Spectroscopic binaries among Hipparcos M giants I. Data, orbits, and intrinsic variations
Key Words.:binaries: spectroscopic - stars: late-type
Context:This paper is a follow-up on the vast effort to collect radial velocity data for stars belonging to the Hipparcos survey.
Aims:We aim at extending the orbital data available for binaries with M giant primaries. The data presented in this paper will be used in the companion papers of this series to (i) derive the binary frequency among M giants and compare it to that of K giants (Paper II) and (ii) analyse the eccentricity – period diagram and the mass-function distribution (Paper III).
Methods:Keplerian solutions are fitted to radial-velocity data. However, for several stars, no satisfactory solution could be found, even though the radial-velocity standard deviation is greater than the instrumental error, because M giants suffer from intrinsic radial-velocity variations due to pulsations. We show that these intrinsic radial-velocity variations can be linked with both the average spectral-line width and the photometric variability.
Results: We present an extensive collection of spectroscopic orbits for M giants with 12 new orbits, plus 17 from the literature. On top of these, 1 preliminary orbit yielded an approximate value for the eccentricity and the orbital period. Moreover, to illustrate how the large radial-velocity jitter present in Mira and semi-regular variables may easily be confused with orbital variations, we also present examples of pseudo-orbital variations (in S UMa, X Cnc, and possibly in HD 115521, a former IAU radial-velocity standard). Because of this difficulty, M giants involving Mira variables were excluded from our monitored sample. We finally show that the majority of M giants detected as X-ray sources are actually binaries.
Conclusions:The data presented in this paper considerably increase the orbital data set for M giants, and will allow us to conduct a detailed analysis of the eccentricity – period diagram in a companion paper (Paper III).
When a mass-losing M giant is present in a binary system, the interaction of the wind of the giant with the companion gives rise to photometric activity or spectroscopic symbiosis (like in symbiotic stars, in VV Cephei-like systems, or in low-mass X-ray binaries like V2116 Oph) that make the system very conspicuous even far away. However, if the M giant does not lose large amounts of mass, the binary nature of the star will not be as conspicuous. Combined with M giants often exhibiting pulsations that cause intrinsic velocity variations, thereby confusing the search for orbital variations, it explains why so few spectroscopic binaries involving M giants are known so far. Indeed, the Ninth Catalogue of Spectroscopic Binary Orbits (; Pourbaix et al. 2004) contains 2746 entries (query in March 2007), among which only 32 systems involve M giants, and yet 21 of these are either well-known symbiotic systems or VV-Cephei-like systems.
Carquillat and collaborators have devoted a series of papers to spectroscopic binaries of spectral types F to M, but only 2 binaries with primaries of spectral type MIII were studied (Carquillat & Ginestet 1996; Prieur et al. 2006). Previously, Stephenson (1967) provided a list of 7 systems with composite spectra involving an M star. But it is the paper by Hinkle et al. (2002) that, to the best of our knowledge, has so far provided the most extensive list of spectroscopic binaries involving non-symbiotic M giants.
With the present paper, we start a series devoted to a detailed study of the properties of spectroscopic binaries involving an MIII primary. The number of such binaries with known orbital elements has nearly doubled, as a result of our observing campaign of an extensive sample of M giants, drawn from the Hipparcos Catalogue, for which CORAVEL radial velocities have been obtained in a systematic way (Udry et al. 1997). The main driver behind this large database lies, of course, with the stellar kinematics in our Galaxy. And indeed the kinematical properties of the present sample of M giants have been fully analysed by Famaey et al. (2005) and Famaey et al. (2008). But this large data set may also be used to search for binaries.
The present paper presents the radial-velocity data (Sect. 2) and orbital elements (Sect. 4) of the newly-discovered spectroscopic binaries, for which a satisfactory orbit could be obtained. It also discusses the intrinsic variations sometimes mimicking orbital variations (Sect. 3). The list of new orbital elements is complemented with an exhaustive list of orbital elements for non-symbiotic M giants drawn from the literature (Table 8). In Paper II (Frankowski et al. 2009), we will use the observational information gathered in this paper to derive the frequency of spectroscopic binaries among M giants, and compare it with that of K giants. Paper III (Jorissen et al. 2009) will then present an in-depth analysis of the eccentricity–period diagram for M giants.
