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1994 A Far-Ultraviolet Atlas of Symbiotic Stars Observed with IUE. I. the SWP Range S. R. Meier George Mason University
Menas Kafatos Chapman University, [email protected]
R. P. Fahey NASA, Goddard Space Flight Center
A. G. Michalitsianos NASA, Goddard Space Flight Center
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Recommended Citation Meier, S.R., Kafatos, M., Fahey, R.P., Michalitsianos, A.G. (1994) A far-Ultraviolet Atlas of Symbiotic Stars Observed with IUE. I. the SWP Range, Astrophysical Journal Supplement Series, 94: 183-220. doi: 10.1086/192078
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Comments This article was originally published in Astrophysical Journal Supplement Series, volume 94, in 1994. DOI: 10.1086/192078
Copyright IOP Publishing
This article is available at Chapman University Digital Commons: http://digitalcommons.chapman.edu/scs_articles/144 1994ApJS...94..183M stages acting accretion lead main-sequence, Aqr). uniquely years. nents systems ary the mass THE © ted tive type that stars compact generally interaction in main-sequence members wind bedded Hall material Terr 1994. Orbital At 2 Symbiotic 1 the Unive_rsity IVE and star. presence AsTROPHYSICAL ::5 surface of semiregular to results of visual The expulsion There lost evolve A Science optical In 100,000 binaries. of Guest intersystem the in due planetary American ln~ernational and These Subject pnmary of spectr~ FAR-ULTRAVIOLET that distinguishes secondary. disk these consist periods may by an This evolution. both temperature © is formation is wavelengths, to from measured. of either of Observer. 274, stars independently and still Laboratory formation, believed has ionized American explain Astronomical mclude the star K, widely Southern absorption atlas from the shown headings: but The variable, of (SWP) of Los JoURNAL much UV. been nebulae. are appropriate the difficulty is one emission general an symbiotics The contains Angeles, they I. suspected. a relevant common believed the Ultraviolet symbiotics separated M of This to tidal kn?wn are Absolute common INTRODUCTION or for ejected to Society. California, in camera outbursts, symbiotic formation jetlike giant, form and presence SuPPLEMENT learn both members binaries: the interact Astronomy features Department repres~nt~tive properties Astronomical In of CA lines interaction as particular All sample a approximate echpsmg a to vary interaction directly to an rights during 90089. In long hot which about envelope c?venng few hne structures binaries, envelope ATLAS that white Exp~orer Space from be many accretion of and and stars from considerably spectroscopic companion reserved. of and fluxes cases, interacting as spectra of of SERIES, characterize high-excitation the is hot outbursts. observing Sciences other mass continua dwarfs systems these Physics both evolutionary Solar of are between often two of the formed of nature Printed OF the Received R. between these (IUE) and processes accretion the (e.g., range the the characterized 94:183-220, from disk outflow to Society range Physics, symbiotics classes P. remain stellar SYMBIOTIC a and in or wavelengths Center, presence s. several with different and system FAHEY Mira systems binaries of U.S.A. CH appropriate -line: during the 25,000 satellite. around by Symbiotics the R. the the symbiotics CSI 1993 symbiotic 1200-2000 the NASA/Goddard an those of that a compo MEIER second streams include permit Cyg, far-ultraviolet or central on Institute, Stauffer binary aspect dozen January stellar inter • 1994 effec stars, or AND tidal and late classes K of em late can identification- ABSTRACT the the Provided that by by In R ::5 a for 1 September of A. STARS ANDM. AND all.; George 183 26; the features A have G. of 394 have accepted 1994 symbiotic silicate classified otics tinuum ~ biotic based upon blackbody presence & flux intersystem with hibit high-ionization bution bwttcs t~e by prominent such source able. and as of of The Balmer tegrated for Space 1907,1909 1660,1666, 1200-2000 MICHALITSIANOS observations been Mason Allen _v, S-type The Allen directly 0 excitatiOn the KAFATOS OBSERVED low-resolution by ~emporal a been is specific U_Y Mg as a thermal I).."").. ( late-type Flight C Nebular -110 stars. generally EUV near (Boyarchuk observed at because the Terr ultraviolet: emission N v N line IV,_ emission University, (1982) visible 1985), ~pectra II systems oflong-period as extracted UV stars 1302-1306, probing reflect c~mtinuum of emission Center, ""A.A March a~d and A NASA lines IR N emission, ""A.""A. type to continuum 2 out behavior that silicate wavelengths. at wavelength of32 III] 2795,2802 M the emission photometry. which 1238, and that the lines far-UV has appropriate He of least in ofO of contain D. at WITH 4 2 the star, in Code extends Fairfax, spectra spectrum ""A.""A. the stars symbiotic luminous from outburst 1975). infrared are 140) defined symbiotic II I lines the Astrophysics such emission 1242, 0 circumstellar IV] 50,000 is suggest 1747-1753, of emission C often high 684.1, flux to variables, afford currently in radiation K-band, high-excitation lines, the II are ""A.""A. IUE. an VA have as from to range 20 from agreement C Thus, )..A excitation distribution to of TypeS two light, M 1397-1407, He a (as Greenbelt, IUE S 22030 IV strong K stars M the JLm an Mira stars from been each 1334,1335, a including types, giant I. ""A.A the II lines. well low-temperature to star, of Terr categories opportunity the while presence e.g., in that archive, ""A.1640 seems THE makes Si suggest nebular 1548, the 100,000 obtained are short-wavelength tabulated. stars or dust. the resonance ~ and as far-UV which III] Data and with Miras, source MD The corresponds 50,000 other IUE included type quiescence). IUE emission in SWP N that to 1550, essentially often have ""A.1892 both Most about 20771 an calibrated, Si of the IV] the presence conditions correlate of K. dominates SWP System D provides long-period with in archive. a II).."").. are in enormous to K blackbody ""A.1487, Tables symbiotic RANGE exhibit presence high-excitation as far-UV. symbiotics forbidden emission Moreover, known D-type these directly and star photoexcited 30 The well lines species the camera 1806,1816, to no (20%) of (Penston C with systems. a 0 a as a of in symbi- symbi contri the source means III] strong In stellar m] ofthe probe range other sym sym lines such stars vari con and this the the the are ex- in A).. A).. · 1994ApJS...94..183M distribution at Table that type, tion burst produced NASA systems an eclipsing absolute if the present Several symbiotics 2000 right tween tra rated. have signal-to-noise and archive. ambivalent duced These AG X-ray systems contains from al. observed in K Feibelman Mira the X-ray LlA. creasing otics uum 1984; 1900-3200 184 1982). applicable, General The Table This The can the the eruptive of 1987). - IUE spectra CH Dra, line show ascension, radio been flux winds. systems A dust, 32 This (Allen Sahade, 4 emission source. 6 rates in 1978-1988. six /UE IUE explain The Goddard atlas nebular of in compares A Cyg), range. with may strength, line wavelength Tracings 1 LWR/LWP an symbiotic binaries Figures CH in with distribution known the Four large observed limiting the lists properties flux, atlas 1982). observed are may A. © these spectral D-type symbiotics D-type spectra M of contains Regional were object intensities orbital 3. Cyg occur in symbiotic The phase-dependent 1982; in A American Brandi, SWP 2. the data ratio giant, the higher Part the are: declination, Mira complements OBSERVATIONS temporal material. of which active complete be Space systems, 1-32. symbiotic DESCRIPTION with resonance Since (Anderson either of the otherS-type, symbiotic these observed We resolution was observational stars V analysis by presented associated at class. from 2 wavelength in phase. Kafatos, in the period, samples the cameras of 1016 than Data spectral (Penston of & well-determined rates IUE an have and the In for Flight no in the the stars made are significantly S-type Fontenla spectra the those flux Thermal inner some all, catalog Cyg, for the hot the 2000-3200 in A Astronomical stars was date Analysis stars line L as routines selected soft etc., D stars. et in atlas were WR/L and various 394low-resolution the final (see quiescent in Center. secondary features variations. most active with Michalitsianos, with high all type. presently AG al. OF RR occultation the secondary accretion et symbiotic not strength, AND range and positively X-ray the in of are two parameters of analysis al. have Kafatos, will examined, 1981) 1984; THE column Atlas Tel, IR Dra, the the WP prominent extensive possible all42 32 as given time, the atlas Accretion written Facility ANALYSIS or other 1983) S-type underexposed Since are A such emission, present ephemerides emission. w-s IUE symbiotics atlas, ATLAS a HM states. quiescent spectra wavelength contains star and Kenyon available have wavelength and region These similar symbiotic were stars SWP of CH in shown identified catalogs indicates Michalitsianos, that effects as or systems because SWP Sge in the the has Table Society R for such continuum all (RDAF) mass far-UV Cyg intercombina emission the may IDL & in w- analyzed Aqr number, with with (Allen include far-UV rises in been IUE each spectra a K a Although presumably UV 1986). in camera the in stage. as Feibelman 4 is are in 3. the spectra (see loss be (Viotti stars available M (AG and with Table range many or the whether T range a the spectral Finally, with giant directly spectra spectra contin known D-type object: 0 buried strong at repro 1200- 1981 - • Allen MEIER spec satu from lines both yr- and, with IUE out that The flux best and Dra soft the Provided be 1 in 0 of of of of 2. of et & it ), 1 6 • ET stars spectra C out lines illustrate objects the ward phases primary star star close citation a are pact ephemeris eral We flux 1238,1242,0 circumstellar comparison calibration over ing there base. era for found lute However, tio. spectra stellar eclipsing fluxes Table we have using presented possible, IUESIPS reflection effect In Figure We AL. III]. In For by other very suggest of the of have these is The is orbital distribution line-emitting emission-line in this the in systems shorter to has reprocessed the present eclipse about Otherwise, near being are The in extinction, 1. (Chochol the the is objects strongest and have lines this the weak spectra in period (see Table 2 For hand, section been systems given provided that its effects, same taken data accepted determined in far-UV shows that continuum minimum phases 4. errors NASA secondary the of eclipsed atlas. wavelengths 1% been the behavior during N extinction where this Fig. at in I DISCUSSION all a mean absolute 2 Munari that these A.A. reduction the calibration from v above most per minimum is Figure are faintest stars faintest lines. we rather et we UV and spectra atlas all region because and in A.A. are co-added in fluxes this flat Further 1302-1306, in 1). 