Identification of red high proper-motion objects in Tycho-2 and 2MASS catalogues using Virtual Observatory tools

4.1 MB·English

by  F. M. Jiménez-Esteban

Astronomy&Astrophysicsmanuscriptno.Jimenez-Esteban (cid:13)c ESO2012
January26,2012
Identification of red high proper-motion objects in Tycho-2 and
2MASS catalogues using Virtual Observatory tools
F.M.Jime´nez-Esteban1,2,3,J.A.Caballero1,R.Dorda4,5,P.A.Miles-Pa´ez4,6,andE.Solano1,2
1 CentrodeAstrobiolog´ıa(INTA-CSIC),DepartamentodeAstrof´ısica,POBox78,E-28691,VillanuevadelaCan˜ada,Madrid,Spain
e-mail:[email protected]
2 SpanishVirtualObservatory
3 SaintLouisUniversity,MadridCampus,DivisionofScienceandEngineering,AvenidadelValle34,E-28003,Madrid,Spain
4 DepartamentodeAstrof´ısicayCienciasdelaAtmo´sfera,FacultaddeCienciasF´ısicas,AvenidaComplutenses/n,E-28040,Madrid,
2
Spain
1 5 DepartamentodeF´ısica,Ingenier´ıadeSistemasyTeor´ıadelaSen˜al,EscuelaPolite´cnicaSuperior,UniversityofAlicante,Apdo.99,
0
E-03080,Alicante,Spain
2 6 InstitutodeAstrof´ısicadeCanarias,E-38200,LaLaguna,Tenerife,Spain

n
Received01Nov2011/Accepted..Jan2012
a
J
ABSTRACT
5
2
Aims.Withavailable Virtual Observatory tools, welooked for new Mdwarfs in thesolar neighbourhood and M giantswith high

tangentialvelocities.
]
R Methods.Fromanall-skycross-matchbetweentheoptical Tycho-2andthenear-infrared2MASScatalogues, weselectedobjects
withpropermotionsµ>50masyr−1 andveryredV −K colours.Forthemostinterestingtargets,wecollectedmulti-wavelength
S T s
photometry,constructedspectralenergydistributions,estimatedeffectivetemperaturesandsurfacegravitiesfromfitstoatmospheric
.
h models,performedtime-seriesanalysisofASASV-bandlightcurves,andassignedspectraltypesfromlow-resolutionspectroscopy
p obtainedwithCAFOSatthe2.2mCalarAltotelescope.
- Results.Wegotasampleof59bright redhighproper-motionobjects,includingfiftyredgiants,four reddwarfs,andfiveobjects
o reported in this work for thefirst time. The five new starshave magnitudes V ≈10.8–11.3mag, reduced proper motions midway
T
r betweenknowndwarfsandgiants,near-infraredcolourstypicalofgiants,andeffectivetemperaturesT ≈2900–3400K.Fromour
t eff
s time-seriesanalysis,wediscoveredalongsecondaryperiodinRuber4andanextremelylongprimaryperiodinRuber6.Withthe
a CAFOSspectra,weconfirmedtheredgiantnatureofRuber7and8,thelastofwhichseemstobeoneofthebrightestmetal-poorM
[ giantseveridentified.

1 Keywords.astronomicaldatabases:miscellaneous–virtualobservatorytools–stars:late-type–stars:oscillations–stars:chemi-
v callypeculiar–stars:peculiar
5
1
3
1. Introduction through small amateur telescopes). With Caballero&Solano
5
. (2008) and Jime´nez-Estebanetal. (2011), we started a project
1 For the Virtual Observatory (VO), there are seductive mottoes
devoted to identifying bright blue objects in the Tycho-2 cata-
0 (e.g.theUniverseatyourfingertips;NVO1)andbombasticdefi-
logue interesting for other follow-up studies. In particular, our
2 nitions(e.g.aninternationalastronomicalcommunity-basedini-
surveys have provided some of the brightest hot subdwarfs
1 tiative[that]aimstoallowglobalelectronicaccesstotheavail-
everfound,whichenormouslyfacilitatesforthcomingastroseis-
:
v ableastronomicaldataarchivesofspaceandground-basedob- mologic, spectroscopic, and multiplicity analyses (Oreiroetal.
Xi servatoriesandotherskysurveydatabases[and]toenabledata 2011;Vennesetal.2011).
analysistechniquesthroughacoordinatingentitythatwillpro-
Here we go on examining high proper-motion objects in
r videcommonstandards,wide-networkbandwidth,andstate-of-
a the-art analysis tools; EURO-VO2). One of the most tangible Tycho-2and2MASScataloguesusingVOtools,thistimetothe
other side of the colour-magnitudediagram, looking for bright
resultsoftheVO endeavourisa suite ofanalysistools(theso-
redobjects.Intheabsenceofdiscsordustenvelopes,redcolours
called “VO tools”), which are used more and more frequently
aresynonymouswithloweffectivetemperatures(T ∼3000K
by the astronomical community,as demonstrated by the grow- eff
ingnumberofVOpapers3(see,forinstance,Caballero2009for forthecooleststarsinTycho-2).Apriori,therearenotmanyal-
ternativesforclassifyingsuchbrightlate-typeobjectswithhigh
agoodexampleofthis).
proper-motion:theycanbeeithernearbyMdwarfsorredgiants
While there is a current trend to discovering the “faintest,
withhightangentialvelocities.
coolest, smallest” objects in our Galaxy (e.g. Delormeetal.