2 Radial-velocity data
The basic sample of M giants
is drawn from the Hipparcos survey stars
(identified by flag ’S’ in field H68 of the Hipparcos
catalogue; ESA 1997).
giants were extracted from the Hipparcos survey stars on the basis of the
spectral type provided in the Hipparcos catalogue and of the absolute
magnitude computed from the Hipparcos parallax and
magnitude. Mira stars or supergiants of luminosity class I (when
explicitly mentioned in the spectral classification) were not included
in the sample (notably because of the confusion that their envelope
pulsation may cause on the radial-velocity variations). This first
sample (defined here as sample I) contains 771
M giants with declinations greater than and corresponds
to the sample of northern M giants analysed in Famaey et al. (2005),
to which 65 M giants with declinations between 0 and have been added.
Two radial-velocity measurements, spanning at least one year, have been obtained with the CORAVEL spectrovelocimeter (Baranne et al. 1979) for all stars of sample I,
as part of a monitoring programme targeting
all Hipparcos survey stars later than about F (Udry et al. 1997).
Note that 22 objects of the sample of Famaey et al. (2005) are not present in sample I because they had only one radial
velocity measurement, making them unsuitable for
binarity analysis. Famaey’s sample was also screened for other irregularities, such as
wrong Hipparcos spectral type or mistaken identity
Subsamples of sample I have been subject to more intensive observing campaigns. Every third star from this sample has received a denser coverage, with (mostly) 4 instead of 2 measurements (7 stars received only 3 measurements), to achieve a better binary detection rate: this subsample of sample I is defined as sample II. Figure 1 displays the histograms of (the number of measurements per star), (average uncertainty of one measurement), and (time spanned by the measurements of a given star) for the 254 stars of sample II.
|Selection||2 measurements in Famaey et al. (2005)||1/3 of I||all km s from II||km s from II|
|Telescope||Swiss 1-m (OHP)||Swiss 1-m (OHP)||1.93-m (OHP)||1.93-m (OHP)|
Seven stars have .
Furthermore, 35 stars from sample II, suspected of being binaries (i.e., with a radial-velocity standard deviation km s at the end of the observing campaign of sample II) have been monitored with the ELODIE spectrograph (Baranne et al. 1996) at the Haute-Provence Observatory to derive their orbital elements. They make up sample III. At the end of the ELODIE monitoring, a late measurement was obtained for 157 stars from sample II with km s (this selection being mainly based on right ascension), in order to detect binaries with very long orbital periods. These constitute sample IV. A summary of the properties of these four samples is presented in Table 1.
The CORAVEL data were put on the ELODIE radial-velocity system to ensure homogeneity (Udry et al. 1999b). The uncertainty of one radial-velocity measurement is approximately 0.3 km s for CORAVEL measurements, but is better for ELODIE measurements. With the ELODIE single-fibre mode used during the present observing campaigns, it may be as good as 50 m s (Baranne et al. 1996). It was not measured in a systematic way; however, to fix the ideas, an accuracy of 0.2 km s has been associated with the ELODIE measurements in the data files.
|(km s)||(km s)||(km s)||(km s)|
The average sigma of a Gaussian fitted
to the cross-correlation profile, corrected for the instrumental width
(7 km s for CORAVEL at the Haute-Provence Observatory);
The flag in this column is the same as in Table 4.
