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J/A+A/359/227       Lindroos binary systems X-ray emission   (Huelamo+, 2000)

X-ray emission from Lindroos binary systems. Huelamo N., Neuhaeuser R., Stelzer B., Supper R., Zinnecker H. <Astron. Astrophys. 359, 227 (2000)> =2000A&A...359..227H
ADC_Keywords: Binaries, X-ray ; Magnitudes Keywords: stars: binaries: visual - stars: early-type - stars: pre-main sequence - stars: individual: HR 4796 - X-rays: stars Abstract: We present a study of the X-ray emission from binary systems extracted from the Lindroos catalogue (Lindroos, 1986A&A...156..223L) based on the ROSAT All-Sky survey as well as ROSAT PSPC and HRI pointings. The studied sample consists of visual binary systems comprised of early-type primaries and late-type secondaries. The ages of the systems were determined by Lindroos (1985, Cat. II/127) from uvbyβ photometry of the primaries. These ages range between 33 and 135Myr, so if the late-type secondaries are physically bound to the early-type primaries, they could be Post-T Tauri stars (PTTS). We have found strong X-ray emission from several secondaries. This fact together with their optical and IR data, make them bona fide PTTS candidates. We have also detected X-ray emission from several early-type primaries and, in particular, from most of the late-B type stars. Because their HRI hardness ratios are similar to those from resolved late-type stars, the presence of an unresolved late-type companion seems to be the cause of this emission. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 90 50 Stellar Data of the binary sample table2.dat 99 37 RASS observations: Detections and upper limits table3.dat 112 5 PSPC pointed observations table4.dat 112 46 HRI observations table5.dat 43 51 X-ray luminosities table6.dat 37 10 HRI soft-band rate and UV-rate for detected early-type stars table7.dat 67 20 Stellar properties of the post-TTau (PTTS) candidates
See also: B/cb : Cataclysmic Binaries, LMXBs, and related objects (Ritter+, 2008) II/127 : Visual Double Stars with Early-Type Primaries. IV (Lindroos 1985) IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999) IX/28 : ROSAT HRI Pointed Observations (1RXH) (ROSAT Team, 2000) IX/30 : Second ROSAT PSPC Catalog (ROSAT, 2000) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 8- 10 A3 --- m_HD (A+BCX ) Multiplicity index on HD 12- 23 A12 --- SpType MK spectral type (1) 25- 26 I2 h RAh Optical right ascension (J2000) (2) 28- 29 I2 min RAm Optical right ascension (J2000) (2) 31- 35 F5.2 s RAs Optical right ascension (J2000) (2) 37 A1 --- DE- Optical declination sign (J2000) (2) 38- 39 I2 deg DEd Optical declination (J2000) (2) 41- 42 I2 arcmin DEm Optical declination (J2000) (2) 44- 48 F5.2 arcsec DEs Optical declination (J2000) (2) 50- 54 F5.1 arcsec Sep Separation angle (1) 56- 61 F6.1 pc Dist Distance (3) 62 A1 --- u_Dist Uncertainty flag on Dist 63 A1 --- r_Dist [+] +: data from Lindroos, 1986A&A...156..223L 64- 68 F5.1 pc e_Dist ? rms uncertainty on Dist 69 A1 --- ueDist Uncertainty flag on e_Dist 71- 74 F4.2 mag VmagA V magnitude of the primary 75 A1 --- n_VmagA [*] Note on VmagA (4) 77- 81 F5.2 mag VmagB ? V magnitude of the secondary 82 A1 --- n_VmagB [*7] Note on VmagB (4), (7) 84- 87 F4.2 mag AV ? Absorption in V band 89- 90 A2 --- Class Classification (6)
