A&A 455, 659-672 (2006)
DOI: 10.1051/0004-6361:20065049
A. Aungwerojwit1 - B. T. Gänsicke1 - P. Rodríguez-Gil1,2 - H.-J. Hagen3 - S. Araujo-Betancor2 - O. Baernbantner4 - D. Engels3 - R. E. Fried5 - E. T. Harlaftis6 - D. Mislis7 - D. Nogami8 - P. Schmeer9 - R. Schwarz10 - A. Staude10 - M. A. P. Torres11
1 -
Department of Physics, University of Warwick, Coventry CV4 7AL, UK
2 -
Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
3 -
Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg
112, 21029 Hamburg, Germany
4 -
Universitäts-Sternwarte, Scheinerstr. 1, 81679 München, Germany
5 -
Braeside Observatory, PO Box 906, Flagstaff AZ 86002, USA
6 -
Institute of Space Applications and Remote Sensing,
National Observatory of Athens, PO Box 20048, Athens 11810, Greece
7 -
Department of Physics, Section of Astrophysics, Astronomy &
Mechanics, University of Thessaloniki, 541 24 Thessaloniki, Greece
8 -
Hida Observatory, Kyoto University, Kamitakara, Gifu 506-1314, Japan
9 -
Bischmisheim, Am Probstbaum 10, 66132 Saarbrücken, Germany
10 -
Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482
Potsdam, Germany
11 -
Harvard-Smithsonian Center for Astrophysics, 60 Garden St,
Cambridge, MA 02138, USA
Received 20 February 2006 / Accepted 11 May 2006
Abstract
Aims. We report the discovery of five new dwarf novae that were spectroscopically identified in the Hamburg Quasar Survey (HQS), and discuss the properties of the sample of new dwarf novae from the HQS.
Methods. Follow-up time-resolved spectroscopy and photometry have been obtained to characterise the new systems.
Results. The orbital periods determined from analyses of the radial velocity variations and/or orbital photometric variability are
min or
min for HS 0417+7445,
min for HS 1016+3412,
min for HS 1340+1524,
min for HS 1857+7127, and
min for HS 2214+2845. HS 1857+7127 is found to be partially eclipsing. In HS 2214+2845 the secondary star of spectral type
is clearly detected, and we estimate the distance to the system to be
pc. We recorded one superoutburst of HS 0417+7445, identifying the system as a SU UMa-type dwarf nova. HS 1016+3412 and HS 1340+1524 have rare outbursts, and their subtype is yet undetermined. HS 1857+7127 frequently varies in brightness and may be a Z Cam-type dwarf nova. HS 2214+2845 is a U Gem-type dwarf nova with a most likely cycle length of 71 d.
Conclusions. To date, 14 new dwarf novae have been identified in the HQS. The ratio of short-period (<3 h) to long-period (>3 h) systems of this sample is 1.3, much smaller compared to the ratio of 2.7 found for all known dwarf novae. The HQS dwarf novae display typically infrequent or low-amplitude outburst activity, underlining the strength of spectroscopic selection in identifying new CVs independently of their variability. The spectroscopic properties of short-period CVs in the HQS, newly identified and previously known, suggest that most, or possibly all of them are still evolving towards the minimum period. Their total number agrees with the predictions of population models within an order of magnitude. However, the bulk of all CVs is predicted to have evolved past the minimum period, and those systems remain unidentified. This suggests that those post-bounce systems have markedly weaker H
emission lines compared to the average known short-period CVs, and undergo no or extremely rare outbursts.
Key words: stars: dwarf novae - stars: individual: HS 0417+7445 - stars: individual: HS 1016+3412 - stars: individual: HS 1340+1524 - stars: individual: HS 1857+7127 - stars: individual: HS 2214+2845
As a measure to probe the completeness of the known CV sample, we have
initiated a search based on one property common to the majority of all
CVs: the presence of Balmer emission lines in their optical
spectra. We are selecting CV candidates from the Hamburg Quasar Survey
(HQS, Hagen et al. 1995), an objective prism Schmidt survey of
the northern hemisphere covering
at high galactic
latitudes with a limiting magnitude
.
The survey
resulted in
50 new CVs, including a number of peculiar objects
(e.g. Rodríguez-Gil et al. 2005b; Araujo-Betancor et al. 2005a; Gänsicke et al. 2000; Rodríguez-Gil et al. 2004b); a general overview has
been given by Gänsicke et al. (2002) and more recently by
Aungwerojwit et al. (2005).
