J/MNRAS/420/757 STEREO magnetic chemically peculiar stars (Wraight+, 2012)
A photometric study of chemically peculiar stars with the STEREO satellites.
I. Magnetic chemically peculiar stars.
Wraight K.T., Fossati L., Netopil M., Paunzen E., Rode-Paunzen M.,
Bewsher D., Norton A.J., White G.J.
<Mon. Not. R. Astron. Soc., 420, 757-772 (2012)>
=2012MNRAS.420..757W 2012MNRAS.420..757W
ADC_Keywords: Stars, peculiar ; Rotational velocities
Keywords: techniques: photometric - catalogues - stars: chemically peculiar -
stars: rotation
Abstract:
About 10% of upper main-sequence stars are characterized by the
presence of chemical peculiarities, often found together with a
structured magnetic field. The atmospheres of most of those chemically
peculiar stars present surface spots, leading to photometric
variability caused by rotational modulation. The study of the light
curves of those stars therefore permits a precise measurement of their
rotational period, which is important to study stellar evolution and
to plan further detailed observations. We analysed the light curves of
1028 chemically peculiar stars obtained with the STEREO spacecraft. We
present here the results obtained for the 337 magnetic chemically
peculiar stars in our sample.
Description:
The stars were observed with the STEREO/HI-1 imager, on board of the
Stereo satellites, launched primarily to observe the coronal mass
ejections. The field of view is 20x20°, with a resolution of
70arcsec/pix. mostly in the 630-730nm wavelength range. Over the
course of an orbit, almost 900,000 stars of 12th magnitude and
brighter are imaged within 10° of the ecliptic plane, at a
cadence of about 40min.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 80 133 Basic properties of the CP2 and CP4 stars identified
as constant or for which the quality of the data
prevented the detection of any variability
table2.dat 110 122 Basic properties of the CP2 and CP4 stars identified
as constant or probably constant after the
individualised analysis
table3.dat 231 82 Properties of the CP2 and CP4 stars identified as
photometrically variable
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See also:
III/260 : General Catalogue of Ap and Am stars (Renson+ 2009)
J/MNRAS/429/119 : STEREO non-magnetic chemically peculiar stars (Paunzen+ 2013)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- Name Name
17- 21 I5 --- R09 Identification number by Renson & Manfroid
(2009A&A...498..961R 2009A&A...498..961R, Cat. III/260,
<Renson NNNNN> in Simbad)
24- 32 F9.5 deg RAdeg Right ascension (J2000)
34- 42 F9.5 deg DEdeg Declination (J2000)
44- 48 F5.2 mag Vmag Average V magnitude
50- 60 A11 -- SpType MK spectral type from Renson & Manfroid
2009A&A...498..961R 2009A&A...498..961R, Cat. III/260)
62- 65 A4 --- Class CP classification (G3)
69- 73 F5.1 km/s vsini ? Average projected rotational velocity
75- 78 F4.1 km/s e_vsini ? rms uncertainty on vsini
80 I1 --- o_vsini [1/6]? Number of averaged vsini
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Name
17- 21 I5 --- R09 Identification number by Renson & Manfroid
(2009A&A...498..961R 2009A&A...498..961R, Cat. III/260)
24- 32 F9.5 deg RAdeg Right ascension (J2000)
34- 42 F9.5 deg DEdeg Declination (J2000)
44- 48 F5.2 mag Vmag Average V magnitude
50- 62 A13 -- SpType MK spectral type from Renson & Manfroid
(2009A&A...498..961R 2009A&A...498..961R, Cat. III/260)
64- 67 A4 --- Class CP classification (G3)
69- 74 F6.4 d Per ? Period
76- 81 F6.4 d e_Per ? rms uncertainty on Per
83- 85 A3 --- Rem [WBSC ] Analysis remark (G1)
