Redalyc.SPECTROSCOPIC ORBITS of THREE BINARIES

Revista Mexicana de Astronomía y Astrofísica ISSN: 0185-1101 [email protected] Instituto de Astronomía México

Scarfe, C. D. SPECTROSCOPIC ORBITS OF THREE BINARIES Revista Mexicana de Astronomía y Astrofísica, vol. 53, núm. 2, octubre, 2017, pp. 333- 347 Instituto de Astronomía Distrito Federal, México

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Research of National cil Astrophysics, of Institute Herzberg ulse yohr,btterrgetbedistribu- regrettable their been but has others, orbit an by then the published Since by used ago. list years a many in author stars velocity of radial ex- the handful published to the a no of led with of one this was most 212989 and HD which occurs, period uncertainty. velocity in a radial in years, of year seven cursion a over about little interval, enough ve- a short unfortunate in the variable been miss possibly in had to was be author 8078 to whose HR claimed orbital locity, stars years. the of 4.3 of list to a percent close is which one which of only most period, velocity, in radial accomplished in is increase rapid a to iha rueto eisrncoet 270 to close periastron of the coupled argument at This, an ways. and with eccentricity. high, different determined, its of poorly in because time attention interesting was author’s Per 6 the to came 2 1 h he iaysasdsusdi hspaper this in discussed stars binary three The us okr oiinAtohsclObservatory, Astrophysical Dominion worker, Canada. Guest BC, Victoria, of University ilb vdn httelte rcdr ed osalrob smaller to leads did. procedure those former latter with the the that spectra evident the be cross-correlating 2004, will in and decommissioned detector, obta was CCD v it were them until Observations of spectrometer two velocity mad coudé years, spectrograph. observations few and from a primarily telescope of determined order were orbits the the of periods and primaries e Words: ´ Key este que evidente Es estándar. dispersión observacional. la estrellas u reduce efectuando de CCD, espectros detector utilizócon des un observaciones se fue entonces Las que de DAO. partir hasta espectrógrfo coudé del radiales el velocidades y espectrómetro para m 1.2 r observaciones de de partir a principalmente muy determinaron ellas se de años, dos algunos per´ıodos de y evolucionadas .INTRODUCTION 1. PCRSOI RISO HE BINARIES THREE OF ORBITS SPECTROSCOPIC hspprpeet e pcrsoi riso he binar three of orbits spectroscopic new presents paper This epeetnnea obtspr rsbnra espectrosc binarias tres órbitas para nuevas presentan Se iais pcrsoi tr:idvda 6Pre,H 8 HR Persei, (6 individual stars: — 212989) HD spectroscopic binaries: eevdMrh2 07 cetdJn 32017 13 June accepted 2017; 28 March Received ◦ leads , , 53 .D Scarfe D. C. ABSTRACT RESUMEN 3–4 (2017) 333–347 , iprino .4n mm nm 0.24 of dispersion at a Domin- telescope, 1.22-m the Observatory’s Astrophysical of ion coudé spectrograph the using tained years. five over little wrong a the is deduce one to correct The them led period. observations of tion n h iaisfrwihec a sdaeindi- are used was each which (2010), for cated. Scarfe binaries of zero-point the and veloc- and scale the the where on 1, are Table ities in with listed stars cross-correlation standard from the results determined the were averaging velocities by Radial Bohlender. developed program D. ‘pipeline’ by a detec- with the as reduced CCD and through a tor, using made but optics, (2010). been spectrograph decommis- same Scarfe have was of by observations spectrometer zero-point defined the sioned, the when scale 2004, adjust the Since to to system used standard the been IAU of have observations stars Numerous et 1982). (Fletcher al. (RVS) with spectrometer telescope radial-velocity the the at determined were velocities dial 1,2 bevtoso l he ytm aebe ob- been have systems three all of Observations aiaa o ltelescopio el con ealizadas x´ nrcs a órbitasexcéntricas. Las otnaoe 04 A 2004. en continuado evtoa cte than scatter servational n ic hnuiga using then since and acorrelación cruzada na ihteDO1.2-m DAO the with e lioprocedimiento ultimo nduigteradial the using ined fsadr tr.It stars. standard of o ia o primarias ópicas con ehceo o el con hicieron se r ceti.All eccentric. ery e ihevolved with ies − 1 ntal h ra- the Initially . 078, 333 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México pcrlclassification. spectral M 07 is 2007) rprmtoso 4 a yr mas 347 of motions proper t pcrltp fG I,gvni the in given III, G8 Catalog of type spectral its 334 I 10366, HIP in binaries. presented three are all elements for orbital and 10 8078 Table The 0.35, HR Persei, being 212989. RVS 6 data, for HD the CCD respectively for the 0.25 weight al- and for the was 0.20 than cases data lower all was CCD In data the com- 1.0. for to the weight set from ways The solution a so- data. those for bined from assigned deviations were standard lutions the weights and upon separately, data based CCD and RVS the from rltms ihrslscutrn rudtevalues the around sev- clustering V determined results with been times, have eral Its constella- colours Andromeda. its and with of magnitude boundary edge the southern near the tion, to close very lies aalxteeyedavlct f1. ms km 17.1 of velocity a yield these parallax yr mas -171 and rmDOadLc bevtr.I aeol rough only gave It Observatory. observations Lick on and DAO based from (1936), Christie by published the as large as velocity. almost radial sight, systemic of line the to pendicular R34 17 x x x x x x x x x 71.71 x 54.36 x 3145 HR -100.28 36.52 Peg 35 Aql 31 Vir 16 κ β β Binaries α α α R.V. Standard v 5.31, = e 1.1xxx x x -10.31 Her p 1.0xx x x x x -12.20 3.28 Oph Gem o 53 x x x x x x -4.25 x -5.30 14.49 Cas Boo Ari trk s km Star The h rgtsa esi(R65 D13530, HD 645, (HR Persei 6 star bright The obtained were solutions binaries, three all For h rtkonsetocpcobto e was Per 6 of orbit spectroscopic known first The 1 = . . 