COMMISSION 27 OF THE I.A.U. INFORMATION BULLETIN ON VARIABLE STARS Number 1213 Konkoly Observatory Budapest 1976 December 5 SPECTRAL INFORMATION ON NEW AND KNOWN LONG-PERIOD AND RELATED VARIABLES AND SOME NEW LATE-TYPE EMISSION-LINE STARS The stars discussed in this Bulletin were all found in the course of the Cleveland objective prism surveys for luminous stars in the Milky Way. Nearly all were found in our recent survey of the southern Milky Way, using plates taken with the Curtis Schmidt at Cerro Tololo in 1967 and 1968. Spectral dispersions were 580 A/mm at H-gamma and 1000 A/mm at H-alpha. The stars in Table 1 are all classifiable as M-type long-period variables, in that they show, besides TiO bands, strong hydrogen emission with Balmer decrement highly distorted (H-delta much the strongest line, etc.) that characterizes Mira-type variables near maximum light. Since the spectra of certain semiregular variable stars grade into those of the Mira stars, a few of the stars of Table 1 may not in fact be true Mira variables, especially in the case of stars previously classified SR variables; nevertheless we feel that the variability classification of such SR stars deserves further attention. The magnitudes quoted are photographic, derived from eye estimates of spectral image densities calibrated by magnitude sequences for each plate, or (with the letter v) visual ones from Kodak 103a-F plates, based on a mean calibration for all plates; the probable error for the former is +-1/3 mag. and for the latter +-1 mag. or so. When both kinds of magnitude are given at rather different phases the blue magnitude, for clarity, also carries the letter p, meaning photographic. Where indicated, these are named variables or have been listed in the Catalogue of Stars Suspected of Variability (CSV); but none are classified, if at all, as Mira- type in the variable star catalogue (GCVS). The quoted coordinates are independent re-determinations, and in general agree very well with the published ones. An asterisk in the Remarks column of all tables denotes additional notes on a star following the table. The format for Table 2 (see heading for contents description) is as for Table 1. In a few cases we have not re-measured the coordinates. Besides providing spectral types (all are M stars), our Balmer-line observations independently confirm these stars as Mira-type. Table 3 is arranged like the others, except that the magnitudes are visual and as described above, unless carrying the letter p, since most of these stars were observed only on H-alpha plates. Apart from the already- named variables, most of these stars (especially the first two) will probably turn out to be variable stars. In the "H-alpha" column we give the H-alpha emission strength as strong, moderate, or weak. C.B. STEPHENSON N. SANDULEAK Warner and Swasey Observatory Cleveland, Ohio, U.S.A. TABLE 1. Stars Not Classified (if listed at all) by the Variable Star Catalogue, Third Edition through Third Supplement, as Mira-Type, but so classified by Us Spectroscopically. GCVS alpha (1900) delta Spec Mag. Remarks 6 29 26.5 -10 12 26 M5 13.9 6 29 52.1 -13 37 04 M4 13.9 CSV 792 6 31 48.6 -16 49 53 M4 14.4 7 09 52.8 -30 24 26 M6e! 13.1 7 10 49.0 -32 49 15 M7 13.1 7 17 18.2 -29 06 35 M7 13.3 * CSV 1084 7 29 50.7 -28 10 40 M8: 13.8 YZ Pup, SR 7 39 58.4 -21 37 30 M5-7 11.7-12.5 7 43 06.8 -38 23 40 M8: 13.7 CSV 1218 8 02 28.0 -37 00 25 M 14.5 8 05 04.9 -45 26 42 M 14.0 8 16 56.2 -26 21 32 M2 12.1 * 8 24 30.8 -29 13 32 M 14.8 CSV 1405 9 00 00.3 -42 06 27 M8 13.3 9 00 30.6 -36 27 13 M 14.2 9 05 32.2 -56 25 07 M3 13.4 9 34 31.7 -44 43 51 M6: 13.4 9 45 27.4 -54 25 47 M6 14.7 CSV 1530 9 50 25.1 -59 53 M5 13.5 10 04 09.4 -60 03 38 M5 13.6 * 10 05.9 -64 17 M 13 10 09 17.7 -49 47 22 M5: 13.5 * CSV 1609 10 20 57.3 -50 44 27 M5 12.9-14.1 VZ Vel, SRa 10 24 09.9 -50 40 25 M6 10.3p-14V HD 298126 10 24 28.7 -49 35 00 M5-6 13.3p-11V * 10 39 11.2 -53 01 49 M5 13.4 * 10 45 42.4 -52 14 18 M5-7e! 14.3, 13.1V CSV 1669? 