AustralieFrV1, PascalFrancis, Corpus, bibRecord, 003958

GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy

Identifieur interne : 003958 ( PascalFrancis/Corpus ); précédent : 003957; suivant : 003959

GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy

Auteurs : A. J. Gosling ; R. M. Bandyopadhyay ; J. C. A. Miller-Jones ; S. A. Farrell

Source :

Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2007.

RBID : Pascal:07-0455421

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.

Notice en format standard (ISO 2709)

Pour connaître la documentation sur le format Inist Standard.

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Format Inist (serveur)

NO :	PASCAL 07-0455421 INIST
ET :	GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy
AU :	GOSLING (A. J.); BANDYOPADHYAY (R. M.); MILLER-JONES (J. C. A.); FARRELL (S. A.)
AF :	Department of Astrophysics, University of Oxford, Keble Road/Oxford OX1 3RH/Royaume-Uni (1 aut.); Department of Astronomy, University of Florida/Gainesville, FL 32611/Etats-Unis (2 aut.); Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403/1098 SJ Amsterdam/Pays-Bas (3 aut.); School ofPEMS, UNSW@ADFA, Northcott Drive/Canberra, ACT 2600/Australie (4 aut.); Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 Avenue du Colonel Roche/31028 Toulouse/France (4 aut.)
DT :	Publication en série; Niveau analytique
SO :	Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2007; Vol. 380; No. 4; Pp. 1511-1520; Bibl. 1/2 p.
LA :	Anglais
EA :	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.
CC :	001E03
FD :	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
ED :	Infrared spectroscopy; Infrared photometry; Pulsars; Circle; Spectral type; Extinction correction; Galactic bulge; Extinction law; Color; Mass function; Emission spectroscopy; Accretion; G stars; K stars; Bright star; Stellar magnitude; S stars; Main sequence stars; Mass transfer; Roche lobe; Magnetic fields; Infrared star; X-ray binary stars; Binary X ray source; Milky Way; Cosmic x-ray sources
SD :	Fotometría IR; Circulo; Tipo espectral; Corrección extinción; Bulbo galáctico; Ley extinción; Función masa; Estrella brillante; Magnitud estelar; Lóbulo Roche; Estrella IR; Fuente RX binaria
LO :	INIST-2067.354000149805370170
ID :	07-0455421

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<front><div type="abstract" xml:lang="en">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.</div>
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<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 spectral</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="ENG"><s0>Spectral type</s0>
<s5>30</s5>
</fC03>
<fC03 i1="05" i2="X" l="SPA"><s0>Tipo espectral</s0>
<s5>30</s5>
</fC03>
<fC03 i1="06" i2="X" l="FRE"><s0>Correction extinction</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="ENG"><s0>Extinction correction</s0>
<s5>31</s5>
</fC03>
<fC03 i1="06" i2="X" l="SPA"><s0>Corrección extinción</s0>
<s5>31</s5>
</fC03>
<fC03 i1="07" i2="X" l="FRE"><s0>Bulbe galactique</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="ENG"><s0>Galactic bulge</s0>
<s5>32</s5>
</fC03>
<fC03 i1="07" i2="X" l="SPA"><s0>Bulbo galáctico</s0>
<s5>32</s5>
</fC03>
<fC03 i1="08" i2="X" l="FRE"><s0>Loi extinction</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="ENG"><s0>Extinction law</s0>
<s5>33</s5>
</fC03>
<fC03 i1="08" i2="X" l="SPA"><s0>Ley extinción</s0>
<s5>33</s5>
</fC03>
<fC03 i1="09" i2="3" l="FRE"><s0>Couleur</s0>
<s5>34</s5>
</fC03>
<fC03 i1="09" i2="3" l="ENG"><s0>Color</s0>
<s5>34</s5>
</fC03>
<fC03 i1="10" i2="X" l="FRE"><s0>Fonction 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>
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<server><NO>PASCAL 07-0455421 INIST</NO>
<ET>GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy</ET>
<AU>GOSLING (A. J.); BANDYOPADHYAY (R. M.); MILLER-JONES (J. C. A.); FARRELL (S. A.)</AU>
<AF>Department of Astrophysics, University of Oxford, Keble Road/Oxford OX1 3RH/Royaume-Uni (1 aut.); Department of Astronomy, University of Florida/Gainesville, FL 32611/Etats-Unis (2 aut.); Astronomical Institute 'Anton Pannekoek', University of Amsterdam, Kruislaan 403/1098 SJ Amsterdam/Pays-Bas (3 aut.); School ofPEMS, UNSW@ADFA, Northcott Drive/Canberra, ACT 2600/Australie (4 aut.); Centre d'Etude Spatiale des Rayonnements, CNRS/UPS, 9 Avenue du Colonel Roche/31028 Toulouse/France (4 aut.)</AF>
<DT>Publication en série; Niveau analytique</DT>
<SO>Monthly Notices of the Royal Astronomical Society; ISSN 0035-8711; Coden MNRAA4; Royaume-Uni; Da. 2007; Vol. 380; No. 4; Pp. 1511-1520; Bibl. 1/2 p.</SO>
<LA>Anglais</LA>
<EA>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.</EA>
<CC>001E03</CC>
<FD>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</FD>
<ED>Infrared spectroscopy; Infrared photometry; Pulsars; Circle; Spectral type; Extinction correction; Galactic bulge; Extinction law; Color; Mass function; Emission spectroscopy; Accretion; G stars; K stars; Bright star; Stellar magnitude; S stars; Main sequence stars; Mass transfer; Roche lobe; Magnetic fields; Infrared star; X-ray binary stars; Binary X ray source; Milky Way; Cosmic x-ray sources</ED>
<SD>Fotometría IR; Circulo; Tipo espectral; Corrección extinción; Bulbo galáctico; Ley extinción; Función masa; Estrella brillante; Magnitud estelar; Lóbulo Roche; Estrella IR; Fuente RX binaria</SD>
<LO>INIST-2067.354000149805370170</LO>
<ID>07-0455421</ID>
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GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy

GRO J1744-28, search for the counterpart : infrared photometry and spectroscopy

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