GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy
Identifieur interne : 003878 ( PascalFrancis/Checkpoint ); précédent : 003877; suivant : 003879GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy
Auteurs : A. J. Gosling [Royaume-Uni] ; R. M. Bandyopadhyay [États-Unis] ; J. C. A. Miller-Jones [Pays-Bas] ; S. A. Farrell [Australie, France]Source :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007.
Descripteurs français
- Pascal (Inist)
- Spectrométrie IR, Photométrie IR, Pulsar, Cercle, Type spectral, Correction extinction, Bulbe galactique, Loi extinction, Couleur, Fonction masse, Spectrométrie émission, Accrétion, Etoile G, Etoile K, Etoile brillante, Magnitude stellaire, Etoile S, Etoile séquence principale, Transfert masse, Lobe Roche, Champ magnétique, Etoile IR, Binaire RX, Source RX binaire, Voie lactée, Source RX cosmique.
English descriptors
- KwdEn :
- Accretion, Binary X ray source, Bright star, Circle, Color, Cosmic x-ray sources, Emission spectroscopy, Extinction correction, Extinction law, G stars, Galactic bulge, Infrared photometry, Infrared spectroscopy, Infrared star, K stars, Magnetic fields, Main sequence stars, Mass function, Mass transfer, Milky Way, Pulsars, Roche lobe, S stars, Spectral type, Stellar magnitude, X-ray binary stars.
Abstract
Using VLT/ISAAC, we have detected two candidate counterparts to the bursting pulsar GRO J1744-28, one bright and one faint, both within the X-ray error circles found using XMM-Newton and Chandra. In determining the spectral types of the counterparts we applied three different extinction corrections; one for an all-sky value, one for a Galactic bulge value and one for a local value. We find that the local value, with an extinction law of a = 3.23 ± 0.01 is the only correction that results in colours and magnitudes for both the bright and faint counterparts that are consistent with a small range of spectral types, and in the case of the bright counterpart are also consistent with the spectroscopic identification. Photometry of the fainter candidate then indicates that it is a K7/M0 V star at a distance of 3.75 ± 1 kpc. Such a star would require a very low inclination angle (i < 9°) to satisfy the mass function constraints; however, this source cannot be excluded as the counterpart without follow-up spectroscopy to detect emission signatures of accretion. Photometry and spectroscopy of the bright candidate indicate that it is most likely a G/K III star. The spectrum does not show Brackett-y emission, a known indicator of accretion. The bright star's magnitudes are in agreement with the constraints placed on the probable counterpart by the calculations of Rappaport & Joss for an evolved star that has had its envelope stripped. The mass function indicates that the most likely counterpart has M < 0.3 M◦. for an inclination of i ≥ 15°; a stripped giant, or a main-sequence M3+V star would be consistent with this mass function constraint. In both cases mass transfer, if present, will be by wind accretion as the counterpart will not fill its Roche lobe given the observed orbital period. In this case, the derived magnetic field strength of 2.4 x 1011 G is sufficient to inhibit accretion of captured material by the propeller effect, hence the quiescent state of the system.
Affiliations:
- Australie, France, Pays-Bas, Royaume-Uni, États-Unis
- Angleterre, Hollande-Septentrionale, Midi-Pyrénées, Occitanie (région administrative), Oxfordshire
- Amsterdam, Oxford, Toulouse
- Université d'Amsterdam, Université d'Oxford