4.1. values absolute al. year the subject Astrophysics exhibit the provide estimate variations by the of weak spectra the 1978 1238,1242 systems N sensitivity important phase. by during poor Several zero. star, atlas 4.2. The et were at 1987). flux than IUE UV component 1 IV), the the years EG (Bohlin is visible. are Kenyon accompanying for out al. UV routines. for the visual OF and to more phase. information weaker AX to continuum C in have signal-to-noise extended IUE continuum distribution The Andromedae to ( eclipse-like variations strong line collected brief fluxes taken of This each 1988) of optical with a spectra E 1988. INDIVIDUAL IV, (BI 1978-1984. IUE precise Principal which increase emission He could extraction 8 AX Persei maximum eclipse degradation .v For and absolute & fluxes susceptible He properties not SWP ( minimum Cru, Using could descriptions object II 1982). active are uncertainties explain Grillmair relative lines at This Per present UV II, A.1640, this, also Data been He minimum a of atmosphere nature the at listed 0 LMC spectra yet of high-excitation, the corresponding is EG among objects indicate about a tables. are clearly II lines flux and insures, III), different The have occur emission-line we approximately well procedures. The UV phases corrected vanishes these A.1640 STARS uncertainty ratio. to signal-to-noise is System of and And in more to in Anon, N and used and quiescent quite 1988). UV variations, the light (e.g., exposed, spectra the with been of the Table III), each eclipses. if the but increases of the variations N that both In the value as the specified continuum are continuum of epochs, affected the maximum of SWP about Si symbiotic uncertain. IV curve, when He emission increases addition, Combin the for analyzed N much of the cool high-ex absolute the III), formed 3. far-UV the A.1718) optical shown in to states, in of fluxes 2-38), v these com inter abso cam latest star. 30% 20% sev and and hot the i.e., to the the on A.A. ra we by as in as 1994ApJS...94..183M SYMus Hen-1092 RX He2-106 RWHya 81 LMC He2-38 Object LMC EG AX Cru Pup And Per S63 Anon 054602.7 08 09 05 01 00' a 14 12 15 13 11 © (1950.0) 53 31 20 29 42 48 33 10 12 American 41• 32.0 29.9 22.7 52.4 55.0 03.7 28.2 40.3 06.0 52.7' /UE -66 -63 -25 -62 -65 -57 -67 -41 -71 a OBSERVATIONS 54 40°24" Astronomical (1950.0) 07 08 04 21 37 33 19 11 00 17 59 29 45 39 36 39 02 18 18 13 22" OF 4300 4613 5834 5908 5020 6940 6238 3876 4767 4074 4939 4451 4690 5894 5532 5051 5050 5771 5908 5638 5261 6111 6560 6248 4950 4831 4831 4767 4504 4939 4503 5976 5272 5748 5537 5386 7396 3874 Julian 4072 4156 4451 4119 4614 4894 4614 83 3753 3873 (244+) Date SELECTED Society 26220 31038 22462 23011 23515 34122 23448 20479 28284 25244 26327 23517 21403 24097 22285 20497 11000 15705 14237 14239 10189 15595 15594 16381 14752 13583 10188 Image 16598 16591 18315 11008 15273 11007 14758 18424 19303 5863 8096 3779 9645 5834 6808 6360 3755 SWP 9644 No. SYMBIOTIC TABLE • Provided Exposure 1 (min.) Time 342 240 295 425 30 40 60 60 60 60 95 90 70 90 45 30 40 45 45 50 50 60 10 10 12 40 18 15 15 15 15 15 15 15 10 10 10 12 15 15 15 15 15 STARS 5 8 9 INTIIE Start Exposure 06 04 20 by 02 00 07 02 02 05 23 21 0247 05 07 00 22 23 20 03 05 03 00 05 21k 17 17 18 18 18 16 15 11 11 14 14 16 11 14 12 14 16 18 15 13 11 16 (UT) 37 31 28 20 21 52 33 33 34 05 28 29 22 22 26 42 44 47 45 ~8 52 56 35 00 03 07 01 07 06 02 26 56 24 24 28 40 44 45 11 17 10 17 17 15 Time FAR-ULTRAVIOLET 34• the NASA 0.57 0.88 0.70 0.30 0.00 0.59 0.84 0.96 0.52 O.oJ 0.99 0.56 0.97 0.37 0.64 0.76 0.96 Orbital 0.91 0.31 0.99 0.22 0.80 0.75 0.24 Phase Astrophysics Quiescence Activity/ Data System 1994ApJS...94..183M CHCyg TCrB V443 CLSco BFCyg AS Object Hl-36 HKSco YY YCrA AGOra ARPav AS 2958 296 Her Her Ara 0! 19 18 19 165140.3 8 15 18 18 18 17 16 18 18 16 15 © (1950.0) 23 20 21 51 57 01 46 12 12 12 10 American 55.2 51.9 02.8 24.6 30.8 24.1 25.9 23.2 29.8 47.3 24.5 14.2 -00 -30 -66 -37 -30 -30 6 -42 50 29 23 20 66 26 Astronomical (1950.0) 52 34 08 25 58 32 06 00 51 56 03 19 8 16 18 31 34 48 53 36 30 07 20 26 39 25 16 6333 6817 6627 6454 6238 4534 4223 5720 5120 5801 5089 5067 6089 6634 6922 7302 4451 4344 4385 4735 4089 4943 4543 4677 4054 5916 5268 5020 5021 6449 7477 7226 4536 4157 4613 4385 4464 4690 4157 4072 4950 4440 5124 5908 5499 6188 6631 6453 3879 Julian 4692 4820 4054 4070 (244+) Date Society TABLE 30134 33579 26720 28682 27571 26219 24956 34725 33047 30924 28734 22056 22707 23582 27542 23520 20209 28715 27556 25834 13956 16857 13477 16710 10439 18389 16380 16392 15652 10510 17070 10456 14640 11002 17104 13582 15709 13605 _mage 5671 9122 5829 6063 7409 8758 5676 5804 6819 9646 6820 9115 3815 9773 9543 SWP No. !-Continued 186 • Provided Exposure (min.) Time 100 105 145 120 150 30 30 80 60 90 30 30 50 55 20 20 25 25 24 40 60 60 60 35 30 35 55 80 35 75 50 55 45 20 20 25 25 12 12 15 15 80 10 15 10 18 18 16 15 15 0.5 6 4 8 Start Exposure 08 03 03 04 01 2241 22 0610 0904 08 07 23 2050 23 09 22 20 12 0426 00 03 07 1146 20 2033 23 20 21 14 10 10 18 15 13 13 11 14 18 16 16 13 14 10 19 17 16 12 16 13 18 11 11 by (UT) 39 45 47 48 52 33 36 32 01 45 27 24 43 41 44 57 09 00 54 55 45 21 48 43 58 07 03 56 05 59 01 22 12 42 11 10 18 17 13 18 19 14 15 Time 18 14 19 the NASA 0.60 0.10 0.31 0.95 0.05 0.27 0.90 0.14 0.70 0.13 0.99 0.91 0.37 0.72 Orbital Phase Astrophysics Quiescent Quiescent Quiescent Quiescent Quiescent Active Active Active Active Active Quiescence Activity/ Data System 1994ApJS...94..183M CICyg Object HMSge Vl016 RR R AG ZAnd HBV Aqr Tel Peg 475 Cyg a 20 20 23 23 21 19 19 © 19 (1950.0) 39 48 00 48 49 31 41 55 American 21.0 41.4 36.2 02.6 20.1 14.3 15.3 19.8 a -15 39 -55 35 35 48 16 12 Astronomical (1950.0> 41 33 52 32 37 33 23 23 30 33 24 37 32 04 27 42 Julian 4831 5142 5073 5294 6889 6657 3877 3920 4613 4119 4477 4074 4036 4536 6045 5567 5816 5097 5423 5074 5422 5480 6736 6770 6772 6461 6374 6949 6563 6286 6353 6213 6354 6730 7ll2 6402 6617 7195 3709 7430 3752 (244+) 3720 3878 4477 4070 4825 4269 4385 4330 4049 4894 4475 4614 4076 4453 7162 7101 Date Society TABLE 30694 28896 20731 32845 34313 32208 32296 31080 32646 29562 29815 29829 27028 27632 28292 26569 26937 26023 26943 29536 27203 22840 Image 28611 24656 20069 16760 11003 15274 10455 17276 16752 18603 14756 19575 16918 14688 19566 11006 SWP 5485 4271 5809 5611 9ll7 5856 5885 6354 9898 9900 7818 3792 3795 9878 9663 2047 2427 2123 8610 No. !-Continued 187 • Provided Exposure (min.) Time 120 60 30 45 45 30 92 25 25 25 25 25 20 20 20 40 40 50 85 60 70 30 45 45 35 35 30 25 25 22 40 42 40 40 40 87 15 15 6 17 16 15 11 15 10 3 3 3 5 8 6 6 3 7 3 2 2 8 1.25 Start Exposure by 05 0023 0003 07 04 02 03 02 22 22 2232 2248 2236 21 0440 0249 09 03 01 09 09 08 03 0721 03 00 02 08 01 23 20 18 11 15 10 10 12 17 14 17 10 16 18 18 13 18 18 19 19 15 13 15 1029 15.44 19 18 (UT) 29 50 54 50 59 53 53 52 38 34 33 30 30 01 02 20 28 20 24 20 47 42 40 49 42 46 40 42 50 56 51 52 34 30 09 04 08 20 20 23 25 25 41 Time 15 10 17 10 the NASA 0.57 0.04 0.25 0.38 0.99 0.90 Orbital 0.87 0.85 0.95 0.05 0.05 0.87 0.58 0.63 0.36 0.61 0.56 O.ll 0.75 0.27 0.01 0.64 0.77 0.06 Phase Astrophysics Quiescence Quiescent Quiescent Quiescent Quiescent Active Active Activity/ Active Active Data System 1994ApJS...94..183M TABLE2 FLUXES OF THE SYMBIOTICS OBSERVED BY /UE
NV Sill 01 Cll SIIV 0 IV] N IV] CIV [Ne V] [Ne IV] He II 0 Ill] NIV N Ill) Sill Sllll] c Ill] @ 1238.8 1264.11 1301.1 1334.5 13113.8 13Q7.2 1483.3 1548.2 1574.7 11W1.5 11140.4 1111W.8 1718.5 17411.8 1808.0 18112.0 19011.7 1242.8 1304.11 1335.7 13911.8 1486.6 1550.8 1111111.1 17411.11 18111.11 1(108.7 1401.1 1749.11 1817.4 ~ Star 1404.8 1752.1 1'1:1 .....'"I 1753.11 ~
~ EGAnd > SWP 1240.0 12511.5 1304.2 1334.5 1394.7 1401.3 14811.0 1548.4 15711.0 1600.2 1113Q,II 111113.11 1717.8 1750.2 1815.4 18111.7 19011.1 [IJ 3753 216.6 .60.3 *423.7 *507.1 *601.4 *2051.0 259.1 *836.1 21.5 *303.4 29.3 *191.8 *475.2 a 5834 *149.5 78.9 *119.6 *294.4 *391.8 *482.1 *1170.0 *302.9 *623.1 156.7 *208.9 *167.0 *222.1 9644 41.6 484.1 422.2 528.0 *4711.0 18.2 372.7 1016.0 34.7 243.0 132.8 563.9 = 11007 *364.3 106.0 *788.2 16.1 *641.6 *741.5 *743.6 *2545.0 24.0 *687.3 *1343.0 113.3 *434.1 118.1 397.5 *678.9 9..... 15273 25.6 505.3 398.1 126.3 *2801.0 41.9 659.9 273.9 16.7 165.2 710.3 ~ 139.9 219.0 309.4 364.9 877.4 *4298.0 320.8 *1886.0 78.9 397.9 12.1 376.1 951.2 e:.. 18424 rJ). 19303 344.7 229.0 327.5 *3649.0 24.2 *787.7 192.1 12.5 160.2 *633.0 0 20497 220.0 616.7 606.6 851.9 1122.0 *5351.0 416.9 2195.0 332.4 496.5 441.1 1185.0 ~ ...... 22285 233.2 87.7 217.4 499.2 634.1 942.8 *4713.0 21.1 329.3 *1895.0 82.5 418.9 49.1 347.9 *918.8 00 24097 251.1 56.6 76.6 256.4 445.6 858.9 *3996.0 36.9 412.8 *1699.0 319.5 ! 00 59.5 290.1 *876.8 • AX Per ~ SWP 12311.11 1303.4 1331.11 1395.1 1402.3 14811.2 1548.8 1575.5 11W1.2 11140.0 111114.5 1720.3 1750.3 1817.2 18112.7 19011.5 '"I 0 3755 171.2 98.4 8.2 140.9 268.2 350.1 *1285.0 4.5 *477.8 *746.2 28.7 *363.2 38.0 *308.2 *608.0 < 6360 105.1 88.1 130.0 161.8 *1072.0 12.2 188.9 317.2 11.1 187.3 9.9 84.9 *464.7 Q: 6808 67.2 88.1 95.5 1072.0 319.1 156.6 68.7 491.1 1'1:1 136.7 129.4 Q. 11008 261.7 119.8 124.5 277.7 344.6 *1117.0 35.9 30.5 *527.8 *517.5 40.2 186.3 33.7 155.8 *352.9 C"' 14758 261.1 61.1 178.2 196.1 1272.0 80.7 49.2 496.0 185.2 112.3 24.7 155.2 "< 20479 126.9 43.8 101.0 86.9 610.7 12.7 16.2 273.3 112.7 9.9 48.5 35.8 113.5 ~ 23448 345.1 129.1 159.0 220.0 253.7 1984.0 25.8 17.2 515.6 508.9 33.4 143.0 21.1 134.8 208.4 1'1:1 25244 111.9 39.2 114.1 125.4 834.4 348.4 179.2 107.0 25.1 18.6 137.4 ~ rJ). LMC Anon > SWP 12311.4 1303.0 1485.8 1548.7 11140.4 111113.1 1722.11 1750.8 181111.7 11104.11 18315 29.1 12.6 4.3 6.8 2.4 2.1 11.0 [IJ> 26327 22.9 2.1 12.7 7.7 5.6 4.4 12.2 =t 34122 20.2 13.3 5.4 3.7 1.6 10.7 0.6 1.3 0 "0 LMC S63 "<= .....[IJ SWP 1245.9 1268.6 1333.7 13Q7.3 1404.7 1488.6 1552.9 11143.2 111115.1 1722.8 1752./l 18111./l 1894.11 11111.8 ~ [IJ 16591 12.9 3.1 2.4 2.4 4.1 18.1 61.2 20.6 14.3 3.0 9.3 1.9 2.1 36.9 ~
~ rJ).
