EC 10246−2707: an eclipsing subdwarf B + M dwarf binary
We announce the discovery of a new eclipsing hot subdwarf B + M dwarf binary, EC 10246−2707, and present multicolour photometric and spectroscopic observations of this system. Similar to other HW Vir-type binaries, the light curve shows both primary and secondary eclipses, along with a strong reflec...
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| Veröffentlicht in: | Monthly notices of the Royal Astronomical Society 2013-03, Vol.430 (1), p.22-31 |
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| creator | Barlow, B. N. Kilkenny, D. Drechsel, H. Dunlap, B. H. O'Donoghue, D. Geier, S. O'Steen, R. G. Clemens, J. C. LaCluyze, A. P. Reichart, D. E. Haislip, J. B. Nysewander, M. C. Ivarsen, K. M. |
| description | We announce the discovery of a new eclipsing hot subdwarf B + M dwarf binary, EC 10246−2707, and present multicolour photometric and spectroscopic observations of this system. Similar to other HW Vir-type binaries, the light curve shows both primary and secondary eclipses, along with a strong reflection effect from the M dwarf; no intrinsic light contribution is detected from the cool companion. The orbital period is 0.118 507 9936 ± 0.000 000 0009 d, or about 3 h. Analysis of our time series spectroscopy reveals a velocity semi-amplitude of K
1 = 71.6 ± 1.7 km s−1 for the sdB and best-fitting atmospheric parameters of T
eff = 28 900 ± 500 K, log g = 5.64 ± 0.06 and log N(He)/N(H) = −2.5 ± 0.2. Although we cannot claim a unique solution from modelling the light curve, the best-fitting model has an sdB mass of 0.45 M and a cool companion mass of 0.12 M. These results are roughly consistent with a canonical-mass sdB and M dwarf separated by a ∼ 0.84 R. We find no evidence of pulsations in the light curve and limit the amplitude of rapid photometric oscillations to
. If EC 10246−2707 evolves into a cataclysmic variable, its period should fall below the famous cataclysmic variable period gap. |
| doi_str_mv | 10.1093/mnras/sts271 |
| format | Article |
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1 = 71.6 ± 1.7 km s−1 for the sdB and best-fitting atmospheric parameters of T
eff = 28 900 ± 500 K, log g = 5.64 ± 0.06 and log N(He)/N(H) = −2.5 ± 0.2. Although we cannot claim a unique solution from modelling the light curve, the best-fitting model has an sdB mass of 0.45 M and a cool companion mass of 0.12 M. These results are roughly consistent with a canonical-mass sdB and M dwarf separated by a ∼ 0.84 R. We find no evidence of pulsations in the light curve and limit the amplitude of rapid photometric oscillations to <0.08 per cent. Using 15 yr of eclipse timings, we construct an observed minus calculated (O − C) diagram but find no statistically significant period changes; we rule out
7.2 \times 10^{-12}$]]>
. If EC 10246−2707 evolves into a cataclysmic variable, its period should fall below the famous cataclysmic variable period gap.</description><identifier>ISSN: 0035-8711</identifier><identifier>EISSN: 1365-2966</identifier><identifier>DOI: 10.1093/mnras/sts271</identifier><language>eng</language><publisher>London: Oxford University Press</publisher><subject>Astronomy ; Diagrams ; Dwarf stars ; Eclipses ; Spectrum analysis ; Star & galaxy formation ; Time series</subject><ispartof>Monthly notices of the Royal Astronomical Society, 2013-03, Vol.430 (1), p.22-31</ispartof><rights>2013 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2013</rights><rights>Copyright Oxford University Press, UK Mar 21, 2013</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c333t-cee0331d70702fe9b1d6271637e1e277d3f638c2eafc68f23caaa5e4be83157e3</citedby><cites>FETCH-LOGICAL-c333t-cee0331d70702fe9b1d6271637e1e277d3f638c2eafc68f23caaa5e4be83157e3</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,777,781,1599,27905,27906</link.rule.ids><linktorsrc>$$Uhttps://dx.doi.org/10.1093/mnras/sts271$$EView_record_in_Oxford_University_Press$$FView_record_in_$$GOxford_University_Press</linktorsrc></links><search><creatorcontrib>Barlow, B. N.