In this paper, we report the identification of five new dwarf novae in the HQS: HS 0417+7445, HS 1016+3412, HS 1340+1524, HS 1857+7127, and HS 2214+2845 (HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214, respectively, hereafter; Fig. 1 and Table 1). In Sect. 2 we provide details about the observations and data reduction, in Sects. 3-7 we describe the data analysis and determine the orbital periods of the new dwarf novae. In Sect. 8, we compare the period distribution of the dwarf novae found in the HQS to that of all known dwarf novae. In Sect. 9 we discuss the implications of our survey work on the space density of CVs.
Table 1: Properties of the five new dwarf novae.
Additional time-resolved spectroscopy of HS 1016 (70 spectra), HS 1340 (78 spectra), HS 1857 (41 spectra), and HS 2214 (41 spectra) was obtained at the Calar Alto Observatory and Roque de los Muchachos Observatory (Table 2). The details of instrument setup and data reduction are described below.
The time-resolved follow-up observations of HS 1016, HS 1340,
HS 1857, and HS 2214 were obtained with the G-100 grating and a
1.2
slit, providing a spectral resolution of
4.1 Å (full width at half maximum, FWHM) over the wavelength range
.
Clouds and/or moderate to poor seeing
affected a substantial fraction of these observations. HS 2214 was
observed under photometric conditions using the B-100 grating along
with a 1.5
slit, providing a resolution of
4 Å (FWHM)
over the range 3500-6300 Å. Two additional red spectra of HS 2214
were taken with the R-100 grating, covering the range 6000-9200 Å at a similar resolution. All follow-up spectroscopy was obtained in
600 s exposures, interleaved with arc calibrations every
40 min to correct for instrument flexure. Flux standards were
observed at the beginning and end of the night - weather
permitting - to correct for the instrumental response. The data
reduction (bias and flat-field correction, extraction, wavelength and
flux calibration) was carried out using the Figaro package
within Starlink and the programs Pamela and Molly
developed by T. Marsh. Special care was given to the wavelength
calibration by interpolating the dispersion relation for a given
target spectrum from the two adjacent arc exposures.
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Figure 2:
Main panel: flux-calibrated CAFOS spectra
of HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214. Fluxes are
labelled alternatingly on the left and right side. HS 1340 was
observed in quiescence and outburst, respectively. Right panel:
close-up plots of the
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Additional images of HS 0417, HS 1016,
HS 1340, and HS 2214 were taken intermittently during the period
May 2004 to April 2005 using the 0.37 m robotic Rigel telescope of
the University of Iowa which is equipped with a
pixel SITe-003 CCD camera. For all four
systems, filterless images with an exposure time of 25 s were obtained.
All five dwarf novae identified on the basis of their emission line spectra in the HQS are also X-ray sources in the ROSAT All Sky Survey (RASS): HS 0417, HS 1340, and HS 2214 are contained in the Bright Source Catalogue (Voges et al. 1999), HS 1016 and HS 1857 within the Faint Source Catalogue (Voges et al. 2000). The X-ray properties of the new systems are summarised in Table 1. All but HS 1340 are hard X-ray sources in the hardness ratio HR1, typical of non- (or weakly-) magnetic CVs (van Teeseling et al. 1996).
Throughout our photometric observations we have found the object near
a mean magnitude of 17.5 (December 2000:
,
February 2003:
,
November 2004: filterless
17.6,
January 2005:
), consistent with the USNO-A2.0
measurements,
and
,
except during January
2001, when the system was found in an outburst near
.
In
the quiescent state, the light curve of HS 0417 is characterised by a
double-humped pattern with a period of
100 min
(Fig. 3, bottom panel). The light curve obtained during
the January 2001 outburst (Fig. 3, top panel) reveals
superhumps that identify HS 0417 as a SU UMa-type dwarf nova
and therefore this outburst as a superoutburst. An additional
outburst of HS 0417 was caught on the rise in April 10, 2005 by one of
us (PS), and
3 h, V-band data obtained by David Boyd on the
evening of April 11, 2005 showed the object already declining at
a rate of
0.85 mag
and no evidence of superhumps was
found. By April 18, the system reached again its quiescent magnitude
of
.
In order to measure the orbital period of the system, a
Scargle (1982) periodogram was computed within the
MIDAS/TSA context from all quiescent data except the February
2003 observations which were of too poor a quality. The periodogram
(Fig. 8) contains a fairly broad sequence of
aliases spaced by 1
with the strongest signal at 13.7
and a nearly equally strong signal at 13.1
.