"<[IJ [ 1994ApJS...94..183M TABLE 2-Continued
NV Sill 01 Cll SIIV 0 IV] N IV] C IV [Ne V] [Ne IV] He II 0 Ill] N IV N Ill] Sill Sl Ill} ~ Ill}
RXPup @ SWP 12311.8 1304.5 1337.8 1385.4 1403.0 1465.3 1548.7 1574.3 1501.5 11540.5 115fS5.1 17115.15 1761.0 11117.0 1182.5 1110Q.O 10189 7.8 80.2 5.2 116.7 135.0 282.5 *1008.0 458.1 *582.4 35.4 *346.1 55.5 *336.1 *557.9 ~ 14239 27.5 99.5 91.6 161.8 344.1 1185.0 26.1 24.1 539.1 591.2 380.8 44.8 419.0 *987.5 1'1:1 16598 40.4 129.6 45.4 162.7 344.1 1171.0 25.2 17.2 586.9 520.9 11.0 349.4 28.8 330.4 *980.1 .....'"I ~ 21403 76.3 21.2 115.6 207.7 309.2 921.5 25.1 600.9 397.5 9.1 251.0 28.1 276.3 *831.6 22462 79.5 23.0 26.9 97.6 226.7 341.2 900.7 550.4 345.4 50.9 223.1 26.9 218.9 *820.9 ~ 28284 115.4 35.1 141.1 250.6 287.9 912.4 501.0 283.6 203.4 42.1 121.5 560.4
>[IJ He2·38 a SWP 1240.7 1385.5 1404.2 1468.2 1550.3 15QB,B 1541.2 16151S.O 1750.4 11118.4 1885.5 1810.15 = 14752 23.1 5.9 4.8 154.4 10.5 48.1 38.9 17.0 5.9 8.2 62.1 23517 7.4 2.0 4.8 5.9 1 04.2 13.9 14.3 12.3 35.6 9..... 9.1 ~ e:.. SYMua rJ). SWP 123US 1253.3 1304.5 1396.3 1401.1 1466.3 1646.7 1574.8 1601.6 11140.1 16114.5 1718.6 1750.8 "1117.7 11110.9 1110Q.O 0 ~ 10188 114.0 7.7 78.7 158.0 88.2 *560.0 24.1 *439.6 97.0 2.9 63.2 60.7 88.3 14237 *1089.0 252.2 *385.0 *663.6 410.3 *1822.0 50.2 9.8 *980.3 427.2 33.9 151.2 21.9 188.3 145.4 00 15594 *1003.0 20.4 254.7 *374.5 *554.5 *367.9 *1505.0 33.6 *882.0 459.2 11.0 150.5 29.5 *207.7 146.7 ! 1.0 • 15705 11 06.0 247.8 328.8 523.1 351.7 *3342.0 11.0 1569.0 468.0 138.8 31.9 204.3 163.7 16381 *709.0 121.1 *213.6 *418.0 254.8 *1236.0 21.5 11.5 *706.9 311.1 10.0 118.5 7.9 124.3 113.3 ~ '"I 23011 91.5 10.8 54.0 137.0 78.1 *473.6 22.5 4.9 *440.5 101.0 13.5 49.3 30.0 72.8 0 < Q: Bl Cru 1'1:1 SWP 12311.4 1335.0 1385.1 1405.11 11541.7 115fS2.4 18115.2 1110Q.7 Q. 1718.2 1755.4 1885.4 13583 6.0 5.1 4.1 5.5 1.4 3.0 2.4 4.4 C"' "< 15595 6.1 3.6 3.7 2.1 10.9 5.7 2.1 12.1 ~ 1'1:1 RWHya
SWP 12311.7 12fS6.1 1305.7 13115.0 1401.8 14615.4 1546.15 1575.8 1501.0 11540.7 115fS4.2 1718.2 1750.3 11116.15 1191.15 IIIOQ.5 ~ 3779 1027.0 121.4 185.5 *3650.0 *2987.0 *7776.0 *1572.0 *2589.0 69.9 423.9 67.6 251.6 422.2 rJ). 5863 719.7 496.2 653.2 1714.0 *4950.0 *4070.0 *10640.0 *2326.0 *3696.0 222.2 462.2 71.0 394.9 498.7 > 9645 *95.9 *222.4 *186.8 *1295.0 *1821.0 *5170.0 54.6 38.9 *822.6 *1 070.0 282.1 57.7 214.7 305.3 11000 1446.0 194.4 67.1 *4637.0 *3744.0 *1 0970.0 [IJ> 41.9 *1497.0 *3008.0 63.2 360.6 31.0 185.5 391.6 =t 26220 1194.0 *4259.0 *3130.0 *1 0580. 56.9 1203.0 2227.0 49.7 331.9 168.4 298.9 0 31038 330.1 21.4 33.4 *1692.0 1429.0 *7807.0 75.8 725.1 1136.0 98.7 54.9 92.5 265.5 "0 = He2-106 "<[IJ ..... SWP 1242.5 1303.3 1467.7 1550.5 11541.1 115fS6.1 ~ 1117.15 1893.0 1812.7 [IJ 23515 4.6 1.8 5.3 23.2 15.0 15.4 1.0 1.4 4.5 ~
~ rJ).
"<[IJ [ 1994ApJS...94..183M TABLE 2-Continued
NV Sill 01 Cll SIIV 0 IV] N IV] C ~e_V] [NeiV] He II 0 IIIJ N IV N IIIJ Sill SIIIIJ C IIIJ
Hen 1092 @ SWP 1238.Q 1304.3 1337.3 13Q3.7 1401.1 1485.7 1648. 1 1674.0 le3Q.3 1ee3.1 171Q.3 174Q.O 1817.2 18Q0.2 111011.6 > 8096 99.2 30.5 3.5 44.9 13.1 83.1 413.0 23.9 383.8 142.7 8.1 18.4 4.5 21.1 34.4 9 (!) TCrB ....'"1 ~ SWP 123Q.e 1264.6 1305.6 1337.0 13Q1.4 1400.8 148e.e 1547.8 1677.4 16QQ.7 !e40.e 1ee5.7 1714.4 1751.1 1817.3 18Q1.7 IQOQ.Q § 3815 135.3 80.6 18.9 38.0 334.3 26.1 83.0 39.3 9.8 158.5 21.1 104.9 86.0 5804 28.1 6.2 49.9 26.2 22.3 158.1 83.5 38.7 60.2 8.4 70.9 38.4 [IJ> 17104 117.2 102.6 14.0 83.7 79.9 76.1 492.8 ..... 129.8 82.6 11.7 154.8 165.0 137.0 '"1 25834 281.9 172.6 19.6 140.2 110.1 108.0 463.9 51.4 156.3 95.3 158.8 12.1 186.7 148.3 0 27556 99.6 73.3 100.6 84.3 35.1 333.1 61.0 59.3 94.2 113.9 80.5 =0 28715 48.4 36.1 7.7 51.2 37.1 82.1 20.7 22.5 31.7 30.8 42.9 ....9 ~ AGOra ~ Active \F.J - SWP 123Q.O 12e4.Q 1304.3 13Q3.6 1401.1 1486.7 1548.6 167e.r !e3Q.I lee4.6 1718.4 174Q.4 1817.Q 18Q2.0 IQ10.6 0 ~.... 11002 2443.0 582.5 1477.0 533.7 3903.0 88.6 *9840.0 331.3 306.3 215.5 (!) ..... 13605 *2933.0 211.4 724.0 1927.0 492.1 *3759.0 *6096.0 533.9 65.8 85.4 239.0 130.2 "--< 14640 *2689.0 185.2 320.3 *438.2 *1282.0 571.4 *2632.0 78.9 *3513.0 502.1 53.2 270.0 64.9 • 15709 *947.2 *123.2 *437.6 *254.0 *1608.0 *2454.0 *85.7 ...... 27542 *3359.0 ""C '-0 219.1 2149.0 658.8 *3905.0 *6990.0 324.0 49.6 45.6 141.1 22.9 '"1 0 Quiescent 0 -< 123Q 12ee 1303.8 13Q6.2 1401.4 !48e 1648.2 1676.8 leQ2.8 le3Q.6 lee4.1 1716.8 17eQ.Q 1817.7 18QI.2 IQI0.4 s: 5676 *590.8 80.1 97.1 446.7 174.9 609.9 50.2 *1806.0 104.4 92.3 (!) 32.7 ~ 1 0456 *906.4 22.8 111.4 173.3 559.8 195.5 953.8 *2172.0 234.1 51.7 96.9 37.0 0' 20209 *1448.0 171.3 332.0 653.2 252.3 1286.0 28.2 31.6 *2389.0 207.6 32.6 71.3 18.9 89.2 25.2 "--< 23520 548.9 95.1 345.9 125.5 376.4 *1453.0 130.7 51.4 23.1 ~ 23582 476.7 51.9 117.9 324.3 135.8 479.1 *1447.0 109.7 39.0 16.5 49.3 (!) HKSco
~ SWP 123Q.1 1302.8 1337.3 13Q3.3 1403.e 14Q0.3 1648.6 1577.2 !e40.2 IU3.6 1750.1 181Q.7 18Q3.1 1Q10.8 \F.J 13582 17.3 6.9 5.5 6.3 19.6 19.0 110.7 6.1 74.7 18.1 8.1 4.1 5.6 > 16392 28.6 1.3 8.3 6.9 30.0 4.2 35.2 8.6 2.4 2.4 3.5 5.0 [IJ> ..... '"1 CLSco 0 SWP 1303.Q 1338.3 13Q5.3 1404.1 ~ 1485.5 1550.8 !e3Q.I lee4.e 18QI.7 IQOQ.I 9543 16.3 6.4 8.9 4.0 5.2 55.9 24.0 68.1 59.7 104.6 "--<= ....[IJ ~ H1·36 Arae [IJ SWP 1300.e 1404.6 14QI.8 1547.1 !e38.1 lee3.o 1747.4 1815.3 IQ07.0 ~ 6819 3.1 3.0 11.2 40.1 17.3 1.9 1.9 ~ 17.3 45.6 ..... ~ YCrA \F.J "--< SWP 123Q.4 1305.Q 1335.5 1401.Q 1487.4 1576.1 1598.9 1639.5 1663.6 1720.6 1748.1 [IJ 1815.3 1891.3 1908.5 ..... 6820 73.0 15.3 2.1 88.1 60.3 16.5 9.7 247.4 9 105.9 5.0 39.0 5.1 22.8 81.8 1994ApJS...94..183M TABLE 2-Continued
NV Sill 01 Cll SIIV 0 IV] N IV] C IV [Ne V] [Ne IV] He II 0 Ill] N IV N Ill] Sl II Sill I] C Ill]
