J/MNRAS/377/1263 Multiperiodic RR Lyrae in ASAS catalog (Szczygiel+, 2007)
Multiperiodic Galactic field RR Lyrae stars in the ASAS catalogue.
Szczygiel D.M., Fabrycky D.C.
<Mon. Not. R. Astron. Soc., 377, 1263-1274 (2007)>
=2007MNRAS.377.1263S 2007MNRAS.377.1263S
ADC_Keywords: Stars, variable
Keywords: methods: statistical - stars: horizontal branch -
stars: individual: SU Col - stars: oscillations -
stars: variables: other
Abstract:
The All Sky Automated Survey (ASAS) monitors bright stars (8<V<14mag)
south of declination +28°. The ASAS Catalogue of Variable Stars
(ACVS) presently contains 50099 objects; among them are 2212 objects
classified as RR Lyrae pulsating variables. We use ASAS photometric
V-band data to search for multiperiodicity in those stars. We find
that 73 of 1435 RRab stars and 49 of 756 RRc stars exhibit the Blazhko
effect. We observe a deficiency of RRab Blazhko variables with main
pulsation periods greater than 0.65d. The Blazhko periods of RRc
stars exhibit a strongly bimodal distribution. During our study we
discovered the Blazhko effect with multiple periods in object
ASAS 0507473351.9 = SU Col. Blazhko periods of 89.3 and 65.8d and a
candidate of 29.5d were identified with periodogram peaks near the
first three harmonics of the main pulsation. These observations may
inspire new models of the Blazhko effect, which has eluded a
consistent theory since its discovery about one hundred years ago.
Long-term light curve changes were found in 29 stars. We also found 19
Galactic double mode pulsators (RRd), of which four are new
discoveries, raising the number of ASAS discoveries of such objects to
16, out of 27 known in the field of our Galaxy.
Description:
The ASAS project is located in Las Campanas Observatory in Chile and
currently consists of two small, wide-field telescopes (200/2.8) with
2kx2k CCD cameras with 15-m pixel size from Apogee, observing in
standard V and I filters.
All the ASAS data that are public domain, as well as an online
catalogue, are available on the WWW:
http://www.astrouw.edu.pl/~gp/asas/asas.html
http://archive.princeton.edu/~asas/
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 89 52 Objects exhibiting BL1 effect
(1 peak in Blazhko period range)
table3.dat 87 70 Objects exhibiting BL2 effect
(2 symetric peaks in Blazhko period range)
table4.dat 88 29 Objects exhibiting long period changes (PCs)
table7.dat 81 19 Parameters for double-mode RR Lyrae stars (RRd)
found in ASAS data.
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See also:
J/AcA/48/35 : All Sky Automated Survey variable stars (Pojmamski 1998)
J/AcA/50/177 : All Sky Automated Survey Catalog (Pojmanski+, 2000)
II/264 : ASAS Variable Stars in Southern hemisphere (Pojmanski+ 2002-05)
Byte-by-byte Description of file: table[24].dat
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Bytes Format Units Label Explanations
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1- 13 A13 --- ASAS ASAS designation (HHMMSS-DDMM.m, J2000)
15- 19 F5.2 mag Vmag V magnitude
21- 29 F9.7 d Per Main period (P=f0-1, where f0 is the main
pulsation frequency)
31- 38 F8.2 d PBl Blazhko period (G1)
40- 43 F4.2 mag A0 Peak-to-peak amplitude of variation as
provided by ASAS Catalog of Variable Stars
45- 48 F4.2 mag A1 Peak-to-peak amplitude of Blazhko modulation
50- 53 F4.2 --- A1/A0 A1/A0 amplitude ratio
55- 58 F4.2 --- Anoise Noise on A0 and A1 amplitudes
60- 78 A19 --- Type Variable type
80- 88 A9 --- OName Other name
89 A1 --- n_ASAS [*] * for stars which had a BL1 frequency in
all three light curves
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- ASAS ASAS designation (HHMMSS-DDMM.m, J2000)
15- 19 F5.2 mag Vmag V magnitude
21- 29 F9.7 d Per Main period (P=f0-1, where f0 is the main
pulsation frequency)
31- 38 F8.2 d PBl Blazhko period (G1)
40- 43 F4.2 mag A0 Peak-to-peak amplitude of variation as
provided by ASAS Catalog of Variable Stars
45- 48 F4.2 mag A- Peak-to-peak amplitude of Blazhko modulation
corresponding to the modulation frequency on
the left-hand side of the main pulsation
frequency
50- 53 F4.2 mag A+ Peak-to-peak amplitude of Blazhko modulation
corresponding to the modulation frequency on
the right-hand side of the main pulsation
frequency
55- 58 F4.2 --- A-/A+ A-/A+ amplitude ratio
60- 63 F4.2 --- Anoise Noise on A0, A- and A+ A1 amplitudes
65- 77 A13 --- Type Variable type
79- 87 A9 --- OName Other name
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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- 13 A13 --- ASAS ASAS designation (HHMMSS-DDMM.m, J2000)
15- 19 F5.2 mag Vmag V magnitude
21- 29 F9.7 d P0 Fundamental mode period
31- 34 F4.2 mag A0 Peak-to-peak amplitude of variation of
fundamental mode
36- 44 F9.7 d P1 First overtone period
46- 49 F4.2 mag A1 Peak-to-peak amplitude of variation of
first overtone
51- 59 F9.7 --- P1/P0 P1/P0 period ratio
61- 64 F4.2 --- A1/A0 A1/A0 amplitude ratio
66- 77 A12 --- OName Other name
79 A1 --- n_ASAS [*] * for new discovery
81 I1 --- Ref ? Reference number (1)
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Note (1): References as follows:
1 = Wils & Otero, 2005IBVS.5593....1W 2005IBVS.5593....1W
2 = Bernhard & Wils, 2006IBVS.5698....1B 2006IBVS.5698....1B
3 = Bragaglia et al., 2003, in Annual Report,
Osservatorio Astronomico di Bologna
4 = Garcia-Melendo et al., 2001IBVS.5167....1G 2001IBVS.5167....1G
5 = Garcia-Melendo & Clement, 1997, Cat. J/AJ/114/1190
6 = Wils, 2006IBVS.5685....1W 2006IBVS.5685....1W
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Global notes:
Note (G1): Blazhko period is defined as PBl=(f1-f0)-1, where f0 is the
main pulsation frequency and f1 is the frequency component caused by
the Blazhko effect. Thus the negative value of PBl means that the
additional frequency is smaller than the main pulsation frequency.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Apr-2008