2008; Kirkpatricketal. 2011), there is still a lot to do with FindingasingleuncataloguedTycho-2dwarflaterthanM3V
relatively bright unknown objects (V & 11mag – i.e. visible would justify the whole current survey. With V ∼ 11mag, a
star like thatwouldhave J . 7magandinevitablybea golden
1 http://www.us-vo.org target for the next high-resolution, near-infrared (NIR), radial-
2 http://www.euro-vo.org velocity surveys seeking Earth-like planets (Reiners&Basri
3 http://www.euro-vo.org/pub/fc/papers.html 2010; Mahadevanetal. 2010; Quirrenbachetal. 2010). Such a
1
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
finding was also one of the aims of Le´pine&Gaidos (2011), Most of the known reddest Tycho-2/2MASS stars with
who presents an all-sky catalogue of M dwarf stars with ap- µ>50masa−1 aregiants.Exceptfora few cases, the fiftystars
parent infrared magnitudes J < 10.0mag. In a sense, the inTable1arewellknownclass-IIIgiants(suchasMiraCetAB,
Le´pine&Gaidos(2011)catalogueandoursarecomplementary. L Pup,g Cen, andRLyr,whichare theonlystars inthe table
2
The other alternative is a late-type giant (spectral class M, at d < 100pc), semi-regular pulsating, irregular, or Mira vari-
C, or S). Since giantsare intrinsically luminous,theyare com- ables.Theyarelocatedatlongparallacticdistances,havestrong
monly located at long heliocentric distances. However, if they fluxdensitiesintheIRAScatalogueofpointsources,saturatein
have appreciable proper motions, of over a few tens of mil- 2MASSJHKsbands,and/oralreadyhavespectraltypeandclass
liarcseconds per year, their tangential velocities must be very determinations (mostly found in the spectral type compilation
high.Asa result,theymaybelongto theGalactic thickdiscor byKwoketal.1997)consistentwithitslocationinthereduced
eventhehalo(Carney&Latham1986;Rocha-Pintoetal.2004; propermotiondiagramfarfromthemainsequence.Theonlyex-
Famaeyetal. 2005). Our work is expected to catalogue all the ceptionstothecollectionofstarswithevidenceof“giantism”are
brightest,reddestgiantsoverthewholesky,whichareexcellent thepoorlyinvestigatedstarsBD+311540andHD150184.The
targetsforinvestigatingthedynamicsandmetallicitystructureof formerwasalreadypresentedasastar witha remarkablespec-
the Milky Way (McWilliam&Rich 1994; Lambertetal. 1986; trum by Espin (1892) in the 19th century, and it has the same
Beersetal. 2002) and their interiors through pulsation analy- propertiesastherestofthestarsinthetable.Thelatterdoesnot
ses (Wood&Cahn 1977; Bergeatetal. 2002; Kiss&Bedding haveaSIMBADentryatall,butwastabulatedasanM3–4giant
2003).Besidesthis,wealsoexpecttodiscoverrareexamplesof starbyHouk&Cowley(1975).
brightredgiants. Thefourotherknownstars,showninTable2,areMdwarfs
in the solar neighbourhood. While two of them have accurate
parallacticdistancesmeasuredbyHipparcos(QYAurAB:d =
6.29±0.12pc;YZCMi:d =5.95±0.07pc;vanLeeuwen2007),
2. Analysisandresults
the other two only have photometric distances placing them at
2.1.Targetselection 8–10pc(Reidetal.1995;Beuzitetal.2004).Threeofthefour
stars have propermotionslargerthanany giantin Table 1, and
We used the sample of 155,384 sources with proper motions one of them up to 1000masa−1. The four stars have spectral
µ>50masa−1 obtained from the cross-match of the whole
typedeterminationsatM3.5–4.5V,consistentwiththeobserved
Tycho-2 (Høgetal. 2000) and 2MASS (Skrutskieetal. 2006)
optical and NIR colours (in contrast to the giants, none of the
cataloguesconstructedbyJime´nez-Estebanetal.(2011).Wese-
dwarfs saturate in the 2MASS JHK bands). Interestingly, the
s
lected red high proper-motion star candidates based on their fourdwarfsare(candidate)membersinmultiplesystemsand/or
position on the reduced proper motion-colour diagram shown
youngmovinggroups:
in Fig. 1. Quantitatively, the applied selection criterion was
V − K > 6.0mag if H ≤ 8mag and V − K > 5.5mag
T s VT T s – BD–21 1074 BC is part of a hierarchical triple system,
if H > 8mag. The abnormally large errors in K because of
VT s WDS05069–2135,whichwasdiscoveredbyDonner(1935).