YYHer @ SWP 1240.0 1265.8 1305.0 13Q5.4 1402.2 14811.4 15411.4 1575.11 11102.0 11140.3 1llll4.1 17111.0 17411.8 18111.1 18111.7 11108.7 > 9115 153.0 53.3 291.6 291.1 392.5 20.9 391.6 390.0 55.8 9.8 38.9 95.4 9773 186.3 45.8 157.7 142.9 287.2 11.7 8.2 *260.3 220.5 12.7 30.5 3.9 28.4 48.8 ~ 15652 20.2 1.9 14.2 24.6 75.4 67.7 168.3 5.8 5.5 *115.9 *180.3 46.1 5.7 *38.4 *1 06.2 ....='"I n ~ AS 296 = SWP 1238.8 1305.7 13Qtl.8 1405.2 1484.11 15411.3 157/l.tl 11103.2 111311.11 1tlll5.2 1720.2 1760.7 18111.0 18113.11 11110.5 [IJ> 16380 16.1 14.0 20.2 229.4 1.9 5.6 25.9 43.6 8.6 16.2 1.6 7.9 10.2 ..... '"I 18389 4.5 6.7 53.3 52.6 11.6 13.4 11.2 7.7 2.7 3.6 0 33047 5.6 12.1 12.1 120.0 20.2 16.8 3.4 15.5 0.6 1.4 10.3 =0 34725 3.8 3.8 5.3 52.6 58.1 22.2 3.5 19.2 37.5 .... =n AS 2956 ~ SWP 123Q.5 1304.2 13Qil.O 1404.3 1487.8 1548./l 1575.11 11141.0 111511.11 1721.2 1747.11 18112.0 11111.0 'JJ.- 6063 9.6 4.3 1.3 4.4 9.8 24.1 2.6 22.3 2.2 1.8 12.6 8.0 2.3 0 n.... ~ AR Pav q SWP 1240.Q 126/l.tl 13011.0 1334./l 13Q5.2 1402.4 1486.11 15411.3 1577.11 11102.6 11l40.1l 1tlll4.tl 1717.4 1751.0 1814.11 18111.8 11108.7 '-0 • 5829 133.2 25.6 58.0 46.0 170.5 282.1 272.6 1579.0 24.6 425.9 960.8 309.4 203.7 922.9 9646 108.5 12.7 86.2 15.2 102.1 144.6 111.8 641.1 40.4 195.0 307.8 125.9 193.3 365.5 ""C '"I 10510 152.2 52.5 7.2 86.5 140.4 93.3 *661.9 4.5 19.9 186.9 290.3 100.7 16.6 112.5 *317.4 0 -< 13956 121.1 9.7 45.6 113.4 300.0 240.7 *933.7 10.4 *457.0 *612.1 182.0 6.4 *185.7 *421.1 a: 16710 118.6 57.6 121.5 196.5 158.7 679.7 257.7 449.7 122.5 112.9 452.5 c.~ 16857 121.2 44.7 88.0 171.7 134.9 *635.9 5.8 11.6 188.0 *380.8 124.6 17.3 *133.1 *318.9 17070 120.2 34.9 87.6 140.8 116.2 *619.2 8.5 6.8 145.5 *349.6 9.1 103.7 10.4 120.8 *349.4 0"' "--< 22707 85.4 27.7 110.7 215.9 107.3 *974.3 297.3 488.1 136.7 23.8 197.4 *370.4 :r ~ V443 Her z SWP 1240.5 1304.1 13Q4.4 1400.5 1485.1 1647.6 1575.6 11100.5 11!38.11 1tlll2.8 17411.0 1813.8 18110.2 11107.0 > 9122 188.6 126.5 253.7 643.3 815.8 *2682.0 83.4 387.0 953.5 254.9 112.4 381.0 'JJ.> 10439 210.7 143.3 267.8 756.3 *852.3 *2961.0 56.9 61.9 "506.7 *1239.0 262.8 27.9 154.4 443.2 BFCyg [IJ> :t SWP 1243.6 1265.2 1305.2 13Q3.8 1402.Q 14811.3 1660.4 1573.8 11102.5 11140.3 111114.0 1720.11 1760.0 18111.11 18111.5 11107.8 0 5671 153.4 32.0 84.4 *78.7 68.6 55.3 *41 0.5 *164.9 *339.1 45.6 *264.8 16.7 *210.7 *307.6 "0 8758 158.6 43.0 171.5 166.7 176.3 863.2 36.9 144.6 624.9 43.4 419.3 37.8 185.4 *671.3 "--<= 13477 15.4 63.9 76.2 90.1 *735.9 70.2 264.8 30.9 *230.1 74.8 *351.8 ....[IJ n 28734 141.1 36.2 304.0 288.2 163.6 108.0 686.2 178.2 956.7 52.4 *733.0 17.7 368.9 *856.7 [IJ 30924 15.9 23.1 3.4 176.5 127.1 29.6 649.0 44.6 21.1 45.0 383.1 369.0 289.9 722.0 ~ 33579 213.4 36.2 416.7 3.5 265.4 237.2 187.8 *937.8 27.9 34.1 140.1 *1118.0 29.4 *846.6 45.2 *540.8 *1127.0 ~ S" 'JJ. "--< [IJ ..... ~ = 1994ApJS...94..183M TABLE 2-Continued
NV Sill 01 Cll SIIV 0 IV] N IV] C IV [Ne V] [Ne IV] He II 0 Ill]__ N IV N IIIJ Sill Sllll] C Ill]
CH Cyg @ SWP 1242.4 1264.0 1306.3 1336.3 1394.1 1403.7 1489.7 1548.1 1578.1 11103.1 11142.2 11187.0 1713.8 1749.1 1817.8 18Q2.1 HIO'i/.8 > 7409 *1426.0 358.2 97.3 790.3 513.6 532.5 662.0 *148.8 *165.4 *217.1 22056 1723.0 1478.0 1683.0 3008.0 2848.0 5315.0 1971.0 1486.0 1469.0 5750.0 1079.0 =~ 24956 1300.0 380.6 3573.0 913.4 364.5 647.5 521.5 1673.0 1689.0 508.6 173.3 1538.0 782.1 1323.0 1608.0 ....'"I n 26219 844.9 287.5 *2128.0 656.0 447.6 687.1 342.5 *2229.0 80.5 80.2 731.3 650.4 832.9 21.2 *1 060.0 *1 063.0 ~ 26720 632.2 339.2 *1594.0 656.9 406.8 622.0 236.1 1647.0 641.8 516.7 624.3 *291.6 *799.1 *947.8 = 27571 472.7 169.5 *1300.0 *588.1 478.5 584.4 209.4 *2038.0 *915.6 *812.1 142.3 *668.0 *630.6 *673.8 [IJ> 28682 339.6 48.7 885.9 313.0 1039.0 945.7 959.9 *3072.0 729.8 1010.0 *1 09.8 *733.9 *1 076.0 *979.6 ..... '"I 30134 153.0 25.8 314.0 256.4 447.3 409.4 168.3 1426.0 291.4 411.1 44.5 332.2 137.3 519.3 592.7 0 =0 HM Sge .... SWP 1240.3 1263.2 1303.1 1335.4 1396.6 1401.8 1486.0 1549.1 15711.1 11101.0 1640.1 16114.4 1717.3 1750.7 1816.5 1893.7 IQ08.3 =n 9898 235.8 10.8 19.1 112.5 200.0 428.9 *1336.0 30.9 88.8 583.5 263.0 6.2 332.5 33.4 291.6 *928.3 ~ 14756 335.3 20.3 92.5 216.7 *509.4 *1164.0 38.1 131.8 *597.3 297.6 *362.3 39.5 316.5 *627.7 'JJ.- 16752 252.8 11.2 19.7 140.3 256.0 538.1 1613.0 14.4 111.4 785.0 374.0 18.3 355.8 37.7 317.3 *1157.0 0 n.... 28896 406.4 383.3 491.5 2045.0 41.9 97.4 1084.0 254.9 344.7 46.1 185.9 1033.0 q~ 30694 *452.8 3.2 6.0 11.9 *477.0 *512.1 *1 032.0 52.4 117.8 *634.9 232.4 11 .1 *309.4 33.7 *99.8 *498.1 • \0 CICyg N Active ""C '"I SWP 1240.0 1304.1 1335.1 1395.3 1402.6 1486.6 1549.1 1577.3 11101.8 1640.4 16114.6 1720.3 1750.9 1815.8 1892.5 IQ08.7 0 153.7 78.3 159.1 -< 5485 110.0 314.8 *1254.0 12.8 24.6 272.4 498.4 356.0 38.3 197.3 *595.7 a: 7818 162.5 23.1 131.4 220.4 318.8 *1158.0 20.7 27.1 *373.6 *462.5 16.3 *302.8 12.3 146.8 *452.6 c.~ 9663 130.3 16.5 13.2 131.6 159.2 225.7 *1339.0 16.5 8.1 274.9 393.1 9.3 256.9 157.5 *575.5 11003 238.8 20.2 3.6 249.2 329.2 *995.4 28.3 39.2 497.2 *380.1 28.8 208.0 20.6 163.0 *446.9 0"' "--< Quiescent :r 1239.8 1264.7 1302.7 1336.3 1395.6 1402.3 1486.6 1549.6 1575.4 11101.8 1840.7 1666.1 1719.2 17110.9 1817.9 1692.9 HI09.Q ~ 15274 222.5 91.3 85.3 226.0 307.4 1039.0 23.2 25.3 510.2 328.6 171.9 16.5 186.6 395.7 z 17276 183.6 22.1 16.5 113.9 222.5 233.0 1203.0 21.8 18.3 576.6 267.7 147.9 15.5 110.0 340.9 > 18603 192.6 14.0 7.3 54.5 139.2 174.8 1230.0 26.3 17.2 404.5 203.8 9.4 115.9 6.7 41.7 283.6 'JJ.> 20731 671.8 23.0 229.7 156.1 366.9 332.9 *2657.0 84.9 39.0 990.3 373.2 20.4 168.6 54.9 183.3 262.1 V1016 Cyg [IJ> :t SWP 1239.8 12115.7 1305.0 1336.4 1396.1 1401.7 1488.3 1548.7 1574.5 11101.2 11139.9 11164.1 1718.3 1750.5 1816.7 1892.4 1907.4 0 2427 *2105.0 42.9 *438.1 28.4 *2084.0 *1335.0 *3064.0 211.7 *443.9 *1870.0 *1196.0 88.4 *691.5 128.8 *826.7 *1406.0 "0 4271 *2605.0 13.6 647.5 1301.0 *1990.0 *1513.0 *3569.0 256.6 430.8 *2180.0 *1356.0 58.6 *784.9 176.2 *1 051.0 *1543.0 "--<= 5611 *3471.0 55.6 748.4 1461.0 *2717.0 *1843.0 *4951.0 233.2 384.0 *2987.0 *1811.0 52.1 *891.8 155.6 *1222.0 *2018.0 ....[IJ n 9878 3646.0 53.4 921.8 44.1 *1430.0 *2588.0 *1756.0 *5074.0 208.1 339.8 *2966.0 *1720.0 65.8 *871.3 196.2 1196.0 *2096.0 [IJ 19566 *3091.0 50.3 387.4 21.8 1239.0 *2202.0 *1477.0 *4288.0 294.1 312.5 *2389.0 *1295.0 27.1 696.3 147.9 *986.0 *1844.0 ~ 24656 *3016.0 42.2 255.7 24.2 1055.0 *2074.0 *1337.0 *4118.0 270.6 248.8 2318.0 1148.0 27.8 581.3 134.4 *779.8 *1634.0 ~ 29829 *3093.0 52.3 3351.2 81.6 808.9 *1916.0 *1307.0 *4190.0 274.7 261.9 *2328.0 *11 06.0 33.0 521.8 120.8 818.55 *1626.0 S" 32296 *3136.0 33.8 407.8 39.3 938.2 *2020.0 *1271.0 *4333.0 280.0 275.1 *2341.0 *1141.0 37.2 545.9 129.7 813.6 *1540.0 'JJ. "--< [IJ ..... ~ = 1994ApJS...94..183M TABLE 2-Continued