10 49 41.0 -48 49 18 M7e! 12.5, 11.4p * 11 07 44.1 -53 42 08 M2 12.4 11 52 25.9 -68 17 00 M6 12.3 12 16 53.3 -55 10 35 M7 13.4 12 21.3 -59 28 M8: 13 12 23 01.1 -68 01 56 M5 13.2: CSV 1889 12 29.7 -60 10 M5: 13 * AL Cen, SRa 12 30 32.8 -53 03 03 M3-4 10.3 HD 109576* RW Cru 12 34 15.5 -60 52 21 M8 13.5 * DW Mus, Cep 13 01 06.8 -68 21 27 M5 12.2 * 13 45.4 -63 58 M 13 CSV 2278 15 04 23.8 -68 21 54 M4 12.4 CSV 2301 15 09 39.6 -70 50 59 M4 11.1 C.P.D. -70d2005 15 19 28.9 -65 16 24 M5 12.4 15 31 40.1 -59 42 54 M4 12.2 15 36.0 -64 49 M 13 SY TrA 15 37.0 -66 22 M 14 15 42.4 -66 37 M8: 13 16 04 03.7 -58 32 29 M5 12.7 CSV 2591 16 04.8 -59 29 M 13 16 27 52.1 -52 01 49 M6 13.3 16 31 21.6 -53 52 37 M4-5 12.9 CSV 2791 16 36 57.3 -56 57 23 M 13.9 V503 Oph, SR 16 47 16.9 - 5 17 23 M3 12.7 CSV 2862 16 52 12.0 -44 41 20 M 12.4 NX Oph, M? 16 53 21.1 -27 50 25 M 13.6 FR Oph, L 16 57 01.6 -28 42 17 M 13.6 GP Oph 16 58 47.2 -27 04 39 M6 13.3 17 01 52.4 -51 33 07 M3 12.4 CSV 3218 17 24 43.2 -16 25 40 M 12.4 17 35 41.3 -15 49 37 M2: 12.4 UV Ser 17 38 28,4 -14 53 30 M 12.9 PU Sco, SRa 17 38 43.8 -43 04 23 M3 12.3 CSV 3420 17 40 00.0 -13 46 21 M 13.2 V1278 Sgr, M? 18 02 02.3 -34 02 35 M5 13.1 * 18 09 14.2 -29 36 19 M1: 13.2 * 18 15 27.9 -30 21 20 M 13.2 18 16 11.9 -29 09 35 M2 13.2 18 17 26.3 -28 10 28 M 13.2 18 18 31.4 -29 06 59 M 12.8 18 19 15.6 -29 04 17 M 13.2 Notes to Table 1. 07h17m Detected in the two-micron survey, therein -30086; type M6 by Hansen and Blanco, Astron. J. 80, 1011, 1975. 08 16 CaI lambda4227 is markedly weak. 10 04 CSV 1563, which has no published identification chart, has a published position differing by 2 1/2'-3 1/2' from ours. Our position is only a single determination. 10 09 Near, but different from, the planetary nebula PK 278+5d1. 10 24 One of the few cases in which, at 1000 A/mm, we have been able to see H-alpha emission in a long-period variable. CaI 4227 weak. 10 39 H-delta ~ H-gamma emission on the blue plate, but H-beta and H-alpha (plate taken 2 days later) are absent so the star should be a long-period variable. 10 49 The CSV star has no published identification chart; the published position is 5s west of us. Our position is the result of two accordant plates. A 12th-mag. F star lies about 1s.5 west of our star, and a 10th-mag. early A star is about 4s.0 west of us. 12 29.7 CSV 1889 has no identification chart, and a published r.a. different from ours by 0m.2. Ours is uncertain by about this amount. AL Cen Spectrum already quoted as Me in the 2nd supplement to the GCVS, and by Houk and Cowley (Mich. Spectral Survey, Vol.1). RW Cru Spectrum given as M6-7e by Loden (no 8765), Astr. & Ap: Suppl. 23, 1976. DW Mus Our identification of the variable is confirmed by the chart published by Van Hoof in IBVS No. 233, 1967. In this paper the author identifies the star as having a one-day period, on the basis of seven hours' unquoted observations plus scattered observations which previously had indicated a much longer period. V1278 Sgr Our position, derived from only one plate measure, differs from the GCVS by about 0.5' in decl. The GCVS already has the spectral type Me. 18 09 V1582 Sgr, which has a published identification chart in the paper following the one cited in the GCVS, is about 2' away. TABLE 2. Named Variables, Classified