry</surname><given-names>M. A.</given-names></name></person-group>, <year>2000</year>, <source>MNRAS</source>, <volume>317</volume>, <fpage>1</fpage></citation>
</ref>
<ref id="b6">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fender</surname><given-names>R.</given-names></name><name><surname>Spencer</surname><given-names>R.</given-names></name><name><surname>Tzioumis</surname><given-names>T.</given-names></name><name><surname>Wu</surname><given-names>K.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name><name><surname>Van Paradijs</surname><given-names>J.</given-names></name><name><surname>Johnston</surname><given-names>H.</given-names></name></person-group>, <year>1998</year>, <source>ApJ</source>, <volume>506</volume>, <fpage>L121</fpage></citation>
</ref>
<ref id="b7">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fender</surname><given-names>R.</given-names></name><name><surname>Wu</surname><given-names>K.</given-names></name><name><surname>Johnston</surname><given-names>H.</given-names></name><name><surname>Tzioumis</surname><given-names>T.</given-names></name><name><surname>Jonker</surname><given-names>P.</given-names></name><name><surname>Spencer</surname><given-names>R.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, <year>2004</year>, <source>Nat</source>, <volume>427</volume>, <fpage>222</fpage></citation>
</ref>
<ref id="b8">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fender</surname><given-names>R.</given-names></name><name><surname>Sault</surname><given-names>B.</given-names></name><name><surname>Dahlem</surname><given-names>M.</given-names></name></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>710</fpage></citation>
</ref>
<ref id="b9">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Fomalont</surname><given-names>E. B.</given-names></name><name><surname>Geldzahler</surname><given-names>B. J.</given-names></name><name><surname>Bradshaw</surname><given-names>C. F.</given-names></name></person-group>, <year>2001</year>, <source>ApJ</source>, <volume>558</volume>, <fpage>283</fpage></citation>
</ref>
<ref id="b10">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Hasinger</surname><given-names>G.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, <year>1989</year>, <source>A&A</source>, <volume>225</volume>, <fpage>79</fpage></citation>
</ref>
<ref id="b11">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Homan</surname><given-names>J.</given-names></name><name><surname>Belloni</surname><given-names>T.</given-names></name></person-group>, <year>2005</year>, <source>Ap&SS</source>, <volume>300</volume>, <fpage>107</fpage></citation>
</ref>
<ref id="b12">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Homan</surname><given-names>J.</given-names></name><etal></etal></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>725</fpage></citation>
</ref>
<ref id="b13">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Homan</surname><given-names>J.</given-names></name><etal></etal></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>748</fpage></citation>
</ref>
<ref id="b14">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Homan</surname><given-names>J.</given-names></name><etal></etal></person-group>, <year>2007</year>, <source>ApJ</source>, <volume>656</volume>, <fpage>420</fpage></citation>
</ref>
<ref id="b15">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Kaiser</surname><given-names>C.</given-names></name></person-group>, <year>2006</year>, <source>MNRAS</source>, <volume>367</volume>, <fpage>1083</fpage></citation>
</ref>
<ref id="b16">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Kennea</surname><given-names>J. A.</given-names></name><etal></etal></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>702</fpage></citation>
</ref>
<ref id="b17">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Körding</surname><given-names>E.</given-names></name><name><surname>Falcke</surname><given-names>H.</given-names></name><name><surname>Corbel</surname><given-names>S.</given-names></name></person-group>, <year>2006</year>, <source>A&A</source>, <volume>456</volume>, <fpage>439</fpage></citation>
</ref>
<ref id="b18">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Körding</surname><given-names>E.</given-names></name><name><surname>Fender</surname><given-names>R.</given-names></name><name><surname>Migliari</surname><given-names>S.</given-names></name></person-group>, <year>2006</year>, <source>MNRAS</source>, <volume>369</volume>, <fpage>1451</fpage></citation>
</ref>