NV Sl II 0 I C II SIIV 0 IV] N IV] C IV [Ne V] [Ne IV] He II 0 Ill] N IV N Ill] Sill SIJJI] C Ill]
RRTel @ SWP 1238.6 1266.9 1303.2 1333.0 1393.9 1400.8 1485.0 1647.7 1573.0 1599.5 11l39.2 UJ63.4 1717.3 1749.7 1816.8 1890.7 1907.4 > 204 7 *27620. 314.8 2134.0 211.6 5273.0 12750.0 6370.0 *4261 0. 1937.0 1172.0 *19980. 6429.0 216.4 2417.0 438.9 4390.0 *11480. 5885 *14890. 150.8 1800.0 292.6 *5403.0 *8839.0 *5558.0 *18150. 1601.0 1217.0 *9346.0 *5388.0 346.2 2061.0 390.6 *3231.0 *5498.0 ~ ....='"I 861 0 23220.0 629.2 1514.0 851.6 4269.0 10690.0 5189.0 *4561 0. 1899.0 1578.0 *19890. 5155.0 1774.0 295.2 *3011.0 *1 0510. n 28292 *14780. 96.7 650.1 2271.0 6815.0 3167.0 *24670. 1465.0 811.5 *1321 0. *3635.0 67.0 1371.0 248.4 2213.0 *6569.0 ~ 29536 *15090. 513.1 2221.0 6361.0 3281.0 *2461 0. 1182.0 713.4 *13680. 3377.0 87.2 1305.0 323.4 2056.0 *6768.0 = 31080 9518.0 353.5 1726.0 4270.0 1934.0 *20060. 677.0 567.2 10040.0 2058.0 172.7 818.3 1134.0 4508.0 [IJ> ..... '"I HBV 475 0 SWP 1239.9 1304.6 1336.9 1395.1 1402.1 14811.7 1549.6 1576.1 1602.7 11140.4 16114.1 1717.1 1751.1 1818.6 1892.3 1QOg.4 =0 9900 249.7 79.4 4.8 54.5 109.7 85.8 *902.6 17.3 ~0 52Q4 9~1 10.0 50.7 12.5 94.8 189.0 .... 14688 44.8 1.4 12.2 40.3 34.6 229.8 7.5 4.9 172.6 38.2 25.7 0.9 17.8 95.6 =n 16760 52.1 ~ 11.8 20.6 31.7 307.1 7.3 193.1 58.8 27.3 25.1 114.1 19575 212.8 56.1 37.3 84.7 68.8 618.5 15.6 7.5 452.3 74.8 38.7 8.0 69.5 137.1 'JJ.- 0 ,22840 37.0 2.1 4.0 23.5 20.7 168.5 7.7 4.9 164.3 81.0 6.2 28.1 5.3 17.5 77.6 n.... 26943 193.3 52.6 75.7 70.8 557.8 2.6 460.9 87.2 3.4 42.4 10.0 62.8 126.2 ~ q 29815 36.4 4.5 10.1 28.3 17.4 *168.8 1.2 *129.3 22.8 1.8 *22.4 1.2 16.4 *68.1 34313 145.6 32.7 3.6 70.4 50.9 497.0 334.9 51.1 36.6 6.5 40.8 92.7 \0 • w ""C AG Peg '"I 0 SWP 1241.3 1306.0 1332.8 1394.2 1403.4 14811.0 1549.5 1576.6 1600.5 11140.0 11l63.4 1719.1 1749.8 1818.4 1890.5 1908.4 -< 2123 *24820.0 1124.0 1042.0 3206.0 *17350. *32760. 157.5 *23050. 8123.0 7270.0 2422.0 1203.0 2247.0 a: 3795 *3154.0 *358.1 *917.5 *5617.0 *8001.0 *5466.0 *979.9 *2821.0 *795.6 ~ *113.2 *422.5 *837.6 c. 6354 *23940.0 1132.0 696.4 1174.0 2288.0 *12400. *2571 0. 290.4 1913.0 5867.0 4709.0 1834.0 260.9 879.2 1592.0 0"' 9117 *21930.0 2911.0 746.0 3199.0 5166.0 *14060. *25690.0 *1681 0. *8129.0 3933.0 2497.0 460.4 1837.0 2214.0 "--< 1 0455 *23620.0 409.6 1480.0 2792.0 *1130.0 *22500.0 *16200. 4166.0 3436.0 1512.0 142.3 690.4 1490.0 :r 26023 *16970.0 451.4 2049.0 *5994.0 *7696.0 *1691 0.0 425.0 *9832.0 *5299.0 924.8 1717.0 408.2 831.4 *1782.0 ~ z ZAnd Active 'JJ.> > SWP 1241.3 1265.8 1305.8 1336.1 1394.9 1403.4 1487.7 1549.9 1577.8 1695.9 11140.9 1665.11 1712.1 1751.5 1817.1 1892.0 1Q0g.ll 26937 *468.6 68.4 19.0 *343.9 *180.4 *1261.0 77.2 *1477.0 *152.5 26.4 *62.2 16.8 *142.7 *215.8 [IJ> 27028 209.8 40.0 293.5 57.9 598.4 *572.3 320.6 *2182.0 *396.6 876.4 548.2 268.1 *592.0 *698.0 :t 27203 84.7 252.6 32.9 510.9 453.1 195.5 1699.0 134.8 309.2 700.3 58.7 597.6 916.5 1046.0 0 "0 27632 72.8 272.3 594.7 524.4 206.8 2247.0 101.3 456.4 835.7 409.7 101.1 773.2 842.1 Quiescent "--<= ....[IJ 1240.2 12611.3 1305.7 1333.1 1396.3 1402 14811.7 1549.5 1576.6 1601.2 11140.7 1664 1720.8 1751.3 1820.7 1891.7 1Q0g.5 n 5809 388.9 72.1 19.0 343.8 [IJ 178.6 1260.0 77.4 *1475.0 152.5 62.4 16.7 138.9 215.7 11006 *1341.0 36.6 *383.4 454.4 *694.0 360.2 *1981.0 43.5 18.9 *1417.0 448.4 48.0 160.7 34.8 *365.1 261.5 ~ ~ 32208 981.3 94.3 308.0 526.5 245.4 *2193.0 83.1 *1917.0 283.6 41.8 127.5 24.3 141.3 268.1 S" 32845 447.6 34.9 147.5 313.1 180.8 *1491.0 60.5 34.3 *1494.0 195.3 18.5 106.0 106.1 227.4 'JJ. "--< [IJ ..... ~ = 1994ApJS...94..183M
@
~ 1'1:1 .....'"I ~
~ > a[IJ = 9..... ~ TABLE 2-Continued e:.. rJ). 0 ~ NV Sill 01 Cll SIIV 01~ Nl~ CIV [Ne~ [Nel~ Hell 0 IIIJ NIV N IIIJ Sill SIIIIJ C IIIJ ! R Aqr • SWP 1242.2 1283.8 13015.5 1335.7 1304.1 1402.11 14111.1 15411.1 1576.4 11100.4 11138.4 1IJIJ3.7 1722.3 1760.1 1117.0 11112.8 11107.11 3792 !54.!5 6.3 79.0 52.3 47.3 62.9 2!50.8 8.7 24.8 48.2 92.2 12.0 11!5.4 22.!5 231.9 *571.0 ~ '"I 5856 48.3 56.7 59.9 21.3 78.7 319.5 42.1 36.4 28.3 68.4 68.4 175.0 523.6 0 < 16918 30.4 84.3 93.1 62.4 105.6 74.5 *396.9 33.8 22.9 58.6 142.7 13.4 135.0 40.0 267.6 *725.6 Q: ..... 20069 23!5.7 9.6 54.2 33.1 68.6 20.2 298.8 42.!5 98.7 16.3 85.9 17.3 160.3 *526.9 1.0 1'1:1 Q. .j:>. 26!569 27.2 20.2 60.4 69.7 55.7 113.4 1!5.!5 291.0 32.7 114.0 13.!5 59.1 12.0 188.7 *510.1 28611 36.1 12.2 12!5.3 100.5 60.4 91.!5 38.3 402.6 42.3 142.4 67.5 14.7 170.3 *521.2 C" « 29562 26.4 29.0 107.6 106.1 76.9 112.4 31.6 *428.7 29.0 18.2 47.7 141.4 4.9 83.0 24.1 *250.1 *382.8 32846 35.1 14.0 80.0 104.7 79.0 102.2 15.8 646.4 13.1 8.0 89.!5 201.4 18.7 144.5 37.8 293.2 *806.4 ~ 1'1:1 NoTES.-Flux units are 10-14 ergs cm- 2 s-1 A- 1• Measured wavelengths are averages. Laboratory wavelengths are in italics in the header. Measured wavelengths, in italics with each star, are averages. Asterisk ( *) indicates a saturated feature. ~ rJ). >
[IJ> =t 0 "0 «= .....[IJ ~ [IJ ~
~ rJ).