Note (1): Taken from Pallavicini et al. (1992A&A...261..245P) Note (2): Coordinates of the primary star Note (3): Deduced from Hipparcos parallax of the primary star, except those marked with + taken from Lindroos, 1986A&A...156..223L Note (4): Adopted from Pallavicini et al. (1992A&A...261..245P) except those marked with an asterisk obtained from the SIMBAD database Note (6): Classification taken by Pallavicini et al. (1992A&A...261..245P) with respect to the presence of the Lithium absorption line and CaII (H and K) chromospheric lines in the spectrum of the secondary: CP (certainly physical); PP (probably physical); LO (likely optical) Note (7): Unknown visual magnitude for the secondary star.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 8- 9 I2 h RAh ? X-ray right ascension (J2000) 11- 12 I2 min RAm ? X-ray right ascension (J2000) 14- 18 F5.2 s RAs ? X-ray right ascension (J2000) 20 A1 --- DE- X-ray declination sign (J2000) 21- 22 I2 deg DEd ? X-ray declination sign (J2000) 24- 25 I2 arcmin DEm ? X-ray declination sign (J2000) 27- 31 F5.2 arcsec DEs ? X-ray declination sign (J2000) 32- 36 F5.1 arcsec DeltaA ? Displacement between the detected X-ray source and the optical position of the primary component (1) 37 A1 --- --- [/] 38- 42 F5.2 arcsec DeltaB ? Displacement between the detected X-ray source and the optical position of the secondary component (1) 43 A1 --- l_Count Limit flag on Count 44- 49 F6.2 ct Count Count of the primary component or of the both is upper limit (2) 50 A1 --- --- [/] 51- 54 F4.1 ct e_Count ? rms uncertainty on Counts 57- 60 F4.2 ct Bcnt ? Counts of the secondary component 63- 68 F6.1 s ExpTime Exposition time 70 A1 --- l_HR1 Limit flag on HR1 71- 75 F5.2 --- HR1 ? Hardness ratio 1 (G1) 77- 80 F4.2 --- e_HR1 ? rms uncertainty on HR1 82 A1 --- l_HR2 Limit flag on HR2 83- 87 F5.2 --- HR2 ? Hardness ratio 2 (G1) 89- 92 F4.2 --- e_HR2 ? rms uncertainty on HR2 94- 99 F6.1 --- ML ? Maximum likelihood
Note (1): Given the low spatial resolution of the PSPC, we cannot resolve the two components of the binary system. As a consequence, the displacement δ between the detected X-ray source and the optical positions of the two components of the system are given. Note (2): In the case of non-detection, upper limits are computed at the positions of both components, A and B, respectively.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 8 I1 --- n_HD [1/2]? Individual note (1) 10- 15 I6 --- ROR ROSAT Observation request number 16 A1 --- m_ROR Multiplicity index on ROR 18- 19 I2 h RAh ? X-ray right ascension (J2000) 21- 22 I2 min RAm ? X-ray right ascension (J2000) 24- 28 F5.2 s RAs ? X-ray right ascension (J2000) 30 A1 --- DE- X-ray declination sign (J2000) 31- 32 I2 deg DEd ? X-ray declination sign (J2000) 34- 35 I2 arcmin DEm ? X-ray declination sign (J2000) 37- 41 F5.2 arcsec DEs ? X-ray declination sign (J2000) 42- 45 F4.1 arcsec DeltaA ? Displacement between the detected X-ray source and the optical position of the primary component 46 A1 --- --- [/] 47- 50 F4.1 arcsec DeltaB ? Displacement between the detected X-ray source and the optical position of the secondary component 52- 56 F5.2 arcmin Offaxis ? Offaxis 58 A1 --- l_Count Limit flag on Count 59- 64 F6.1 ct Count Count of the primary component or of the both is upper limit (2) 65 A1 --- --- [/] 66- 69 F4.1 ct e_Count ? rms uncertainty on Counts 71- 75 F5.2 ct Bcnt ? Counts of the secondary component 77- 83 F7.1 s ExpTime Exposition time 85- 89 F5.2 --- HR1 ? Hardness ratio 1 (G1) 91- 94 F4.2 --- e_HR1 ? rms uncertainty on HR1 96- 99 F4.2 --- HR2 ? Hardness ratio 2 (G1) 101-104 F4.2 --- e_HR2 ? rms uncertainty on HR2 106-112 F7.1 --- ML ? Maximum likelihood
Note (1): Individual notes as follows: 1 = The source is very close to the support structure of the telescope, so we are not sure about the reliability of the upper limit 2 = This source has two PSPC observations: 201271p and 201271 p-1. There are no detections in the individual observations, so we have added up both files to improve the S/N ratio. Note (2): In the case of non-detection, upper limits are computed at the positions of both components, A and B, respectively.