<ref id="b19">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Krauss</surname><given-names>M. I.</given-names></name><name><surname>Juett</surname><given-names>A. M.</given-names></name><name><surname>Chakrabarty</surname><given-names>D.</given-names></name><name><surname>Jonker</surname><given-names>P. G.</given-names></name><name><surname>Markwardt</surname><given-names>C. B.</given-names></name></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>777</fpage></citation>
</ref>
<ref id="b20">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Maccarone</surname><given-names>T.</given-names></name><name><surname>Gallo</surname><given-names>E.</given-names></name><name><surname>Fender</surname><given-names>R. P.</given-names></name></person-group>, <year>2003</year>, <source>MNRAS</source>, <volume>345</volume>, <fpage>L19</fpage></citation>
</ref>
<ref id="b21">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>McHardy</surname><given-names>I.</given-names></name><name><surname>Körding</surname><given-names>E.</given-names></name><name><surname>Uttley</surname><given-names>P.</given-names></name><name><surname>Knigge</surname><given-names>C.</given-names></name><name><surname>Fender</surname><given-names>R.</given-names></name></person-group>, <year>2006</year>, <source>Nat</source>, <volume>444</volume>, <fpage>730</fpage></citation>
</ref>
<ref id="b22">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Maitra</surname><given-names>D.</given-names></name><name><surname>Bailyn</surname><given-names>C.</given-names></name></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>712</fpage></citation>
</ref>
<ref id="b23">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Maitra</surname><given-names>D.</given-names></name><name><surname>Bailyn</surname><given-names>C.</given-names></name><name><surname>Nelan</surname><given-names>J.</given-names></name><name><surname>Espinoza</surname><given-names>J.</given-names></name></person-group>, <year>2006</year>, <source>Astron. Tel.</source>, <fpage>706</fpage></citation>
</ref>
<ref id="b24">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Merloni</surname><given-names>A.</given-names></name><name><surname>Heinz</surname><given-names>S.</given-names></name><name><surname>Di Matteo</surname><given-names>T.</given-names></name></person-group>, <year>2003</year>, <source>MNRAS</source>, <volume>345</volume>, <fpage>1057</fpage></citation>
</ref>
<ref id="b25">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Migliari</surname><given-names>S.</given-names></name><name><surname>Fender</surname><given-names>R.</given-names></name></person-group>, <year>2006</year>, <source>MNRAS</source>, <volume>366</volume>, <fpage>79</fpage></citation>
</ref>
<ref id="b26">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Migliari</surname><given-names>S.</given-names></name><name><surname>Fender</surname><given-names>R.</given-names></name><name><surname>Blundell</surname><given-names>K.</given-names></name><name><surname>Mendez</surname><given-names>M.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, <year>2005</year>, <source>MNRAS</source>, <volume>358</volume>, <fpage>860</fpage></citation>
</ref>
<ref id="b27">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Mirabel</surname><given-names>I. F.</given-names></name><name><surname>Rodriguez</surname><given-names>L. F.</given-names></name><name><surname>Cordier</surname><given-names>B.</given-names></name><name><surname>Paul</surname><given-names>J.</given-names></name><name><surname>Lebrun</surname><given-names>F.</given-names></name></person-group>, <year>1992</year>, <source>Nat</source>, <volume>358</volume>, <fpage>215</fpage></citation>
</ref>
<ref id="b28">
<citation citation-type="book">
<person-group person-group-type="author">
<name><surname>Penninx</surname><given-names>W.</given-names></name></person-group>, <year>1989</year>, in <person-group person-group-type="editor"><name><surname>Hunt</surname><given-names>J.</given-names></name><name><surname>Battrick</surname><given-names>B.</given-names></name></person-group>, eds, ESA SP-296, <source>23rd ESLAB Symp. on Two Topics in X-ray Astronomy</source>. <publisher-name>ESA</publisher-name>, Noordwijk, p. <fpage>185</fpage></citation>
</ref>
<ref id="b29">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Penninx</surname><given-names>W.</given-names></name><name><surname>Lewin</surname><given-names>W. H. G.</given-names></name><name><surname>Zijlstra</surname><given-names>A. A.</given-names></name><name><surname>Mitsuda</surname><given-names>K.</given-names></name><name><surname>Van Paradijs</surname><given-names>J.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, <year>1988</year>, <source>Nat</source>, <volume>336</volume>, <fpage>146</fpage></citation>