The high-frequency
range of the periodogram of HS 0417 is nicely reproduced by the
window function (shifted to 13.7
in the top panel of
Fig. 8), but excess power is present at
frequencies below 10
,
most likely associated with the short
length of the observing runs. Sine-fits to the data result in the
periods corresponding to the two highest peaks in the periodogram,
min and
min, respectively. We
interpreted these values as possible orbital periods of HS 0417.
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Figure 3: Sample light curves of HS 0417 obtained at the Wendelstein observatory. Top panel: B-band data obtained during superoutburst on January 14, 2001. Bottom panel: filterless data obtained during quiescence. |
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Figure 4: Sample filterless light curves of HS 1016 obtained at the Kryoneri observatory. |
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Figure 5: Sample light curves of HS 1340. Top panel: R-band data obtained at the Kryoneri observatory. Bottom panel: filterless data obtained at the IAC80 telescope. |
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Figure 6: Sample R-band light curves of HS 2214 obtained at the Braeside observatory. |
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The Scargle periodogram computed from the superoutburst data obtained
on January 14, 2001 (Fig. 3, top panel) provides a
broad signal with a peak at 13.3
,
or
min. The light curve folded over this period shows,
however, a significant offset between the two observed superhump maxima. A
periodogram computed using Schwarzenberg-Czerny's
(1996) analysis-of-variance (AOV)
method using orthogonal polynomial fits to the data (implemented as
ORT/TSA in MIDAS) results in a much narrower peak
compared to the Scargle analysis, centred at 12.95
(
min). This period provides a clean folded
light curve. This improvement in the period analysis underlines the
fact that AOV-type methods provide better sensitivity for strongly
non-sinusoidal signals (such as superhumps) compared to
Fourier-transform based methods.
The analysis of our photometric data left us with two candidate
orbital periods,
min or
min, and two
candidate superhump periods,
min or
min.
Table 4 lists the fractional superhump excess,
calculated from all possible
combinations of the candidate periods. We consider cases (2) and (3)
as very unlikely, as no dwarf nova with
is found below
the period gap and no short-period dwarf nova with a negative
superhump excess is known (e.g. Patterson et al. 2003; Rodríguez-Gil et al. 2005a; Nogami et al. 2000). In fact, most dwarf novae
with
min have
(Patterson et al. 2005), which would make case (1) look most
likely. However, based on our data, we prefer case (4) as
min gave the cleanest folded superhump light curve. In
this case, HS 0417 would have a rather low value of
,
similar only to KV And (
min) which has
(Patterson et al. 2003). An unambiguous
determination of both
and
would be important, as
may be used to estimate the mass ratio of a CV
(Patterson et al. 2005).
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Figure 7: Sample R-band and filterless light curves of HS 1857 folded over the ephemeris in Eq. (1). See Sect. 6.2 for details. |
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Figure 8:
Main panel: the Scargle
periodogram of HS 0417 during quiescence computed from all photometric data
except February 27, 2003. Top panel: the window function shifted to
13.7
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Table 4:
The fractional superhump excess of HS 0417 computed from
.
The single-peaked profile found in the emission lines suggests a relatively low orbital inclination. No spectral contribution from the secondary star is detected in the red part of the spectrum. The equivalent widths (EWs) from the CAFOS and INT average spectra do not show any noticeable variation in each epoch throughout our run. Table 1 lists FWHM and EW parameters of the CAFOS average spectrum measured from Gaussian fits.
In order to determine the orbital period of HS 1016, we measured
the radial velocity variation of
,
the strongest emission line,
from the CAFOS and IDS spectra. We first rebinned the individual
spectra to a uniform velocity centred on
,
followed by normalising
the slope of the continuum. We then measured the
radial velocity
variation using the double Gaussian method of
Schneider & Young (1980) with a separation of 1000
and an
FWHM of 200
.
A Scargle periodogram calculated from the
radial velocity variation contains a set of narrow aliases spaced by
1
,
with the strongest signal found at
(Fig. 9, top panel). We tested the significance of this
signal by creating a faked set of radial velocities computed from a
sine function with a frequency of 12.6
,
and randomly offset
from the computed sine wave using the observed errors. The periodogram
of the faked data set is plotted in a small window of the top panel in
Fig. 9 which reproduces well the alias structure of the
periodogram calculated from the observation. A sine-fit to the folded
radial velocities refined the period to
min, which we
interpreted as the orbital period of
HS 1016. Figure 10 (top panel) shows a sine-fit to
the phase-folded radial velocity curve; the fit parameters are
reported in Table 5.