«[IJ [ 1994ApJS...94..183M TABLE3 GENERAL PROPERTIES OF THE SYMBIOTIC STARS IN THIS ATLAS OBSERVED WITH JUE
Star liD# Spectal Typea Sym- #of Eo-v Radio X-rafEclip- Mira Orbital vr Distance Tbot Tc DC biotic IUE (6cm) Flux sing? Period Period (km/s) (kpc) @ Typeb Obs. Fiur (days) (days) (1o3K) (1o3K) (em-~ > (mJy) 9 1'1:1 EO .ADd 4174 M 2.4 III s 21 0.05-0.09 <0.26 yes 470-482 -96 0.32-0.63 60-80 .....'"I ~ ~ AX Per M5.2 II-III s 21 0.25-0.29 <0.71 maybe 682 105 10 >106 = LMC.Ailon D 2 0.25-0.30 600 10-20 106-107 >[IJ .... c'"I LMCS63 M s 2 0.02 49-55 50-80 10-20 107-108 =c RXPup 691~ ~M5 D 9 0.3-1.1 ~34 580 1.0-1.3 75-90 9 ..... 106-107 ~ He2-38 ~M5 D 2 0.93 433 113±4 3.8 10-30 ~ 1010 rJ). SYMus 100336 M4 III s 9 0.3-0.5 yes 625 1.1 >65 -c .....~ BICru M1III D 2 1.5±0.5 280 2.3-3.8 27 ....1'1:1 ~ -1.0 RWHya 117970 M2III s 9 0.01-0.13 <0.26 372 1.3 75-100 108-109 • Ul He2-106 >M5 III D 2 1.3 ~20 400-450 2.6-9.4 ~ '"I c Hen 1092 s 2 ~108 <..... Q. T'ers 143454 M4III s 12 0.08-0.15 <0.88 227 1.4 30-45 1'1:1 Q. 1010_1011 C" AGOra s 29 0.01-0.06 <0.46 3.6 554 87 ~ HKSco KSIII s 3 <0.36 ~ 1'1:1 z CLSco s 1 0.1-0.5 <0.42 625 4-8 100 rJ).> H1-36Arac D 1 0.27 ~46 450-500 7.6 > YCrA 166813 s 1 0.56 <0.54 150 (?) >[IJ .... YYHcr M2 II-III s 3 0.10-0.25 <0.32 150-200 3.6-8.3 50-100 c'"I "0 AS296 M5111 s 5 0.43 0.43 2.2 ~=- .....[IJ AS29SB 1 <0.21 66 ~ [IJ ARPav M3-4 II-III s 26 0.1-0.3 yes 605 4.5-5.8 ~ ....~ ~ rJ). ~ [IJ .... 1'1:1 9 1994ApJS...94..183M
@ > 9 1'1:1 .....'"I ~ =~ >[IJ .... TABLE 3-Continued c'"I Spectal Typea =c Star liD# Sym- #of Es-v Radio x-rarEclip- Mila Orbital vr Distance Thot Tc DC .....9 biotic IUE (6cm) Flux sing? Period Period (km/s) (kpc) ~ Typeb Obs. Flur (days) (days) (lolK) (lolK) (em-~ ~ (mJy) rJ).- c V443Hcr M5 III 2 0.2-0.3 <0.44 597 -60 0.9 80 -109 .....~ s 1'1:1 .... 109-1010 ~ BPCyg M5 III s 23 0.3-0.4 2.01 maybe 757 15-2 40-60 • CHCyg 182917 M6.5 III s 23 ?? 0.4-18 12 maybe 5750 -60 ?? 107-109 ~ '"I c HMSge ~MS III D 8 0.40-0.65 15 48 527 1-4? ?? ? <...... -1010 Q. \0 aeyg M4-5 III D 40 0.3-0.5 <0.42 yes 855 -20 15 150-175 10-14 1'1:1 0\ Q. Vl016 Cyg M4-7 III D 17 0.2-0.4 45 0.82 472 3467 1.3-6.0 125-160 106 C" ~ RRTcl ~MSIII D 13 0.1 28 0.67 374 -53 1.9-2.6 135-150 12-19 1oS-1o7 ~ 1'1:1 HBV47S M4-6 III s 34 0.3-0.6 1.07 maybe 950-975 1.2-3.4 50&170 15 106-107 z AGPeg 207757 M2-3 III s 8 0.1-0.2 7.51 733-827 1.3 30-95 11 1o10 rJ).> > ZAnd 221650 M3-6 Ill s 44 0.3 1.01 756 1.1 100-150 3.2 -1o10
>[IJ .... RAqr 222800 M7111 D 19 0.05-0.10 12 20 386 44 yr. 0.2-0.3 50-150 ?? c'"I "0 NoTES.- The symbol§ indicates X-ray flux at -0.2 keY in 10-12 ergs cm- 2 s- 1, corrected for interstellar extinction. =- • Kenyon & Fernandez-Castro ( 1987); Schulte-Ladbeck ( 1988). ~ b Kenyon ( 1986)...... [IJ ~ c Seaquist & Taylor (1990); Seaquist (1988). [IJ d Viotti ( 1993). ~ ....~ ~ rJ). ~ [IJ .... 1'1:1 9 1994ApJS...94..183M
@ > TABLE4 a QUALITATIVE SPECTRAL FEATURES OF THE SYMBIOTIC STARS IN THIS ATLAS ('tl ...."1 n Star J!Jg. Principal Resonance Lilies Principal Intersystem Lilies Continuum Flux Continuum Shape Commenb; ~ = # (NV, C IV, He D)f (0 IV, N IV, 0 lll, N lll, Si lll, C ID)] :1: >[IJ ..... "1 EO And 1 C IV dominates except at t = 0.2, 0.8 variable with phase absent at min. "'blue vanishing continuum at t=O.O implies eclipse 0 AX Per 2 2-3x stronger at optical maximum weaker at optical minimum strong at max. C III] and 0 III] " with time =0 flat,"' red ....a 3 N V stronger than He II, C IV n LMCAnon N IV), N Ill) very strong weak flat, "'blue possible CNO processing ~ LMCS63 4 C IV strong C III) strong "' blue steeply hot star and an M III -rJJ. 0 ....n RXPup 5 C IV, He II strong C Ill) strong flat, "' red intersystem emission decreasing since 1980-82 ('tl ~ Jle2-38 6 C IV strong 0 III], C III] strong noisy spectra weak • SYMus 7 2x less at t=O.O; C IV, He II strong weak in UV drops at min. N V and C IV very prominent out of eclipse ~ "1 0 Bl Cru 8 NV present 0 III], Si III) strong noisy noisy even when co-added ....< ~ -'.0 RWIIya 9 many broad, high ionization lines seen forbidden doubly ionized lines weak low on one obs. "'blue possibly eclipsing, in compact high density nebula ('tl -...1 ~ Ile2-106 10 C IV, He II seen 0 III], C III] seen > 1600 A, weak noisy, even when co-added «C"' Hen 1092 11 C IV, He II equally strong veryweak > 1700A flat very dense nebula ? ~ ('tl TCrB 12 strong when continuum strong strong when continuum strong varies flat substantial variation in continuum and line flux ~ > AGDn 13 He II stronger than C IV in both states weak in both outburst & quiescent states very strong "'blue at 15 year activity cycle for outbursts >rJJ. at outburst outburst - anomalous outburst in 1985, 86 14 N V, C IV, He II observed weak in UV noisy flat 1982 C IV, He II > 1981 C IV, He II >[IJ HKSco ..... "1 0 CLSco 15 C IV predominates 0 III), Si III], C III) unusually strong noisy "'red low density, photoionization region ? "0 «=- 111-36Arae 16 C IV, He II broad N III), C III) broad none broad emission lines ....[IJ YCrA 17 strong, narrow He II narrow weak flat main sequence, accreting star 7 [IJn ~ YY Her 18 all strong 0 IV], N IV], 0 III) strong; constant flat much weaker in 12/81 and in 5/80 a. weak> 1700 A ~ rJJ. AS296 19 " after outburst "' after outburst, especially > 1600 A noisy, weak -flat outburst in 1988 June «[IJ ..... a('tl AS 29SB 20 C IV, He II broad broad none only one IUE spectrum available 1994ApJS...94..183M
©
~ ('I) ....., ~ § TABLE 4-Continued Ill> Star Fag. Principal Raonanc:c Lines Principal Intersystem Lines Continuum Flux Continuum Shape Comments -§ # 0 ...a ARPav 21 stronger by 2x out of eclipse weaker during eclipse weak in eclipse , red non-eclipse effects of eclipse arc VCI}' noticeable !. V443Her 22 NV, C IV strong 0 IV], N III], Si III], C III] strong strong flat 11/80 spectrum -1.25x strength of 5/80 r:r.. 0 BPCyz 23 N V, 0 I VCI}' weak, except prominent; weaker during eclipse vel}' strong , blue at max. possibly eclipsing; emission in '86-'88 > '79-'80 ...~ ('I) at visual maximum flat at min. ~ CHCyg 24 strength varies with system state strength varies with state of the system varies erratically often flat; several active phases; • , red opaque, circumstellar, iron shell ..,"'C 0 JIM Sge 25 all lines intense many intense lines almost none flat variable emission intensity < ,_ 1.0 aeyg 26 stronger during '82 eclipse than '80 brighter during '80 eclipse than '82 weak; 0 at min. flat excitations WI}' from one eclipse to another ~ 00 !:lo ;;' V1016 Cyg 27 vel}' strong; 2x at UV maximum VCJ}' strong, 15x at UV maximum weak flat [Ne IV], [file V] present '-< RRTcl 28 strong, .. from '78 to '87 strong, gradually decreasing VCI}' weak flat consistent with a slow nova on the decline ~ ('I) lffiV47S 29 C IV, He II, strongest at visual max. somewhat weak, val}' with visual phase vel}' weak flat consistent with an eclipsing binal}'
~ AGPcg 30 strong N IV] exceptionally strong, strong , blue one of the brightest; has a dense nebular region r:r.. > weaker > ·1700 A Ill> ZAod 31 strong, He II much stronger in strong, 2-3x as much during outburst outburst: strong , red relative strength of intersystem lines greater at :;'" quiesence quies.: moderate flat outburst, implying material-from cool component 0 being photoionized "C RAqr 32 N V weak, C IV dominates C III) dominates, most are present strong flat has a jet seen in both radio and UV !... ~ NOTES.-Dagger (t) indicates N v XX 1238,1240; C IV XX 1548; 1550; He II X1640. Double dagger(;) indicates 0 IV] XX 1397, 1407; N IV] Xl487; 0 III] AX 1660, 1666; N III] AX 1747, 1753; Si III] >..1892; C III] XX 1906, 1909. The arrow pointing up (?)means "increasing toward," and the arrow pointing down (\.)means "decreasing toward." ~ ;. r:r.. l 1994ApJS...94..183M phases FIG. determined I.-Low-resolution © ..... N ~ ...... 1- ID ..J ::;) ..J ::;) 0 C/) w u.. X c. 0 ct in E ... Ill u ICl CD American by Chochol 1200 8 0 4 8 8 6 6 6 6 2 2 2 4 4 4 IUE eta!. Astronomical spectra 1400 (1987) WAVELENGTH of with EG 1600 Andromedae obtained Andromedae min (UBV) Society (A) SWP SWP 1800 SWP3753 SWP9644 SWP5834 cf> cf> cf> cf> cf> ======11007 15273 0.96 0.37 0.03 0.22 0.80 JD • 2,446,336.7 2000 Provided in the 199 SWP + 474.0dE_ ..... N N ...... 1- ID ..J ..J ::;) ::;) C/) u.. w X c. 0 ct 0 e in ... ICl CD Ill u by XA 1200-2000 the 8 8 8 8 6 6 6 6 2 4 4 4 8 6 2 2 2 4 4 NASA wavelength 1400 Astrophysics WAVELENGTH region. 1600 The (A) SWP24097 SWP22285 SWP19303 SWP18424 1800 cf> spectra 4>:0.76 cf> cf> Data ___ = = = ~- 0.24 0.99 0.75 ,A were System 2000 taken at orbital 1994ApJS...94..183M gest ionization lengths to symbiotics, very 1238,1242, distribution intense gions seen from are line the most lengths. near 2,436,679.4 200 Three FIG. increase both 0 emission increases, weak (Fig. optical maximum, prominent coming III] consistent 2.