25 Hipparcos TNADSASUE FOR USED STARS STANDARD B π ± − α CROSS-CORRELATION 0 V 2 = . 15 = 7 smgtb xetdfo its from expected be might as 07, 0.93, = − − 1 h 1 ndciain oehrwt the with Together declination. in aalxo e vnLeeuwen (van Per 6 of parallax 13 .6PERSEI 6 2. AL 1 TABLE . m 4 e R87 D212989 HD 8078 HR Per 6 U 36 ± − Hipparcos s B 0 , . δ a,wihyields which mas, 5 .2 ossetwith consistent 0.62, = 51 = − 1 nrgtascension right in ◦ 3 lomeasured also ′ 57 rgtStar Bright ′′ (J2000)) − 1 UBV per- SCARFE eec sta u ausof dif- values notable our most that The is and here ference precision. determined Medeiros greater is much de period with the by only and obtained (1999), Udry those from slightly Ta- in respectively. presented 3 cycles. are and orbital velocities 2 eight bles CCD than The and more RVS 2457295. little The to a 2453213 is J.D. span total from 68 and CCD 2453040, the and with 2444257 J.D. between RVS the further making obser- of so hope theirs, the improvements. in to pursued comparable were quality vations of orbit yielded obser- spectrometer an velocity author’s radial the the however, with vations then, and By Medeiros de (1999). by Udry published a was that orbit way, when better under 1999, much until well not were by was observations it present (poor) But the ‘e’ (1989). graded al. was et and Batten elements the of values rejected sign. A plus circles a circles. filled as open shown as is as shown velocity data are CCD spectrometer data the CCD and DAO through The drawn elements the adopted them. with the Persei, 6 from of derived velocities curve radial observed The 1. Fig. t pcrltp sgvna 0II n its and III, Cepheus. K0 with as two given boundary about is Cygnus, the type of spectral of part Its south northern the degrees in lies I 103956, HIP pre- is elemsts 1. new Figure in the sented from derived curve velocity and Radial velocity (km/s) 10 20 30 40 50 0 0101030507091.1 0.9 0.7 0.5 0.3 0.1 −0.1 o esi h lmnsi al 0dffronly differ 10 Table in elements the Persei, 6 For with obtained were observations 155 Persei, 6 For h rgtsa R87 H 200817, (HD 8078 HR star bright The f ( M ,aesgicnl mle hnter.The theirs. than smaller significantly are ), α 21 = .H 8078 HR 3. h 3 m 48 Phase s K , δ n ec of hence and , 53 = ◦ 17 ′ 9 ′′ (2000)) a 1 sin BV i © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México a eetdobservation. Rejected − uinDt yl o ..O R.V. No. Cycle Date Julian 74.8.293. . 19.6.512. -0.4 0.0 -0.1 20.9 -0.5 21.4 -0.3 21.8 .7521 -0.5 21.5 -0.8 .7470 -0.3 22.1 .7268 51492.86 25.2 .7217 51484.83 25.2 .7027 25.8 51452.91 .5199 51444.89 0.4 .5009 51414.99 0.5 .4933 51126.79 -0.0 51096.91 35.0 0.5 51084.94 41.3 -0.6 44.3 .1219 0.0 44.5 0.1 .0385 41.1 -0.4 .0164 47346.98 38.4 .0094 47215.60 13.7 .0062 7.5 47180.71 2.0043 47169.65 .9974 47164.60 .9948 47161.60 47150.74 47146.69 70.3.7783-. 11.0.592. 0.8 -0.7 -0.9 27.6 -1.1 27.8 -0.6 28.3 -0.1 .4509 -0.8 28.2 .3510 0.8 29.4 .3155 51018.00 30.3 -0.2 .3092 50860.60 30.2 -0.7 .2744 50804.65 1.0 2.4 35.2 .2567 0.5 35.1 50794.75 -0.3 .2320 50739.87 36.0 0.5 1.1 .1245 7.4 50711.92 0.2 39.2 0.2 .1068 8.3 50673.02 40.5 -0.0 -0.1 .0821 50503.61 13.2 1.1 41.8 .9897 .0624 0.9 -0.0 50475.69 13.5 42.1 0.9 .9707 .0447 -0.4 50436.69 15.1 44.0 0.6 .9480 .0352 -0.5 50405.76 47138.63 21.2 1.1 .9372 .0313 10.0 40.3 50377.71 47108.63 0.6 22.2 0.7 .9132 .0093 9.5 -0.4 47072.81 22.3 50362.78 0.1 .7969 5.4 50356.76 47055.91 23.7 .9960 4.0048 -0.5 0.2 .7519 50321.97 47017.98 0.0 25.6 10.2 0.3 .7322 .9959 9.8 46834.68 0.5 26.0 50314.84 .6924 -0.8 .9827 50301.01 46763.80 27.1 16.4 -0.2 0.4 .5627 .9655 50300.90 46732.81 30.3 18.5 -0.2 0.2 .5077 .9617 50279.98 46670.00 29.5 19.4 -0.4 .4456 .8841 0.9 50252.98 0.6 46465.59 31.5 19.2 0.5 .2773 .8473 50246.96 46378.82 0.1 35.2 19.2 0.4 .2641 .8347 50124.60 46280.99 19.1 -0.5 0.5 44.5 .2261 .8214 5.9 50066.72 46015.78 0.2 21.8 .1129 .8208 0.3 50046.79 45994.84 19.9 24.4 0.1 .8176 1.0211 50025.76 45935.01 21.3 24.0 0.5 .9857 .7511 50024.82 45756.59 24.9 0.5 .8161 .6000 25.4 50019.86 45611.86 25.2 0.7 .7712 .5910 45556.01 26.1 49914.98 0.5 .5763 49676.74 45288.82 26.2 .5519 1.0 .5517 49662.63 45218.01 28.3 1.0 .5213 44910.82 28.4 .5149 49600.98 -0.4 44871.93 29.0 1.1 .4043 44824.02 29.6 0.7 .3884 44814.00 28.9 .3777 -0.1 44639.62 33.4 .3467 44614.62 33.6 .3112 44597.68 32.9 .1835 44548.87 .1664 44492.98 0.1620 44291.60 44264.66 44257.69 2,400,000 a hs ms km Phase & V AILVLCTE F6PERSEI 6 OF VELOCITIES RADIAL RVS HE PCRSOI IAIS335 BINARIES SPECTROSCOPIC THREE − 1 ms km − a uinDt yl o ..O R.V. No. Cycle Date Julian C − AL 2 TABLE 1 − 17.4.852. -0.1 26.1 .4845 51070.94 ,0,0 hs ms km Phase & 2,400,000 − 1 ms km − C − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México hc yields which codn othe to according antd n oorare colour and magnitude a 336 aalx(a eue 07 is 2007) Leeuwen (van parallax eetdobservation. Rejected − uinDt yl o ..O R.V. No. Cycle Date Julian 99.0.232. 