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD ? HD (Cat. III/135) number) 8- 10 A3 --- n_HD Note on HD (1) 13- 18 I6 --- ROR ROSAT Observation request number 19- 23 A5 --- m_ROR Multiplicity index on ROR 25- 26 A2 --- n_Comp Note on elongation (2) 27- 32 A6 --- Comp Composant designation 34- 35 I2 h RAh ? X-ray right ascension (J2000) 37- 38 I2 min RAm ? X-ray right ascension (J2000) 40- 44 F5.2 s RAs ? X-ray right ascension (J2000) 46 A1 --- DE- X-ray declination sign (J2000) 47- 48 I2 deg DEd ? X-ray declination (J2000) 50- 51 I2 arcmin DEm ? X-ray declination (J2000) 53- 56 F4.1 arcsec DEs ? X-ray declination (J2000) 58- 61 F4.1 arcsec DeltaA ? Displacement between the detected X-ray source and the optical position of the binary system or of the primary component if DeltaB exist (3) 62 A1 --- --- [/] 63- 65 F3.1 arcsec DeltaB ? Displacement between the detected X-ray source and the optical position of the secondary component (3) 67- 71 F5.2 arcmin OffAxis ? Displacement of the sources with respect to the axis of the telescope 73 A1 --- l_Count Limit flag on Count 74- 80 F7.2 ct Count Total counts in the broad band 82- 85 F4.1 ct e_Count ? rms uncertainty on Counts 87- 93 F7.1 s ExpTime Exposition time (4) 95 A1 --- l_HR Limit flag in HR 96-100 F5.2 --- HR ? Hardness ratio 102-105 F4.2 --- e_HR ? rms uncertainty on HR 107-112 F6.1 --- ML ? Maximum of likelihood coefficient
Note (1): Notes as follows: 1 = If both components are detected, coordinates of both X-ray sources are given. The displacement of the secondary with respect to the detected X-ray source is computed comparing with its optical coordinates. 2 = The two stars of the system are not completely resolved so each star is contributing to the count rate of the companion. 3 = The undetected component is so close to the X-ray source that no reliable upper limit can be computed. 4 = HD74146 has another observation, 200186h, but with very low exposure time (texp=357.5s). s = stars previously studied by Schmitt et al. (1993ApJ...402L..13S). Note (2): Elongation information as follows: e = for elongated sources; * = The elongated shape is due to attitude problems in the processed data Note (3): When we cannot resolve the two components of the binary system, the displacement δ between the detected X-ray source and the optical positions of the two components of the system are given. Note (4): For ROR 201685h B, the printed value is "4535.3.8", modified in 45353.8 in the present table.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 8- 10 A3 --- Comp Component designation 12 A1 --- l_logNH Limit flag on logNH 13- 17 F5.2 [cm-2] logNH Computed hydrogen column density 19 I1 --- r_logNH ? Source of logNH (1) 21 A1 --- Obs [HRP] Type of observations (2) 23 A1 --- l_logLX Limit flag on logLX 24- 28 F5.2 [10-7W] logLX X-ray luminosity (3) 31- 35 F5.2 [10-7W] e_logLX ? rms uncertainty on logLX 36 A1 --- n_logLX [*] *: Mean X-ray luminosity computed from several observations 38 A1 --- l_logLX2 Limit flag on logLX2 39- 43 F5.2 [10-7W] logLX2 ? X-ray luminosity of the secondary
Note (1): Source of logNH as follows: 1 = Adopted from Berghofer et al. (1996, Cat. J/A+AS/118/481) 2 = Adopted from Fruscione et al. (1994, Cat. J/ApJS/94/127) Note (2): Type of observation as follows: R = RASS (ROSAT All-Sky Survey, Cat. IX/10) P = PSPC (Position-Sensitive Proportional Counter, Cat. IX/30) H = HRI (High Resolution Imager, Cat. IX/28) Note (3): If the binary system is observed and resolved by the HRI, we provide the fluxes and luminosities for both members of the pair. If unresolved, we just can provide one X-ray luminosity associated with the pair. In hese cases we have adopted a temperature of 1keV to compute the ECF's although, in principle, both stars could be contributing to the total emission. he last method has also been applied to those systems with only RASS or PSPC pointed observations, given that they are always unresolved. In the case of RASS or PSPC non-detections, we have estimated two upper limit luminosities, corresponding to the count rates computed at the optical positions of the primary and the secondary star, respectively (see Table 2).