The light curves of HS 1016 display short-time scale flickering
with an amplitude of
0.2-0.3 mag (Fig. 4). A Scargle periodogram
computed from the entire photometry as well as from individual subsets
did not reveal any significant signal.
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Figure 9: The Scargle periodogram of the radial velocities of HS 1016, HS 1340, HS 1857, and HS 2214. The periodograms constructed from faked sets of data at the corresponding orbital frequency are shown in small windows. |
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Figure 10:
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Table 5:
Sine fits to the
radial velocities of
HS 1016, HS,1340, and HS 1857. For HS 2214 a combination of
and
radial velocities were fitted, as the September 2000 Calar
Alto spectra did not cover
.
For HS 1857 and HS 2214, the periods
were fixed to their values determined from the photometry.
A second outburst reaching an unfiltered magnitude of 14.2 was
recorded on April 15, 2005 with the Rigel telescope, again, the
duration of the outburst was of the order of 2-3 days.
The light curves of HS 1340 obtained during quiescence are
predominantly characterised by variability on time scales of
15-20 min with peak-to-peak amplitudes of
0.4 mag
(Fig. 5, bottom panel). On some occasions, the light
curves shows hump-like structures which last for one to several hours,
superimposed by short-time scale flickering
(e.g. Fig. 5, top panel). Our period analysis of the
photometric data did not reveal any stable signal in the combined data.
In summary, HS 1340 appears to have rather infrequent and short-lived outbursts, and displays a substantial amount of short-term variability as well as variability of its mean magnitude during quiescence.
The orbital period of HS 1340 was determined using the spectroscopic
data taken in quiescence. The
radial velocity variation was
measured in the same manner as in HS 1016 with a separation of
1000
and an FWHM of 200
.
Figure 9 (second
panel) shows the Scargle periodogram. The strongest signal is found
at
where the error is estimated from the FWHM
of the strongest peak in the periodogram, corresponding to an orbital
period of
min. The
radial velocity curve folded
over this period is shown in Fig. 10 (second panel)
along with a sine-fit; the fit parameters are given in
Table 5. The periodogram of a faked data set
constructed from this frequency agrees well with the entire observed
alias structure (insert in Fig. 9, second panel).
With the spectroscopic period being determined, we re-analysed the
time-series photometry of HS 1340, and found no significant signal in
the range of the orbital frequency when we combined all quiescent
data. However, a weak signal at a frequency of 15.5
and
its one-day aliases were detected intermittently on some occasions,
e.g. in the 2003 Kryoneri data and the 2004 FLWO observations.
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Figure 11:
Main window: the mean magnitudes of
HS1340 obtained from May 2001 to May 2005 in R-band (filled
triangles), V-band (filled circles), and white light (open circles). The
photometric error on the individual points is <0.05 mag. An
additional systematic uncertainty arises from the combination of
different band passes. Considering the apparent magnitudes of HS 1340
listed in the Sloan Digital Sky Survey which are g=17.3, r=17.1,
and i=17.1, the errors due to colour terms are likely to be within
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Figure 12: The HST/STIS spectrum of HS 1857 taken on August 17, 2003 during an outburst. |
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Table 6: The times of eclipse minima of HS 1857 obtained during the 2002 to 2004 runs.
The overall shape of the light curves and that of the eclipse profiles
show a large degree of variability (Fig. 7). On
April 22, 2002, the light curve shows an orbital modulation with a
bright hump preceding the eclipse, typically observed in
quiescent eclipsing dwarf novae (e.g. Zhang & Robinson 1987),
produced by the bright spot. A shallow (0.4 mag) eclipse is
recorded, implying a partial eclipse of the accretion disc in the
system. On September 16, 2002, the system was apparently caught on the
rise to an outburst, with the eclipse depth reduced to
0.2 mag. During several intermediate and bright states the
signature of the bright spot disappeared, and was replaced by a broad
orbital modulation with maximum light near phase 0.5, superimposed by
short time scale flickering (Fig. 7, bottom four
panels). On May 3, 2004, a narrow dip (
)
centred
at
precedes the eclipse during both observed cycles. A
similar feature, though of lower depth, has been observed on April 22,
2003.
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Figure 13: The periodogram of HS 1857 computed from nine eclipses obtained during the 2002 to 2004 runs. |
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During our spectroscopic and photometric follow-up studies, HS 2214
was consistently found at 16.5-15.5 mag, with night-to-night
variations of the mean magnitude of 0.2-0.4 mag. The dwarf nova
nature of HS 2214 was confirmed through the visual monitoring by one
of us (PS), which led to the detection of outbursts on December 10,
2004, and on May 2, July 14, September 22, 2005, and April 23,
2006. The mean cycle length appears to be 71 d, and the maximum
brightness recorded during outburst was
.