035005 74 220.5 0.9 -0.0 22.2 -0.1 23.2 -0.1 22.6 1.5 .7340 0.2 22.7 .7062 23.0 -0.2 .6898 53040.58 24.9 -0.1 .6815 52996.74 -1.6 24.0 .6676 52970.76 -0.2 0.3 25.3 .6498 0.6 52957.83 26.1 -0.3 .6283 1.0 24.9 52935.86 0.0 .5285 27.4 26.5 52907.79 0.1 0.1 .4848 27.0 27.6 52873.90 -0.3 -0.6 .4671 27.6 28.1 52716.62 -0.5 .4356 -0.5 .4544 28.0 52647.76 0.1 27.5 .4203 -0.2 .4417 52619.80 27.7 1.0 27.6 .4051 -0.1 .4323 52599.73 49417.62 1.2 28.0 27.7 .3848 -0.4 0.1 .4132 52579.87 49393.60 28.8 29.9 .3634 -0.0 0.2 .3841 52564.89 49369.65 28.7 0.2 .3519 31.3 .3695 49337.73 29.5 31.8 52534.91 0.1 -3.1 .3248 .2862 31.6 49303.81 31.9 52489.02 0.2 -0.5 .3374 32.3 .2627 52465.98 49285.77 33.0 0.0 -1.3 .2816 .2507 49243.00 38.1 29.5 52334.60 .2139 -0.1 .1970 -1.0 49262.92 39.0 .1912 1.1 52297.56 32.2 .1691 -0.4 52278.68 49174.96 40.1 0.1 32.5 .0653 .1740 52220.68 0.5 0.3 49041.62 40.8 40.1 .0564 -0.1 52184.92 .1697 48997.65 42.7 -0.2 42.5 .0443 0.2 .1386 52157.82 48833.98 44.3 -0.3 0.4 .0316 42.0 .0432 5.2 0.3 48819.95 34.6 52151.00 0.3 .0240 .0343 0.3 48800.98 0.3 9.1 52101.99 34.9 .0171 48780.96 5.0337 9.7 22.8 51951.67 0.1 1.4 .0029 .9893 5.2 48768.97 51937.64 11.6 -0.2 .9672 3.0029 9.3 48757.98 12.7 51936.65 .9997 -0.2 .9628 51866.71 48735.67 10.4 13.1 .9896 -0.5 .9539 48735.66 17.2 51831.89 .9687 -0.1 .9450 48730.66 17.5 51824.86 .9686 -0.0 .9399 48714.72 18.7 51810.94 0.3 .8724 51796.85 48681.67 19.3 .8667 -0.0 48681.60 23.3 51788.84 .8280 -0.3 48529.90 23.9 .8210 -0.3 48520.93 23.9 0.1 .6535 48459.99 23.9 .6414 -0.2 48448.94 24.3 .6204 48184.85 27.6 .6084 48165.78 27.9 .5844 48132.77 .4098 48113.92 .3750 48075.98 47800.74 47745.99 79.5.183. 055646 82 84-0.3 -0.2 0.5 18.4 18.7 21.1 .8421 .8351 .7786 51634.64 51623.62 51534.61 -2.1 -0.5 0.6 26.2 -0.1 30.8 33.3 .3623 33.5 .2188 .1701 47726.00 .1460 47499.75 47422.94 47385.01 2,400,000 a M v yh- Catalogue Tycho-2 hs ms km Phase & 0.46 = ± V 5.92, = .2 ossetwith consistent 0.12, π 8.05 = Its . − 1 B − ± AL (CONTINUED) 2 TABLE V Hipparcos .3mas, 0.43 ms km 1.01, = − a uinDt yl o ..O R.V. No. Cycle Date Julian C − 1 SCARFE − rprmtoso 9msyr mas 59 of motions proper n 1msyr mas 11 and h aalxteeyedavlct f3. ms km 34.4 of velocity a yield these parallax the t pcrlclassification. spectral its 13.9.071. -0.4 15.2 .9077 51737.99 ,0,0 hs ms km Phase & 2,400,000 − 1 ndciain oehrwith Together declination. in Hipparcos − 1 nrgtascension right in − 1 lomeasured also ms km − a C − 1 − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México evr 18) R87 a nyasalvaria- and small period, a seven-year its only of years has six 8078 nearly for HR tion by published velocity (1985). variable Beavers possibly with stars of the to velocity. comparable sight, radial of systemic line the to perpendicular a eetdobservation. Rejected − uinDt yl o ..O R.V. No. Cycle Date Julian 42.8.132.807 79.2.312.6-0.23 -0.08 -0.20 26.86 -0.71 0.69 27.42 .4331 29.13 -0.09 28.73 .4090 -0.18 31.87 .3086 0.34 57294.92 .3029 32.18 0.12 57256.99 .2249 32.64 -0.21 57098.65 42.32 .1851 57089.63 -0.02 0.75 44.69 .1673 0.65 56966.69 6.17 -0.58 .0307 0.72 56903.97 -0.02 10.38 24.88 .0124 0.45 0.15 56876.00 22.66 23.81 .9808 -0.09 0.02 56660.71 23.03 24.87 .9604 .6103 -0.06 56631.77 -0.07 26.87 25.51 .7201 .5951 -0.10 56581.94 -0.10 29.67 26.93 .7061 .5660 -0.05 56549.88 54421.78 30.25 -0.64 27.43 .4739 .5381 2.77 56171.03 54397.84 -0.78 30.53 28.03 .2873 .4440 0.10 56148.99 54351.96 -0.44 .2619 37.87 27.98 .4091 0.14 55782.99 54307.99 -0.28 0.20 43.58 28.06 .2474 .3731 55488.88 54159.60 -0.33 42.86 30.93 .0659 .3459 -0.03 55448.84 54104.60 -0.16 31.32 44.28 .0387 .3339 0.12 -0.04 55426.02 54047.87 44.77 -0.09 31.34 .0260 .2175 55139.83 54004.95 44.05 -0.24 31.54 -0.08 .2086 .0177 0.06 55096.96 53986.05 .0127 33.41 5.37 -0.01 38.65 .2061 55077.00 53802.61 -0.46 0.05 .0095 34.42 .2048 15.34 53788.60 55063.98 -0.19 0.06 34.93 .1478 7.0044 55055.99 .9860 16.89 53784.59 -0.17 35.08 .1193 0.17 55051.00 18.63 53782.59 -0.57 .9097 36.28 .1149 -0.31 55042.98 19.72 53692.79 .8836 0.06 55013.97 40.71 .1016 -0.46 0.12 53647.89 .8444 0.10 20.12 36.46 .0858 54893.62 0.09 53640.93 19.93 .8122 .0056 54852.61 25.84 0.28 53619.93 22.78 -0.12 23.35 0.25 .8027 .0037 54790.80 53594.96 23.48 .7925 23.30 54739.93 -0.46 6.0005 53468.65 .6591 12.04 .9999 -0.13 23.71 54724.96 53465.65 9.22 .6514 .9999 54708.98 -0.25 53460.64 8.50 .9967 54498.62 -0.30 6.6268 53459.65 5.83 .9955 54486.58 53459.64 6.85 -0.01 .9955 0.00 53454.63 7.78 54447.76 .9929 0.14 53452.63 15.05 .9777 0.23 53452.62 15.53 .9732 53448.62 0.12 16.80 .9150 53424.60 17.86 .9080 53417.60 .8884 18.71 53325.81 .8682 53314.84 5.8441 53283.88 53251.96 53213.99 2,400,000 R87 aet h uhrsatnini list a in attention author’s the to came 8078 HR a hs ms km Phase & C AILVLCTE F6PERSEI 6 OF VELOCITIES RADIAL CCD HE PCRSOI IAIS337 BINARIES SPECTROSCOPIC THREE − 1 ms km − uinDt yl o ..O R.V. No. Cycle Date Julian C − AL 3 TABLE 1 − rlyasteato rsne rlmnr orbit preliminary a presented author sev- the for years variation variability the eral show following to After unable certainty. such therefore with missing was in and year, unfortunate observ- a was began sev- Beavers he the while after in soon ing, variation very the occurred that year enth lucky was author the ,0,0 hs ms km Phase & 2,400,000 − 1 ms km − C a − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México nTbe6 tsol entdta epoie his s provided km he 0.1 given that only of noted are precision be a solution, should to data orbital It the 6. con- Table to kindly in and him Griffin by by 19 tributed obtained the were perias- addition, that near In minima tron, the orbital respectively. of one presented 5 4.75 covering are observations and about velocities 4 