saturationofthebrightestobjectsbarelyaffectthedatapointlo-
The primary (A, GJ 3331) is a nearby flare M1.5V star at
cation in the diagram. The application of this simple selection
8.22arcsectoatightersystem(BC,GJ3332)oftwoslightly
criterion resulted in 73 objects with redder colours than these
cooler stars separated by only 0.80arcsec. Neither Tycho-
values,whichisanappropriatenumberofsourcestobestudied
2 nor 2MASS were able to resolve the tight binary, which
individuallyonareasonabletimescale.
is 1.15mag redder than the primary in V − K . Based on
T s
Next, we carried out a visual inspection of the 73 se- a significant amount of Li i in absorption in the spectra of
lected candidates in a similar way to the one described in both A and BC components,X-ray emission, and kinemat-
Jime´nez-Estebanetal. (2011). Six of them were found to have
ics,daSilvaetal.(2009)classifiedthesystemasamember
erroneous proper motions in the Tycho-2 catalogue. As an ex- oftheveryyoungβPictorisassociation(τ∼12Ma).
ample, the catalogue gives a proper motion (µαcosδ, µδ) = – QYAurABisa“classic”doubleinthesolarneighbourhood.
(–14, –84)masa−1 for the star TYC 6238–480–1, while we
It is a spectroscopic binary with an approximate period of
measured (+0.9±1.4, −12.4±0.6)masa−1 using six astromet- 10.43dandarelativelyhighorbitaleccentricityof0.34with
ric epochs covering 43.7 years and the method exposed by nopreviousreportofmembershipinayoungmovinggroup.
Caballero (2010). In this case, the Tycho-2 measurement was
– YZ CMi, although it has a Washington Double Star cata-
likely affected by a visual (unbound)companion at 8arcsec to logueentry,seemstobesingle(Lafrenie`reetal.2007).Itis
the North, ∼2.8mag fainter in the R band. The five other dis- anemission-linedwarfwithmegaflares,whichhasbeenre-
carded stars have even lower actual proper motions. In addi-
peatedlyinvestigated(e.g.,Kunkel1969;Kahleretal.1982;
tion,we discardedanothereightclosebinarystars, resolvedby Kunduetal.1988;Benz&Alef1991).Montesetal.(2001)
Tycho-2 but unresolved by 2MASS, because of their incorrect classifythestar asa memberoftheLocalAssociation(τ ∼
resultingcolours.
10–150Ma).
– The magnetically active binary star DG CVn AB
(WDS13318+2917),oneoftheonlythreeknownMdwarf
2.2.Preliminarytargetclassification
ultra-fast rotators within 10pc (Delfosseetal. 1998), was
Of the 59 remainingunresolvedobjects, 54 have some kind of firstresolvedbyBeuzitetal.(2004)intoapairseparatedby
publishedspectral type information.We list their basic proper- only0.17arcsec.Montesetal.(2001)classifiedthebinaryas
tiesinTables1and2,whereweprovidetheirTycho-2identifi- amemberoftheyoungdisc(τ∼600Ma).
cation,coordinates,Tycho-2V and2MASSJHK magnitudes,
T s
total proper motion µ, parallax (from vanLeeuwen 2007 in all Theremainingfiveunknownstars,listedinTable3andplot-
buttwodwarfs),spectraltype,mostcommonname,andatleast tedin Fig. 1with filled (blue)circles,havenoHipparcosentry
oneofthemostrepresentativereferences. and haveneverbeen reportedin the literature.Actually, oneof
2
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
Fig.1. Tycho-2/2MASSreducedproper motion diagram(H versus V −K , where H = V +5logµ+5). Objects selected
VT T S VT T
forfollow-upareredwardsofthedashedline.Previouslyunreportedredhighproper-motionobjectsaredepictedwith[blue]filled
circles,already-knownobjectswith[red]opensymbols(giantswithtriangles,dwarfswithsquares),binarysystemsunresolvedby
2MASS with [black] crosses, and objects with wrong proper motion with [black] sails. The remaining objects bluewards of the
dashed line are markedwith small dots. The dwarf located halfwaybetween giants (to the top) and the remainingdwarfs (to the
bottom)isBD–211074BC.ComparethisdiagramwiththeoneinFig.2ofJime´nez-Estebanetal.(2011).