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 7 A1 --- n_Umag Note on U-magnitudes (1) 9- 12 F4.2 mag Umag U magnitude (from HR catalogue V/50) 14- 18 F5.2 ct/ks Srate S-band count rate (2) 20- 24 F5.2 ct/ks UVrate UV count rate (2) 26- 32 F7.2 --- S/UV S to UV rates ratio 34- 37 F4.1 --- log(LX/Lbol) Bolometric to X-ray Luminosity ratio
Note (1): *: No U-magnitudes available. We derived them from their spectral types and their V-magnitudes, according to Kenyon & Hartmann (1995, Cat. J/ApJS/101/117). Note (2): The S-band rate and the UV rate have been both computed in channels 1-8 of the detector.
Byte-by-byte Description of file: table7.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD (Cat. III/135) number 8 A1 --- Comp Component designation 9 A1 --- u_Comp [?] Uncertainty flag on Comp 10 A1 --- n_HD [t] Note on HD (1) 12- 15 A4 --- SpType MK Spectral type 17 A1 --- l_logLX Limit flag on logLX 18- 22 F5.2 [10-7W] logLX X-ray luminosity 25 A1 --- l_EWLi Limit flag on EWLi 26- 30 F5.3 0.1nm EWLi Li I absorption line equivalent width 32- 36 F5.3 0.1nm e_EWLi ? rms uncertainty on EWLi 38 A1 --- n_EWLi [1-3] Note on EWLi (2) 40- 44 F5.3 Jy F12um ? 12mum flux density (3) 45 A1 --- u_F12um [?] ?: unknown value 47- 51 F5.3 Jy F100um ? 100mum flux density (3) 52 A1 --- u_F100um [?] ?: unknown value 54- 55 A2 --- f_RV [Ee :] Radial velocity comment (4) 57 A1 --- Xray [±] X-ray emission ? (5) 60 A1 --- LiI [±] Li I equivalent width ? (5) 63 A1 --- IR-ex [±?] Measured IR excess ? (5) 65- 67 A3 --- RV [±? ()] Measured radial velocity of pair ? (5)
Note (1): The two sources marked with a t are located close to the Galactic plane and this seems to be the reason of not being detected by IRAS Note (2): Most of the Li I EW values have been adopted Pallavicini et al. (1992A&A...261..245P). These measurements were derived from high-resolution spectra (resolution of 0.1Å), except those with a note (1, 2 or 3): 1 = obtained from low-resolution spectra (resolution of 2Å) 2 = taken from Martin et al., 1992A&A...257..186M (disp. of 0.22Å/pix) 3 = adopted from Webb et al. (1999ApJ...512L..63W); Note (3): The IR data are taken from Ray et al. (1995ApJ...440L..89R) Note (4): If similar radial velocities have been measured for both members of the pair it is indicated by an 'e' (if taken from Gahm, 1982, Stockholm Obs. Rep. No.20 ) and by an 'E' (if taken from Martin et al., 1992A&A...257..186M). If the measurements are doubtful, it is indicated by a ":" (see Gahm, 1982, Stockholm Obs. Rep. No.20, and Martin et al., 1992A&A...257..186M, for more details) Note (5): We have summarized the data of the table in these columns using the symbols +,- and ? for positive, negative and unknown properties respectively. The (+) symbols indicate doubtful properties.
Global notes: Note (G1): Hardness ratio: HR1=(H1+H2-S)/(H1+H2+S) and HR2=(H2-H1)/(H2+H1) where S=0.1-0.4keV (Soft), H1=0.5-0.9keV (Hard1), H2=0.9-2.0keV (Hard2)
History: Prepared via OCR at CDS.
(End) James Marcout, Patricia Bauer [CDS] 24-Jan-2001
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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