J/A+A/573/A61 Photometry of new eclipsing CVs (Southworth+, 2015)
Orbital periods of cataclysmic variables identified by the SDSS.
IX. NTT photometry of eight eclipsing and three magnetic systems.
Southworth J., Tappert C., Gaensicke B.T., Copperwheat C.M.
<Astron. Astrophys. 573, A61 (2015)>
=2015A&A...573A..61S 2015A&A...573A..61S
ADC_Keywords: Binaries, cataclysmic ; Binaries, eclipsing
Keywords: stars: dwarf novae - novae, cataclysmic variables -
binaries: eclipsing - white dwarfs
Abstract:
We report the discovery of eclipses and the first orbital period
measurements for four cataclysmic variables, plus the first orbital
period measurements for one known eclipsing and two magnetic systems.
SDSS J093537.46+161950.8 exhibits 1-mag deep eclipses with a period of
92.245 min. SDSS J105754.25+275947.5 has short and deep eclipses and
an orbital period of 90.44 min. Its light curve has no trace of a
bright spot and its spectrum is dominated by the white dwarf
component, suggesting a low mass accretion rate and a very low-mass
and cool secondary star. CSS J132536+210037 shows 1-mag deep eclipses
each separated by 89.821 min. SDSS J075653.11+085831.8 shows 2-mag
deep eclipses on a period of 197.154 min. CSS J112634-100210 is an
eclipsing dwarf nova identified in the Catalina Real Time Transit
Survey, for which we measure a period of 111.523 min. SDSS
J092122.84+203857.1 is a magnetic system with an orbital period of
84.240 min; its light curve is a textbook example of cyclotron
beaming. A period of 158.72 min is found for the faint magnetic system
SDSS J132411.57+032050.4, whose orbital light variations are
reminiscent of AM Her. Improved orbital period measurements are also
given for three known SDSS cataclysmic variables. We investigate the
orbital period distribution and fraction of eclipsing systems within
the SDSS sample and for all cataclysmic variables with a known orbital
period, with the finding that the fraction of known CVs which are
eclipsing is not strongly dependent on the orbital period.
Description:
Light curves are presented of eleven cataclysmic variable stars, eight
of which are eclipsing. The other three cataclysmic variables contain
magnetic white dwarf components. The data were obtained using the
ESO/NTT/EFOSC2 and CAHA/3.5/LAICA telescopes and instruments. For the
NTT a Tyson B filter was used (ESO filter #724) whereas for the CAHA
3.5 a Gunn g filter was used.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 118 11 Full and abbreviated names, references and SDSS
apparent ugriz magnitudes of the targets (table1)
and orbital periods and CV classification
obtained in this work (table5)
table2.dat 75 33 Log of the observations presented in this work
alldata.dat 44 1400 All photometry of the nine CVs studied
css1325.dat 25 880 Spectrum of CSS J132536+210037
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See also:
J/MNRAS/373/687 : Spectra of 5 faint cataclysmic variables (Southworth+, 2006)
J/A+A/507/929 : Light curves of SDSS J100658.40+233724.4 (Southworth+, 2009)
J/A+A/510/A100 : Light curves of four new eclipsing CVs (Southworth+, 2010)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 A24 --- Name Name of the target star
26- 34 A9 -- SName Short name of target star
36 I1 -- Ref Reference (2)
38- 42 F5.2 mag umag SDSS u magnitude
44- 48 F5.2 mag gmag SDSS g magnitude
50- 54 F5.2 mag rmag SDSS r magnitude
56- 60 F5.2 mag imag SDSS i magnitude
62- 66 F5.2 mag zmag SDSS z magnitude
68- 72 F5.2 mag gspec ? Spectroscopic apparent magnitude (1)
74 A1 --- LC [*] * indicates photometric data in
alldata.dat file
76- 84 F9.5 min Per Orbital period
86- 92 F7.5 min e_Per rms uncertainty on Per
93 A1 --- u_Per [)] Uncertainty flag on Per
95-118 A24 --- Notes Notes
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Note (1): gspec is a spectroscopic apparent magnitude calculated by convolving
the SDSS flux-calibrated spectra with the g-band response function.