In order to determine the spectral type of the secondary star in
HS 2214, we used a library of spectral templates created from
Sloan Digital Sky Survey data, covering spectral types M0-M9. For
each spectral type, we varied the flux contribution of the M-dwarf
template until the molecular absorption bands cancelled out as much as
possible in the difference spectrum of HS 2214 minus template. The best
match in the relative strength of the TiO absorption bands is achieved
for a spectral type M,
contributing 25% of the observed
V-band flux of HS 2214 (Fig. 14). The
extrapolated
spectrum of the secondary
star
agrees
fairly well with the 2MASS
magnitudes of HS 2214
(14.5, 13.9, and 13.5, respectively), suggesting that the accretion
disc contributes only a small amount to the infrared flux.
Using Beuermann & Weichhold's
(1999) calibration of the surface
brightness in the 7165/7500 Å TiO band, and assuming a radius of
cm, based on the orbital period determined
below and various radius-orbital period relations
(e.g. Beuermann & Weichhold 1999; Warner 1995), we estimate the
distance of HS 2214 to be
pc, where the error is dominated
by the uncertainty of the secondary's radius.
We first measured the radial velocity variation of
in the INT
spectra and in the CAFOS spectra taken with the R-100 grism, as well
as that of
in the B-100 CAFOS spectra by using the double
Gaussian method of Schneider & Young (1980). The Scargle
periodogram calculated from these measurements contained a peak near
5.5
,
but was overall of poor quality. In a second attempt,
we determined the
and
radial velocities by means of the
V/R ratios, calculated from having equal fluxes in the blue and red
line wing, fixing the width of the line to
2500
in order
to avoid contamination by the He I
6678 line adjacent
to
.
The Scargle periodogram calculated from these sets
of radial velocities contains the strongest signal at 6.6
and
an 1
alias of similar strength at 5.6
(see
Fig. 9, bottom panel). Based on the spectroscopy alone,
an unambiguous period determination is not possible.
A crucial clue in determining the orbital period of HS 2214 came from
the analysis of the two longest photometric time series obtained at
the Braeside Observatory in September 2000
(Fig. 6). These light curves display a double-humped
structure with a period of 4 h, superimposed by relatively
low-amplitude flickering. The analysis-of-variance periodogram
(AOV, Schwarzenberg-Czerny 1989) calculated from these two
light curves contains two clusters of signals in the range of
4-7
and 10-13
,
respectively (see
Fig. 15). The strongest peaks in the first cluster
are found at
5.58
and
5.92
and at
11.14
and
11.48
in the second
cluster. Based on the fact that two of the frequencies are
commensurate, we identify f1=5.58
and f2=11.14
as
the correct frequencies, with f1 being the fundamental and f2its harmonic. The periodogram of a faked data set computed from a
sine wave with a frequency of 5.58
,
evaluated at the times of
the observations and offset by the randomised observational errors
reproduces the alias structure observed in the periodogram of the data
over the range 4-7
very well (Fig. 15, top
panel). A two-frequency sine fit with
to the data
results in
f1=5.581(12)
.
The Braeside photometry folded over
that frequency displays a double-hump structure
(Fig. 16, two bottom panels). We identify f1 as
the orbital frequency of the system, hence,
min
based on the following arguments. (a) The fundamental frequency
detected in the photometry coincides with that of the second-strongest
peak in the periodogram determined from the
and
V/R-ratio
radial velocity measurements (Fig. 9, bottom
panel). (b) Double-humped orbital light curves are observed in a large
number of short-period dwarf novae, e.g. WX Cet
(Rogoziecki & Schwarzenberg-Czerny 2001), WZ Sge
(Patterson 1998), RZ Leo, BC UMa, MM Hya, AO Oct, HV Vir
(Patterson et al. 2003), HS 2331+3905
(Araujo-Betancor et al. 2005a), and HS 2219+1824
(Rodríguez-Gil et al. 2005a); the origin of those double-humps is not
really understood, but most likely associated with the accretion
disc/bright spot. In long-period dwarf novae, double-humped light
curves are observed in the red part of the spectrum caused by
ellipsoidal modulation of the secondary star, e.g. U Gem
(Berriman et al. 1983) or IP Peg (Martin et al. 1987; Szkody & Mateo 1986). In both cases, a strong and sometimes dominant,
signal at the harmonic of the orbital period is seen in the periodogram
calculated from their light curves.