themhasaBonnerDurchmusterungentry(Scho¨nfeld1886),but 2.3.VirtualObservatoryanalysis
ithasgonewithoutbeingnoticedforover120years.Fornam-
2.3.1. Spectralenergydistributions
ingthestars,wefollowedthe“Ruber”(redinLatin)nomencla-
ture introducedby Caballero&Solano(2008) and followedby Another way to obtain information of the Ruber objects is
Caballero(2009).OurnewRuberobjectsgofromthefourthto by analysing their spectral energy distributions (SEDs). We
theeighthinthisseries. searched for additional photometric data of the five Ruber ob-
jects using the “all-VO Discovery tool” of Aladin sky atlas
The five new red high proper-motion objects fall between (Bonnareletal. 2000). This utility allows the user to query
the giant and (ordinary) dwarf branches in the reduced proper a large number of photometric catalogues in a convenient
motion-colourdiagram.AretheRuberobjectsunresolvedbinary way. Besides Tycho-2 and 2MASS, we collected observa-
dwarfsintheβPictorismovinggroup,suchasBD–211074BC, tional data from the following astrophotometric catalogues:
or peculiar underluminousgiants? To shed some light on their UCAC3 (Zachariasetal. 2010), DENIS (Epchteinetal. 1997),
nature,wefirstanalysedtheirnear-infraredcolours. WISE(Wrightetal.2010),GLIMPSE(Churchwelletal.2009),
MSX6C (Eganetal. 2003), AKARI/IRC (Ishiharaetal. 2010),
Figure2 shows the location of our sources in an H − and IRAS (Beichmanetal. 1988). Table 3 compiles all this in-
K vs.J − H colour-colour diagram, which is an excellent di- formation.
s
agnostic tool for distinguishing between red giants and dwarfs We took advantage of another VO tool, VOSA4 (VO SED
(Bessell&Brett1988). Allfifty Mgiantsin Table1areclearly Analyzer;Bayoetal.2008),tofittheobservedSEDstotheoret-
segregatedfromthefourMdwarfsinTable2,whichmatchtheir icalmodelsavailableattheVO.VOSAallowstheusertoquery,
expected intrinsic colours. The five new Ruber objects are lo- inanautomaticandtransparentway,differentcollectionsofthe-
cated in the giant region, indicating that they are probably M
giantswithveryhightangentialvelocities. 4 http://svo.cab.inta-csic.es/theory/vosa
3
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
Fig.2.SameasFig.1butforthenear-infraredcolour-colourdiagram.Dashedandcontinuouslinesdepicttheintrinsiccoloursof
M dwarfs and giants, respectively (Bessell&Brett 1988). The two reddest dwarfs, QY Aur AB and YZ CMi AB, have almost
coincidentnear-infraredcolours.
oretical models, calculate their synthetic photometry, and per- 2.3.2. Photometricvariability
forma statisticaltestto determinewhichmodelreproducesthe
Another piece of information that may help in classifying the
observeddatabest.
five Ruber stars in Table 3 is their photometric variability,
which is often detected in red giant stars and in magnetically-
active field M dwarfs. In general, active M dwarfs rotate fast
TofittheSEDsofourRuberobjects,weusedtheNextGen (Stauffer&Hartmann1986;Bouvieretal.1993;Delfosseetal.
collectionofstellaratmospheremodels(Hauschildtetal.1999) 1998; Rockenfelleretal. 2006), while giants pulsate with
and solar metallicity. The effective temperatures(Teff) and sur- long periods (Stebbins&Huffer 1930; Percy&Polano 1998;
facegravities(logg)obtainedwithVOSArangedbetween2900 Koen&Eyer2002;Catelan2009).Periods,ifdetected,mayalso
and3400K andbetween3.5and4.0,respectively(see the bot- helpdifferentiatethetwokindsofobjects.
tom ofTable 3).The accuracyin determiningthese parameters WesearchedintheAllSkyAutomatedSurvey(ASAS)cata-
wassetbythemodelgridsizeto100KinTeff and0.5inlogg. logueofvariablestars(Pojman´ski2002)fordataonourobjects.
Estimatedtemperaturesandsurfacegravitiescorrespondtolate- Oneof them,Ruber4 (ASAS152557–4844.6),was catalogued
type M stars with logg midway between dwarfs and giants. In tohaveaperiodofphotometricvariabilityP=43dwithanam-
Figure3weplotthetheoreticalfittingoftheobservationalSEDs. plitudeof0.30magintheVband.Tabulatedvariabilitytypewas
A VOSA upgrade,with new gridsof theoreticalisochronesfor “MISC/SR”(“mostlysemi-regular”withtimescalesofvariation
dwarfandgiantstarswithlowerTeffsthanthoseprovidedbythe between10and200d).
Kuruczmodelsandwideintervalsofmetallicity,iscurrentlyun- Todoourowntime-seriesanalysis,welookedfortheorig-
der developmentby the Spanish Virtual Observatoryteam but, inal light-curve data set of the five Ruber targets at the ASAS
unfortunately, was not available to us at the time of writing. webpage5 asinCaballeroetal.(2010).Thelightcurves,which
Nevertheless,theeffectofthemetallicityontheoverallSEDsof contain approximately between 400 and 700 data points after
dwarfswouldprobablybenotstrongenoughtoproduceanotice- discardinglow-qualitymeasurements,spanfromFebruary2001
ablechangeintheTeffandloggfitvalues,especiallywhenfitting toOctober2009andaredisplayedinFig.4.Byeye,moststars
broad-band photometry (Bonfilsetal. 2005; Rojas-Ayalaetal.