</ref>
<ref id="b30">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Philips</surname><given-names>C.</given-names></name><etal></etal></person-group>, <year>2007</year>, <source>MNRAS</source>, submitted</citation>
</ref>
<ref id="b31">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Prandoni</surname><given-names>I.</given-names></name><name><surname>Parma</surname><given-names>P.</given-names></name><name><surname>Wieringa</surname><given-names>M. H.</given-names></name><name><surname>De Ruiter</surname><given-names>H. R.</given-names></name><name><surname>Gregorini</surname><given-names>L.</given-names></name><name><surname>Mignano</surname><given-names>A.</given-names></name><name><surname>Vettolani</surname><given-names>G.</given-names></name><name><surname>Ekers</surname><given-names>R. D.</given-names></name></person-group>, <year>2006</year>, <source>A&A</source>, <volume>457</volume>, <fpage>517</fpage></citation>
</ref>
<ref id="b32">
<citation citation-type="other">
<person-group person-group-type="author">
<name><surname>Remillard</surname><given-names>R.</given-names></name><name><surname>Lin</surname><given-names>D.</given-names></name><collab>ASM Team at MIT</collab></person-group>, <year>2006</year>, Astron. Tel., <fpage>696</fpage></citation>
</ref>
<ref id="b33">
<citation citation-type="book">
<person-group person-group-type="author">
<name><surname>Sault</surname><given-names>R. J.</given-names></name><name><surname>Teuben</surname><given-names>P. J.</given-names></name><name><surname>Wright</surname><given-names>M. C. H.</given-names></name></person-group>, <year>1995</year>, in <person-group person-group-type="editor"><name><surname>Shaw</surname><given-names>R.</given-names></name><name><surname>Payne</surname><given-names>H. E.</given-names></name><name><surname>Hayes</surname><given-names>J. J. E.</given-names></name></person-group>, eds, ASP Conf. Ser. Vol. 77, <source>Astronomical Data Analysis Software and Systems IV</source>. <publisher-name>Astron. Soc. Pac.</publisher-name>, San Francisco, p. <fpage>433</fpage></citation>
</ref>
<ref id="b71">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Stewart</surname><given-names>R. T.</given-names></name><name><surname>Caswell</surname><given-names>J. L.</given-names></name><name><surname>Haynes</surname><given-names>R. F.</given-names></name><name><surname>Nelson</surname><given-names>G. J.</given-names></name></person-group>, <year>1993</year>, <source>MNRAS</source>, <volume>261</volume>, <fpage>593</fpage></citation>
</ref>
<ref id="b35">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Tudose</surname><given-names>V.</given-names></name><name><surname>Fender</surname><given-names>R. P.</given-names></name><name><surname>Kaiser</surname><given-names>C. R.</given-names></name><name><surname>Tzioumis</surname><given-names>A. K.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name><name><surname>Spencer</surname><given-names>R. E.</given-names></name></person-group>, <year>2006</year>, <source>MNRAS</source>, <volume>372</volume>, <fpage>417</fpage></citation>
</ref>
<ref id="b36">
<citation citation-type="book">
<person-group person-group-type="author">
<name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, <year>2006</year>, in <person-group person-group-type="editor"><name><surname>Lewin</surname><given-names>W.</given-names></name><name><surname>Van Der Klis</surname><given-names>M.</given-names></name></person-group>, eds, <source>Cambridge Astrophys. Ser. No. 39</source>, Compact Stellar X-ray Sources. <publisher-name>Cambridge Univ. Press</publisher-name>, Cambridge, p. <fpage>39</fpage></citation>
</ref>
<ref id="b37">
<citation citation-type="journal">
<person-group person-group-type="author">
<name><surname>Wang</surname><given-names>R.</given-names></name><name><surname>Wu</surname><given-names>X.-B.</given-names></name><name><surname>Kong</surname><given-names>M.-Z.</given-names></name></person-group>, <year>2006</year>, <source>ApJ</source>, <volume>645</volume>, <fpage>890</fpage></citation>
</ref>
</ref-list>
<fn-group>
<fn fn-type="other" id="fn1">
<label>1</label>
<p><ext-link ext-link-type="uri" xlink:href="http://simbad.u-strasbg.fr/simbad/">http://simbad.u-strasbg.fr/simbad/</ext-link></p>
</fn>
</fn-group>
</back>