Figure 10 (bottom panel) shows the radial velocity data folded over the photometric orbital period (258.02 min), along with a sine-fit (Table 5). The radial velocities are shown again in Fig. 16 together with the Braeside photometry, all folded using the photometric period but the spectroscopic zeropoint (Table 5). The photometric minima occur near orbital phase zero (inferior conjunction of the secondary) and 0.5, consistent with what is expected for ellipsoidal modulation. Very similar phasing is observed also for the double-humps in short-period systems, e.g. WZ Sge (Patterson 1980) shows maximum brightness close to phases 0.25 and 0.75. However, given the strong contribution of the secondary star to optical flux of HS 2214 (Fig. 14), and the fact that the filterless Braeside photometry is rather sensitive in the red, we believe that the origin of the double-hump pattern seen in HS 2214 is indeed ellipsoidal modulation.
The binary parameters of HS 2214 could be improved in a future study by a measurement of the radial velocity of the secondary star, e.g. using the Na doublet in the I band, and a determination of the orbital inclination from modelling the ellipsoidal modulation.
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Figure 14:
The average CAFOS spectrum of
HS 2214 (black line) along with the best-matching M-dwarf
template of spectral type M 2.5, scaled to fit the strength of the
molecular bands in HS 2214. The 2MASS
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Figure 15: Main panel: the analysis-of-variance (AOV) periodogram of HS 2214 calculated from the two longest light curves obtained at the Braeside Observatory, which show a double-humped pattern. Top panel: the AOV periodogram created from a sine wave with the orbital period of 258.02 min. |
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Figure 16:
The spectroscopic and
photometric data of HS 2214 are folded on the photometric period of
258.02 min using the spectroscopic zero-point
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Figure 17: Top panel: the orbital period distribution of known CVs and dwarf novae from Ritter & Kolb (2003, 7th edition, rev. 7.5, July 2005) are shown in gray and shade, respectively. Bottom panel: the period distribution of known dwarf novae according to their subtype, U Gem (UG), Z Cam (ZC), SU UMa (SU), WZ Sge (WZ), ER UMa (ER), and unclassified subtype (XX). The dashed lines are the conventional 2-3 h period gap. |
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Inspecting the Ritter & Kolb catalogue
(2003, edition 7.5 of July 1, 2005)
within the orbital period range of 1 h to
1 d
and removing AM CVn systems, it is found that nearly half of all
known CVs (262 systems out of 572, or 46%) are dwarf novae of which
166 (63%) have
h, 26 (10%) are found in the 2-3 h
orbital period gap, and 70 (27%) have long periods,
h. The conventional definition of the period gap as
being the range 2-3 h is somewhat arbitrary, and these numbers vary
slightly if a different definition is used, but without changing the
overall picture. Figure 17 (top panel) shows the
orbital period distribution of all known CVs and dwarf novae with
periods between
1 h and
1 d. Whereas the total
population of all CVs features the well-known period gap, i.e. the
relatively small number of CVs with periods 2 h
h, the
number of dwarf nova reaches a minimum in the range 3-4 h. In fact,
the number of dwarf nova with 3 h
h is a half (15, or
6% of all dwarf novae) of that in the "standard'' 2-3 h period
gap (26, or 10%). The dearth of known dwarf novae in the 3-4 h
period range was pointed out by Shafter et al. (1986) and
Shafter (1992), who compared the observed dwarf nova period
distribution with those constructed from various magnetic braking
models, and concluded that none of the standard magnetic braking
models can satisfactorily explain the lack of observed dwarf novae in
the 3-4 h period range.
The bottom panel of Fig. 17 displays all known dwarf
novae according to their subtypes which are 159 (61%) SU UMa, 37
(14%) U Gem, 18 (7%) Z Cam, and 48 (18%) unclassified subtypes
(XX). For completeness, we note that the SU UMa class includes 8
ER UMa stars (which have very short superoutburst cycles) and 19
WZ Sge stars (which have extremely long outburst cycles). All
confirmed U Gem and Z Cam stars lie above the period gap, in fact
all but one Z Cam star (BX Pup) have
h
. It is clearly
seen that the majority (85%) of SU UMa lie below the period gap and
only a small fraction (15%) inhabits the 2-3 h period
range
.