2011;Schlaufman&Laughlin2010;Woolfetal.2009). 5 http://www.astrouw.edu.pl/asas/
4
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
Fig.3.TheoreticalSEDfitsofRuber4to8,fromtoptobottom. Fig.4. ASAS V-band light curvesof Ruber4 to 8, from top to
Solid lines represent the NextGen models for solar metallicity bottom.
that best fit the observational data. Filled [red] circles indicate
the observational photometric data used for the fit. Error bars
areusuallysmallerthanthesizeofthecircles.
the abnormalobserved V − K colours with respect to the re-
T s
ducedpropermotions.
We performed the same variability analysis as in
display amplitudes of variability between two and three times Jime´nez-Estebanetal. (2006), using a sinusoidal light curve
the uncertainty of the photometry. In particular, for Ruber4, as a first approximationof the real one. The least mean square
which is the most variable star in our small sample, the mean method (Stellingwerf1978) was applied for a range of periods
error bar and standard deviation of the light curve are 40 and from0.1dto10,000d,andthequalityofthefitwasdetermined
116mmag, respectively. The photometric variability (Tycho-2, with a normalisedχ2 test, weightingeach observationwith the
2MASS,ASAS dataare notcoincidentin time) cannotexplain inverseofthesquareoftheobservationalerror.
5
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
Fig.5.PeriodogramsoftheASASlightcurvedofRuber4to8, Fig.6. ASAS V-band light curves as a function of phase of
fromtoptobottom. Ruber4to8,fromtoptobottom.Continue(red)linesshowthe
correspondingsymmetricsinusoidalmodellightcurvefit.Light
curvesofRuber5and8arehighlytentative.
TheperiodogramsforRuber4to8areshowninFig.5.Asil-
lustratedbythefirstpanel,apartfromconfirmingthePojman´ski
(2002) period of Ruber4 within uncertainties(P=42.3±0.1d), longerthanthetimecoverageofthemonitoring,theyshouldbe
we report on the discovery of a long secondary period (LSP) considered highly tentative so need to be confirmed. All peri-
at around 520d. A similar period (P∼420d) was found for odograms show a similar pattern around 300–400d, which is
Ruber7, while Ruber6 displayed a period longer than half the dueto the frequencyof theASAS observations,with blocksof
totaltimecoverageof3150–3200d(cf.bottomofTable3).For dataseparatedbyaboutayear.
Ruber5 and Ruber8, two extremely long periods were found The presence of LSPs, as in the case of Ruber4, is very
(P∼4000and∼7000d,respectively).Sincetheyaremuchmore common among pulsating red giant stars. At least one third
6
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
of the semi-regular variables in the solar vicinity are in fact SomethingsimilarhappenstoHD98500andHD122132.After
multiperiodic, with an LSP roughly one order of magnitude consulting additionalM giant standards in Danks&Dennefeld
longer than the primary period of pulsation (Woodetal. 2004; (1994), we gave the M2III spectral type, with one dex uncer-
Percyetal. 2004). In spite of that, LSP is the only type of tainty, to both Ruber7 and TYC 6238−480−1. However, the
large-amplitude stellar variability that remains completely un- spectrumofRuber8deservedfurtherattention.
explained. Woodetal. (2004) discuss several mechanisms, but ThepseudocontinuumofRuber8reasonablyfitsthatofother
findnoclearexplanationforany,andspeculatethatasymptotic M2 giants. However,its absorptionbandsand (alkali)lines are
giantbranchstarswithLSPmaybetheprecursorsofasymmetric far less marked, so we gave it the “wk” code of spectral pecu-
planetary nebulae. More recent studies (Soszyn´skietal. 2007; liarity (from “weak lines”). This weakness of bands and lines
Soszyn´ski2007)havepointedtowardsabinaryorigin.Thislast maybeexplainedbyaverylowmetallicity.Metal-poorstarsare
explanationisconsistentwiththelocationofRuber4 inthere- thought to be the survivors of the earliest generations of stars.
ducedpropermotiondiagram,whereothermultiplestellarsys- Theirstudyhelpstoputconstraints,forexample,onthechemi-
temarefound. calhistoryoftheMilkyWay(Holleketal.2011;Cayrel2006).
Another peculiar object is Ruber6, which presents an ex- Bright low-metallicity stars are very rare, so if the metal-poor
tremely long period (P∼2200d) with low-amplitude variabil- natureofRuber8isconfirmed,itwouldbecomeanexcellenttar-
ity (∼0.07mag), and relatively blue near-infrared colour (H − getfordetailed follow-upstudies.Until now,we havefailed to
K ∼0.35mag). We did not find any other star with a longer obtaina higherresolutionspectrumofRuber8,fromwhichwe
s
period reported in the bibliography. Two kinds of red gi- wouldmeasureradialvelocities,determinegalactocentricspace
ant stars could present such long periods: Mira-like variables velocitiesUVW, andassign membershipfor the Galactic kine-
(Engelsetal. 1983; Jime´nez-Estebanetal. 2006) and semi- maticcomponents(i.e.thin/thickdisc,halo).