</article></istex:document></istex:metadataXml><mods version="3.6"><titleInfo><title>The variable radio counterpart and possible large-scale jet of the new Z source XTE J1701−462</title></titleInfo><titleInfo type="alternative" contentType="CDATA"><title>The variable radio counterpart and possible large-scale jet of the new Z source XTE J1701−462</title></titleInfo><name type="personal" displayLabel="corresp"><namePart type="given">R. P.</namePart><namePart type="family">Fender</namePart><affiliation>School of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ</affiliation><affiliation>E-mail: rpf@phys.soton.ac.uk</affiliation><affiliation></affiliation><affiliation>E-mail: rpf@phys.soton.ac.uk</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">M.</namePart><namePart type="family">Dahlem</namePart><affiliation>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">J.</namePart><namePart type="family">Homan</namePart><affiliation>Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139, USA</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">S.</namePart><namePart type="family">Corbel</namePart><affiliation>AIM–Unité Mixte de Recherche CEA–CNRS, Université Paris VII, UMR 7158, CEA Saclay, Service d'Astrophysique, F-91191 Gif-sur-Yvette, France</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">R.</namePart><namePart type="family">Sault</namePart><affiliation>CSIRO/ATNF, Paul Wild Observatory, Locked Bag 194, Narrabri, NSW 2390, Australia</affiliation><role><roleTerm type="text">author</roleTerm></role></name><name type="personal"><namePart type="given">T. M.</namePart><namePart type="family">Belloni</namePart><affiliation>INAF – Osservatorio Astronomico di Brera, via Bianchi 46, 23807 Merate, Italy</affiliation><role><roleTerm type="text">author</roleTerm></role></name><typeOfResource>text</typeOfResource><genre type="research-article" displayLabel="research-article" authority="ISTEX" authorityURI="https://content-type.data.istex.fr" valueURI="https://content-type.data.istex.fr/ark:/67375/XTP-1JC4F85T-7">research-article</genre><originInfo><publisher>Blackwell Science Ltd</publisher><place><placeTerm type="text">Oxford, UK</placeTerm></place><dateIssued encoding="w3cdtf">2007-09</dateIssued><copyrightDate encoding="w3cdtf">2007</copyrightDate></originInfo><abstract>We report radio observations, made with the Australia Telescope Compact Array, of the X-ray transient XTE J1701−462. This system has been classified as a new ‘Z’ source, displaying characteristic patterns of behaviour probably associated with accretion on to a low magnetic field neutron star at close to the Eddington limit. The radio counterpart is highly variable, and was detected in six of 16 observations over the period 2006 January–April. The coupling of radio emission to X-ray state, despite limited sampling, appears to be similar to that of other ‘Z’ sources, in that there is no radio emission on the flaring branch. The mean radio and X-ray luminosities are consistent with the other Z sources for a distance of 5–15 kpc. The radio spectrum is unusually flat, or even inverted, in contrast to the related sources, Sco X-1 and Cir X-1, which usually display an optically thin radio spectrum. Deep wide-field observations indicate an extended structure 3 arcmin to the south which is aligned with the X-ray binary. This seems to represent a significant overdensity of radio sources for the field and so, although a background source remains a strong possibility, we consider it plausible that this is a large-scale jet associated with XTE J1701−462.</abstract><subject><genre>Keywords</genre><topic>binaries: close</topic><topic>stars: individual: XTE J1701−462</topic><topic>ISM: jets and outflows</topic><topic>radio continuum: stars</topic></subject><relatedItem type="host"><titleInfo><title>Monthly Notices of the Royal Astronomical Society: Letters</title></titleInfo><titleInfo type="abbreviated"><title>MNRAS</title></titleInfo><genre type="journal" authority="ISTEX" authorityURI="https://publication-type.data.istex.fr" valueURI="https://publication-type.data.istex.fr/ark:/67375/JMC-0GLKJH51-B">journal</genre><identifier type="ISSN">1745-3925</identifier><identifier type="eISSN">1745-3933</identifier><identifier type="PublisherID">mnrasl</identifier><identifier type="PublisherID-hwp">mnrasl</identifier><part><date>2007</date><detail type="volume"><caption>vol.</caption><number>380</number></detail><detail type="issue"><caption>no.</caption><number>1</number></detail><extent unit="pages"><start>L25</start><end>L29</end></extent></part></relatedItem><identifier type="istex">3B723459C00807DB77E08578A576EC5D9DCDCEE8</identifier><identifier type="DOI">10.1111/j.1745-3933.2007.00350.x</identifier><accessCondition type="use and reproduction" contentType="copyright">© 2007 The Authors. 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