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Mid-infrared Period-luminosity Relations of RR Lyrae Stars Derived from the WISE Preliminary Data Release
Interstellar dust presents a significant challenge to extendingparallax-determined distances of optically observed pulsationalvariables to larger volumes. Distance ladder work at mid-infraredwavebands, where dust effects are negligible and metallicitycorrelations are minimized, has been largely focused on few-epochCepheid studies. Here we present the first determination of mid-infraredperiod-luminosity (PL) relations of RR Lyrae stars from phase-resolvedimaging using the preliminary data release of the Wide-field InfraredSurvey Explorer (WISE). We present a novel statistical framework topredict posterior distances of 76 well observed RR Lyrae that uses theoptically constructed prior distance moduli while simultaneouslyimposing a power-law PL relation to WISE-determined mean magnitudes. Wefind that the absolute magnitude in the bluest WISE filter is MW1 = (- 0.421 ± 0.014) - (1.681 ±0.147)log10(P/0.50118 day), with no evidence for acorrelation with metallicity. Combining the results from the threebluest WISE filters, we find that a typical star in our sample has adistance measurement uncertainty of 0.97% (statistical) plus 1.17%(systematic). We do not fundamentalize the periods of RRc stars toimprove their fit to the relations. Taking the Hipparcos-derived meanV-band magnitudes, we use the distance posteriors to determine a newoptical metallicity-luminosity relation. The results of this analysiswill soon be tested by Hubble Space Telescope parallax measurements and,eventually, with the GAIA astrometric mission.
| Random forest automated supervised classification of Hipparcos periodic variable stars
We present an evaluation of the performance of an automatedclassification of the Hipparcos periodic variable stars into 26 types.The sub-sample with the most reliable variability types available in theliterature is used to train supervised algorithms to characterize thetype dependencies on a number of attributes. The most useful attributesevaluated with the random forest methodology include, in decreasingorder of importance, the period, the amplitude, the V-I colour index,the absolute magnitude, the residual around the folded light-curvemodel, the magnitude distribution skewness and the amplitude of thesecond harmonic of the Fourier series model relative to that of thefundamental frequency. Random forests and a multi-stage scheme involvingBayesian network and Gaussian mixture methods lead to statisticallyequivalent results. In standard 10-fold cross-validation (CV)experiments, the rate of correct classification is between 90 and 100per cent, depending on the variability type. The main mis-classificationcases, up to a rate of about 10 per cent, arise due to confusion betweenSPB and ACV blue variables and between eclipsing binaries, ellipsoidalvariables and other variability types. Our training set and thepredicted types for the other Hipparcos periodic stars are availableonline.
| The luminosities and distance scales of type II Cepheid and RR Lyrae variables
Infrared and optical absolute magnitudes are derived for the type IICepheids κ Pav and VY Pyx using revised Hipparcos parallaxes andfor κ Pav, V553 Cen and SW Tau from pulsational parallaxes.Revised Hipparcos and HST parallaxes for RR Lyrae agree satisfactorilyand are combined in deriving absolute magnitudes. Phase-corrected J, Hand Ks mags are given for 142 Hipparcos RR Lyraes based onTwo-Micron All-Sky Survey observations. Pulsation and trigonometricalparallaxes for classical Cepheids are compared to establish the bestvalue for the projection factor (p) used in pulsational analyses.The MV of RR Lyrae itself is 0.16 +/- 0.12 mag brighter thanpredicted from an MV-[Fe/H] relation based on RR Lyrae starsin the Large Magellanic Cloud (LMC) at a modulus of 18.39 +/- 0.05 asfound from classical Cepheids. This is consistent with the prediction ofCatelan & Cortés that it is overluminous for its metallicity.The results for the metal- and carbon-rich Galactic disc stars, V553 Cenand SW Tau, each with small internal errors (+/-0.08 mag) have a meandeviation of only 0.02 mag from the period-luminosity (PL) relationestablished by Matsunaga et al. for type II Cepheids in globularclusters and with a zero-point based on the same LMC-scale. Comparingdirectly the luminosities of these two stars with published data on typeII Cepheids in the LMC and in the Galactic bulge leads to an LMC modulusof 18.37 +/- 0.09 and a distance to the Galactic Centre of R0= 7.64 +/- 0.21kpc. The data for VY Pyx agree with these results withinthe uncertainties set by its parallax. Evidence is presented thatκ Pav may have a close companion and possible implications of thisare discussed. If the pulsational parallax of this star is incorporatedin the analyses, the distance scales just discussed will be increased by~0.15 +/- 0.15 mag. V553 Cen and SW Tau show that at optical wavelengthsPL relations are wider for field stars than for those in globularclusters. This is probably due to a narrower range of masses in thelatter case.