The orbital period distribution of short-period dwarf novae in
Fig. 17 (the majority of all CVs in this period
range) differs markedly from the predictions made by the standard CV
evolution theory (e.g. Kolb 1993; Howell et al. 2001; Kolb & Baraffe 1999): the minimum period is close to 77 min,
contrasting with the predicted minimum period of
65 min
(Paczynski & Sienkiewicz 1983), and the distribution of systems is
nearly flat in
,
whereas the theory predicts a substantial
accumulation of systems at the minimum period. Several modifications
of the CV evolution theory have been suggested to resolve this
discrepancy, however, none with indisputable success
(Renvoizé et al. 2002; King et al. 2002; Barker & Kolb 2003).
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Figure 18: Top panel: the orbital period distribution of 41 new CVs and 14 dwarf novae identified in HQS are shown in gray and shade, respectively. Bottom panel: the period distribution of HQS dwarf novae according to their subtype, U Gem (UG), Z Cam (ZC), SU UMa (SU), WZ Sge (WZ), and unclassified subtype (XX). The dashed lines are the conventional 2-3 h period gap. |
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Table 7: Dwarf novae discovered in the HQS with their subtype, U Gem (UG), SU UMa (SU), Z Cam (ZC), and unclassified (XX). Uncertain classifications are marked by a colon.
We have so far obtained orbital periods for 41 new CVs found in the HQS; their period distribution is shown in Fig. 18 (top panel). The first thing to notice is that the majority of the new CVs identified in the HQS are found above the period gap, with a large number of systems in the period range 3-4 h (for a discussion of the properties of CVs in this period range, see Aungwerojwit et al. 2005). As for the overall CV population, a dearth of systems is observed in the 2-3 h period range (Fig. 18, top panel), with the gap being wider for dwarf novae (Fig. 18, bottom panel).
To date 14 (26%) out of 53 new CVs discovered in the HQS have been
classified as dwarf novae, including the five systems, HS 0417,
HS 1016, HS 1340, HS 1857, and HS 2214, presented in this paper
(Table 7). The fraction of long-period (
h)
systems is larger in the HQS sample (43%) than in the total
population of known dwarf novae (27%, see Sect. 8.1).
The total number of new HQS dwarf novae is relatively small,
and subject to corresponding statistical uncertainties. However, the
tilt towards long-period dwarf novae among the new HQS CVs is likely
to be underestimated, as a significant number of long-period HQS CVs
have still uncertain CV subtypes, and several of them could turn out
to be additional a Z Cam-type dwarf nova
(Aungwerojwit et al. 2005 plus additional unpublished
data). Optical monitoring of the long-term variability of these
systems will be necessary to unambiguously determine their CV type.
Overall, the dwarf novae identified within the HQS fulfill the above
expectations of being "low-activity'' systems, i.e. dwarf novae that
have either infrequent outbursts (e.g. KV Dra, HS 0941+0411,
HS 2219+1824) or low-amplitude outbursts (e.g. EX Dra). We found
only one system that resembles the WZ Sge stars with their very long
outburst intervals found near the minimum period that is HS 2331+3905
(Araujo-Betancor et al. 2005a) which has a period of 81.1 min, and no
outburst has been detected so far.
Thus, our search for CVs in the HQS has been unsuccessful in identifying the predicted large number of short-period CVs, despite having a very high efficiency in picking up systems that resemble the typical known short-period dwarf novae.
Because of the large differences in mass transfer rates, and, hence,
absolute magnitudes, of long (
h) and short (
h)
period CVs, magnitude limited samples appear at a first glance utterly
inappropriate for the discussion of CV space densities. However,
taking the theoretical models at face value, the space density of long
period CVs is entirely negligible compared to that of short period CVs
(Howell et al. 1997; Kolb 1993), and hence a discussion of the total
CV space density can be carried out on the basis of short-period
systems alone. In the following, we assess the expected numbers of
systems in the HQS separately for short-period CVs that are still
evolving towards the minimum period (pre-bounce), and those that
already reached the minimum period, and evolve back to longer periods
(post-bounce). For both cases, we assumed (1) a space density of
as an intermediate value between
the predictions of de Kool (1992) and Politano (1996), (2)
that 70% of all CVs are post-bounce systems, and 30% are pre-bounce
systems (Howell et al. 1997; Kolb 1993) (ignoring, as stated above,
the small number of long-period CVs), (3) a scale height of 150 pc
(e.g. Patterson 1984), and (4) that the luminosity of
short-period CVs is dominated by the accretion-heated white dwarf.