is CCD Tables and 8078 in RVS HR The for 2457295. cycles. to span 2453144 2452971, total J.D. from and The CCD 2444548 the with J.D. 43 between and RVS the with definitive a of con- determination to the orbit. offered to kindly data very his he abstract tribute author’s 2001) the (Scarfe seeing print on But in cycle. the to of begun por- tion variable also rapidly the had through Griffin observations obtain R.F. mean- Prof. the however, In time, Society. Astronomical Canadian the to cross. a rejected as a 1. shown and 8078, Figure is triangles, in velocity filled HR RVS as as shown shown of are are data data velocities Griffin’s DAO drawn elements The radial adopted them. the observed through from derived The curve the with 2. Fig. 338 eoiycredrvdfo hmi rw through 2. drawn Figure is in data them the from derived curve velocity of adjustment small point. a so- zero after the their weight, in unit included with were a lution They merit to digit. appear decimal they second that sugggest residuals small 14 ietln between line direct Radial velocity (km/s) ′ −36 −32 −28 −24 −20 −16 o R87,14osrain eeobtained were observations 164 8078, HR For D228 HP110900, (HIP 212989 HD the and 10 Table in presented are elements The 55 0101030507091.1 0.9 0.7 0.5 0.3 0.1 −0.1 ′′ 20) st efudi eau,ams na on almost Pegasus, in found be to is (2000)) ǫ .H 212989 HD 4. and α Phase e,adsihl lsrto closer slightly and Peg, α 22 = − h 1 28 u hi very their but , m 7 s , δ 12 = SCARFE ◦ h eodr,sgetn httepiaysa is of sequence. star main light cos primary the the from the by evolved that for somewhat accounted suggesting secondary, be type, can the spectral than its from more expected by be would than nous ulmgiueof magnitude sual π ic h urn eaaini ls ooeacsec- arc one to close is ond. colours, separation con- and current magnitude doubt the above no magni- the since to but 2.28 little primary, is a the tributes secondary than The fainter binary, a years. tudes visual with 554 J22281+1215, a of WDS of or noted period primary 15972 be ADS the should as is It known V. 212989 K0 HD type, that MK its with sistent ih seso n 9msyr mas -9 and ascension right u,1966) gue, Its latter. the ntr il eoiyo 73k s km 57.3 of velocity a yield turn in lomd ihteCDdt n h f aaof data CfA the and data CCD was the 7 solution with Tables separate made in a also Because presented cycles. are respectively. orbital 8 data 6.5 and CCD over is and case RVS 2457295. this The to in 2453180 2452971, span J.D. total from and The CCD 2444823 the with J.D. 51 between and RVS the with magnitude. the absolute brighter of value even recent an more by A obtained it IV. parallax that K0 suggest as and reclassified the 3.0, be that is to find magnitude also not absolute They appear star’s they orbit. its although ratio redetermined system, mass have the uncertain for rather 0.72 com- a of secondary obtained (2014) and spectroscopic Mas- al. faint ponent of et very data Halbwachs a recently the detected More with al. consistent et be sarotti observations to author’s shown the is from value and paper correct this The in to derived period. them incorrect led data an their determine of of distribution case the which the 212989 for in HD binaries Unfortunately of orbits. list in- determined long who they a (2008), in ob- 212989 other al. HD of cluded et attention Massarotti the including to the servers, came in However also it since. ever meantime followed The been the and has discovered 1980s. system soon was early nature the binary primary’s in spec- velocity available radial to became the try list trometer after not observing until did lack He his that velocity. was on remedy radial stars it known of no when had handful student, that small graduate a a of still one was he when sight. of line the to 15 = The o D228,19osrain eeobtained were observations 169 212989, HD For attention author’s the to came first 212989 HD lomaue rprmtoso 9 a yr mas 196 of motions proper measured also . 87 Hipparcos ± V 1 . 7.06, = 8ms hc ilsa bouevi- absolute an yields which mas, 18 UBV M antd n oor r (Ar- are colours and magnitude aalxo D228 is 212989 HD of parallax GAIA B-V v 3.06 = 0.90, = 11 a,wudyield would mas, 11.14 , − 1 ndciain which declination, in ± U-B .6 oelumi- more 0.16, − 1 perpendicular .6 con- 0.56, = Hippar- − 1 in © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México uinDt yl o ..O R.V. No. Cycle Date Julian − 60.7.69-01-. 09.6.95-88-1.1 -0.5 -0.1 -18.8 -0.4 -18.2 -0.3 -17.8 .2905 -0.2 -18.2 .2823 -0.7 -18.2 .2668 -0.6 50995.96 -18.2 .2079 -1.0 50973.96 -18.8 .1982 -1.0 50932.01 -18.8 .1846 50774.59 -0.8 -19.2 -0.2 .1703 0.8 50748.69 0.1 -19.3 .1595 -0.3 50711.77 -19.7 -0.1 .1566 0.6 50673.83 -20.1 -18.3 0.5 .1465 0.9 50644.91 -19.6 -20.8 0.1 0.4 .1122 50636.78 -19.2 .7639 0.2 -20.7 .1071 0.1 -18.5 50609.95 .7516 0.1 -20.9 .0703 0.9 -18.8 50518.07 .6885 -22.3 0.3 46902.97 .0598 50504.09 -18.7 -0.2 .6770 -23.7 0.2 46870.05 .0544 50405.56 -18.2 -0.1 .6665 -23.4 -0.1 .0468 46700.86 -0.3 -18.0 50377.59 .6572 -25.5 -0.4 .0390 46669.81 -0.7 -18.0 50362.68 .5609 0.1 -27.4 46641.86 .0366 50342.65 -18.2 0.3 .5560 -31.0 0.8 0.1 46616.96 .0312 50321.80 -18.4 .5389 -32.2 -0.0 0.8 46358.65 .0234 -17.9 50314.86 .5036 -0.4 .0133 46345.79 -32.9 -17.1 -1.0 50300.94 .4883 -34.7 0.8 .0111 1.0 46299.90 -17.9 50279.87 .4748 -33.4 0.3 46204.99 0.7 50252.96 -18.2 3.0058 .4531 -33.6 -0.1 .9988 0.4 46164.05 50246.92 -17.0 .4456 -28.8 -0.8 .9869 0.1 46128.09 -17.5 50232.85 .4251 -24.4 -0.3 0.2 46069.55 .9791 50213.90 -17.8 .4095 -23.3 