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J." last="Gosling">A. J. Gosling</name><affiliation wicri:level="4"><inist:fA14 i1="01"><s1>Department of Astrophysics, University of Oxford, Keble Road</s1><s2>Oxford OX1 3RH</s2><s3>GBR</s3><sZ>1 aut.</sZ></inist:fA14><country>Royaume-Uni</country><wicri:noRegion>Oxford OX1 3RH</wicri:noRegion><orgName type="university">Université d'Oxford</orgName><placeName><settlement type="city">Oxford</settlement><region type="nation">Angleterre</region><region type="région" nuts="1">Oxfordshire</region></placeName></affiliation></author><author><name sortKey="Bandyopadhyay, R M" sort="Bandyopadhyay, R M" uniqKey="Bandyopadhyay R" first="R. M." last="Bandyopadhyay">R. M. Bandyopadhyay</name><affiliation wicri:level="1"><inist:fA14 i1="02"><s1>Department of Astronomy, University of Florida</s1><s2>Gainesville, FL 32611</s2><s3>USA</s3><sZ>2 aut.</sZ></inist:fA14><country>États-Unis</country><wicri:noRegion>Gainesville, FL 32611</wicri:noRegion></affiliation></author><author><name sortKey="Miller Jones, J C A" sort="Miller Jones, J C A" uniqKey="Miller Jones J" first="J. C. A." last="Miller-Jones">J. C. A. Miller-Jones</name><affiliation wicri:level="4"><inist:fA14 i1="03"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403</s1><s2>1098 SJ Amsterdam</s2><s3>NLD</s3><sZ>3 aut.</sZ></inist:fA14><country>Pays-Bas</country><wicri:noRegion>1098 SJ Amsterdam</wicri:noRegion><orgName type="university">Université d'Amsterdam</orgName><placeName><settlement type="city">Amsterdam</settlement><region>Hollande-Septentrionale</region></placeName></affiliation></author><author><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. 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In determining the spectral types of the counterparts we applied three different extinction corrections; one for an all-sky value, one for a Galactic bulge value and one for a local value. We find that the local value, with an extinction law of a = 3.23 ± 0.01 is the only correction that results in colours and magnitudes for both the bright and faint counterparts that are consistent with a small range of spectral types, and in the case of the bright counterpart are also consistent with the spectroscopic identification. Photometry of the fainter candidate then indicates that it is a K7/M0 V star at a distance of 3.75 ± 1 kpc. Such a star would require a very low inclination angle (i < 9°) to satisfy the mass function constraints; however, this source cannot be excluded as the counterpart without follow-up spectroscopy to detect emission signatures of accretion. Photometry and spectroscopy of the bright candidate indicate that it is most likely a G/K III star. The spectrum does not show Brackett-y emission, a known indicator of accretion. The bright star's magnitudes are in agreement with the constraints placed on the probable counterpart by the calculations of Rappaport & Joss for an evolved star that has had its envelope stripped. The mass function indicates that the most likely counterpart has M < 0.3 M<sub>◦.</sub> for an inclination of i ≥ 15°; a stripped giant, or a main-sequence M3+V star would be consistent with this mass function constraint. In both cases mass transfer, if present, will be by wind accretion as the counterpart will not fill its Roche lobe given the observed orbital period. In this case, the derived magnetic field strength of 2.4 x 10<sup>11</sup> G is sufficient to inhibit accretion of captured material by the propeller effect, hence the quiescent state of the system.</div></front></TEI><inist><standard h6="B"><pA><fA01 i1="01" i2="1"><s0>0035-8711</s0></fA01><fA02 i1="01"><s0>MNRAA4</s0></fA02><fA03 i2="1"><s0>Mon. Not. R. Astron. Soc.</s0></fA03><fA05><s2>380</s2></fA05><fA06><s2>4</s2></fA06><fA08 i1="01" i2="1" l="ENG"><s1>GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy</s1></fA08><fA11 i1="01" i2="1"><s1>GOSLING (A. J.)</s1></fA11><fA11 i1="02" i2="1"><s1>BANDYOPADHYAY (R. M.)</s1></fA11><fA11 i1="03" i2="1"><s1>MILLER-JONES (J. C. A.)</s1></fA11><fA11 i1="04" i2="1"><s1>FARRELL (S. A.)</s1></fA11><fA14 i1="01"><s1>Department of Astrophysics, University of Oxford, Keble Road</s1><s2>Oxford OX1 3RH</s2><s3>GBR</s3><sZ>1 aut.</sZ></fA14><fA14 i1="02"><s1>Department of Astronomy, University of Florida</s1><s2>Gainesville, FL 32611</s2><s3>USA</s3><sZ>2 aut.</sZ></fA14><fA14 i1="03"><s1>Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403</s1><s2>1098 SJ Amsterdam</s2><s3>NLD</s3><sZ>3 aut.