The data for sample I (average velocity, radial-velocity standard
deviation, and binarity flag) may be found in Table A.1
|HD||JD2 400 000||Inst|
A flag identifying the spectrograph: COR = CORAVEL; ELO = ELODIE; CAM = Cambridge spectrovelocimeter
3 Binaries, intrinsic radial-velocity jitter, and pseudo-orbits caused by pulsation
3.1 Binarity diagnostic
The search for spectroscopic binaries (SBs) among M giants is made
difficult by the bulk mass motion existing in the atmospheres of these
stars (all M giants being variable to some extent;
e.g. Eyer & Grenon 1997; Jorissen et al. 1997; Soszyński et al. 2004), since such motion triggers
some intrinsic radial-velocity jitter
In a first step, to flag a star as a binary in samples II, III, and IV, we therefore rely solely on the visual examination of the radial-velocity variations, and whether or not it is possible to obtain a meaningful orbital solution. The binarity diagnostic is then complemented by two criteria, described in detail in Sects. 3.1.1 and 3.1.2: (i) the location of the star in a diagram (Fig. 2), where denotes the intrinsic width of spectral lines (Sect. 3.1.1), and (ii) its location in a diagram (Fig. 3), where is the standard deviation of the Hipparcos magnitude (Sect. 3.1.2). The final binarity diagnostic for all stars from sample III (and for stars from sample IV, which are SB or suspected SB) is listed in Table 4 according to the following categories:
“ORB” : a satisfactory orbit could be computed (see Fig. 4);
“ORB:” : the orbit is preliminary, because the number of data points or the time coverage are not large enough, or two different solutions are possible (see Fig. 4);
“SB” : the star is a spectroscopic binary, but there are not enough data points to even compute a preliminary orbit (see Fig. 5);
“SB / jitter?” : it is not clear whether the radial velocity variations are of intrinsic or extrinsic nature (see Fig. 7): the star falls close to the dividing line in the – diagram (Fig. 2).
The radial-velocity variations (of intrinsic nature) of non-SB stars of sample III are plotted in Fig. 8.
Intrinsic width of spectral lines
We note that the parameter , measuring the intrinsic width of spectral lines, provides useful guidance in distinguishing radial-velocity jitter from orbital motion. This parameter is defined as , where is the standard deviation of a Gaussian fitted to the CORAVEL cross-correlation dip (see Baranne et al. 1979) and the instrumental width (7 km s for CORAVEL at the Haute-Provence Observatory; for details see Jorissen & Mayor 1988; Van Eck & Jorissen 2000, also Paper II). Indeed, Fig. 2 reveals that stars for which no orbital solution could be found (open squares) have radial-velocity standard deviations that increase as increases. In Paper II, we will show that correlates closely with the stellar radius. We thus foresee that radial-velocity variations in stars falling well below the dashed line in Fig. 2 are most likely of intrinsic (rather than orbital) origin. Of course, binaries with an orbit seen almost face on, or with a long period, or insufficiently sampled, may also fall below the dashed line. Let us stress that the slope of this dividing line in Fig. 2 can be influenced by both the number of radial-velocity data points for a given object and the total number of objects in the sample (see Sect. 2.1 of Paper II).
Examples of radial-velocity variations for such stars from sample III, falling below the dividing line in Fig. 2, are plotted in Fig. 8, and it is clear that no orbital solution can be found for them. On the other hand, stars along the dashed line, whose velocity variations are plotted in Fig. 7, could either be SB or exhibit radial-velocity jitter. These 10 stars are listed in Table 4c.
On the other hand, among stars from samples III and IV, for which 5 or more measurements have been made, 22 certain spectroscopic binaries have been found, as listed in Table 4a. Of those, only 3 (HD 89758, HD 108907, and HD 132813) were previously known to be spectroscopic binaries, and a new satisfactory orbit could be computed for 12 of them (with the help of supplementary data points from the Cambridge spectrovelocimeter for HD 182190 and HD 220088; see Table 3). The orbital elements are presented in Sect. 4. The radial-velocity data points of the binary stars are displayed in Fig. 4 for those binaries with an orbit available (labelled in Table 4 as ORB or, for preliminary solutions, ORB:), and in Fig. 5 for the SBs without orbits. On top of the firm binaries, 5 stars were identified whose radial-velocity variations are very likely orbital (listed in Table 4b and displayed in Fig. 6).
a. Spectroscopic binaries (marked as black circles in Figs. 2 and 3)
|(d)||(km s)||(km s)||(km s)||(mag)||(d)|
|111129||10||3633||M2III||6.81||0.23||4.20||ORB||BY CVn *||Irr||0.070|
|165374||37||7349||M2III||5.03||0.33||3.61||ORB||V980 Her *||Irr||0.031|
|212009||9||5008||M0III||4.72||0.23||3.66||ORB||KT Aqr *||0.028|
|134627||5||3922||M0||1.82||0.28||3.31||SB||FF Boo *||0.031|
An asterisk in this column means that the variability
of the star has been discovered by Hipparcos.