0.4 .9657 46049.57 0.8 50181.94 -18.5 .4028 -22.8 0.2 0.7 45994.72 .9282 -18.0 50161.05 .3786 -22.5 -0.0 .9077 45952.86 50125.13 -17.3 -0.1 .3574 0.2 -21.0 .8937 45934.93 -0.0 -17.5 50024.67 .3214 -20.6 0.1 .8872 45869.96 0.3 49969.74 -17.7 .3079 -20.6 -0.6 0.0 45813.02 .8630 49931.87 -17.5 .2954 -20.4 0.3 .8460 45716.61 49914.87 0.4 -17.6 .2823 -20.0 -0.7 45680.57 .8040 0.3 -18.4 49849.92 .2659 -20.1 0.0 .7984 45646.74 -0.4 49804.04 -17.5 .2615 0.2 -19.2 45611.74 .7933 -18.5 49691.57 -0.6 .2238 0.3 -18.9 .7805 45567.81 49676.62 -18.0 .2193 -19.3 -0.4 45555.85 .7358 -17.9 49662.60 .2138 0.6 -19.4 45454.00 .7021 49628.71 -17.9 .1774 -0.7 .6593 45443.03 -18.8 .1617 49508.88 0.1 45428.03 .6526 -17.9 49418.06 .1540 -0.6 45330.59 49303.64 -20.1 .1405 0.7 45288.57 -24.2 .1349 49285.72 45267.73 0.2 -26.3 .0967 -0.1 45231.72 -27.4 .0360 0.5 45216.78 .0297 -33.2 45113.99 0.3 -34.5 .0207 44951.54 -31.5 1.0051 44934.72 .9884 -22.3 44910.63 .9765 44868.72 0.8857 44823.92 44791.94 44548.67 ,0,0 hs ms km Phase & 2,400,000 V AILVLCTE FH 8078 HR OF VELOCITIES RADIAL RVS HE PCRSOI IAIS339 BINARIES SPECTROSCOPIC THREE − 1 ms km − uinDt yl o ..O R.V. No. Cycle Date Julian C − AL 4 TABLE 1 − ,0,0 hs ms km Phase & 2,400,000 − 1 ms km − C − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México a 340 eetdobservation. Rejected uinDt yl o ..O R.V. No. Cycle Date Julian − 97.4.41-90-. 27.8.20-70-0.6 0.6 -0.0 -27.0 1.1 0.7 -27.1 0.8 -30.5 .0270 1.0 .0222 -32.8 -34.3 -0.5 .0140 52970.58 -34.2 1.5 4.0035 52957.65 -33.8 .9954 -1.2 52935.68 -31.1 .9935 -0.7 52907.72 -28.4 -0.2 .9909 -3.9 52885.82 0.2 -30.3 -0.2 .9701 52880.90 -0.3 -28.5 -0.6 .9667 -19.0 52873.85 0.6 -31.1 -0.1 .9622 -18.9 52817.98 0.2 0.9 -23.4 .9540 -19.2 52808.94 -23.1 .6471 0.2 0.3 .9493 -18.7 52796.97 .6366 0.2 -21.7 -0.1 .9065 -18.3 52775.00 0.4 .6235 -21.2 .8886 -0.5 49270.64 -17.8 52762.02 .6113 0.5 -21.6 -0.3 49242.80 .8756 -18.1 52647.56 .5915 0.9 -21.5 -0.6 49207.88 .8722 52599.63 -18.5 1.0 -21.0 .4800 -0.1 49174.88 .8645 -18.2 52564.76 .4778 -20.7 -0.8 -0.7 49121.98 .8577 -18.3 52555.70 .4718 -19.9 .8473 -0.4 48822.90 -0.1 -17.8 52534.88 -18.7 .4457 0.2 -0.1 48816.92 .8389 -18.5 52516.81 .3811 0.3 -20.1 -0.4 48800.91 .8212 52488.90 -18.1 .3733 0.6 .7472 -19.5 -0.3 48731.02 -17.5 52465.93 .3404 -0.1 -19.3 -0.2 48557.63 .7240 -18.1 52418.94 .3294 0.2 -18.8 -0.0 48536.80 .7212 52220.59 -18.1 .2420 0.2 -0.2 -18.0 48448.75 .7011 -18.1 52157.78 -18.6 .2348 -0.4 -0.2 48418.94 .6845 -19.1 52150.82 .2141 -18.2 -0.2 -0.2 48184.79 .6152 -19.1 52096.96 0.1 -18.5 .2014 0.1 .6022 48165.69 -20.3 52051.98 -18.3 .1065 -1.0 -0.0 48109.84 .5863 -20.7 51866.58 .0988 -18.1 .5672 -0.7 48075.93 0.4 51831.66 -21.3 -17.7 .0782 -0.0 .4579 -0.8 47821.65 -23.8 51788.72 -18.8 .0708 -0.5 -0.1 47800.70 .4547 51737.91 .0593 -24.3 -18.5 .4285 -0.5 -1.0 47745.87 51444.73 -34.9 -17.7 .0391 0.1 -0.5 .4207 47725.82 -33.2 51435.76 -18.2 -0.3 -0.0 2.0343 47694.83 .3966 51365.95 -32.9 0.5 .9864 0.4 -18.7 .3392 47641.02 51344.98 -29.6 -18.2 .9815 0.0 .3362 47627.94 -28.4 51280.04 -18.0 .9786 -0.5 47499.64 .3282 51126.60 -24.7 -17.2 .9655 0.6 .3236 47486.60 51118.60 -24.5 .9577 0.3 .3184 47478.63 -24.5 51096.68 .9295 .2988 -0.4 47443.60 51084.77 -22.5 .9212 1.1 47422.72 51070.77 -21.5 .9134 0.2 47346.94 51017.88 -22.0 .8971 -0.1 47324.92 -19.8 .8603 1.0 47303.95 -20.6 .8547 1.2 47260.00 -20.6 .8272 0.3 47161.55 -19.3 .8208 47146.64 -19.0 .8067 47072.69 -19.6 .7945 47055.73 .7881 47017.92 .7676 46984.90 46967.92 46913.02 ,0,0 hs ms km Phase & 2,400,000 − 1 AL (CONTINUED) 4 TABLE ms km − uinDt yl o ..O R.V. No. Cycle Date Julian C − 1 SCARFE − 2,400,000 a hs ms km Phase & − 1 ms km − a C − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México uinDt yl o ..O R.V. No. Cycle Date Julian − uinDt yl o ..O R.V. No. Cycle Date Julian − 56.7.01-05 .35247 69 1.7-0.13 0.05 0.08 -18.87 0.10 -18.60 0.23 -18.05 .6398 0.33 .6257 -17.92 0.01 .5219 -17.77 57294.76 0.22 -17.66 .4940 57256.90 0.13 -17.68 .4877 56978.70 0.04 -0.08 -17.46 .4836 0.33 56903.80 0.03 -17.54 .3486 0.33 56886.86 0.09 -20.93 -17.73 .3385 56875.91 0.12 0.08 -17.49 -20.54 .3310 56513.90 0.43 -17.56 -0.05 -20.42 .8226 .2258 0.06 56486.95 -0.14 .2124 -20.13 -18.83 .8081 56466.90 0.39 -0.17 .1968 -19.19 -19.79 .8047 55103.77 56184.74 -20.53 0.11 -0.60 -19.23 .7891 .1124 56148.88 55064.87 -0.06 -0.24 -19.22 -21.28 .6924 .0759 56106.97 55055.83 -0.03 .0696 -0.06 -19.56 .6868 -24.52 55013.96 55880.59 0.06 -29.91 -0.25 -18.54 .6813 .0558 54754.74 55782.96 0.27 0.38 -18.21 -29.05 .6705 5.0346 55765.98 54739.75 0.12 .9662 -18.37 -25.91 .5619 54724.82 55728.96 -0.30 -17.40 .5336 .9614 -24.91 55672.00 54695.94 -0.20 -17.56 .5202 .9383 55488.69 54404.69 0.52 -17.98 .2796 .9308 54328.98 55475.86 -0.24 -17.96 .2702 54292.97 55413.87 0.13 -17.23 .2598 53647.76 0.12 55393.93 -18.46 .2412 53622.82 -0.21 -18.35 .2341 53594.88 -0.02 -18.67 .1553 53544.97 -19.23 0.17 .1349 53525.97 -19.11 .1177 53314.70 .1080 -19.34 53259.81 .1054 53213.89 4.0920 53187.93 53180.90 53144.96 23.6.76-22-. 