</sZ></fA14><fA14 i1="04"><s1>School ofPEMS, UNSW@ADFA, Northcott Drive</s1><s2>Canberra, ACT 2600</s2><s3>AUS</s3><sZ>4 aut.</sZ></fA14><fA14 i1="05"><s1>Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 Avenue du Colonel Roche</s1><s2>31028 Toulouse</s2><s3>FRA</s3><sZ>4 aut.</sZ></fA14><fA20><s1>1511-1520</s1></fA20><fA21><s1>2007</s1></fA21><fA23 i1="01"><s0>ENG</s0></fA23><fA43 i1="01"><s1>INIST</s1><s2>2067</s2><s5>354000149805370170</s5></fA43><fA44><s0>0000</s0><s1>© 2007 INIST-CNRS. All rights reserved.</s1></fA44><fA45><s0>1/2 p.</s0></fA45><fA47 i1="01" i2="1"><s0>07-0455421</s0></fA47><fA60><s1>P</s1></fA60><fA61><s0>A</s0></fA61><fA64 i1="01" i2="1"><s0>Monthly Notices of the Royal Astronomical Society</s0></fA64><fA66 i1="01"><s0>GBR</s0></fA66><fC01 i1="01" l="ENG"><s0>Using VLT/ISAAC, we have detected two candidate counterparts to the bursting pulsar GRO J1744-28, one bright and one faint, both within the X-ray error circles found using XMM-Newton and Chandra. In determining the spectral types of the counterparts we applied three different extinction corrections; one for an all-sky value, one for a Galactic bulge value and one for a local value. We find that the local value, with an extinction law of a = 3.23 ± 0.01 is the only correction that results in colours and magnitudes for both the bright and faint counterparts that are consistent with a small range of spectral types, and in the case of the bright counterpart are also consistent with the spectroscopic identification. Photometry of the fainter candidate then indicates that it is a K7/M0 V star at a distance of 3.75 ± 1 kpc. Such a star would require a very low inclination angle (i < 9°) to satisfy the mass function constraints; however, this source cannot be excluded as the counterpart without follow-up spectroscopy to detect emission signatures of accretion. Photometry and spectroscopy of the bright candidate indicate that it is most likely a G/K III star. The spectrum does not show Brackett-y emission, a known indicator of accretion. The bright star's magnitudes are in agreement with the constraints placed on the probable counterpart by the calculations of Rappaport & Joss for an evolved star that has had its envelope stripped. The mass function indicates that the most likely counterpart has M < 0.3 M<sub>◦.</sub> for an inclination of i ≥ 15°; a stripped giant, or a main-sequence M3+V star would be consistent with this mass function constraint. In both cases mass transfer, if present, will be by wind accretion as the counterpart will not fill its Roche lobe given the observed orbital period. In this case, the derived magnetic field strength of 2.4 x 10<sup>11</sup> G is sufficient to inhibit accretion of captured material by the propeller effect, hence the quiescent state of the system.</s0></fC01><fC02 i1="01" i2="3"><s0>001E03</s0></fC02><fC03 i1="01" i2="3" l="FRE"><s0>Spectrométrie IR</s0><s5>26</s5></fC03><fC03 i1="01" i2="3" l="ENG"><s0>Infrared spectroscopy</s0><s5>26</s5></fC03><fC03 i1="02" i2="X" l="FRE"><s0>Photométrie IR</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="ENG"><s0>Infrared photometry</s0><s5>27</s5></fC03><fC03 i1="02" i2="X" l="SPA"><s0>Fotometría IR</s0><s5>27</s5></fC03><fC03 i1="03" i2="3" l="FRE"><s0>Pulsar</s0><s5>28</s5></fC03><fC03 i1="03" i2="3" l="ENG"><s0>Pulsars</s0><s5>28</s5></fC03><fC03 i1="04" i2="X" l="FRE"><s0>Cercle</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="ENG"><s0>Circle</s0><s5>29</s5></fC03><fC03 i1="04" i2="X" l="SPA"><s0>Circulo</s0><s5>29</s5></fC03><fC03 i1="05" i2="X" l="FRE"><s0>Type 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masse</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="ENG"><s0>Mass function</s0><s5>35</s5></fC03><fC03 i1="10" i2="X" l="SPA"><s0>Función masa</s0><s5>35</s5></fC03><fC03 i1="11" i2="3" l="FRE"><s0>Spectrométrie émission</s0><s5>36</s5></fC03><fC03 i1="11" i2="3" l="ENG"><s0>Emission spectroscopy</s0><s5>36</s5></fC03><fC03 i1="12" i2="3" l="FRE"><s0>Accrétion</s0><s5>37</s5></fC03><fC03 