-Low-resolution narrow relatively UV UV A.A. 2) lines + but N © are the of spectra 681.6d 1660,1666 steadily minimum emission ~ ... N IV] ~ ~ 0 m :;) -1 into <( rn :;) ..J ...... >< w u.. ~ b lines .. Gl E Ill u Cl American consistent AX shows not emission signal-to-noise of emission A.1487 with showing E. flat view during C Per nearly 0.5 1.5 2.5 0.5 1.5 present 2.5 0.5 2.5 1.5 0.5 1.5 2.5 ofLMC The decrease, 2 IV 1200 0~~~~~~~~~~~ 3 2 3 1 2 3 2 3 (independent a 4.3. hot, is line to and and and SWP slight UV similar lines with maximum. as line a stellar LMC Anon intensities Astronomical C in N continuum He Anon spectra intense slight 1400 m] III] (Kenyon progressively increase while this the in ratio. WAVELENGTH 11, to A.A. blackbody A.A. the that have which orbital spectrum of of rise the 1907,1909 1747-1753 compared the C spectra. The wavelength) increases 1600 vary ofCI toward IV been symbiotic 1986). toward Hen are phase. A.A. UV by higher emission. Cyg co-added (Table present Society 1548,1550 A.1640 SWP6808 The toward SWP3755 (A) «1>=0.97 «1>=0.56 factors 1800 continuum shorter emission with are longer star The because and strength density the AX longer emission 3). N v N in UV N v N (Fig. exhibit of stron wave wave Persei. • 2000 High most is MEIER lines they and flux 2-3 wavelength Provided the A.A. re of 3) is Orbital ET tra 17 ...... , ... ~ phases b 'UI :;) ::J ...I ...I ...... u.. Ol 0 >< rn w ~ <( when !!I E u Ul Ill 4 FIG. ~ ... N ~ ... are 0 rn m :;) ...... -1 <( w :;) 7-17 -1 >< u.. ~ b AL. .. Ill Gl Cl in E u by not the 3.- were 53 the 0.5 1.5 2.5 0.5 1.5 2.5 0.5 1.5 2.5 0.5 1.5 2.5 well star are o~--~~~~~~~~~ 3 0.5 2 1.5 1200 2 3 3 2 Three 2 3 found 1200 OL-~~~~~~~~~~~~~~ NASA particularly is exposed. near co-added from 1400 a WAVELENGTH Astrophysics maximum. an v N 1400 strong. spectra ephemeris >.>. WAVELENGTH 1600 1238,1240, ofLMC by SWP25244 SWP23448 1600 SWP20479 SWP14758 (A) Kenyon «1>=0.84 «1>=0.52 «1>=0.99 «1>=·0.96 1800 Anon Data N IV] (A) are ( 1982) >.1487, SWP34122 SWP SWP System 2000 shown. 1800 using 26327+ 18315+ and These min N Vol. III] 2000 spec (pg) A>. 94 = 1994ApJS...94..183M and C continuum processing N shorter bidden a hot No.1, UV IV The FIG. IV], ...... ,. ,... C)l ';" (/) 0 --' c:( m .... :::1 :::1 w u.. ::::.. -1 X b star ... Cl Cll E u rn rn strong nitrogen strong lines, continuum which UV 4.- with emission wavelengths 1994 10 1200 8 6 0 2 4 respectively. This spectrum (Kafatos T.tr © flux ...... N C)l m .... ::::.. :::1 :::1 0 (/) c:( -1 -1 w u.. b >< in E ... Dl Cll rn u are > increasing American spectrum 25,000 lines distribution about 0.5 1.5 0.5 0.5 1.5 1.5 2 2r-----,------.------.-----. 2 et and emission of 1400 (e.g., al. K. of 4.4. The LMC toward 2-3 contains WAVELENGTH LMC FIG. 1983). N presence times Astronomical LMCS63 1400 S63 v, which shorter 5.-Low-resolution lines S63, WAVELENGTH N 1600 shown many stronger obtained IV], suggests wavelengths, characteristic increases of 1600 C relatively (A} allowed IV, in FAR-UV in than SWP Figure 1800 He evidence SWP SWP14239 SWP 1982 (A} Society 1800 steeply IUE II, the 16591 March, and weak 16598 10189 0 4 spectra m], exhibits He ATLAS semifor of toward carbon 2000 exhibits II 2000 N CNO • ofRX and III], Provided of a a OF Puppis, SYMBIOTIC gest gest the co-added the Si sion (Swings far-UV of of and component to the the times 1548,1550, 1907,1909...... N C)l 0 m :::1 (/) -1 w .... ::::.. :::1 b c:( -1 >< u.. in E ... Dl Cll rn u SY The RX 111], covering 1986. RX RX by phase most spectrum UV emission C lines lines Mus increases III]}, and 0.5 1.5 0.5 1.5 1.5 Pup the two Pup. Pup spectrum 1200 0~~~~~~~~~~~~ 2 & continuum 2r-----.------r-----,r-----, prominent of to in that Allen 1980 exhibits C with spectra is NASA He the and increase taken the STARS The III] lines ofLMC a are September toward 625 C II D-type decreased a 1972). SWP 1400 ofRX intersystem IV were cool A.1640, superposed dramatic between of WAVELENGTH day emission and Astrophysics and the S63 He 4.7. range 4.5. longer detected M Six symbiotic orbital 4.6. Pup to the C signal-to-noise 1600 0 indicate giant one. 2-38 in III] of 1986 SY RX 1980-1986 various UV III) are He exhibits intensity lines the wavelengths. being emission on Muscae period. shown May Puppis above SWP28284 SWP22462 SWP 2-38 AX variability N nine a (A} star present the 1800 v the continuum, 1660,1666 emission Data a 21403 XX ultraviolet background. presence during The similar in variety strongest. lines ratio. are 1238,1242, Figure in ephemeris C which 2000 System in the of IV the Only lines to of Figure of and UV 0 and which 6 observations strong a period The depends a III], The have slow present the hot spectrum C C C of slope 5. III) III] N stron stron some stellar IV emis Ken- nova been 1980 The III], 201 are on A.X AX in of 1994ApJS...94..183M drops spectrum factors eclipse yon ( added weak. 202 <1> FIG. FIG. = 0 m :;) .... rn -1 c:( :;) u.. >< -1 w & 0.0 I N N I - 3 0 :c. X u. 1- w 3 (/) 0 < Ill I E .... Cl 0 Cl) Cl) Q) to noticeably, Bateson ?.-Low-resolution 6.- of at ± increase 0.1 in 3-4. q, 1.5 Two 4 5 3 2 4 1 2 1 3 3 4 5~=:!!:=::!::!...F===~~~~¥=~=-I © 2..------.------.------,------. 2 0~~~~~~~~~:!::::=~=-J ). 1200 1 Figure - ~-----r------r------r-----. All N (1984) American low-resolution 0.5 the orbital v, and (±0.1 signal-to-noise 7. C was At IV, the phases 1400 IUE ), minimum and used emission indicating WAVELENGTH WAVELENGTH far-UV Astronomical SWP were Hen to ratio. spectra determine determined spectra 1600 are line ( q, The the = very of strengths of 0.0), presence UV He (A) the from the SWP prominent SWP SWP23517 SWP SWP (A) 2-38 1800 Society continuum 4>=0.88 symbiotic 4>=0.30 the 4>=0.57 phase the 10188 14237 14752+ decrease 15594 have continuum of ephemeris for the been star out is MEIER • 2000 each hot very SY Provided by co of min Muscae. ( ET V) I I N N are hot characterized - distribution densities 0 lines noise star. 1548,1550, some (e.g., :c. tent which 3 u. a 1- 0 X spectrum. w 3 (/) 0 Ill 1979 < E I Cl) 0 Cl) ~ Q) = These few AL. Two The JD m], 2-3 by photoionized C in with 2,435, reduction. Si and emission 4 4 5~----~------~-----. 3 3 5~~~~~~~~~*=~~ cases, 2 2 4 5~==~!!=~~~~~+==~~ 3 increases 1 1 N 2 1 o~----~-A~~~~~~~~ spectra SWP 1200 IV the all SWP times IV ne;;:: III], li.A. the hot 175.7 1987, He + NASA which spectra of exhibit 1548,1550 Si spectra IUE by smaller 10 0 stellar II lines noticeably III], + many Even 8 a nebular exhibit A.1640, 1400 IV] cm- 627 increases spectra noisy a ofRW C Astrophysics can nearly .OdE of A.A. so, in WAVELENGTH blackbody 3 III] broad, 4.8. 4.9. (Michalitsianos and BI SWP be and the region. (K~nyon a continuum, 1393-1407, are ofSY flat toward Hya Crucis UV clearly toward Bl RWHya He UV 1600 0 generally UV 31038 high-ionization Crucis in II m] Mus. continuum The spectrum continuum & emission. shorter A.1640 Figure (Fig. identified Bateson shorter A.A. emission-line than Data The if N SWP SWP SWP (A) 1660,1666) weak, et 1800 8) any, 4>=0.59 4>=0.70 are IV] wavelengths, 4>=0.0 9, al. intersystem those of 1984). were wavelengths. near 15705 16381 obtained The 23011 System flux the A.1487, this in with 1982). suggesting emission visual the co-added found most presence, symbiotic distribution a 2000 intensities suggests enhanced minimum UV C between intense lines Vol. consis in IV Only lines high flux the for A.A. 94 of in is a 1994ApJS...94..183M ofBI the which No. FIG...... ~ .., FIG. ... ' b )( c. UV :;) ...I ..... 0 w u. :;) ...I en m c( E u en ... Cl Gl en Cru 1, increases ~ I C\1 ... ~ 3 1- 0 >< T"" 11. 3 0 w <{ OJ en (/) continuum E> E Q) 8.- X 9.-Low-resolution 1994 have 6 The 5 3 4 2 1 1200 0 1.2 1.6 © 1.2 1.2 been 8 8 toward 4 8 1200 0 low-resolution American .------.,....-----r--- ~----~----~------~----~ co-added is still shorter 1400 noisy. SWP to 1400 WAVELENGTH wavelengths, increase /UE X Astronomical spectra WAVELENGTH indicates spectrum 1600 the ofRW 1600 signal-to-noise a consistent with cosmic-ray of (A) Hydrae FAR-UV BI SWP13583+ SWP15595 1800 Crucis. SWP Society SWP (A) SWP9645 ..... 1800 obtained hit. ---..., ratio. 3779 5863 Two a ATLAS hot Even 2000 between spectra subdwarf. • 2000 Provided so, OF 1979 SYMBIOTIC -< I C\1 ... January gest ~ C tinuum hibits which weakness but 11. 3 SWP suggests and litsianos, 1- 0 >< T"" made particularly preceding 3 0 en i\i\ w <{ OJ (/) E E> Q) X IV The by 1907, UV that C i\i\ range. 1.2 1.2 to an both and the UV m] 8 4 8 4 0 1200 1548,1550, and continuum determine that He 1909 IR of & ~----~~~~~~--._--~~ 1985 1987 i\i\ spectrum NASA the high Gutierrez- forbidden excess 2-106 STARS Hobbs the R W 1907,1909 are May. primary June densities, significant the 1400 Hya is due ifRW He The Astrophysics emission ( (SWP an of 1980). WAVELENGTH Moreno, 4.10. lines most II majority to and He is optically i\.1640, implies circumstellar Hya in possibly 26220) N 2-106 secondary decline He prominent Further 1600 agreement is m] of is Moreno, 2-106 Om) present spectra AX that an thick (Fig. spectrum. an in 1747-1753, eclipsing Data observations i\i\ the stars SWP emission-line eclipsing SWP D-type (A) 10) have dust. emission with 1800 longward & 1660,1666 compact Cortes is are System a 11000 31038 Kafatos, The far-UV generally system object embedded Si system. lack lines ( of 2000 m] should 1986) nebula continuum and . strength 1600 that Micha of i\.1892, in noisy, C con sug The 203 has the ex III) A. be in 1994ApJS...94..183M - .,... ~ """ .,... 'en - I ..... ::::> >< 0 ..J LL 1- w ::l ..J 0 en <( CD E (/1 u ~ Gl both N sity C lines March, permitted range ne several He cosmic with 2-106 204 The III] Figure FIG. IV], FIG. ~ II to a Al640. beyond permitted 10 taken AX C few 65,000 ray IVE 11.- 10.