| Proper identification of RR Lyrae stars brighter than 12.5 mag
RR Lyrae stars are of great importance for investigations of Galacticstructure. However, a complete compendium of all RR-Lyraes in the solarneighbourhood with accurate classifications and coordinates does notexist to this day. Here we present a catalogue of 561 local RR-Lyraestars (V_max ≤ 12.5 mag) according to the magnitudes given in theCombined General Catalogue of Variable Stars (GCVS) and 16 fainter ones.The Tycho2 catalogue contains ≃100 RR Lyr stars. However, manyobjects have inaccurate coordinates in the GCVS, the primary source ofvariable star information, so that a reliable cross-identification isdifficult. We identified RR Lyrae from both catalogues based on anintensive literature search. In dubious cases we carried out photometryof fields to identify the variable. Mennessier & Colome (2002,A&A, 390, 173) have published a paper with Tyc2-GCVSidentifications, but we found that many of their identifications arewrong.
| RR Lyrae stars: kinematics, orbits and z-distribution
RR Lyrae stars in the Milky Way are good tracers to study the kinematicbehaviour and spatial distribution of older stellar populations. Arecently established well documented sample of 217 RR Lyr stars withV<12.5 mag, for which accurate distances and radial velocities aswell as proper motions from the Hipparcos and Tycho-2 catalogues areavailable, has been used to reinvestigate these structural parameters.The kinematic parameters allowed to calculate the orbits of the stars.Nearly 1/3 of the stars of our sample have orbits staying near the MilkyWay plane. Of the 217 stars, 163 have halo-like orbits fulfilling one ofthe following criteria: Θ < 100 km s-1, orbiteccentricity >0.4, and normalized maximum orbital z-distance>0.45. Of these stars roughly half have retrograde orbits. Thez-distance probability distribution of this sample shows scale heightsof 1.3±0.1 kpc for the disk component and 4.6±0.3 kpc forthe halo component. With our orbit statistics method we found a(vertical) spatial distribution which, out to z=20 kpc, is similar tothat found with other methods. This distribution is also compatible withthe ones found for blue (HBA and sdB) halo stars. The circular velocityΘ, the orbit eccentricity, orbit z-extent and [Fe/H] are employedto look for possible correlations. If any, it is that the metal poorstars with [Fe/H] <1.0 have a wide symmetric distribution aboutΘ=0, thus for this subsample on average a motion independent ofdisk rotation. We conclude that the Milky Way possesses a halo componentof old and metal poor stars with a scale height of 4-5 kpc having randomorbits. The presence in our sample of a few metal poor stars (thus partof the halo population) with thin disk-like orbits is statistically notsurprising. The midplane density ratio of halo to disk stars is found tobe 0.16, a value very dependent on proper sample statistics.
| Stars with the Largest Hipparcos Photometric Amplitudes
A list of the 2027 stars that have the largest photometric amplitudes inHipparcos Photometry shows that most variable stars are all Miras. Thepercentage of variable types change as a function of amplitude. Thiscompilation should also be of value to photometrists looking forrelatively unstudied, but large amplitude stars.
| Kinematics of Metal-poor Stars in the Galaxy. II. Proper Motions for a Large Nonkinematically Selected Sample
We present a revised catalog of 2106 Galactic stars, selected withoutkinematic bias and with available radial velocities, distance estimates,and metal abundances in the range -4.0<=[Fe/H]<=0.0. This updateof the 1995 Beers & Sommer-Larsen catalog includes newly derivedhomogeneous photometric distance estimates, revised radial velocitiesfor a number of stars with recently obtained high-resolution spectra,and refined metallicities for stars originally identified in the HKobjective-prism survey (which account for nearly half of the catalog)based on a recent recalibration. A subset of 1258 stars in this cataloghave available proper motions based on measurements obtained with theHipparcos astrometry satellite or taken from the updated AstrographicCatalogue (second epoch positions from either the Hubble Space TelescopeGuide Star Catalog or the Tycho Catalogue), the Yale/San Juan SouthernProper Motion Catalog 2.0, and the Lick Northern Proper Motion Catalog.Our present catalog includes 388 RR Lyrae variables (182 of which arenewly added), 38 variables of other types, and 1680 nonvariables, withdistances in the range 0.1 to 40 kpc.