regular variables (e.g. Glass&vanLeeuwen 2007, and refer-
ences therein). In the first case, stars present very red near-
3. Summaryandfinalremarks
infrared colours (H − K >3mag) and a large amplitude of
s
variability (>1mag); in the second case, the stars have bluer We identified red high proper-motion objects in the Tycho-2
colours and present lower amplitudes. Ruber6 may be a semi- and 2MASS catalogues using Virtual Observatorytools, in the
regularvariablestarwithanextremelylongperiodandverylow- same way as Jime´nez-Estebanetal. (2011) did with blue ob-
amplitudevariability. jects. After discarding six sources with erroneous proper mo-
tions and eight close binaries, we got a sample of 59 objects
with proper motions larger than 50masyr−1 and red colours
2.4.Spectroscopy
V −K >5.5–6.0mag.Ofthem,54wereknowntobeM-typegi-
T s
ThebestwaytoascertainthenatureoftheRuber4to8sources antsanddwarfs.Theotherfive,namelyRuber4to8,arestudied
is with spectroscopic data. Consequently, we used another VO inthisworkforthefirsttime.
tool,VOSED6 (Gutie´rrezetal.2008),tolookforspectrainthe We collected and analysed all available data of the Ruber
VO archives. Developed by the Spanish Virtual Observatory, objects. From SED theoretical fits, we estimated temperatures
VOSED allows the user to gather spectroscopic information that correspond to late-type M stars and surface gravities mid-
available throughout the VO. Unfortunately, no spectroscopic way between dwarfs and giants (subject to uncertainties in the
datawerefound. usedmodels),butfromnear-infraredcolours,weconcludedthat
To complement our VO analysis, we collected low- allofthemarelikelyredgiantswithhightangentialvelocities.
resolution optical spectra for Ruber7 and 8, TYC 6238–480– The analysis of their ASAS light curves yielded interest-
1 (the discarded low-proper motion giant in Section 2.1) and ing results.We established reliableperiodsforthree ofthe five
elevencomparisonstarswithagroundtelescope.On2011Mar Ruber objects. In the case of Ruber4, we also found a sec-
20,weusedtheCalarAltoFaintObjectSpectrograph7(CAFOS) ondaryperiodthatisroughlytentimeslongerthantheprimary
at the 2.2m telescope on the Calar Alto Observatory,Almer´ıa, one.Ruber6presentsanextremelylongperiod(P∼2200d),al-
Spain, with the grism Green–100 and the SITe1d detector of thoughwithalargeerrorduetotheshorttimecoverage.Ruber5
24µm pixels. The resulting resolution was only R∼1600, but and8presentevenlongerperiods,buttheyareuncertain.
the wavelength coverage was very wide, from 4900 to 7800Å With the help of low-resolution spectra obtained with
withoutvignetting.Neededexposuretimeswereintherangeof CAFOS on Calar Alto, we determined the spectral type of
100–200s.NootherRuberstarscouldbeobservedbecauseof Ruber7 and8 atM2III:and M2III:wk,respectively.Thespec-
theirlowdeclinationforCalarAlto. trumofRuber8displayslowmarkedabsorptionbandsandlines,
The eleven comparison stars were seven nearby late-type probablyduetoametal-poornature.
dwarfsandfourM-typegiants.Wereduced,extracted,andcor- Becauseoftheirbrightness,thefiveRuberobjectscanserve
rected all the spectra for instrumental response (with the stan- asusefultargetsfordetailedstudiesofold-populationgiants.
dard star Feige 34) using standard tasks within the IRAF envi-
Acknowledgements. WeareindebttoD.Montes forsupervisingthespectro-
ronment.ThefourteenspectraareshowninFig.7. scopicobservationsonCalarAlto,toA.Klutschfortryingtogetadditionalspec-
From the visual inspection of the pseudocontinuum of the traforRuberobjects,andtoC.Rodrigoforclarifyingwhichmodelsareactually
CAFOSspectra,weconcludedthatbothRuber7and8areinthe availableinVOSA.ThisresearchmadeuseofVOSAandVOSED,developedby
theSpanishVirtualObservatorythroughgrantsAyA2008-02156andRI031675,
giantclass.Therefore,weestimatedtheirspectraltypesfromthe
andofAladinandSIMBADdevelopedattheCentredeDonne´esastronomiques
comparisonwith the fourotherobservedgiants.Unfortunately, deStrasbourg,France.FinancialsupportwasprovidedbytheSpanishMinisterio
their spectral type determinations do not seem to be fully re- deCienciaeInnovacio´n,UniversidadComplutensedeMadridandComunidad
liable: the spectra of BW CVn and BZ CVn are identical, Auto´noma de Madrid under grants CSD2006-00070 (under the Consolider-
but the reported spectral types are different (M1III vs. M3III). Ingenio 2010 Programme First Science with the Gran Telescopio Canarias),
AyA2008-00695, AyA2008-06423-C03-03, and SP2009/ESP-1496. This re-
searchmadeuseoftheNASA/IPACInfraredScienceArchive, whichisoper-
6 http://sdc.cab.inta-csic.es/vosed
ated bytheJetPropulsion Laboratory, California Institute ofTechnology, un-
7 http://www.caha.es/alises/cafos/cafos.html dercontractwiththeNationalAeronauticsandSpaceAdministration.Basedon
7
F.M.Jime´nez-Estebanetal.:Redhighproper-motionobjectsinTycho-2and2MASS
4 4
3.5 3.5
3 3
2.5 2.5
x x
u u
d fl d fl
e e
s s
ali 2 ali 2
m m
or or
N N
1.5 1.5
1 1
0.5 0.5
0 0
4500 5000 5500 6000 6500 7000 7500 8000 8500 4500 5000 5500 6000 6500 7000 7500 8000 8500
λ [A] λ [A]
Fig.7.CAFOSspectraofRuber7and8,TYC6238–480–1,andelevencomparisonstars.Leftpanel(dwarfs):fromtoptobottom,
BD+39 2801 (K5V), HD 147379 A (K7V), GJ 1170 (M1V), HD 95735 (M2V), GJ 4040 (M3V), GJ 687 (M3V), and GJ 1101
(M3.5Ve). All the spectral types are from Hawleyetal. (1996). Right panel (giants): from top to bottom, HD 98500 (M0III;
Moore&Paddock1950), HD 122132(M2III;Moore&Paddock1950), Ruber8 [in red],Ruber7 [in red], TYC 6238–480–1[in
magenta],BWCVn(M1III;Upgren1960),andBZCVn(M3III;Schild1973).