HD 89758, HD 132813: an orbit is also available in the literature, as listed in Table 8.
HD 219215: Preliminary orbital period: 2500 d
b. Suspected binaries (marked as black triangles in Figs. 2 and 3)
|(d)||(km s)||(km s)||(mag)||(d)|
c. Binarity doubtful (marked as crosses in Figs. 2 and 3)
|153698||12||4209||M4III||0.86||4.09||SB + jitter?||III||*||0.033|
d. Non-SB (radial-velocity jitter) (marked as open squares in Figs. 2 and 3)
|6262||9||3702||M3III||1.04||4.51||V360 And *||SR||0.066|
This column specifies whether the
binarity suspicion resulted from campaign III or IV (see
HD 24693 and HD 66875: Orbital solutions with an eccentricity of about 0.5 and periods of and d, respectively, are possible, but their reality is questionable. The stars are irregular (Lb) variables (varying from to 7.26 and 5.94 to 6.11, respectively, in the Hipparcos catalogue) falling right on the dividing line in Fig. 2.
HD 129902 and HD 149165 are probably spectroscopic binaries, given their location in Fig. 2 just above the dashed line. Unfortunately, the radial-velocity data presented in Fig. 6 are too scarce to confirm that conclusion.
HD 189063: Orbital period larger than 3600 d
Although Mira stars have been excluded from our sample, some semi-regular variables are nevertheless present. Both classes of variables often exhibit pseudo-orbital variations caused by shock waves associated with the envelope pulsation (Udry et al. 1998; Hatzes & Cochran 1998; Wood 2000; Hinkle et al. 2002; Setiawan et al. 2004; Derekas et al. 2006; Soszyński 2007; Hekker et al. 2008). For semi-regular variables, Hinkle et al. (2002) obtain semi-amplitudes between 1.6 and 3.1 km s, whereas for Miras the semi-amplitudes may reach 20 km s in the most extreme cases (Alvarez et al. 2001). In terms of standard deviations, these values become 1.1, 1.7, and 14 km s, respectively (remember that for sinusoidal variations, ). Semi-regular and Mira variables may thus be expected to exhibit values anywhere in the range of 1 to about 14 km s.
Moreover, the radial-velocity curves of these stars may often be fitted by a Keplerian orbit with a period of a few hundred days (Udry et al. 1998; Hinkle et al. 2002; Wood et al. 2004; Lebzelter et al. 2005). However, it happens that this Keplerian solution fits the data for 4 to 10 cycles, and then becomes invalid. Two illuminating examples of this kind of behaviour are discussed in the Appendix for stars that do not belong to the samples considered in this paper (the Mira S star S UMa and the semiregular carbon star X Cnc). If the time span of the radial-velocity monitoring is not long enough (i.e., shorter than the 4 to 10 cycles mentioned above), the inadequacy of the Keplerian solution may not be noticed, thus leading to the erroneous suspicion of binarity.
It is therefore very important to check that the Keplerian solutions proposed in Sect. 4 hereafter are valid, by eliminating the possibility that they have an intrinsic origin, as often observed for Mira and semi-regular variables. For this purpose, we collected from the literature the photometric properties of all the stars listed in Table 4 (including those flagged as having ‘radial-velocity jitter’, among which we should expect to find a large fraction of photometric variables). We searched the Hipparcos Variability Annex, which has the advantage of being an unbiased information source containing all our stars. The results are plotted in Fig. 3 [– diagram], and listed in Table 4. As we can see, all stars flagged as spectroscopic binaries (Fig. 3), have much larger radial-velocity standard deviations than expected from the relation between radial velocity and photometric variability for single stars (as reported by Hinkle et al. 1997). We also see that this relation exhibits some scatter (Fig. 3), and that stars flagged as ‘SB/jitter?’ define a rough dividing curve between intrinsic and extrinsic radial velocity variations in the – diagram.