| CCD Photometry of the Globular Cluster ω Centauri. I. Metallicity of RR Lyrae Stars from CABY Photometry
We present new measurements of the metallicity of 131 RR Lyrae stars inthe globular cluster ω Centauri, using the hk index of the Cabyphotometric system. The hk method has distinct advantages over ΔSand other techniques in determining the metallicity of RR Lyrae starsand has allowed us to obtain the most complete and homogeneousmetallicity data to date for the RR Lyrae stars in this cluster. For RRLyrae stars in common with the ΔS observations of Butler, Dickens,& Epps and Gratton, Tornambe, & Ortolani, we have found that ourmetallicities, [Fe/H]hk, deviate systematically from theirΔS metallicity, while our [Fe/H]hk for well-observed,field RRab stars are consistent with previous spectroscopicmeasurements. We conclude that this is because of the larger errorsassociated with the previous ΔS observations for this cluster. TheMV(RR)-[Fe/H] and period shift-[Fe/H] relations obtained fromour new data are consistent with the evolutionary models predicted byY.-W. Lee, confirming that the luminosity of RR Lyrae stars depends onevolutionary status as well as metallicity. Using the period-amplitudediagram, we have also identified highly evolved RRab stars in the range-1.9<=[Fe/H]<-1.5, as predicted from the synthetichorizontal-branch models.
| The absolute magnitudes of RR Lyraes from HIPPARCOS parallaxes and proper motions
We have used HIPPARCOS proper motions and the method of StatisticalParallax to estimate the absolute magnitude of RR Lyrae stars. Inaddition we used the HIPPARCOS parallax of RR Lyrae itself to determineit's absolute magnitude. These two results are in excellent agreementwith each other and give a zero-point for the RR Lyrae M_v,[Fe/H]relation of 0.77+/-0.15 at [Fe/H]=-1.53. This zero-point is in goodagreement with that obtained recently by several groups usingBaade-Wesselink methods which, averaged over the results from thedifferent groups, gives M_v = 0.73+/-0.14 at [Fe/H]=-1.53. Taking theHIPPARCOS based zero-point and a value of 0.18+/-0.03 for the slope ofthe M_v,[Fe/H] relation from the literature we find firstly, thedistance modulus of the LMC is 18.26+/-0.15 and secondly, the mean ageof the Globular Clusters is 17.4+/-3.0 GYrs. These values are comparedwith recent estimates based on other "standard candles" that have alsobeen calibrated with HIPPARCOS data. It is clear that, in addition toastrophysical problems, there are also problems in the application ofHIPPARCOS data that are not yet fully understood. Table 1, whichcontains the basic data for the RR Lyraes, is available only at CDS. Itmay be retrieved via anonymous FTP at cdsarc.u-strasbg.fr (130.79.128.5)or via the Web at http://cdsweb.u-strasbg.fr/Abstract.html
| Early evolution of the Galactic halo revealed from Hipparcos observations of metal-poor stars
The kinematics of 122 red giant and 124 RR Lyrae stars in the solarneighborhood are studied using accurate measurements of their propermotions obtained by the Hipparcos astrometry satellite, combined withtheir published photometric distances, metal abundances, and radialvelocities. A majority of these sample stars have metal abundances of(Fe/H) = -1 or less and thus represent the old stellar populations inthe Galaxy. The halo component, with (Fe/H) = -1.6 or less, ischaracterized by a lack of systemic rotation and a radially elongatedvelocity ellipsoid. About 16 percent of such metal-poor stars have loworbital eccentricities, and we see no evidence of a correlation between(Fe/H) and e. Based on the model for the e-distribution of orbits, weshow that this fraction of low-e stars for (Fe/H) = -1.6 or less isexplained by the halo component alone, without introducing the extradisk component claimed by recent workers. This is also supported by theabsence of a significant change in the e-distribution with height fromthe Galactic plane. In the intermediate-metallicity range, we find thatstars with disklike kinematics have only modest effects on thedistributions of rotational velocities and e for the sample at absolutevalue of z less than 1 kpc. This disk component appears to constituteonly 10 percent for (Fe/H) between -1.6 and -1 and 20 percent for (Fe/H)between -1.4 and -1.