in GCVS as Mira-Type, But Lacking Published Spectral Types or Observations of Emission. All Show Emission of the LPV Type on Our Plates. GCVS alpha (1900) delta Spec Mag Remarks DL CMa 6 47 26.7 -18 55 00 M6-8 11.8-12.7 * BI CMa 6 58 33.6 -23 43 41 M5 13.5 UV CMa 7 01 08.9 -28 09 20 M5-8 12.0 SY CMa 7 06 12.1 -19 40 16 M4-6 11.4-12.3 * EG Pup 7 32 01.8 -26 16 49 M8: 13.4-15.0 CN Pup 8 00 30.3 -48 10 38 >M5 13.5 BK Vel 8 05 20.3 -43 41 57 M 14.2 FP Pup 8 11 39.5 -23 00 45 M4 14.3 CC Vel 9 34 14.5 -44 56 35 M7 12.5 DW Vel 9 46 28.9 -51 31 56 M8: 14.1p, 13.5V DY Vel 9 48 31.9 -49 03 13 M7 13.1 AF Car M8 13: * TT Car 10 17 17.6 -61 14 34 M6 13.6 BQ Mus 11 25 16.7 -69 16 38 M6 12.9 Y Cru M6: 13: UU Cen M8 14: QU Cen M 13 UU Cir 14 03 25.4 -66 35 25 M6 13.1 VX Cir 14 14 34.2 -69 30 13 M7 11.1-12.4 AA Lup 15 02 00.9 -48 30 35 M5 12.8 AU Lup 14 17 18.5 -44 02 48 M5: 13.0 BN Lup 15 27 24.1 -47 37 12 M2 14.0 AS Nor 15 49 00.8 -44 20 53 M6 11.8-13.6 BM Nor 15 57 51.7 -59 28 34 M6 12.7 CD Nor 16 02 42.5 -57 17 06 M4 12.7 CC TrA 16 14 11.7 -61 31 28: M 13.2 RY Nor 16 23 38.3 -58 08 17 M7 12.7 CR Oph 16 49 02.3 -28 44 32 M 13.5 DU Oph 16 51 48.6 -27 51 12 M 14.0 HR Oph 17 01 02.1 -28 03 47 M 14.0 AK Ara 17 12 42.4 -47 16 02 M5: 12.9 KZ Sco 17 14 54.0 -45 28 39: M4 13.3p, 10.5V LO Sco 17 18 23.9 -44 22 27 >M5 11.9 V439 Sco 17 50 36.6 -37 16 05: M0 13.2 FY Sgr 18 04 39.7 -33 06 54 M4 13.1 LP Sgr 18 21 43.9 -27 44 08 M 12.9 V3876 Sgr 18 27 17.3 -20 10 19 M8 14.3 * BI Aql 19 16 45.5 - 8 34 32 M0 13.4 V497 Aql 19 44 25.4 + 6 36 04 M1 13.3 V427 Aql 19 52 39.5 + 8 26 23 M4 12.6 * EK Aql 20 08 42.5 - 5 28 21 M3-4 11.8-12.3 V519 Aql 20 09 29.9 - 1 28 47 M 13.3 Notes to Table 2. DL CMa Already classified M7 by Hansen and Blanco, Astron. J. 80, 1011. Identified in the two-micron survey, -20110 therein. SY CMa Spectrum washed out. AF Car H-alpha emission seen by Henize, Astrophys. J. Suppl. 30, 491. BQ Mus Our position, based on only one measured plate but confirmed (to about 0.2') by computer overlay, differs from the GCVS position by 0.7' in decl. and 0.3' in r.a. V3876 Sgr Found in the two-micron survey; there numbered -20494. Also classified M8 by Hansen and Blanco, Astron. J. 80, 1011. Emission outstanding on our plate. V427 Aql The published identification chart makes our star the variable, but our position, checked by computer overlay, disagrees with the GCVS one. TABLE 3 Definite or Suspected Late-Type Stars Showing H-alpha or Other Emission alpha delta Spec H-alpha Mag. Remarks 8 08 49.4 -33 56 09 ? s 13.5: * 8 10 10.0 -35 49 50 m 13.5: Wray 18.* 8 52 25.7 -48 07 11 M4 w 12.5 8 57 43.9 -49 22 05 M4: m 12.5 10 50 36.4 -50 10 59 M6: m 12.5 11 02 08.6 -48 45 35 M5 w 12.1 12 34 08.2 -61 47 47 M2 m 9.7 14 19 51.7 -57 52 20 M1 s 11.7 17 04 32.5 -27 33 20 Red m 12.5 * 17 16 32.9 -29 06 28 M5 - 11.7p V520 Oph, SRd.* 17 19 04.5 -47 12 48 M1 - 12.9p AN Ara, SR.* 17 21 18.7 -44 19 36 M1 s 11.4 18 35 48.1 - 4 50 06 M1: m 12.5 19 10 50.0 - 8 28 16 M? m 13.0 19 15 56.4 - 6 57 56 M? s 12.8 BH Aql, L. Notes to Table 3 8h08m A deep blue plate shows a weak continuum without absorption features at 580 A/mm, with Balmer series and H and K emission. 8 10 Our declination, based on only one plate, is 27" north of Wray's (table XV of his Ph.D. thesis, unpublished). A blue plate shows, at the plate limit, no absorption features, with Ca H and K and probably H-beta, in emission. 17 04 May be early M-type. On the boundary of a dark cloud. V520 Oph. GCVS spectrum K0? The blue-region hydrogen emission is suggestive, but inconclusively, of a Mira variable. AN Ara Blue-region emission inconclusively suggestive of a Mira variable.