observationscollectedattheCentroAstrono´micoHispanoAlema´n(CAHA)at Beichman,C.A.,Neugebauer,G.,Habing,H.J.,Clegg,P.E.,&Chester,T.J.
CalarAlto,operatedjointlybytheMax-PlanckInstitutfu¨rAstronomieandthe 1988,inInfraredastronomicalsatellite(IRAS)catalogsandatlases.Volume
InstitutodeAstrof´ısicadeAndaluc´ıa(CSIC). 1:Explanatorysupplement
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1 Table1.Already-knownbrightredhighproper-motionobjects:giants.
0
TYC α δ V J H K µ π Spectral Name Ref.a
T s
(J2000) (J2000) [mag] [mag] [mag] [mag] [masa−1] [mas] type
5846–131–1 002146.27 –200328.9 5.926±0.009 0.5: –0.5: –0.8: 64.6±1.0 3.7±0.5 M5–6SIIe TCet 1
4681–469–1 011414.83 –021046.2 8.694±0.014 3.0: 2.0: 1.7: 60.4±1.1 ... M4III ANCet 2
2308–2170–1 015803.77 +310803.8 7.157±0.010 1.5: 0.4: 0.2: 62.8±0.8 5.1±0.5 M5III AATri 2
5278–1494–1 020026.82 –083125.9 5.656±0.009 0.8: –0.2: –0.5: 88.7±0.8 6.8±0.3 M3III ARCet 3
630–507–1 020238.63 +074036.5 9.96±0.03 1.4: 0.4: 0.0: 54.3±1.7 ... M7III BD+06319 4
4693–1144–1 021920.79 –025839.5 6.654±0.010 –0.7: –1.6: –2.2: 238.6±0.7 10.9±1.2 M2–7IIIe+DA MiraCetAB 5
F
641–24–1 025346.22 +092008.9 6.816±0.011 1.7: 0.6: 0.5: 61.5±0.8 5.8±0.6 M6III EGCet 6 .
M
8054–1103–1 025352.77 –495322.7 8.253±0.013 0.7: –0.1: –0.6: 133±2 4.8±1.0 M7IIIe RHor 7 .
5338–890–1 051122.87 –115056.7 5.869±0.010 –0.2: –1.1: –1.4: 64.5±0.9 6.7±0.4 M6III RXLep 8 Jim
6530–1428–1 065300.30 –265727.5 6.586±0.009 1.6: 0.6: 0.3: 66.1±1.3 3.6±0.5 M6III KXCMa 9 ´e
n
87962412––118446–11–1 007711931342..6352 ––647413181253..21 84..177647±±00..001029 –31..41:: –21..59:: –22..13:: 34520..98±±11..20 152..64±±10..05 MM45IIIIIIe WL2WPuVpol 1101 ez-E
s
2451–1111–1 072045.69 +312732.9 8.81±0.02 3.6: 2.8: 2.4: 64.2±1.3 ... M5:III BD+311540 12 te
b
9381–22–1 075521.37 –762952.3 8.786±0.014 3.4: 2.4: 2.0: 54.0±1.3 ... M5III HD66424 2 a
n
6015–2511–1 083953.54 –171810.7 6.846±0.011 0.6: –0.3: –0.6: 151.7±1.3 6.4±0.4 M6III AKHya 13 e
t
818–577–1 090826.54 +131313.6 9.271±0.016 1.4: 0.4: 0.1: 60.7±1.2 4.1±0.9 M6III CWCnc 14 a
8968–918–1 103238.42 –661054.3 8.971±0.015 2.7: 1.8: 1.4: 50.8±1.4 ... M6III: HD91600 2 l.:R
5495–421–1 103751.80 –120115.3 8.997±0.017 1.9: 1.0: 0.7: 54±2 ... M6III FFHya 15 ed
6653–720–1 111437.78 –260430.8 7.739±0.011 2.7: 1.8: 1.5: 65.3±1.4 ... M4III HYHya 16 h
ig
7202–37–1 111850.10 –302825.4 10.05±0.03 2.9: 2.0: 1.6: 60.7±1.7 ... M8III V444Hya 17 h
8972–291–1 113734.06 –605411.6 6.764±0.010 1.2: 0.3: 0.0: 67.3±1.3 6.1±0.5 M4III V913Cen 18 pr