-An C 8 stages. has IV, 5 Snr-----.r-----~------r------~ 4 3 2 1200 o~~~~~~~~~LW~~~~~~ cm- 1907,1909 12 hit. narrow IV © in line The He a spectrum displays 1986 AX 1700 3 American relatively ~ • Emission SWP II, far-UV forming and emission Thot 1548,1550 July. 0 4.12. A low-resolution III]. could intersystem ofN the 1400 ~ spectrum The 4.11. of He flat 100,000 T region lines lines variable WAVELENGTH Hen UV III] Coronae indicate Astronomical II continuum suggests - Hen N ,... ,... C') of AX continuum A.1640 'e I - I are ..J :::> ,... en 0 1- 0 X u. ::J ..J UJ of m ct ... u (/1 C) en Cl) 1092 C is Hen emission 1747-1753, spectrum K. IV, more UV 1092 1600 quite a Borealis having The I He (Fig. very 092 that continuum is pronounced 11, flux 6~------r------r------r------~ hot, obtained underexposed weak of dense and lines {A) the 11), comparable the Society distribution Si probably SWP23515 C high-excitation symbiotic III] taken semiforbidden of lll]. nebula in ofT N A.1892, 1980 X when v, and in denotes • CrB March. in 0 star inten where MEIER 1980 noisy, with Provided and IV], 2000 the the WAVELENGTH He at a This ET star tively However, tions quence levels A.1640 ther taken timescales brightest Si (SWP factor C are associated outburst cence. C Kenyon tinuum with while strongest Meier, UV 1985/1986 1980/1981 optically yr- tions has by AL. IV, One The IV, III], 1 continuum a a is a He in He in the in weak Si 3815 flat compared strong are of C of IUE high-density The & the the star, decreases. 1986 the II, & or III] m]) line thin II), continuum the 3 Martin emission both (A) v N NASA of 0 outburst continuum Garcia a and outburst to hot spectra continuum UV UV and and rather (Fig. continuum least m], flat, being (SWP disk about with SWP8096 6 present AX flux SWP companion. continuum during continuum Si C weak with 1993). weak studied may 13). With intense 1238,1242, Astrophysics and ( lines m], than C III] 27556 taken nebula (SWP 1986) is 1 4.13. (SWP 5804) 4.14. IV strong yr strong more suggesting intersystem level. Emission-line be are continuum and level active increasing AX a in rising could responsible of symbiotics, and suggest 27542). white permitted always AG C (10 exhibit HK 1548,1550. both 11002, emission and These AG that recent Fluctuations and m] was SWP C 10 phases, Draconis toward be Scorpii become emission-line dwarf, Ora ~ become a IV active is considerably that weak N in continuum vastly hot emission associated UV ne SWP 28715) Data spectra. lines relatively AX emission v, quiescence. intensities for are HK ~ source shorter compared an Spectra C continuum that 1548,1550 and ofC or more the 10 different characterized weak IV, 15709) Sco associated accreting System suggest 11 absent, IV gains substantial The lines quiescent and cm- 65,000 with flat lines AX prominent, wavelengths exhibits variations flux when taken higher increase 1548,1550 He Both two than (e.g., 3 with continuum large and -10- ) and consistent observed. accretion. (e.g., flux, (Kafatos, main-se II ~ the with in spectra Vol. are phases a in in noisy. states, Thot quies N varia by varia He 6 1979 rela N with N con by M III], and the the the the ei an 94 in v, v, ~ II 0 a 1994ApJS...94..183M sity semiforbidden C intersystem March the region, ness N strongest inent 10 relatively 100,000 1907,1909. 1548,1550, emission No. IV Although The In 10 IV] FIG. continuum is cm- of flux this 1, evident and lines and semiforbidden far-UV i.e., 12.-IUE 1994 lines. Kin 3 UV emission decreased • weak. others A 1982 © The 10 He lines the are spectrum decrease in the 4 American lines spectrum rise ~ This II low-resolution spectra spectrum the continuum February. the are line-forming shortward ne ")...1640, ~ "' M ~ lines !/) m ..J 0 1- ::J ::J ..J :::::. LL < IL m ::;) ::;) ...1 <( rn w .. E Ill u Gl &:II © American 16 12 12 12 16~-----r----~------~----~ 8 4 8 4 8 4 SWP spectra 22056 Astronomical was WAVELENGTH of CH taken Cyg following obtained SWP SWP24956 (A) SWP7409 Society outburst, from 26219 1979 2000 when • December Provided the UV ...... :r .... b N 5 ::;) ...1 0 >< rn IL m ...1 <( w E u e' Gl Ill continuum to 1987 by 16 12 12 12 12 16~-----r-----,------~----- 1200 8 0 4 4 8 8 8 the January. was NASA heavily 1400 The WAVELENGTH blanketed continuum Astrophysics 1600 by is Fe highly SWP28682 SWP30134 SWP27571 SWP26720 (A) n absorption. Data variable 2000 System in flux level and 1994ApJS...94..183M very emission C There ing the mitted between 0 The that emission and lines both (1988). emission in mined UV Si source eclipse. eclipse flat were :.\1601, such (SWP (Aller lines line ing the tinuum that shown 9898) factor He 1982 1986 212 IV, The 111], The The The The III], Figure behavior outburst. II, system from continuum circumstellar emission-line the intensities is weak spectrum and of (e.g., increase much as during August and 0 are and and accompanied far-UV of 28896). SWP 1954). far-UV and in in interacted UV usually using IUE which During Many UV with III], the v N lines lines He 2 Fe spectra many Figure 1980 C UV 27, N C 1981 is through brighter © intersystem III], continuum Si spectrum 1978 spectra of II n the III]) IV], in spectra many to and During in the are that spectrum of that the (NV, III], is American spectra continuum of slow This weak and decreased a a strong reflecting August 1987 which strength earlier 25 the not C superposed UV low-excitation, reproduced and V1016 near more reddening. UV intensities C He emission include provide IV, 1982. intense novae are during 4.28. activity 1982 by shown 0 III]. intersystem in apparent. 4.27. 4.25. of maximum, the April. 1987 in II 4.29. He permitted of UV ephemeris I, 4.26. weak most disappears characterized eclipse (SWP is with lines ofHBV These the were 0 Figure by Cyg. There slightly V a strongly April 1982 11, which RR flux N maximum. the evidence IV], broad HM emission V/016 IUE in 1016 Astronomical a was lines HBV 0 symbiotics, on emission D-type have the v, CI that are factor 14756) Figure stronger Telescopii spectra 1980 III], All phase. and N eclipse, Si (SWP are a 26 Sagittae observations, Cygni quiescent lines exhibit lines 475 followed M between Cyg range SWP IV], weak [Ne of includes IV, reduced varied Cygni 475 at and orbital show many a = giant eclipse, of of lines symbiotic (or Nussbaumer wide 0 by but 28 0.5 C from visual (e.g., features, show 167 displays Whitelock v] a about C than continuum. of 5611 many IV], IV, a a hot are V1329 exhibit CI by III]) (±0.1), increased prominent slow atmosphere ionization :.\1574 52) ofN very by phases state. 1980 by assortment 0 N He the N suggesting that Cyg star very a minimum during and Society superposed a 2. III], both v, to resonance factor consistent IV], decline II, spectra weak, suggesting v, decrease many The August star Cyg) Line the Thot many in Si the 1986 strong and 0 N ( SWP were N C 1987) interstellar & and by IV, III], As III], emission IV, the strongest energies. of IV], emission emission ~ HM exhibits blanket flat Schmid [Ne than about follow ofN intense August of the shown strong 0 10 2 out deter N He in C (SWP 9878, phase • MEIER finds C from with 1980 lines con or per on 5 that IV], m]) III], hot Sge the Provided IV] K. IV, v, 11, in of 3 a a ET strongest superposed exhibits AL. FIG. by ...... ~ N )( b :!::. u...... ' 0 en w ID ...... ::;) ::;) ot Ul Cl E ... u Ul Ql 25.-Low-resolution many the emission on 0.5 2.5 1.5 1.5 0.5 0.5 0.5 0.5 2.5 2.5 2.5 2.5 1.5 1.5 1.5 3 3 2 2 2 NASA 3 3 3 2 2 intense a flat lines UV permitted in Astrophysics continuum. the /UE spectra. WAVELENGTH and spectra intersystem C IV, of He Data HM n, (A) emission SWP16752 SWP and SWP28896 SWP30694 SWP9898 Sagittae. System C 14756 III] lines This produce 2000 that system the are 1994ApJS...94..183M occurred continuum FIG. 26.-Low-resolution in is 1980 ...... slightly .... b Jl ~ © rn 0 IL ::;) ::;) ..... -1 -1 ot m w X \n E Ill u ~ July American and elevated. 25 25 25 15 15 35~----~~~~~~~~~~~ 35~-----r------~-----r----~ 25 15 15 5 1982 spectra Orbital November. Astronomical of WAVELENGTH phases 1980 CI During Cygni ECLIPSE for each taken a minimum SWP Society (A) spectrum SWP9663 SWP7818 SWP5485 <1>=0.57 <1>=0.06 <1>=0.85 <1> between = 11003 0.25 phase, were 1979 2000 • = Provided found June 0.0 and from (±0.1), ...... , .... ";" ~ 0 :::. ::;) rn ..... -1 b m w X IL ::;) -1 ot ... Ill Cl E Ill u CD 1983 Aller by the August. (1954) UV 35 35 35 25 25 25 15 35 25 15 15 15 the 5 5 5 5 continuum NASA These min(V) spectra = WAVELENGTH disappears, Astrophysics 1982 JD 2,411,902 were ECLIPSE obtained while + SWP20731 SWP SWP SWP (A) at <1> <1> <1> 855~25. <1> maximum, before = = = = Data 18603 17276 0.36 15274 0.04 0.87 0.58 and 2000 System = after 0.5 eclipses (±0.1), that the 1994ApJS...94..183M and FIG. intersystem 27.-Low-resolution ...... N C'!- ... :::1 :::1 c en 1- II.. 0 0 <1: m w X _. _. © In E .... CD u Cl t/1 emission American 8 8 6 6 6 2 2 2 4 4 4 8 8 6 4 lines. spectra Orbital Astronomical of WAVELENGTH (A) phases V 1016 were Cygni determined obtained SWP4271 SWP2427 SWP9878 SWP Society ci> ci> ci> ci> = = = = 0.32 0.36 0.52 0.41 5611 between from 2000 • Nussbaumer Provided 1978 214 August ...... N C'!- ... 1- :::1 :::1 c 0 en <1: m w X LL 0 _. _. In E .... u Cl t/1 CD & and Schmid by 8 6 2 4 8 8 8 6 6 6 2 2 2 4 4 4 1987 the (1988) November. NASA min(UV) WAVELENGTH Astrophysics V 1016 = JD Cygni 2,444,101 (A) SWP32296 SWP29829 SWP24656 SWP exhibits ci> ci> ci> ci> = = = = Data 19566 0.28 0.19 0.98 0.80 + many 3470dE. 2000 System broad, permitted, 1994ApJS...94..183M C IV FIG. and 28.-Low-resolution He 11. © -- ...... b c:' :::::. ..J ..J >< 0 en ::l ::l IXl ..... LL. w