These correspond to a different epoch to the photometric magnitudes, but may
be affected by 'slit losses' due to errors in astrometry or fibre positioning.
Note (2): References as follows:
1 = Szkody et al. (2007AJ....134..185S 2007AJ....134..185S, Cat. J/AJ/134/185)
2 = Szkody et al. (2011AJ....142..181S 2011AJ....142..181S, Cat. J/AJ/142/181)
3 = Szkody et al. (2009AJ....137.4011S 2009AJ....137.4011S)
4 = Szkody et al. (2005AJ....129.2386S 2005AJ....129.2386S)
5 = Southworth et al. (2009A&A...507..929S 2009A&A...507..929S, Cat. J/A+A/507/929)
6 = Drake et al. (2009ApJ...696..870D 2009ApJ...696..870D, Cat. J/ApJ/696/870)
7 = Szkody et al. (2004AJ....128.1882S 2004AJ....128.1882S)
8 = Wils et al. (2010MNRAS.402..436W 2010MNRAS.402..436W)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SName Short name of target star
11- 20 A10 "Y/M/D" Obs.date Date of first observation in the observing
sequence (UT)
22- 26 A5 "h:m" Obs.time Start time (UT) (1)
28- 32 A5 "h:m" t.end End time (UT) (1)
34- 44 A11 --- Tel Telescope/Instrument: "CA35/ LAICA" (Calar Alto
3.5m) or "NTT/ EFOSC2" (ESO)
46- 58 A13 --- Filt Optical element (grism or filter)
60- 62 I3 --- Nobs [2/162] Number of observations
64- 66 I3 s Texp [30/900] Exposure time
67 A1 --- --- [-]
68- 70 I3 s Texp2 [60/300]? Second exposure time
72- 75 F4.1 mag ? Mean magnitude in Filt (2)
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Note (1): The start and end times indicate the beginning of the first and
last exposures in the observing sequence.
Note (2): The mean magnitudes are calculated using only observations
outside eclipses.
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Byte-by-byte Description of file: alldata.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SName Short name of target star
11 A1 --- Filter [Bg] Filter used (B for Btyson, g for Gunn g)
14- 27 F14.6 d HJD Heliocentric JD for the midpoint of each
observation, on the UTC timescale
30- 36 F7.4 mag mag Apparent magnitude of the target star
39- 44 F6.4 mag e_mag Measurement error of the apparent magnitude
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Byte-by-byte Description of file: css1325.dat
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Bytes Format Units Label Explanations
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1- 9 F9.4 0.1nm lambda Wavelength of summed pixel in spectrum
12- 17 F6.2 ct Counts Counts recorded over summed pixel
20- 25 F6.2 ct e_Counts Measurement error of the counts
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Acknowledgements:
John Southworth, astro.js(at)keele.ac.uk
References:
Southworth et al., Paper I 2007MNRAS.378..635S 2007MNRAS.378..635S
Southworth et al., Paper II 2007MNRAS.382.1145S 2007MNRAS.382.1145S
Dillon et al., Paper III 2008MNRAS.386.1568D 2008MNRAS.386.1568D
Southworth et al., Paper IV 2008MNRAS.388..709S 2008MNRAS.388..709S
Southworth et al., Paper V 2008MNRAS.391..591S 2008MNRAS.391..591S
Southworth et al., Paper VI 2009A&A...507..929S 2009A&A...507..929S, Cat. J/A+A/507/929
Southworth et al., Paper VII 2010A&A...510A.100S 2010A&A...510A.100S, Cat. J/A+A/510/A100
Southworth et al., Paper VIII 2010A&A...524A..86S 2010A&A...524A..86S, Cat. J/A+A/524/A86
(End) John Southworth [Keele Univ., UK], Patricia Vannier [CDS] 10-Dec-2014