o
292–330–1 123021.01 +042459.1 8.328±0.015 0.5: –0.4: –0.7: 53.2±1.2 5.5±0.7 M7III BKVir 19 p
e
5540–333–1 131120.83 –103050.8 7.640±0.013 2.8: 1.9: 1.6: 55.7±1.2 ... Mb... V339Vir 20 r-
m
899–580–1 133752.93 +132648.4 8.614±0.015 2.5: 1.6: 1.3: 58.9±0.9 4.1±0.7 M6III DHBoo 21 o
8269–1422–1 133959.81 –495659.8 6.044±0.009 0.5: –0.6: –0.8: 101.0±0.9 6.4±0.3 M6III V744Cen 22 tio
n
6728–19–1 134902.00 –282203.5 7.788±0.012 –1.7: –2.7: –3.2: 78.3±1.3 9.6±1.1 M8IIIe WHya 23 o
b
7287–1891–1 134926.72 –342702.8 4.416±0.009 –0.6: –1.5: –1.8: 73.9±1.1 17.8±0.2 M4.5III gCen 24 je
1467–355–1 135355.19 +171650.8 9.58±0.03 4.1: 3.1: 2.8: 50.7±1.2 ... M5III XZBoo 25 cts
6724–764–1 135519.31 –262557.4 8.018±0.012 2.5: 1.6: 1.3: 83.0±1.2 0.3±0.6 M5III V349Hya 26 in
9427–2476–1 140519.88 –764748.3 5.791±0.009 –0.7: –1.7: –2.1: 94.4±0.7 8.8±0.5 M6.5III θAps 27 T
y
1478–509–1 144605.95 +150754.4 6.021±0.010 0.5: –0.4: –0.7: 87.7±0.9 4.0±0.4 M5IIIab EKBoo 28 ch
o
5594–455–1 151921.81 –090847.5 7.223±0.011 2.2: 1.4: 1.1: 51.8±1.1 2.8±1.0 M4III FZLib 29 -
2
2578–824–1 155830.77 +360119.7 7.606±0.010 2.5: 1.6: 1.3: 51.6±1.4 3.0±0.4 M7III RSCrB 30 a
n
3491–136–1 160239.17 +471425.3 6.624±0.010 –0.1: –0.9: –1.3: 94.8±1.1 7.3±0.4 M6IIIe XHer 31 d
2
4190–653–1 163500.72 +602805.3 7.498±0.011 2.7: 1.7: 1.5: 58.0±1.3 2.9±0.5 M4IIIe TXDra 32 M
8717–558–1 164219.86 –552303.7 8.828±0.015 3.6: 2.6: 2.2: 71±2 ... M3–4II: HD150184 33 A
S
5087–261–1 175303.32 –023445.6 7.710±0.012 1.7: 0.8: 0.5: 56.9±0.9 2.7±0.7 M6III V533Oph 34 S
1029–3054–1 183957.12 +095821.9 8.056±0.012 2.0: 1.2: 0.9: 54±2 ... M6IIIe HD172450 35
3131–2155–1 185520.10 +435645.9 4.355±0.009 –0.7: –1.6: –1.8: 83.7±0.7 10.94±0.12 M5III RLyr 36
461–458–1 185718.34 +064153.4 9.57±0.02 3.6: 2.5: 2.2: 65±2 ... M7III V840Aql 37
1040–241–1 190622.25 +081348.0 8.225±0.014 0.7: –0.4: –0.8: 72.2±1.6 2.4±0.9 M7IIIev RAql 38
8782–316–1 194313.64 –561537.0 7.914±0.011 2.1: 1.3: 0.9: 54.5±1.3 5.1±0.6 M5–M6III V341Tel 39
7942–935–1 195842.87 –415057.9 8.272±0.014 2.8: 2.0: 1.6: 58.0±1.1 2±2 M4IIIe RUSgr 40
6913–836–1 200655.25 –271329.8 8.179±0.012 –0.1: –1.1: –1.5: 51.3±1.6 5.1±0.6 M8III V1943Sgr 41
5743–34–1 201007.02 –103212.5 8.92±0.02 3.5: 2.5: 2.2: 53.5±1.3 ... M3III HD191429 42
1637–2033–1 203754.73 +181606.9 6.362±0.010 0.3: –0.8: –1.0: 72.1±1.0 8.6±0.5 M6III EUDel 43
4460–2400–1 210931.78 +682927.2 8.338±0.012 –0.5: –1.3: –1.8: 63.7±1.2 5.3±0.9 M7IIIe TCep 44