In the column ‘Var’ of Table 4, we see that almost all stars later than M3 are semi-regular (SR) variables, as expected. It is very clear that the fraction of SR variables with mag increases among stars with (or suspected of having) radial-velocity jitter. A specific case (HD 114961, marked as a suspected binary ‘SB?’ in Table 4) will be discussed in Sect. 3.3. Such stars are not very numerous among the ones flagged as SB. Therefore, one can be confident that all the stars flagged as SB in Table 4a are indeed binaries. Only two among those are semi-regular variables with large photometric amplitudes (i.e., HD 16058 = 15 Tri and HD 132813 = RR UMi), and there are good arguments in favour of their binary nature. HD 16058 is a newly flagged spectroscopic binary, but it is an X-ray source. As we show in Sect. 3.2, X-ray detection in M giants is a strong indication of binarity. The binary nature of HD 132813 has already been claimed by Dettmar & Gieseking (1983) and Batten & Fletcher (1986), who obtained consistent orbital parameters (Table 8). Our recent radial-velocity measurements are consistent with these orbital parameters (see Fig. 9), thus clearly demonstrating the binary nature of HD 132813 from the stability of the Keplerian solution.
3.2 X-ray emission as binarity diagnostic
X-rays are normally not observed in single M giants lying to the right of the so-called dividing line, an almost vertical boundary in the HR diagram separating stars with hot coronae emitting X-rays (to the left) from stars with high mass loss (to the right), which are normally not X-ray emitters (Hünsch et al. 1998). Since X-rays may be generated by several physical processes in a binary system, their detection in an M giant is a strong argument in favour of its binary nature. First, X-rays may be produced at the shocks resulting from the collision of streams in the complex flow pattern associated with wind accretion in a detached binary system involving an AGB star (Theuns & Jorissen 1993; Theuns et al. 1996; Mastrodemos & Morris 1998; Jahanara et al. 2005). Second, X-rays are generated when the gravitational energy of the M giant wind falling in the potential well of the companion star is converted into radiative energy when hitting the stellar surface. The accretion luminosity will either be radiated away in the form of hard X-rays if the infalling matter is optically thin; or if that matter is optically thick, half will be converted into thermal energy and half will be radiated away in the form of blackbody radiation (according to the virial theorem).
A search for X-ray sources among M giants is therefore an efficient way of finding binary systems. The ROSAT all-sky survey of X-ray sources detected only 11 out of 482 M giants of luminosity classes I to III from the Bright Star Catalogue (Hünsch et al. 1998). They are listed in Table 5, along with a comment regarding the binary nature. These few detections justify using radial-velocity variations to detect binaries among M giants in our paper.
|750||16058||15 Tri||M3 III||SB|
|2216||42995||Gem||M3 III||ORB + visual GV comp.|
|3013||62898||Gem||M1 III||X-ray offset|
|4765||108907||4 Dra||M4 III||ORB|
|5512||130144||-||M5 IIIab||Vr constant?|
|5589||132813||RR UMi||M4.5 III||ORB - X-ray offset|
|6200||150450||42 Her||M2.5 IIIab|
|6374||155035||-||M1-2 III||X-ray offset|
|6406||156014||Her||M5 Ib-II||visual GV companion|
|8992||222800||R Aqr||M7 IIIpe||SB (symbiotic)|
It may be seen from Table 5 that, in most cases, the M giants detected as X-ray sources are flagged as binaries (4 from the present work, 1 from the literature, and 1 symbiotic). In three cases (HD 62898, HD 132813, and HD 155035), the X-ray source is offset by more than 1’ from the optical position of the giant, which casts doubts on the M giant being the source of the X-rays (see Hünsch et al. 1998, for details). In two other cases, there is a visual G-type companion, where X-rays may arise from coronal emission. Thus only HD 130144 and HD 150450 have no satisfactory explanation for the origin of the X-rays. In Fig. 3, it is HD 130144 that appears amidst the non-binary M giants.