87- 89 A3 --- r_Plit Reference for literature period (G2)
90 A1 --- --- [:]
91- 97 F7.4 d Plit ? Literature period
99-103 F5.1 km/s vsini ? Average projected rotational velocity
105-108 F4.1 km/s e_vsini ? rms uncertainty on vsini
110 I1 --- o_vsini [1/5]? Number of averaged vsini
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- Name Name
17- 21 I5 --- R09 Identification number by Renson & Manfroid
(2009A&A...498..961R 2009A&A...498..961R, Cat. III/260)
23- 31 F9.5 deg RAdeg Right ascension (J2000)
33- 41 F9.5 deg DEdeg Declination (J2000)
43- 47 F5.2 mag Vmag Average V magnitude
49- 61 A13 -- SpType MK spectral type from Renson & Manfroid
(2009A&A...498..961R 2009A&A...498..961R, Cat. III/260)
63- 66 A4 --- Class CP classification (G3)
68- 74 F7.4 d Per Period
76- 81 F6.4 d e_Per rms uncertainty on Per
83- 89 F7.4 d Per2 ? Second period
91- 96 F6.4 d e_Per2 ? rms uncertainty on Per2
98-103 F6.4 d Per3 ? Third period
105-110 F6.4 d e_Per3 ? rms uncertainty on Per3
112-120 F9.3 d MJD ? MJD of the epoch for the first recorded
maximum
122-124 A3 --- Rem [WBS* ] Analysis remark (G1)
126-165 A40 d Plit Reference for literature period with
literature period(s) (G2)
167 A1 --- r_Bl Reference for literature magnetic field (G2)
168 A1 --- --- [:]
169-172 I4 10-4T Bl ? Literature magnetic field, Gauss
174-178 F5.1 km/s vsini ? Average projected rotational velocity
180-183 F4.1 km/s e_vsini ? rms uncertainty on vsini
185 I1 --- o_vsini [1/5]? Number of averaged vsini
187-191 I5 K Teff ? Effective temperature
193-196 I4 K e_Teff ? rms uncertainty on Teff
198-199 I2 --- o_Teff [1/99]? Number of averaged temperature
(99 when Teff from Netopil et al.,
2008A&A...491..545N 2008A&A...491..545N)
201-204 F4.2 [Lsun] logL ? Luminosity
206-209 F4.2 [Lsun] e_logL ? rms uncertainty on logL
211 A1 --- n_logL [ZT] ZAMS or TAMS stage (1)
213-216 F4.2 Msun Mass ? Mass
218-221 F4.2 Msun e_Mass ? rms uncertainty on Mass
223-226 F4.2 --- tau [0/1]? Fractional age τ (fraction of
main sequence lifetime completed) (1)
228-231 F4.2 --- e_tau ? rms uncertainty on tau
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Note (1): the Zero-Age Main Sequence (ZAMS) corresponds to τ=0,
and the Terminal-Age Main Sequence (TAMS) corresponds to τ=1.
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Global notes:
Note (G1): Analysis remark as follows:
B = possible presence of blending
S = systematic effects
* = exceptionally strong signal
W = weak signal
C = when we concluded the star was constant
Note (G2): References as follows:
B1 = Bychkov, Bychkova & Madej (2005, Cat. J/A+A/430/1143)
B = Bychkov et al. (2009, Cat. J/MNRAS/394/1338)
C98 = Catalano & Renson (1998A&AS..127..421C 1998A&AS..127..421C, Cat. III/199)
C01 = Renson & Catalano (2001, Cat. J/A+A/378/113)
K = Kudryavtsev et al. (2006MNRAS.372.1804K 2006MNRAS.372.1804K)
KE = Koen & Eyer (2002, Cat. J/MNRAS/331/45)
K07 = Kraus et al. (2007, Cat. J/AJ/134/1488)
R = Romanyuk & Kudryavtsev (2008AstBu..63..139R 2008AstBu..63..139R)
S = Samus et al. (2009, GCVS, Cat. B/gcvs)
W = Watson (2006, n Soc. Astron. Sci. Annu. Symp. 25. 2006. p. 47)
Note (G3): the chemically peculiar stars are subdivided into the classes:
CP1 = metallic-line stars (Am, Fm, ...)
CP2 = magnetic Ap stars
CP3 = HgMn stars
CP4 = He-weak stars
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History:
From electronic version of the journal
References:
Paunzen et al., Paper II 2013MNRAS.429..119P 2013MNRAS.429..119P, Cat. J/MNRAS/429/119
(End) Patricia Vannier [CDS] 17-Mar-2014