| RR Lyrae Star Metallicities From Caby Photometry
Abstract image available at:http://adsabs.harvard.edu/abs/1996AJ....112.2132B
| Template K Light Curves for RR Lyrae Stars
We discuss a technique to compute using templates developed by fitting aFourier series to existing high-quality K light curves of field RRLyraes. We find that a series of order 2 is sufficient to model thelight curves of first-overtone RRc variables, but 4 different 6th-ordertemplates are needed for the fundamental RRab stars due to changes inthe light curves that appear to correlate with the B amplitude. Applyingthe appropriate template to single-phase observations yield estimatedvalues whose deviation from the true is randomly distributed over phase,and is of the same order of magnitude as the observational uncertainty,as long as the ephemeris phase is accurate. The addition of a secondpoint, separated by at least 0.2 in phase from the first, allows the useof template-shifting to remove deviations that may arise fromuncertainties in the ephemeris phase, and template and scaling factorselection, with final systematic errors reduced to less than 0.03 mag.We find that the use of templates yield superior results to thosederived using other techniques, which can produce values that showsystematic deviations over phase. (SECTION: Stars)
| The Rotation of RR Lyrae Stars
We report upper limits to rotation from the measurement of line breadthsvia cross-correlation analysis for 27 RR Lyrae variables. The eightbest-observed stars of type RRab show the same variation of breadth withphase: the breadth peaks sharply during the rise to maximum light, dropsgradually, and reaches a broad minimum during the phase of maximumradius. During this phase the breadth is always narrow, consistent withinstrumental resolution and turbulence alone. For the threewell-observed RRc variables, the breadth is this narrow at all phasesexcept for a slight increase during the rise to maximum light. Theremaining stars also conform to these patterns, albeit with sparse phasecoverage and lower signal-to-noise ratio. We interpret these results asindicating that lines are broadened in RRab stars by shock-inducedplumes or turbulence during the rise to maximum light, and perhaps byother causes as well, but not by rotation in RR Lyrae stars of eithertype. We estimate an upper limit of v sin i < 10 km s-1 in all cases.This is in stark contrast to the rotation seen in field blue horizontalbranch stars, where v sin i > 10 km s-1 in three out of sixwell-studied field stars, and to the more rapid rotation, oftenexceeding 100 km s-1, of the Population I delta Scuti variables whichoccupy adjacent regions of the instability strip.
| Vitesses radiales. Catalogue WEB: Wilson Evans Batten. Subtittle: Radial velocities: The Wilson-Evans-Batten catalogue.
We give a common version of the two catalogues of Mean Radial Velocitiesby Wilson (1963) and Evans (1978) to which we have added the catalogueof spectroscopic binary systems (Batten et al. 1989). For each star,when possible, we give: 1) an acronym to enter SIMBAD (Set ofIdentifications Measurements and Bibliography for Astronomical Data) ofthe CDS (Centre de Donnees Astronomiques de Strasbourg). 2) the numberHIC of the HIPPARCOS catalogue (Turon 1992). 3) the CCDM number(Catalogue des Composantes des etoiles Doubles et Multiples) byDommanget & Nys (1994). For the cluster stars, a precise study hasbeen done, on the identificator numbers. Numerous remarks point out theproblems we have had to deal with.
| Kinematics of metal-poor stars in the galaxy
We discuss the kinematic properties of a sample of 1936 Galactic stars,selected without kinematic bias, and with abundances (Fe/H) is less thanor equal to -0.6. The stars selected for this study all have measuredradial velocities, and the majority have abundances determined fromspectroscopic or narrow-/intermediate-band photometric techniques. Incontrast to previous examinations of the kinematics of the metal-poorstars in the Galaxy, our sample contains large numbers of stars that arelocated at distances in excess of 1 kpc from the Galactic plane. Thus, amuch clearer picture of the nature of the metal-deficient populations inthe Galaxy can now be drawn.