For a complete assessment of the short-period content of the HQS, one
has obviously to include in the statistics the short-period CVs that
are contained within the HQS data base, but were already
known - subject to the same selection criteria that were applied to
identify the twelve new systems. Gänsicke et al. (2002) analysed
the properties of the previously known CVs within the HQS data base,
and came to the following conclusions. 18 previously known
short-period (
h) systems with HQS spectra are correctly
(re-)identified as CVs, including 12 dwarf novae, five polars, and one
intermediate polar
. Gänsicke et al. (2002) also found that only
two previously known short-period systems with HQS spectra failed to
be identified as CVs; this "hit rate'' of 90% underlines the extreme
efficiency of the HQS of finding short period CVs. Five out of those
18 systems have measured white dwarf temperatures, all of them in the
range
11 000-16 000 K (MR Ser, ST LMi, AR UMa, SW UMa,
T Leo: Hamilton & Sion 2004; Gänsicke et al. 2005,2001; Araujo-Betancor et al. 2005b). The remaining 13 systems
all have spectra dominated by strong Balmer and He emission,
suggesting accretion rates too high to detect the white dwarf.
In summary, the HQS contains a total of 30 short-period CVs (12 new identifications plus 18 previously known systems); all of which are consistent with being pre-bounce systems. At face value, this number agrees rather nicely with the 36 expected systems derived above, but one has to bear in mind that this number is an absolute lower limit, as hotter white dwarfs and/or accretion luminosity from the disc and hot spot will increase the volume sampled by the HQS.
While there may still be some shortfall of pre-bounce systems, it is
much more worrying that so far no systems with the clear signature of
a post-bounce CV that evolved significantly back to longer periods has
been found - neither in the HQS, nor elsewhere. The coldest CV white
dwarfs have been found, to our knowledge, in the polar EF Eri
(
K, Beuermann et al. 2000), and
HS 2331+3905 (
K,
Araujo-Betancor et al. 2005a), both systems with orbital periods of
81 min - which may hence be either pre- or post-bounce
systems.
A final note concerns the number of WZ Sge stars, i.e. short-period
dwarf novae with extremely long outburst intervals. Given the strong
Balmer lines in the known WZ Sge stars e.g. WZ Sge itself
(Gilliland et al. 1986), BW Scl (Abbott et al. 1997), GD 552
(Hessman & Hopp 1990), and GW Lib
(Szkody et al. 2000; Thorstensen et al. 2002), we believe that any
WZ Sge brighter than
would have easily been identified in the
HQS - yet, only a single new WZ Sge system has been discovered,
HS 2331+3905 (Araujo-Betancor et al. 2005a).
Thus, we conclude that while our systematic effort in identifying new CVs leads to a space density of pre-bounce short period CVs which agrees with the predictions within an order of magnitude, the bulk of all CVs, which are predicted to have made it past the minimum orbital period, remains unidentified so far.
Acknowledgements
A.A. thanks the Royal Thai Government for a studentship. B.T.G. and P.R.G. were supported by a PPARC Advanced Fellowship and a PDRA grant, respectively. M.A.P.T. is supported by NASA LTSA grant NAG-5-10889. R.S. is supported by the Deutsches Zentrum für Luft und Raumfahrt (DLR) GmbH under contract No. FKZ 50 OR 0404. A.S. is supported by the Deutsche Forschungsgemeinschaft through grant Schw536/20-1. The HQS was supported by the Deutsche Forschungsgemeinschaft through grants Re 353/11 and Re 353/22. We thank Tanya Urrutia for carrying out a part of the AIP observations. P.S. thanks Robert Mutel (University of Iowa) and his students for taking CCD images with the Rigel telescope. Tom Marsh is acknowledged for developing and sharing his reduction and analysis package MOLLY. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.
Based in part on observations collected at the Centro Astronómico Hispano Alemán (CAHA) at Calar Alto, operated jointly by the Max-Planck Institut für Astronomie and the Instituto de Astrofísica de Andalucía (CSIC); on observations made at the 1.2 m telescope, located at Kryoneri Korinthias, and owned by the National Observatory of Athens, Greece; on observations made with the IAC80 telescope, operated on the island of Tenerife by the Instituto de Astrofísica de Canarias (IAC) at the Spanish Observatorio del Teide; on observations made with the OGS telescope, operated on the island of Tenerife by the European Space Agency, in the Spanish Observatorio del Teide of the IAC; on observations made with the Isaac Newton Telescope, which is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the IAC; on observations made at the Wendelstein Observatory, operated by the Universitäts-Sternwarte München; on observations made with the 1.2 m telescope at the Fred Lawrence Whipple Observatory, a facility of the Smithsonian Institution; and on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
Table 2: Log of the observations.
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Figure 1:
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Table 3: Comparison stars used for the differential CCD photometry of HS 0417, HS 1016, HS 1340, HS 1857, and HS 2214, see Fig. 1.