3.3 Special cases
Since semi-regular and Mira variables may be expected to exhibit values anywhere in the range from 1 to about 14 km s, the value km s observed for the semi-regular variable HD 114961 (SW Vir) in sample II is not incompatible with intrinsic variations (although we flagged it as a suspected binary; indeed, HD 114961 is the triangle in Fig. 2 with the largest for km s). Let us note, however, that the radial-velocity data available for this star are unfortunately too scarce to infer any periodicity, so no firm conclusion can be reached at this point regarding the intrinsic or orbital origin of the large radial-velocity scatter exhibited by SW Vir.
HD 115521 is an interesting case, similar to those discussed in the appendix. It belongs to sample I (and therefore does not appear in Table 4 since it has only been measured twice in our observing campaign), but being a radial-velocity standard star till the 1990s (Udry et al. 1999a), it was measured very frequently and turned out in the first place to be variable with a small amplitude ( km s) and a period around 500 d (Duquennoy & Mayor 1991). The 127 measurements are listed in Table 6, only available electronically at the CDS, Strasbourg. Later on, variations on a much longer time scale became apparent, exceeding the measurements’ time span of 6358 d. The orbital period therefore cannot be determined with good accuracy. Moreover, owing to this insufficient sampling of the orbital cycle, the value adopted for the orbital period strongly influences the value derived for the eccentricity. Table 7 lists the (pseudo-)orbital elements used to draw the radial-velocity curve of Fig. 10. The high uncertainties on the elements of the long-period orbit should serve as a reminder that these elements are very uncertain. Only lower bounds to the orbital period and the eccentricity are therefore listed in Table 8.
The properties of the short-period variations would imply
a rather low mass for the companion: assuming a mass of
1.3 for the giant, the minimum mass for the companion is
0.054 , corresponding to a brown dwarf.
It is not entirely clear whether the short-period variations are
indeed due to an orbital motion, for several reasons. First, as for
S UMa and X Cnc discussed in the Appendix, the data deviate from the Keplerian
solution after a dozen cycles, and this is very clearly seen in
Fig. 10, where the first data points do not fall on the
solution defined by later measurements.
and km s (Table 7),
the short-period variations of HD 115521 fall on the ( being the semi-amplitude of the radial-velocity variations)
relationship as defined by Hekker et al. (2008) for K giants
However, if the shorter-period radial-velocity variations are intrinsic, then one expects photometric variations with a period of 475 d; unfortunately, we could not find any mention of them, in either the Catalogue of Suspected Variable Stars, where HD 115521 is entry NSV 6173, or in the Hipparcos Photometry Annex, or in the ASAS Catalogue of Variable Stars (Pojmański 2002).
4 Orbital elements of newly-discovered binaries
The complete set of orbital elements for the 12 newly discovered binaries are listed in Table 8. Figure 11 presents the phase diagrams for those firm orbital solutions. The second part of Table 8 provides a preliminary period and eccentricity for the binary with not enough data points to derive meaningful orbital solutions. For the sake of completeness, the last part of Table 8 collects periods, eccentricities, and mass functions for (non-symbiotic) M giants available in the literature, or kindly communicated by R. Griffin. This combined data set will be used in Paper III to discuss general properties (like the eccentricity–period diagram) of systems involving M giant primaries. It must be stressed that Table 8 includes orbits neither for symbiotics nor for VV-Cephei-like systems (VV Cep, AZ Cas, etc.). A list of orbital elements for the former may be found in Belczyński et al. (2000) and Mikołajewska (2003). Mikołajewska (2007) and Fekel et al. (2007) provide references for the most recent symbiotic orbits.