</creatorcontrib><creatorcontrib>Kilkenny, D.</creatorcontrib><creatorcontrib>Drechsel, H.</creatorcontrib><creatorcontrib>Dunlap, B. H.</creatorcontrib><creatorcontrib>O'Donoghue, D.</creatorcontrib><creatorcontrib>Geier, S.</creatorcontrib><creatorcontrib>O'Steen, R. G.</creatorcontrib><creatorcontrib>Clemens, J. C.</creatorcontrib><creatorcontrib>LaCluyze, A. P.</creatorcontrib><creatorcontrib>Reichart, D. E.</creatorcontrib><creatorcontrib>Haislip, J. B.</creatorcontrib><creatorcontrib>Nysewander, M. C.</creatorcontrib><creatorcontrib>Ivarsen, K. M.</creatorcontrib><title>EC 10246−2707: an eclipsing subdwarf B + M dwarf binary</title><title>Monthly notices of the Royal Astronomical Society</title><addtitle>Mon. Not. R. Astron. Soc</addtitle><description>We announce the discovery of a new eclipsing hot subdwarf B + M dwarf binary, EC 10246−2707, and present multicolour photometric and spectroscopic observations of this system. Similar to other HW Vir-type binaries, the light curve shows both primary and secondary eclipses, along with a strong reflection effect from the M dwarf; no intrinsic light contribution is detected from the cool companion. The orbital period is 0.118 507 9936 ± 0.000 000 0009 d, or about 3 h. Analysis of our time series spectroscopy reveals a velocity semi-amplitude of K
1 = 71.6 ± 1.7 km s−1 for the sdB and best-fitting atmospheric parameters of T
eff = 28 900 ± 500 K, log g = 5.64 ± 0.06 and log N(He)/N(H) = −2.5 ± 0.2. Although we cannot claim a unique solution from modelling the light curve, the best-fitting model has an sdB mass of 0.45 M and a cool companion mass of 0.12 M. These results are roughly consistent with a canonical-mass sdB and M dwarf separated by a ∼ 0.84 R. We find no evidence of pulsations in the light curve and limit the amplitude of rapid photometric oscillations to <0.08 per cent. Using 15 yr of eclipse timings, we construct an observed minus calculated (O − C) diagram but find no statistically significant period changes; we rule out
7.2 \times 10^{-12}$]]>
. If EC 10246−2707 evolves into a cataclysmic variable, its period should fall below the famous cataclysmic variable period gap.</description><subject>Astronomy</subject><subject>Diagrams</subject><subject>Dwarf stars</subject><subject>Eclipses</subject><subject>Spectrum analysis</subject><subject>Star & galaxy formation</subject><subject>Time series</subject><issn>0035-8711</issn><issn>1365-2966</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2013</creationdate><recordtype>article</recordtype><recordid>eNp9kL1OwzAUhS0EEqWw8QCWGBgg1Nc3sRM2qMqPVMQCs-U41yhVmwS7EeINmHlEnoRAmJnuHT6dc_QxdgziAkSBs00TbJzFbZQadtgEUGWJLJTaZRMhMEtyDbDPDmJcCSFSlGrCisWcg5Cp-vr4lFroS24bTm5dd7FuXnjsy-rNBs-v-Rl_4ONf1o0N74dsz9t1pKO_O2XPN4un-V2yfLy9n18tE4eI28QRCUSohmwhPRUlVGqYp1ATkNS6Qq8wd5Ksdyr3Ep21NqO0pBwh04RTdjLmdqF97SluzartQzNUGsAMlcpApQN1PlIutDEG8qYL9WaYaUCYHznmV44Z5Qz46Yi3ffc_-Q1tvWQ1</recordid><startdate>20130321</startdate><enddate>20130321</enddate><creator>Barlow, B. N.</creator><creator>Kilkenny, D.</creator><creator>Drechsel, H.</creator><creator>Dunlap, B. H.</creator><creator>O'Donoghue, D.</creator><creator>Geier, S.</creator><creator>O'Steen, R. G.</creator><creator>Clemens, J. C.</creator><creator>LaCluyze, A. P.</creator><creator>Reichart, D. E.</creator><creator>Haislip, J. B.</creator><creator>Nysewander, M. C.</creator><creator>Ivarsen, K. M.</creator><general>Oxford University Press</general><scope>AAYXX</scope><scope>CITATION</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope></search><sort><creationdate>20130321</creationdate><title>EC 10246−2707: an eclipsing subdwarf B + M dwarf binary</title><author>Barlow, B. N. ; Kilkenny, D. ; Drechsel, H. ; Dunlap, B. H. ; O'Donoghue, D. ; Geier, S. ; O'Steen, R. G. ; Clemens, J. C. ; LaCluyze, A. P. ; Reichart, D. E. ; Haislip, J. B. ; Nysewander, M. C. ; Ivarsen, K. M.