30.0.38-41-0.3 -0.2 -0.0 -24.1 -0.2 -25.6 -0.2 -26.4 .0388 -0.1 -29.1 .0310 0.0 -30.4 .0269 0.1 53002.30 -31.1 .0183 52981.27 -0.2 .0146 -31.9 52970.37 -34.6 -0.2 .0124 52947.32 -0.2 -35.2 4.0098 52937.44 -0.4 .9993 -34.2 52931.43 0.6 .9938 -32.2 52924.42 -0.3 -30.8 52896.47 .9859 -0.1 -28.0 .9766 52881.57 -0.1 -27.3 .9692 -0.3 52860.55 -23.8 .9591 -0.2 52835.56 -22.7 .9479 52815.56 -0.1 -22.4 .9079 52788.55 -21.9 .8856 52758.65 .8710 -21.3 52651.23 .8587 52591.41 3.8405 52552.41 52519.49 52470.57 ,0,0 hs ms km Phase & 2,400,000 ,0,0 hs ms km Phase & 2,400,000 .F RFI’ AILVLCTE FH 8078 HR OF VELOCITIES RADIAL GRIFFIN’S F. R. C AILVLCTE FH 8078 HR OF VELOCITIES RADIAL CCD HE PCRSOI IAIS341 BINARIES SPECTROSCOPIC THREE − − 1 1 ms km ms km − − uinDt yl o ..O R.V. No. Cycle Date Julian C uinDt yl o ..O R.V. No. Cycle Date Julian C − − AL 5 TABLE AL 6 TABLE 1 1 − − 2,400,000 2,400,000 a a hs ms km Phase & hs ms km Phase & − − 1 1 ms km ms km − − C C − − 1 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México 342 uinDt yl o ..O R.V. No. Cycle Date Julian − 79.76.96020354284 17 11-1.0 -0.9 -0.8 -1.1 -0.8 -0.8 -1.1 -1.1 -0.2 .1873 -1.2 -1.4 -1.5 .1830 -1.6 .1783 51452.8244 -0.9 .1672 -1.1 51444.7755 -0.4 -2.2 .1460 51435.8225 -2.4 .1413 -0.3 51414.8650 0.3 -0.8 -2.0 51374.9610 .1300 1.1 -0.5 0.2 .1201 51365.9580 0.0 -1.0 1.7 0.2 0.2 .1116 -0.4 51344.9580 2.4 51325.9787 .0349 0.2 -0.8 -1.2 4.5 0.5 0.1 -0.7 51309.9924 3.8 .0286 .1936 5.0 0.8 51165.5722 .0142 -0.1 0.5 .0902 5.2 0.3 2.2 -0.7 4.0027 51153.6808 .0603 7.6 47694.9736 3.2 .9984 -1.2 51126.6860 0.8 .9921 .0492 9.3 47499.6503 -0.3 51104.7283 -0.2 4.2 .9847 .0291 9.2 47443.7666 5.1 -0.5 51096.7384 -0.1 .9566 51084.7842 .0201 8.7 47422.7953 -0.3 10.7 0.3 .9333 51070.8479 9.5 47384.8836 9.8 -0.9 2.0092 0.3 .8434 51017.9478 .9973 9.0 47367.9293 -0.0 10.0 0.8 .8381 50973.9700 .9106 9.0 47346.9512 0.8 -0.0 10.3 .8275 50804.5674 .9026 8.0 47324.9611 0.3 -0.6 10.1 .8090 50794.5989 .8825 8.4 47161.5570 0.6 10.4 -0.0 .7942 50774.6409 .8548 6.7 47146.6255 0.5 8.3 -0.8 .7736 50739.7690 .8344 6.0 47108.6186 1.6 7.6 -0.1 .7402 50711.7828 .8184 47055.8070 0.8 7.7 0.8 6.4 .6318 50672.9380 .6831 5.4 47017.9251 0.6 7.3 -0.7 .6169 50609.9699 .6661 5.9 46987.9038 0.9 8.2 -0.9 50405.6555 .6500 .6090 46732.7450 1.2 5.2 6.8 -0.8 .5984 50377.6916 .6349 5.2 46700.8650 0.4 4.6 -0.9 .5873 .6216 46669.8700 0.6 4.8 50362.7435 4.9 -1.0 50342.7957 .4778 .5836 46641.9320 1.5 5.0 4.8 0.7 .5762 50321.8482 .4534 46616.9760 1.6 4.2 4.6 -0.6 .4437 .5651 46345.8030 4.1 50314.8741 4.3 0.0 -0.4 50300.9262 .4397 .5561 46299.9150 0.3 3.7 0.7 4.4 .4349 46280.9340 0.8 3.5 50279.9381 .5476 0.2 3.1 .4211 0.3 .5401 46273.9730 1.1 50262.9676 3.4 -0.1 .3312 46264.9560 1.2 1.3 .4297 3.9 50246.9377 0.0 .3189 46238.9500 1.4 50232.9694 .4270 3.2 0.4 .2915 3.1 46069.6450 0.4 .4122 0.2 50024.6762 .2597 46045.6200 0.5 .4005 50019.7456 1.4 -0.0 .2349 45994.7110 .3804 49991.7588 0.2 -0.4 .3714 .2253 45934.8600 49969.8287 -0.6 -0.1 .1443 45887.9810 49931.9626 -0.7 .2827 0.1 49914.9269 .1249 45869.9720 -0.0 1.4 .1069 45716.5710 -0.2 1.3 49747.5866 .0883 45680.6430 1.2 0.3 .0692 45646.7660 0.6 10.6 .0655 45611.8360 11.4 -0.9 45575.8180 1.0587 11.4 .9391 45567.8790 8.8 .8867 45555.8980 6.4 .8793 45330.6020 .7168 45231.7660 45217.8230 0.6703 44910.6780 44823.9450 ,0,0 hs ms km Phase & 2,400,000 V AILVLCTE FH 212989 HD OF VELOCITIES RADIAL RVS − 1 ms km − uinDt yl o ..O R.V. No. Cycle Date Julian C − AL 7 TABLE 1 SCARFE − ,0,0 hs ms km Phase & 2,400,000 − 1 ms km − C − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México uinDt yl o ..O R.V. No. Cycle Date Julian − 97.11.40080059062 92 . 0.0 -0.2 -0.4 5.4 -1.1 5.4 -0.5 0.8 5.6 .9926 1.0 5.9 .9895 0.4 7.6 52970.6423 .9855 9.6 0.0 52964.7858 9.9 .9741 -1.1 0.1 .9593 52957.7361 9.5 0.6 0.0 -0.6 .9477 52935.7296 10.0 .9451 0.8 0.1 52907.8713 9.0 1.0 0.2 .9411 52885.9212 10.3 -0.4 8.7 0.8 52880.9527 .9116 -1.1 -0.6 1.4 0.7 9.3 .9005 52873.9128 -0.0 .2529 .8212 9.3 0.0 -0.0 52817.9582 -0.1 .7958 .2450 1.1 7.8 0.2 -0.4 52796.9670 .2375 .7850 49691.5942 52647.5825 0.7 9.5 -0.5 -0.1 52599.6763 .2196 1.9 .7773 49676.6171 8.4 -0.5 -0.1 .2048 9.3 .7667 49662.6172 52579.7688 1.3 -0.3 -0.8 .1820 0.3 .7614 49628.7905 52564.7953 8.9 0.0 -0.7 .1735 0.2 9.7 49600.8302 0.2 52544.8153 .7371 -0.9 .7247 .1560 49557.9418 52534.8593 -0.6 8.1 -0.3 -1.5 .1465 6.2 .7222 49541.9573 0.1 52488.9514 -0.6 -0.5 .7000 52465.9794 .1300 0.8 6.0 49508.9641 0.1 -0.1 .0890 5.1 49490.9800 0.4 52460.9678 .6355 -0.1 -0.0 .5757 52418.9850 .0821 0.2 49460.0146 0.8 5.7 0.3 .5686 .0651 6.0 49382.5814 0.2 1.8 0.8 52297.5801 .5646 52184.7969 .0472 49369.5881 2.1 0.7 5.0 -0.1 52171.7932 .0375 5.0 .5577 49337.5972 0.4 -0.1 3.5 .5291 52163.8354 .0296 49303.6637 5.1 4.7 -0.2 0.6 .0254 .5169 49285.6724 0.3 6.1 52150.9223 0.3 4.6 .5056 52096.9782 49270.7531 0.5 7.0 0.1 3.2 3.0148 .9964 .4445 49262.7455 0.1 52073.9694 0.2 2.8 10.7 52052.9794 .9836 .4440 49242.8377 9.7 0.4 3.3 -0.1 .9788 0.1 .4069 49207.8844 0.3 9.8 51937.5796 3.0 .8847 .3884 49183.9248 9.3 51936.5844 0.2 2.9 -0.3 .7979 .3845 49174.9253 0.2 9.0 51866.6362 -0.0 3.1 .7948 2.8 .3773 48997.6181 9.2 51831.7639 -0.2 -0.9 .7888 .3699 48833.9026 8.6 51824.7739 2.3 -0.0 .7804 -0.6 0.5 .3656 48827.9263 9.0 51810.7897 -0.3 -1.0 .3641 .7698 48816.9241 6.8 51796.8018 -0.8 -0.8 .7634 -0.9 .3247 48800.9651 6.8 51788.7770 -0.9 -0.7 .2307 51785.9237 .7577 48780.9738 6.5 -1.1 -1.2 .6513 .2043 48768.9631 5.4 51711.9709 -0.4 -1.1 51534.5825 .6365 48757.9716 5.2 .1936 -0.4 .1873 .6317 48557.6834 0.0 4.7 51484.7367 .5994 48529.7689 3.6 .1830 -0.4 51464.6950 51452.8244 .5937 48520.7706 0.1 3.5 .5777 48459.9031 3.4 -0.2 51444.7755 .4534 48448.8345 2.7 -0.7 .4434 48418.9670 0.3 0.9 .4137 48184.7600 0.2 -0.5 .3959 48165.7557 -0.6 .2497 48109.9291 0.2 .2206 48075.9130 -1.2 .2100 47800.8056 .1936 47745.9113 .0902 47725.9248 47694.9736 47499.6503 ,0,0 hs ms km Phase & 2,400,000 HE PCRSOI IAIS343 BINARIES SPECTROSCOPIC THREE − 1 AL (CONTINUED) 7 TABLE ms km − uinDt yl o ..O R.V. No. Cycle Date Julian C − 1 − ,0,0 hs ms km Phase & 2,400,000 − 1 ms km − C − 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México evto ntewogbac ftevlct curve. velocity the of ob- branch final wrong their the simply placing on is in servation solu- (2008) unfortunate erroneous were al. the they et of that Massarotti origin by the In presented that solution. tion clear new is in the it to way fact conform satisfactory data very CfA the the the DAOwhich to seen from attesting be that only, to can similar data As very respectively. is solution 4 CfA-CCD and data 3 corresponding Figures the in CfA-CCD through the drawn from so- are and the only, solution, from data curves DAO velocity from The lution 10. Table in- in and are cluded above mentioned they solution where CfA-CCD data, the CfA from the for except solution, of nal adjustment CfA no the necessary. but was solution point 0.5, also that zero weight are their In given data were CfA 9. data those Table (2008), in reproduced al. et Massarotti data. rejected no as are there meaning that same except the 1, have Figure symbols for drawn The elements adopted them. the through from 212989, derived HR curve of velocities the radial with DAO observed The 3. Fig. 344 nua eaaino h tr taato,o two plausi- the on make we apastron, both, at For stars likely assumptions. different the the of of values separation it below angular this, interfer- estimate companions Despite We the detect ometrically. similar. to are possible be types might spectral least especially their at primaries, must if the be it than must fainter and companions magnitudes data, 2.5 the our that in concluded be companions faint of trace Radial velocity (km/s) −3 12 naltbe h eiul r hs rmtefi- the from those are residuals the tables all In l he iaisdsusdi hspprso no show paper this in discussed binaries three All 0 3 6 9 0101030507091.1 0.9 0.7 0.5 0.3 0.1 −0.1 .DISCUSSION 5. Phase SCARFE qain.Tefis steeuto ftems func- two mass following the which of the in equation of the tion, and is use first 8078, make The HR evidence We equations. and of want contrary. Per for the 6 212989, to HD of for cases masses the solar 1.2 in that Sun twice is the mass of primary’s the that assumption ble data CfA the and circles, circles. The filled open elements as them. as shown the through are drawn from data data derived DAO those curve all the from with obtained (2008) HR Massarotti by of used al. were velocities et that radial CfA from CCD those DAO and observed 212989, The 4. Fig. asratio mass tion ftescnay and secondary, the of periastron a eaain taato f8,2 n 1msfor mas 81 and 20 binaries. 87, three of the apastron at separations lar respectively. the 212989 and cos HD elements, relevant and the 8078 values, These HR Persei, 6 for o a eetdwt icly ee e sassume us let compan- Here, the difficulty. that where with (2007), detected of was al. components et ion the Scarfe for by found 6046 was HR as mass, are in they similar stars, the between differences luminosity the in()gvsiciain f43 of inclinations gives (1) tion Radial velocity (km/s) −3 12 h eodeuto sfrtepoetdsepara- projected the for is equation second The u rtmto eisb suigta despite that assuming by begins method first Our 0 3 6 9 aalxs nee noeuto 2,yedangu- yield (2), equation into entered parallaxes, 0101030507091.1 0.9 0.7 0.5 0.3 0.1 −0.1 ρ q ρ = 0 = taato,i em fteparallax the of terms in apastron, at π ( . o l he iais nta aeequa- case that In binaries. three all for 9 ω q a n h eccentricity the and , 1 h inclination the , sin M M i 1 f 1+ (1 ) 1 stepiaysmass, primary’s the is ( sin M q ) 3 q = i − = Phase 1 M 1+ (1 ) 1+ (1 2 i /M and , q 3 ◦ 1 6 31 .6, q e e . ) sin ) h ruetof argument the , 2 a 1 sin ◦ ω 2 n 26 and .2, cot M i . 2 i Hippar- sthat is π the , (1) (2) ◦ .9 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México uinDt yl o ..O R.V. No. Cycle Date Julian − 49.95.4879 06 79.42.8910 -0.41 -0.12 -0.04 1.01 -0.18 1.07 -0.08 1.05 .2869 -0.22 0.71 .2726 -0.09 -0.85 .2668 57294.8452 0.66 -1.02 .2541 57267.9632 -0.06 -0.17 -0.37 .1329 57256.9600 -0.05 -0.66 1.07 .1017 57232.9913 9.30 -0.09 -0.14 0.06 .0647 57004.6682 8.72 9.96 -0.29 0.67 56945.7682 7.95 7.0530 10.06 -0.26 0.42 .9350 56875.9542 8.36 7.84 .7805 -0.37 0.66 .9086 56853.9864 7.93 8.23 .7498 -0.15 0.82 .8726 56631.6417 7.76 7.90 .7430 54455.6695 -0.42 0.19 .6980 56581.7966 7.48 5.29 .7255 54397.6975 -0.22 .6837 56513.9475 7.51 0.12 5.20 .7128 54384.8422 -0.09 .6789 56184.8531 4.91 -0.20 -0.64 .7022 54351.8404 -0.04 0.01 .4932 56157.9509 5.06 .6905 54327.9855 -0.01 -0.59 .4763 56148.9217 4.55 -0.01 5.26 .5392 54307.9768 .1101 -0.34 55798.8729 3.04 9.20 0.36 .5361 54285.9683 -0.29 55766.9888 6.0921 2.83 -0.09 .4937 54000.8800 9.48 55076.8316 -0.02 .9911 2.13 -0.16 .3911 53994.8867 55042.9717 -0.07 .9392 10.08 2.12 9.82 .3757 53914.9421 -0.18 54852.5847 2.22 .9313 0.05 .3519 53721.6642 9.86 54754.7573 2.16 .9234 0.24 .3482 53692.6898 .9149 2.04 54739.8310 .3376 53647.8253 0.26 2.07 54724.8892 .9080 .3371 53640.8079 0.32 54708.8515 1.82 .3366 53620.8551 -0.00 -0.07 54695.9571 .3239 53619.8451 -0.06 -0.28 .2963 53618.8871 0.21 -0.71 .1752 53594.9464 0.58 -0.89 .1530 53542.9589 -0.62 .1419 53314.7687 .1170 53272.8604 -0.23 .1079 53251.8758 53204.9695 5.1042 53187.9541 53180.9457 uinDt yl o ..O R.V. No. Cycle Date Julian − 91.65.5410 .359847 .9442 -0.63 -1.03 0.49 4.24 0.12 0.19 -0.64 0.69 0.30 4.9984 0.14 0.13 .2259 0.01 52978.4776 .2137 -0.11 -0.11 49638.6335 .2010 -0.45 .1867 -0.11 49615.6679 -0.62 0.53 .1687 49591.6643 .1528 49564.7900 -0.40 -0.24 .0852 49530.7768 -0.22 1.06 49500.8219 0.87 -0.10 .0698 0.65 49373.4591 2.18 0.29 .0534 49344.5245 3.38 0.19 .0407 6.10 0.78 .0253 49313.5625 6.99 49289.6171 3.0131 9.72 -0.21 .9925 49260.7318 9.84 .9787 49237.7163 8.67 .8188 49198.7784 .7871 49172.8300 48871.6095 2.7754 48811.8584 48789.8289 ,0,0 hs ms km Phase & 2,400,000 ,0,0 hs ms km Phase & 2,400,000 C AILVLCTE FH 212989 HD OF VELOCITIES RADIAL CCD F AILVLCTE FH 212989 HD OF VELOCITIES RADIAL CFA HE PCRSOI IAIS345 BINARIES SPECTROSCOPIC THREE − − 1 1 ms km ms km − − uinDt yl o ..O R.V. No. Cycle Date Julian C uinDt yl o ..O R.V. No. Cycle Date Julian C − − AL 8 TABLE AL 9 TABLE 1 1 − − ,0,0 hs ms km Phase & 2,400,000 ,0,0 hs ms km Phase & 2,400,000 − − 1 1 ms km ms km − − C C − − 1 1 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México units. ae,b en feuto 3,i which in (3), equation paral- of their means and by Law major laxes, Third systems’ the Kepler’s of using sizes semiaxes, angular the estimate to is mas. 73 of apastron at separation l 21) hc ilsa nlnto f32 of et inclination Halbwachs an by yields found which 0.72 (2014), of al. ratio mass liminary apastron. than other separation phases angular at the larger Per, be 6 may of the despite orbit so eccentric inclination, very high the result to smaller due This primarily is mas. 27 of separation apastron an 104 of inclination an esi oraxadBffi 20)md s of use made (2003) Boffin and the Pourbaix Persei. 6 magnitude. of order in er and years 346 wc hto h u,a ehv oeaoe found above, done have we as Sun, q the of that twice h ao eixsadparallax, and semiaxis major the oasm o l he iaisteaeaevalue average the binaries three namely sin 23052, all of HD for for assume (2012) to Griffin and Scarfe by Saf 90.Ti un qain()it cubic a into (1) equation in turns equation This 1970). (Scarfe rno 3 2ad4 a o ah hs eut are results for These those each. for than mas smaller 44 slightly and 12 apas- and 63, at order, of separations above tron angular the yields in (2) stars equation three then the for 0.405 and 0 = natraie n oehtdffrn approach different somewhat and alternative, An o D228 ecncos oaottepre- the adopt to choose can we 212989 HD For ecnprasd itebte ntecs of case the in better little a do perhaps can We h eodmto sflo h rcdr used procedure the follow is method second The Hipparcos . γ ω a s (km 1) (wt. S.E. f e K T bet6PrH 08H 199H 212989 HD 212989 HD CfA CCD, 8078 HR CCD RVS, RFG CCD, RVS, Per 6 CCD RVS, P used Data Object 3 6 sn hs eut neuto 2 yields (2) equation in results these Using 56. 1 ( i k s (km hc o admdsrbto s0.589 is distribution random a for which , M dges 266.4 (degrees) (J.D. dy)1576.23 (days) k s (km sin M ( ) q i M hc ilsms aiso .8 0.47 0.68, of ratios mass yields which , stettlms ftesse nsolar in system the of mass total the is − G)201.8 (Gm) − − nemdaeatoercdt ofind to data astrometric intermediate 1 ⊙ 1 25.84 ) ,5,0)307.31 2,450,000) 19.82 ) 0.1321 ) a = ◦ n suigapiaymass primary a assuming and , P π − 1 2 / .3 .3 .2 0.316 0.328 0.235 0.333 ) 3 M 1 0.8828 q / 3 0 = P stepro in period the is . ± ± ± ± ,btsimilar but 9, ± ± ± ± .070.0564 0.0017 .070.7350 0.0007 0.04 .68.66 0.06 .22898.3 0.12 . 197.2 0.3 . 216.5 0.9 .42681.08 0.04 a and RIA ELEMENTS ORBITAL ◦ 7ada and .7 π are (3) AL 10 TABLE SCARFE − 20.24 ± ± ± eso h A tff npriua .Bohlender, D. particular in staff, the DAO acknowledge mem- the to of of assistance like bers and also to support would 8078 appreciated He greatly HR of work. observations this his contributing ously prop- fundamental other erties. and masses de- confident of permit termination will interfer- secondaries reliable the Ultimately, that of conclusion detection possible. the is not observation but ometric results, parallaxes the better of and values, of larger from apas- magnitude give than of may other order phases tron since the discussion separations, above give likely the to the that noted only be intended to is is It three. on all information valuable much yield ob- Interferometric would un- servations is systems. two but HD other al., of the et for Halbwachs case proven of the work in the That from correct 212989, be object. to compact un- main- more appears a our a assumption not is of and secondary star correctness the sequence the de- that on interferometry, assumption derlying course, modern of to pending, amenable 8078 are HR that for mas 212989. 46 HD Per, for 6 mas major for 60 angular mas and to 61 lead of values semiaxes Those 212989. HD for d il ueroso h oa ascoeto close mass total the of roots 1.5 cube yield ods ± ± ± ± ± .020.0238 0.0012 .040.436 0.0024 .55.50 0.05 . 90.7 0.4 . 128.4 1.6 . 1099.7 0.9 .21884.8 0.62 .34.70 0.03 h uhri rtflt ..Ginfrgener- for Griffin R.F. to grateful is author The separations angular yield approaches these of All si apn l h rvosydsrbdmeth- described previously the all happens it As M GAIA ⊙ 1 / 3 o oh6PradH 08 n 1.25 and 8078, HR and Per 6 both for rohrsucsmyatrtedetails the alter may sources other or ± ± ± ± ± ± ± ± .44.64 0.04 .080.0230 0.0008 . 89.4 1.5 .0 0.435 0.008 .55.44 0.05 . 2981.4 5.5 . 1884.2 1.5 . 126.9 1.4 ± ± ± ± ± ± ± ± 0.04 0.0009 0.010 0.06 1.6 7.0 1.9 1.8 M ⊙ 1 / 3 © Copyright 2017: Instituto de Astronomía, Universidad Nacional Autónoma de México .D cre eateto hsc n srnm,Universi Astronomy, and Physics of Department Scarfe: D. C. 532 346, A&A, 1999, S. Udry, & R., 433 J. 83, Medeiros, ApJ, de 1936, H. W. Christie, G. A. ed. Velocities, Radial Stellar 1985, I. 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