|(km s)||(d)||(d)||()||(JD 2 400 000)||()||(km s)||(km s)||( km)|
Orbits from the literature
|9053||M0III||193.8||0.0||0.083||Phe: Luyten (1936)|
|42995||M3III||2983||0.53||0.13||Gem: McLaughlin & van Dijke (1944)|
|89758||M0III||230.089||0.061||0.01||UMa: Jackson et al. (1957); Lucy & Sweeney (1971)|
|108815||M||Griffin, priv. comm.|
|111307||M0||0:||Griffin, priv. comm.|
|115521||A+a||(5), revised but orbital nature doubtful (Sect. 3.3.2)|
|126947||M3III||2812.3||0.432||0.045||Prieur et al. (2006)|
|132813||M4.5III||748.9||0.13||0.0043||RR UMi (SRb, d):|
|Dettmar & Gieseking (1983); Batten & Fletcher (1986)|
|147395||M2III||335.5||0.24||0.154||Carquillat & Ginestet (1996)|
|187076||M2II+late B||Griffin, priv.comm.|
|Sge: A Aur/VV Cep-like system (Reimers & Schroeder 1983)|
Remarks: (1) this work (2) Reimers et al. (1988) (3) combined solution (see text)
(4) SS Lep: M4III + accreting A1 star (Welty & Wade 1995). Verhoelst et al. (2007) shows, from interferometric measurements of the M-giant radius, that the giant fills its Roche lobe (see also Paper III)
(5) Possibly a triple system,
formerly a radial-velocity standard star;
Duquennoy & Mayor (1991) found a preliminary 509 d period for the inner pair, but the
orbital nature of the short-period variations is questionable (Sect. 3.3.2)
(6) HD 190658 = V1472 Aql = HIP 98954: semiregular or most likely
eclipsing or ellipsoidal variable with d, almost
exactly half the orbital period (Samus 1997). Orbital elements
from Lucke & Mayor (1982). A (physical?) companion is present at
2.3” (Tokovinin 1997; Frankowski et al. 2007)
For HD 108907 (4 Dra = CQ Dra), Table 8 lists three orbital solutions. The first entry is obtained with our own CORAVEL and ELODIE data alone. The second entry is a solution computed by Reimers et al. (1988), based on their 57 recent data points plus 14 much older ones. The third orbit has been computed by merging our 15 data points with the 57 Cambridge/CORAVEL/Victoria data points from Reimers et al. (1988), and this combined solution is presented in Fig. 12. This system is of special interest, since Reimers (1985) and Reimers et al. (1988) argued that the companion of the red giant is a cataclysmic variable, because International Ultraviolet Explorer spectra revealed a steep rise shortward of 140 nm along with broad lines (full widths of 1000 km s) of highly excited species like He II and C IV. That conclusion has been challenged, however, by more recent studies (Wheatley et al. 2003; Skopal 2005a, b) based on ROSAT X-ray observations. They conclude instead that the companion is a single WD accreting from the wind of its red giant companion, as in normal symbiotic systems. The residual radial-velocity jitter of 0.6 km s (listed as (O-C) in Table 8) appears normal for a star with km s, as seen from Fig. 2.
Acknowledgements.The authors have the pleasure of thanking Roger Griffin for his generous donation of unpublished RV measurements for HD 182190 and HD 220088, which made it possible to compute their orbits. We are also indebted for his permission to quote in Table 5 several of his new orbits of M giants prior to their publication and for his helpful comments on the manuscript of this paper. We thank the referee, F. Fekel, whose comments greatly improved the paper, and in particular stimulated the addition of Fig. 3. This work has been partly funded by an Action de recherche concertée (ARC) from the Direction générale de l’Enseignement non obligatoire et de la Recherche scientifique – Direction de la recherche scientifique – Communauté française de Belgique.
Appendix A Pseudo-orbits among Mira and semiregular variables
This Appendix presents two cases of (suspected) pseudo-orbital variations exhibited by Mira and semi-regular variables. These stars do not belong to the samples studied earlier in this paper.
a.1 Hd 110813
HD 110813 (S UMa) is a Mira S star with a light cycle of 225.9 d (as listed in the General Catalogue of Variable Stars – GCVS; the analysis below shows that a period of 222 d seems more appropriate), and was considered a spectroscopic binary of period d by Udry et al. (1998). It deserves a follow-up discussion here, since recent datapoints no longer support this orbital solution; in fact, no satisfactory fit can be found to the radial-velocity data. This star provides a good illustration of the difficulties encountered while trying to find spectroscopic binaries among long-period variable stars.
