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J/A+AS/146/103 CaII H&K to CaII IRT echelle spectra (Montes+, 2000)
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Multiwavelength optical observations of chromospherically active binary systems.
III. High resolution echelle spectra from CaII H & K to CaII IRT.
Montes D., Fernandez-Figueroa M.J., De Castro E., Cornide M., Latorre A.,
Sanz-Forcada J.
<Astron. Astrophys. Suppl. Ser. 146, 103 (2000)>
=2000A&AS..146..103M
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ADC_Keywords: Binaries, spectroscopic ; Spectroscopy
Keywords: stars: activity - stars: binaries: close -
stars: binaries: spectroscopic - stars: chromospheres -
stars: late-type
Abstract:
This is the third paper of a series aimed at studying the chromosphere
of active binary systems using the information provided for several
optical spectroscopic features. High resolution echelle spectra
including all the optical chromospheric activity indicators from the
CaII H&K to CaII IRT lines are analysed here for 16 systems. The
chromospheric contribution in these lines has been determined using
the spectral subtraction technique. Very broad wings have been found
in the subtracted H{alpha} profile of the very active star HU Vir.
These profiles are well matched using a two-component Gaussian fit
(narrow and broad) and the broad component can be interpreted as
arising from microflaring. Red-shifted absorption features in the
H{alpha} line have been detected in several systems and excess
emission in the blue wing of FG UMa was also detected. These features
indicate that several dynamical processes, or a combination of them,
may be involved. Using the E_H{alpha}_/E_H{beta}_ ratio as a
diagnostic we have detected prominence-like extended material viewed
off the limb in many stars of the sample, and prominences viewed
against the disk at some orbital phases in the dwarfs OU Gem and BF
Lyn. The He I D_3_ line has been detected as an absorption feature in
mainly all the giants of the sample. Total filling-in of the He I
D_3_, probably due to microflaring activity, is observed in HU Vir.
Self-absorption with red asymmetry is detected in the CaII H&K lines
of the giants 12 Cam, FG UMa and BM CVn. All the stars analysed show
clear filled-in CaII IRT lines or even notable emission reversal. The
small values of the E_8542_/E_8498_ ratio we have found indicate CaII
IRT emission arises from plage-like regions. Orbital phase modulation
of the chromospheric emission has been detected in some systems, in
the case of HU Vir evidence of an active longitude area has been
found.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 34 16 Star positions (from Simbad)
table3.dat 71 56 H{alpha} line measures in the observed and
subtracted spectra
table5.dat 66 36 H{beta} line measurements in the observed and
subtracted spectra
table6.dat 70 35 CaII H&K and H{epsilon} lines measures in
the observed and subtracted spectra
table7.dat 75 58 CaII IRT lines measures in the observed and
subtracted spectra
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See also:
V/76 : Chromospherically Active Binaries (Strassmeier+ 1993)
J/A+A/312/221 : Excess CaII H+K emission in active binaries (Montes+, 1996)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Star name
12- 13 I2 h RAh Right ascension (J2000.0)
15- 16 I2 min RAm Right ascension (J2000.0)
18- 21 F4.1 s RAs Right ascension (J2000.0)
23 A1 --- DE- Declination sign (J2000.0)
24- 25 I2 deg DEd Declination (J2000.0)
27- 28 I2 arcmin DEm Declination (J2000.0)
30- 31 I2 arcsec DEs Declination (J2000.0)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
12- 17 A6 --- Obs Telescope and observation run (G1)
19- 22 F4.2 --- phi [0/1[? Orbital phase
24 A1 --- E [HCTP] Type of emission (G2)
26- 29 F4.2 --- SH ? Relative contribution of the hot
component to the total continuum
30 A1 --- --- [/]
31- 34 F4.2 --- SC ? Relative contribution of the cool
component to the total continuum
36 A1 --- Halpha [AEF] Observed H{alpha} profile:
A: absorption, E: emission,
F: totally filled-in by emission
38- 41 F4.2 0.1nm Wobs ? Full width at half maximum in the
observed spectrum
43- 46 F4.2 --- Rc Residual intensity in the observed
spectrum (Rc=Fc/Fcont)
48- 51 F4.2 0.1nm EWobs ? Equivalent width in the observed
spectrum
53- 56 F4.2 0.1nm Wsub ? Full width at half maximum in the
subtracted spectrum
58- 61 F4.2 --- Int ? Peak emission intensity in the
subtracted spectrum
63- 66 F4.2 0.1nm EWSub Excess H{alpha} emission equivalent width
in the subtracted spectrum (1)
68- 71 F4.2 [10mW/m2/nm] logFS(Ha) Absolute flux at the stellar surface
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Note (1): Equivalent width corrected for the contribution of each component to
the total continuum
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
12- 17 A6 --- Obs Telescope and observation run (G1)