| Pulsation and stability of RR Lyrae stars. 1: Instability strip
In order to provide a detailed analysis of RR Lyrae instability striptopology, an extensive grid of nonlinear, nonlocal, and time-dependentconvective models of RR Lyrae stars has been computed at fixed mass (M =0.65 solar mass) and chemical composition (Y = 0.299, Z = 0.001). Fourseries of envelope models at different luminosity levels (log(L/solarluminosity) = 1.81, 1.72, 1.61, 1.51) and on a large range of effectivetemperatures (5700 K less than Te less than 8000 K) have beeninvestigated. The nonlinear modal stability has been evaluated atlimiting amplitude for both the fundamental and the first overtone. Theequations governing both dynamical and convective interactions have beenintegrated in time until the initial perturbations and the nonlinearfluctuations due to superposition of higher order modes settled down.The theoretical observables obtained by the present survey (radius,luminosity, velocity and temperature amplitudes, periods) describe thepulsation characteristics of the models at full amplitude, hence theycan be properly compared with observations. A linear, nonadiabaticsurvey of the first three modes of RR Lyrae models has been alsocomputed to supply the static structure of the envelope to the nonlinearstability analysis. Several numerical simulations have been performed totest both the numerical accuracy (boundary conditions, time-step size,zoning) and the adequacy of the physical assumption (efficiency of theturbulent regime, artificial viscosity dependence, convective structureinitialization) adopted to describe the coupling between dynamical andconvective fields. The structure of the instability strip shows severalstriking features concerning the width in temperature of the regionwhere only the first overtone is unstable. Indeed, the fundamental blueedge, moving from higher to lower luminosity levels, becomes redder, incontrast to previous findings but in agreement with globular clustersobserved data. Moreover, using an improved treatment of the convectivetransport, the first-overtone red edge has been directly evaluated andhence also the width of the 'either-or' region (i.e., the region whereboth the fundamental and the first overtone are simultaneouslyunstable). It has been found that the periods of the nonlinearconvective models are systematically smaller than the correspondingperiods of both linear and nonlinear radiative models. The differencesbetween linear and nonlinear results are smaller than 2% of the period,however. This effect has been explained as a consequence of the changesinduced during the phases of maximum compression by the convectivetransport on the adiabatic exponent, and on the density inversionlocated in coincidence with the hydrogen ionization reigon.
| The Absolute Magnitudes of Rr-Lyrae Stars - Part Five - Wy-Antliae W-Crateris Rv-Octantis Bb-Puppis
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1993MNRAS.265..301S&db_key=AST
| A re-analysis of the period shifts in RR Lyrae stars
The period shift in both field and globular cluster RR Lyrae stars isexamined. The stellar pulsation theory called the Sandage Period Shiftto determine the mean M(V) of RR Lyrae stars is investigated. Theadvantages of (V-K) compared to (B-V) as a temperature indicator for RRLyraes are discussed in detail. Period shift-metallicity relations arederived using recently published infrared photometry of field RR Lyraesand globular cluster RR Lyraes. Other method for determining mean M(V)for RR Lyraes are critically reviewed. It is argued that results formain sequence fitting, statistical parallax, and Red Giant Branch theoryare presently too uncertain to be used. The slope of themass-metallicity relation from pulsation theory is in seriousdisagreement with that from Horizontal Branch Theory.
| UBVRI photometry of RR Lyrae stars.
Not Available
| Hydrodynamic Models for the Rrc-Stars
Hydrodynamic pulsation models are constructed for the RR Lyrae stars,including a large grid of RRc models and a pair of models withparameters corresponding to the RRd stars. The latter calculations areused to argue that LNA periods are sufficient when comparing RRd modelswith observations. The RRc models are subjected to Fourierdecomposition, and a discussion of various Fourier parameters isundertaken to complement a treatment given elsewhere of the phaseparameter ?31. It is shown that the theoretical lightcurves mimic the observations rather well, including the observed run of(1)31 with period and the fall-off of ?31 withR21. The greatest deficiency of the models lies in theirfailure to reproduce observed values of the phase parameter?21. Finally, turning to the velocity curves, we showthat the first-order phase lag (??)1 betweenvelocity and light is related in the models to the linear driving?1 and thus potentially may be used to measure thedistances of observed RRc stars from their respective blue edges.
| On metallicity and RR Lyrae light curves
Fourier decompositions are performed for the light curves of sixRRab and 3 RRc field stars. These are added toprevious work to form a sample of 61 RRab and 12RRc pulsators. The authors use this sample to establish avery regular decrease in the Fourier parameter ?21 withdecreasing metal content among field RRab stars with period P< 0d.575. They show that this relation can be tentativelyexplained as an opacity effect, using simple one-zone models. No trendof ?21 with metallicity is found for the RRcfield stars.
| A Determination of Interstellar Absorption for Rrc-Lyrae Variables
Interstellar absorption is determined for 13 RRc Lyrae variables and 3dwarf Cepheids using the method described in Astron. Tsirk., No. 1503,1987.