Figure 13 shows the radial-velocity curve of S UMa and a (pseudo-)orbital solution based on 17 measurements (from 1987.946 to 2002.464 or JD 2 447 141.743 to JD 2 452 444.403; Tables 9 and 10). This pseudo-orbit is slightly different from the one found by Udry et al. (1998). Although the radial-velocity data could be fitted with a period of 576 d for 10 cycles, the last two measurements (JD 2 452 824.356 and JD 2 453 048.562) deviate markedly from this solution. The radial-velocity variations cannot therefore be ascribed to orbital motion. In any case, a system with such a short orbital period cannot be detached. Using the period–radius relationship for Mira stars pulsating in the fundamental mode (van Leeuwen et al. 1997), a radius of 258 is inferred from the 222-d period, assuming a mass of 1.5 . Adopting a mass of 1 for the companion, for the Roche radius to be larger than the stellar radius requires an orbital period of at least 1130 d, which is inconsistent with the observed value of 576 d.
What then is the origin of this 576 d period? The Stellingwerf (phase-dispersion minimisation) statistics (Stellingwerf 1978) are shown in Fig. 14, constructed from all datapoints but the last two outliers. It shows that all the prominent peaks are combinations of the Mira frequency d and of the yearly frequency d, or harmonics of . In particular the 576 d period may be identified with the frequency . This finding, along with the previous result for the minimum period allowed by the Roche radius, definitely denies the reality of the binary nature of HD 110813. Alvarez et al. (2001) have shown that S UMa exhibits an asymmetric cross-correlation dip, as usual among Mira variables. Asymmetric profiles observed in Mira variables are often associated with radial-velocity variations, which indeed mimick an orbital motion (see also Hinkle et al. 2002).
a.2 Hd 76221
The semiregular carbon star HD 76221 (X Cnc) behaves similarly to HD 110813 (Udry et al. 1998): a satisfactory (pseudo-)orbital solution with a period of 530 d (Table 9) could be found with the first 13 data points, but is not confirmed by the last two data points (bottom panel of Fig. 13). The phase-dispersion minimisation statistics (Fig. 15, based on the first 13 data points) reveals several harmonics of the 195 d photometric period, but this time, the 530-d periodicity of the radial velocities does not seem to be one of these. This 530-d-signal may be yet another example of the long secondary periods (of unknown origin) found by Houk (1963) (see also Hinkle et al. 2002) among SR variables, since the ranges of periods, mass functions, and semi-amplitudes found by Hinkle et al. (2002) (and listed in Table 9) all match the values for HD 76221. Only the eccentricity does not conform to the Hinkle et al. range (0.32 – 0.37, with one case at 0.08). Soszyński (2007) also notes that the long secondary periods sometimes undergo phase shifts; however, we do not find it very plausible that these photometric and spectroscopic phase shifts have the same physical origin. The phase shifts in the light-curve are attributed by Soszyński (2007) to dust clouds in the vicinity of a companion, whereas the phase shifts in radial velocity preclude the orbital nature of the radial velocity variations.
|HD 110813||HD 76221||LSP|
|’’ (d)||300 – 1000|
|0||0.08, 0.32 – 0.37|
|()||–||240 – 320|
|(JD 2 400 000)|
|(km s)||1.6 – 3.1|
The ranges found by Hinkle et al. (2002) for semi-regular variables with long secondary periods.
|JD 2 400 000||Instr.|
|(km s)||(km s)||(km s)|
- thanks: Based on observations carried out at the Swiss telescope installed at the Observatoire de Haute Provence (OHP, France), and at the 1.93-m OHP telescope
- thanks: Tables 2, 3, and 6 are only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/
- The only mistake found in Famaey et al. (2005) was the star HIP 26247 = RR Cam = BD +72275, which was wrongly assigned radial velocity measurements from the binary star J275 in the Hyades cluster. The former star should therefore be discarded from the CORAVEL sample.
- As a result of the confusion between HIP 26247 and a binary star (see footnote 1), the star HIP 26247 is erroneously flagged as a binary in that table.
- A term introduced by Gunn & Griffin (1979) in this context.
- Mayor et al. (1984) have shown that stars located at the tip of the giant branch in the globular cluster 47 Tuc have a jitter of km s, while the jitter reduces to 0.27 km s for 1 mag-fainter stars. This trend goes further down the red-giant branch, as shown with much higher accuracy levels by Setiawan et al. (2004) and da Silva et al. (2006).
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