19- 22 F4.2 --- phi [0/1[? Orbital phase
24 A1 --- E [HCTP] Type of emission (G2)
26- 29 F4.2 0.1nm Wobs ? Full width at half maximum in the
observed spectrum
31- 34 F4.2 --- Rc Residual intensity in the observed spectrum
36- 39 F4.2 0.1nm EWobs ? Equivalent width in the observed spectrum
41- 44 F4.2 0.1nm Wsub ? Full width at half maximum in the
subtracted spectrum
46- 49 F4.2 --- Int ? Peak emission intensity in the subtracted
spectrum
51- 54 F4.2 0.1nm EWSub Excess H{alpha} emission equivalent width
in the subtracted spectrum (1)
56- 59 F4.2 --- EW(Ha)/EW(Hb) ? Ratio of excess emission EW in
the H{alpha} and H{beta} lines
61- 65 F5.2 --- E(Ha)/E(Hb) ? Corrected ratio of excess emission (2)
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Note (1): Equivalent width corrected for the contribution of each component to
the total continuum
Note (2): Ratio of excess emission with the correction:
E(Ha)/E(Hb) = EW(Ha)/EW(Hb)*0.2444*2.512^(B-R)
given by Hall & Ramsey (1992AJ....104.1942H)
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
12- 17 A6 --- Obs Telescope and observation run (G1)
19- 22 F4.2 --- phi [0/1[? Orbital phase
24 A1 --- E [CHTPS] Type of emission (G2)
26- 29 F4.2 0.1nm EW(K)r CaII K equivalent width obtained by
reconstruction of the absorption
line profile
31- 34 F4.2 0.1nm EW(H)r CaII H equivalent width obtained by
reconstruction of the absorption
line profile
36- 39 F4.2 0.1nm EW(He)r ? H{epsilon} equivalent width obtained by
reconstruction of the absorption
line profile
41- 44 F4.2 0.1nm EW(K)s CaII K equivalent width using spectral
subtraction technique (1)
46- 49 F4.2 0.1nm EW(H)s CaII H equivalent width using spectral
subtraction technique (1)
51- 54 F4.2 0.1nm EW(He)s ? H{epsilon} equivalent width using
spectral subtraction technique (1)
56- 59 F4.2 [10mW/m2/nm] logF(K) CaII K surface flux (2)
61- 64 F4.2 [10mW/m2/nm] logF(H) CaII H surface flux (2)
66- 69 F4.2 [10mW/m2/nm] logF(He) ? H{epsilon} surface flux (2)
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Note (1): Equivalent width corrected for the contribution of each component to
the total continuum
Note (2): Surface flux obtained by means of the linear relationship between the
absolute surface flux at 3950{AA} (in erg/cm^2^/s/{AA}) and the
colour index (V-R) by Pasquini et al. (1988A&A...191..253P).
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name Name
12- 17 A6 --- Obs Telescope and observation run (G1)
19- 22 F4.2 --- phi [0/1[? Orbital phase
24 A1 --- E [CHTPS] Type of emission (G2)
26- 29 F4.2 0.1nm EW(8498)r ? {lambda}8498 equivalent width
obtained by absorption line
profile reconstruction
31- 34 F4.2 0.1nm EW(8542)r ? {lambda}8542 equivalent width
obtained by absorption line
profile reconstruction
36- 39 F4.2 0.1nm EW(8662)r ? {lambda}8662 equivalent width
obtained by absorption line
profile reconstruction
41- 44 F4.2 0.1nm EW(8498)s ? {lambda}8498 equivalent width using
spectral subtraction technique (1)
46- 49 F4.2 0.1nm EW(8542)s ? {lambda}8542 equivalent width using
spectral subtraction technique (1)
51- 54 F4.2 0.1nm EW(8662)s ? {lambda}8662 equivalent width using
spectral subtraction technique (1)
56- 59 F4.2 --- EW(8582)/EW(8498) ? Ratio of excess emission EW (2)
61- 64 F4.2 [10mW/m2/nm] logF(8498) ? {lambda}8498 surface flux (3)
66- 69 F4.2 [10mW/m2/nm] logF(8542) ? {lambda}8542 surface flux (3)
71- 74 F4.2 [10mW/m2/nm] logF(8662) ? {lambda}8662 surface flux (3)
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Note (1): Equivalent width corrected for the contribution of each component to
the total continuum.
Note (2): For the observing runs in which the {lambda}8542 and {lambda}8498
lines are included we also give the ratio of excess emission EW,
E_8542_/E_8498_, which is also an indicator of the type of
chromospheric structure that produces the observed emission.
Note (3): Absolute fluxes at the stellar surface have been obtained using the
calibration of Hall (1996PASP..108..313H) as a function of (V-R).
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Global notes:
Note (G1): Observations:
CAHA95 German Spanish Observatory, 12 June 1995
INT 99 Isaac Newton Telescope, 7-8 January 1999
McD 98 Otto Struve Telescope, 12-21 January 1998
NOT 96 Nordic Optical Telescope, 1-2 March 1996
NOT 98 Nordic Optical Telescope, 5-10 April 1998
Note (G2): Type of emission:
H: emission from the hot component
C: emission from the cool component
T: at these phases the spectral features cannot be deblended
P: emission from the primary component (for MS Ser only)
S: emission from the secondary component (for MS Ser only)
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History: From A&AS electronic version
References:
Montes et al., Paper I 1997A&AS..125..263M
Montes et al., Paper II 1998A&A...330..155M
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(End) Patricia Bauer [CDS] 09-Nov-2000