| The HEAO A-1 all-sky survey of fast X-ray transients
Ten fast X-ray transient sources were discovered in the first completepass of the sky by the HEAO A-1 Sky Survey Experiment, including 7relatively faint sources and 3 bright ones. The survey technique andeach of the transients are described. Four of the transients areidentified with active coronal sources; the remaining ones areunidentified. The statistical properties of the total sample of 10sources are discussed, including event rates, distribution on the sky,and the number-flux distribution.
| Population studies. II - Kinematics as a function of abundance and galactocentric position for (Fe/H) of -0.6 or less
A catalog is presented of some 1200 Galactic objects which have radialvelocities and (Fe/H) abundances of -0.6 or less. These data areanalyzed to yield information on the kinematic properties of the olderpopulations of the Galaxy and on the interdependence between kinematicsand abundance. It is found that the kinematics of the availablekinematically selected stars differ from those of the nonkinematicallyselected objects. No evidence is found for any significant difference inthe kinematic properties of the various halo subgroups, nor for anydependence of kinematics on abundance. While the rotation of the halo issmall at about 37 km/s for (Fe/H) of -1.2 or less, it rises quickly forhigher abundances to a value of about 160 km/s at (Fe/H) = 0.6. Objectsin the abundance range -0.9 to -0.6 appear to belong predominantly to apopulation possessing the kinematic characteristics of a thick disk. Theimplications of these findings for the suggestion that globular clustersbelong to the same population as the noncluster objects, for the originof the thick disk, and for the mass of the Galaxy are discussed.
| Absolute magnitudes and kinematic properties of RR Lyrae stars
A maximum-likelihood statistical analysis of several subgroups of thefield RR Lyrae stars was performed to determine the relative solarmotion, velocity ellipsoid parameters, and mean absolute visualmagnitude for each group. The full sample of 159 stars was taken from arecent Chinese proper-motion survey, and new mean radial velocities wereused for 46 of the stars. A geometric minimization technique known assimplex optimization was used to apply a rigorous maximum-likelihoodmodel to the data. The best estimate for the mean absolute visualmagnitude is 0.76 + or - 0.14 mag for the entire RR ab-type sample.
| A spectroscopic study of the c-type RR Lyraes
Image tube scanner observations have been made for a sample of fieldc-type RR Lyraes. Using these spectra, it is shown how Preston's metalabundance indicator Delta-S can be applied to the RRc's to derive (Fe/H)on Butler's system. Mean temperatures for the field RRc's based onreddening free colors determined from the strength of the H-beta line.These abundances and temperatures allow the delineation of Oosterhoffgroups among field stars. It is shown that, as in clusters, theOosterhoff effect for field stars occurs star by star and not just formean properties of the group. There is a temperature region in thefield-star instability strip where the RRc's and RRab's can both existat the same temperature. Data on the temperature boundaries of theinstability strip provide no convincing case for helium abundancedifferences among field RR Lyraes with differing metal abundances.
| Reddening and blanketing of RR Lyrae stars
Based on complete light curves in the five channels of the WalravenVBLUW photometric system, a discussion is given of the determination ofblanketing and reddening for RR Lyrae stars. A photometric accuracy ofthe order of 0.005 mag has been reached. Blanketing derived from thereddening-free color index /B-L/ is shown to be equivalent to other waysof determining the metallicity of RR Lyrae stars, such as delta (u-B)s,m1, and delta S. Two independent ways to find the interstellar-reddeningcorrection are studied; they lead to identical results. A table is givenwith high-accuracy blanketing and reddening values for 73 RRab, 13 RRc,and a few short-period (RRs) variables. The relation between the presentobservations and those in other intermediate-band systems is considered.
| An atlas of light and colour curves of field RR Lyrae stars
An atlas is presented of light and color curves in the Walraven VBLUWphotometric system for 90 field RR Lyrae and short-period variables. Theobservational program and the reduction procedure are briefly described.Tables are presented containing the colors at mean and minimum light.
| Photoelectric UBV observations of RR Lyrae variable stars, second list.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1977RMxAA...2..235B&db_key=AST
| Cracow Observations of Variable Stars
Not Available
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| Takýmyýldýz: | Basakci |
| Sað Açýklýk: | 13h24m48.00s |
| Yükselim: | -06°58'45.5" |
| Görünürdeki Parlaklýk: | 11.127 |
| özdevim Sað Açýklýk: | -13.8 |
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| B-T magnitude: | 11.589 |
| V-T magnitude: | 11.166 |
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