</author></sort><facets><frbrtype>5</frbrtype><frbrgroupid>cdi_FETCH-LOGICAL-c333t-cee0331d70702fe9b1d6271637e1e277d3f638c2eafc68f23caaa5e4be83157e3</frbrgroupid><rsrctype>articles</rsrctype><prefilter>articles</prefilter><language>eng</language><creationdate>2013</creationdate><topic>Astronomy</topic><topic>Diagrams</topic><topic>Dwarf stars</topic><topic>Eclipses</topic><topic>Spectrum analysis</topic><topic>Star & galaxy formation</topic><topic>Time series</topic><toplevel>peer_reviewed</toplevel><toplevel>online_resources</toplevel><creatorcontrib>Barlow, B. N.</creatorcontrib><creatorcontrib>Kilkenny, D.</creatorcontrib><creatorcontrib>Drechsel, H.</creatorcontrib><creatorcontrib>Dunlap, B. H.</creatorcontrib><creatorcontrib>O'Donoghue, D.</creatorcontrib><creatorcontrib>Geier, S.</creatorcontrib><creatorcontrib>O'Steen, R. G.</creatorcontrib><creatorcontrib>Clemens, J. C.</creatorcontrib><creatorcontrib>LaCluyze, A. P.</creatorcontrib><creatorcontrib>Reichart, D. E.</creatorcontrib><creatorcontrib>Haislip, J. B.</creatorcontrib><creatorcontrib>Nysewander, M. C.</creatorcontrib><creatorcontrib>Ivarsen, K. M.</creatorcontrib><collection>CrossRef</collection><collection>Technology Research Database</collection><collection>Aerospace Database</collection><collection>Advanced Technologies Database with Aerospace</collection><jtitle>Monthly notices of the Royal Astronomical Society</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext_linktorsrc</fulltext></delivery><addata><au>Barlow, B. N.</au><au>Kilkenny, D.</au><au>Drechsel, H.</au><au>Dunlap, B. H.</au><au>O'Donoghue, D.</au><au>Geier, S.</au><au>O'Steen, R. G.</au><au>Clemens, J. C.</au><au>LaCluyze, A. P.</au><au>Reichart, D. E.</au><au>Haislip, J. B.</au><au>Nysewander, M. C.</au><au>Ivarsen, K. M.</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>EC 10246−2707: an eclipsing subdwarf B + M dwarf binary</atitle><jtitle>Monthly notices of the Royal Astronomical Society</jtitle><stitle>Mon. Not. R. Astron. Soc</stitle><date>2013-03-21</date><risdate>2013</risdate><volume>430</volume><issue>1</issue><spage>22</spage><epage>31</epage><pages>22-31</pages><issn>0035-8711</issn><eissn>1365-2966</eissn><abstract>We announce the discovery of a new eclipsing hot subdwarf B + M dwarf binary, EC 10246−2707, and present multicolour photometric and spectroscopic observations of this system. Similar to other HW Vir-type binaries, the light curve shows both primary and secondary eclipses, along with a strong reflection effect from the M dwarf; no intrinsic light contribution is detected from the cool companion. The orbital period is 0.118 507 9936 ± 0.000 000 0009 d, or about 3 h. Analysis of our time series spectroscopy reveals a velocity semi-amplitude of K
1 = 71.6 ± 1.7 km s−1 for the sdB and best-fitting atmospheric parameters of T
eff = 28 900 ± 500 K, log g = 5.64 ± 0.06 and log N(He)/N(H) = −2.5 ± 0.2. Although we cannot claim a unique solution from modelling the light curve, the best-fitting model has an sdB mass of 0.45 M and a cool companion mass of 0.12 M. These results are roughly consistent with a canonical-mass sdB and M dwarf separated by a ∼ 0.84 R. We find no evidence of pulsations in the light curve and limit the amplitude of rapid photometric oscillations to <0.08 per cent. Using 15 yr of eclipse timings, we construct an observed minus calculated (O − C) diagram but find no statistically significant period changes; we rule out
7.2 \times 10^{-12}$]]>
. If EC 10246−2707 evolves into a cataclysmic variable, its period should fall below the famous cataclysmic variable period gap.</abstract><cop>London</cop><pub>Oxford University Press</pub><doi>10.1093/mnras/sts271</doi><tpages>10</tpages><oa>free_for_read</oa></addata></record> |
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| title | EC 10246−2707: an eclipsing subdwarf B + M dwarf binary |
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