i1="12" i2="3" l="ENG"><s0>Accretion</s0><s5>37</s5></fC03><fC03 i1="13" i2="3" l="FRE"><s0>Etoile G</s0><s5>38</s5></fC03><fC03 i1="13" i2="3" l="ENG"><s0>G stars</s0><s5>38</s5></fC03><fC03 i1="14" i2="3" l="FRE"><s0>Etoile K</s0><s5>39</s5></fC03><fC03 i1="14" i2="3" l="ENG"><s0>K stars</s0><s5>39</s5></fC03><fC03 i1="15" i2="X" l="FRE"><s0>Etoile brillante</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="ENG"><s0>Bright star</s0><s5>40</s5></fC03><fC03 i1="15" i2="X" l="SPA"><s0>Estrella brillante</s0><s5>40</s5></fC03><fC03 i1="16" i2="X" l="FRE"><s0>Magnitude stellaire</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="ENG"><s0>Stellar magnitude</s0><s5>41</s5></fC03><fC03 i1="16" i2="X" l="SPA"><s0>Magnitud estelar</s0><s5>41</s5></fC03><fC03 i1="17" i2="3" l="FRE"><s0>Etoile S</s0><s5>42</s5></fC03><fC03 i1="17" i2="3" l="ENG"><s0>S stars</s0><s5>42</s5></fC03><fC03 i1="18" i2="3" l="FRE"><s0>Etoile séquence principale</s0><s5>43</s5></fC03><fC03 i1="18" i2="3" l="ENG"><s0>Main sequence stars</s0><s5>43</s5></fC03><fC03 i1="19" i2="3" l="FRE"><s0>Transfert masse</s0><s5>44</s5></fC03><fC03 i1="19" i2="3" l="ENG"><s0>Mass transfer</s0><s5>44</s5></fC03><fC03 i1="20" i2="X" l="FRE"><s0>Lobe Roche</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="ENG"><s0>Roche lobe</s0><s5>45</s5></fC03><fC03 i1="20" i2="X" l="SPA"><s0>Lóbulo Roche</s0><s5>45</s5></fC03><fC03 i1="21" i2="3" l="FRE"><s0>Champ magnétique</s0><s5>46</s5></fC03><fC03 i1="21" i2="3" l="ENG"><s0>Magnetic fields</s0><s5>46</s5></fC03><fC03 i1="22" i2="X" l="FRE"><s0>Etoile IR</s0><s5>47</s5></fC03><fC03 i1="22" i2="X" l="ENG"><s0>Infrared star</s0><s5>47</s5></fC03><fC03 i1="22" i2="X" l="SPA"><s0>Estrella IR</s0><s5>47</s5></fC03><fC03 i1="23" i2="3" l="FRE"><s0>Binaire RX</s0><s5>48</s5></fC03><fC03 i1="23" i2="3" l="ENG"><s0>X-ray binary stars</s0><s5>48</s5></fC03><fC03 i1="24" i2="X" l="FRE"><s0>Source RX binaire</s0><s5>49</s5></fC03><fC03 i1="24" i2="X" l="ENG"><s0>Binary X ray source</s0><s5>49</s5></fC03><fC03 i1="24" i2="X" l="SPA"><s0>Fuente RX binaria</s0><s5>49</s5></fC03><fC03 i1="25" i2="3" l="FRE"><s0>Voie lactée</s0><s5>50</s5></fC03><fC03 i1="25" i2="3" l="ENG"><s0>Milky Way</s0><s5>50</s5></fC03><fC03 i1="26" i2="3" l="FRE"><s0>Source RX cosmique</s0><s5>90</s5></fC03><fC03 i1="26" i2="3" l="ENG"><s0>Cosmic x-ray sources</s0><s5>90</s5></fC03><fN21><s1>295</s1></fN21><fN44 i1="01"><s1>OTO</s1></fN44><fN82><s1>OTO</s1></fN82></pA></standard></inist><affiliations><list><country><li>Australie</li><li>France</li><li>Pays-Bas</li><li>Royaume-Uni</li><li>États-Unis</li></country><region><li>Angleterre</li><li>Hollande-Septentrionale</li><li>Midi-Pyrénées</li><li>Occitanie (région administrative)</li><li>Oxfordshire</li></region><settlement><li>Amsterdam</li><li>Oxford</li><li>Toulouse</li></settlement><orgName><li>Université d'Amsterdam</li><li>Université d'Oxford</li></orgName></list><tree><country name="Royaume-Uni"><region name="Angleterre"><name sortKey="Gosling, A J" sort="Gosling, A J" uniqKey="Gosling A" first="A. J." last="Gosling">A. J. Gosling</name></region></country><country name="États-Unis"><noRegion><name sortKey="Bandyopadhyay, R M" sort="Bandyopadhyay, R M" uniqKey="Bandyopadhyay R" first="R. M." last="Bandyopadhyay">R. M. Bandyopadhyay</name></noRegion></country><country name="Pays-Bas"><region name="Hollande-Septentrionale"><name sortKey="Miller Jones, J C A" sort="Miller Jones, J C A" uniqKey="Miller Jones J" first="J. C. A." last="Miller-Jones">J. C. A. Miller-Jones</name></region></country><country name="Australie"><noRegion><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. Farrell</name></noRegion></country><country name="France"><region name="Occitanie (région administrative)"><name sortKey="Farrell, S A" sort="Farrell, S A" uniqKey="Farrell S" first="S. A." last="Farrell">S. A. Farrell</name></region></country></tree></affiliations></record>Pour manipuler ce document sous Unix (Dilib)
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