CDROM/AJ/V110/P1838 Northern M Dwarfs (Reid+ 1995) ================================================================================ The Palomar/MSU Nearby-Star Spectroscopic Survey. I. The Northern M Dwarfs - Bandstrengths and Kinematics I. Neill Reid, Suzanne L. Hawley, & John E. Gizis <1995, AJ, 110, 1838> =1995AJ....110.1838R ================================================================================ Abstract: The Third Catalogue of Nearby Stars (Gliese & Jahreiss Preliminary Version of the third Catalogue of Nearby Stars, 1991) includes over 1850 stars which lie north of Dec. = -30 deg and are either identified as spectral type M, or are unclassified but with an absolute visual magnitude estimate M_V > +8.0. Although there is no uniformity in selection criteria, and many of the stars lack basic data (radial velocities, spectral types, accurate photometry), the observational properties of these stars underlie most estimates of the fundamental characteristics of the Galactic Disk. We have obtained optical spectroscopy of 1746 of the 1876 stars -- the remaining 130 are binary companions of brighter stars and inaccessible to our observations. These spectra allow us, first, to exclude 61 stars as either degenerates or as misclassified earlier-type (B-K) stars lying beyond the 25 pc limit; to establish radial velocities accurate to +/- 10 km/s for all stars confirmed as late-type dwarfs; to determine spectral types and absolute magnitudes from the TiO bandstrength, allowing more accurate distance estimates for stars with inaccurate (or no) trigonometric parallax measurements; and to identify stars with Halpha emission (chromospherically active stars) and with strong CaH absorption (perhaps including some metal-poor disk subdwarfs). We have determined the nearby-star luminosity function from complete samples derived by applying both the distance limits defined by Wielen (1974) and by using limits derived from our own analysis. In both cases, we find good agreement with Wielen's results to M_V ~ +11, but lower densities at the maximum (M_V ~ +12). The latter analysis results in a luminosity function, Phi(CNS), which closely matches photometric parallax analyses for M_V < +11 and M_V > +14 -- we do not recover the apparent excess of low-luminosity stars inferred from analysis of the 5 pc sample. However, Phi(CNS) does lie below Phi(phot) at the peak (M_V ~ 12), and we suggest that this offset is caused by the inclusion of unrecognized binaries in the photometric surveys. We have also reanalyzed the local stellar kinematics using the complete sample and find that the velocity distributions show significant departures from single Gaussian velocity dispersions. File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- table1a.dat 80 1685 Basic data - main sample table1b.dat 78 130 Unobserved binary companions table1c.dat 74 61 Early-type stars, giants and degenerates table1d.dat 74 5 Additional stars table3.dat 64 1690 Bandstrengths table5.dat 48 1685 Radial velocities and space motions table1a.tex 124 1784 AASTeX version of table1a.dat table1b.tex 143 192 AASTeX version of table1b.dat table1c.tex 115 109 AASTeX version of table1c.dat table1d.tex 105 54 AASTeX version of table1d.dat table3.tex 85 1761 AASTeX version of table3.dat table5.tex 73 1759 AASTeX version of table5.dat -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1a.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Star Star number 5 1X --- --- Blank 6-18 A13 --- Name *Star name 19 A1 --- Note1 *Note flag 20 A1 --- Bin *[ps] Primary or secondary binary comp. 21 1X --- --- Blank 22-24 I3 h RAh Right ascension, 2000 25-27 I3 min RAm R.A. 28-32 F5.1 s RAs R.A. 33 1X --- --- Blank 34 A1 --- DE- Declination sign 35-36 I2 deg DEd Declination, 2000 37-39 I3 arcmin DEm Dec. 40-42 I3 arcsec DEs Dec. 43-44 2X --- --- Blank 45-47 A3 --- Src *Source of positional data 48-53 F6.2 mag M_V Absolute V magnitude 54 A1 --- Note2 *Note flag 55-59 F5.1 pc r *Distance 60-62 I3 % e_r *Distance uncertainty 63 1X --- --- Blank 64 A1 --- CNS [C ] Indicates r & M_V taken from CNS3 65-67 I3 % Pi []? Weight for trigonometric parallax 68-71 I4 % S []? Weight for spectroscopic parallax 72 1X --- --- Blank 73 A1 --- l_Sp Limiting character on Sp 74-78 A5 --- Sp Spectral type 79 1X --- --- Blank 80 A1 --- Note3 *Note flag -------------------------------------------------------------------------------- Notes for file: table1a.dat -------------------------------------------------------------------------------- Name: Gl - Gliese (1969, Veroff. Astr. Rechen-Instituts, Heidelberg, Nr. 22) GJ - Gliese & Jahreiss (1979, A&AS, 38, 423) Wo - Woolley et al (1970, R. Obs. Ann., No. 5) LHS - Luyten Half-Second Catalogue LTT - Luyten Two-Tenths Catalogue LP - Luyten Palomar proper-motion catalogue G - Giclas et al (1971, The Lowell Proper Motion Survey) GR - Giclas et al (1971) red star GH - Giclas et al (1971) Hyades star Rob - Robertson (1984, AJ, 89, 1229) Steph - Stephenson (1986, AJ, 91, 137) PS - Pesch & Sanduleak (1978, AJ, 83, 1090) San - Sanduleak (1976, AJ, 81, 350) vA - van Altena (1969, AJ, 74, 2) V - Vyssotsky (1963, Stars and Stellar Systems III, Basic Astronomical Data, edited by K. Aa Strand; University of Chicago Press, Chicago; p. 192) Note1: e 629 (Hy 207) appears twice in the preliminary version of the CNS3 g 2064: The CNS3 notes that GJ 1167B does not exist. h 2172: This star is not listed as double in the LHS i 2426 (GJ 2112 A): Eggen (1980, ApJS, 43, 457) notes that this star appears to be a double in good seeing, but there are no confirming observations. j 2772: The CNS3 lists Gl 678.1B as a line-of-sight optical companion k 2805 (GSC036B-821) is listed in the CNS3 as a companion of V796, but the authors find that the radial velocity differs by 50 km/s l 2935: Echelle spectra of GJ 1230A indicate that this `star' is actually a near equal-mass spectroscopic binary (Reid & Gizis, in prep.). The absolute magnitude estimate has been adjusted to take this into account. k 199 (Gl 49/Vys. 2): This star forms a wide cpm pair with Gl 51. l 1527 (Gl 360/Vys. 550/G235-35): This star forms a cpm pair with Gl 362 (G235-36), Delta = 90", p.a.= 75 deg m 2259 (Gl 541.2/Vys. 716): Weis (1993, AJ, 105, 1962) lists a possible companion of V=14.10, (V-I)_K=2.93 at Delta = 58", p.a. = 250 deg o CNS3 lists optical companions for these stars. There are as yet no observations to determine whether the stars are binaries. Bin: Components in a binary system are identified as p (primary) or s (secondary, tertiary). Src: Source of positional data: 1 - P60 (36 stars), 2 - P200, Keck, AAT (35), 3 - GSC (1479), 4 - CNS3 (6), 5 - Digital Sky Survey (129); Since completing the text of this paper, the authors used the on-line Digital Sky Survey to check all stars where the positions differ by more than 15 arcseconds from the CNS3 data. They assumed mean epochs of 1954.0 and 1980.0 for POSS I and UKST plates in deriving positions from the DSS. Note2: a CNS3 lists a photographic magnitude - the authors assumed an (m_pg-V) colour of 1.5 magnitudes b CNS3 lists a `photometric' magnitude for this star r, e_r: Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. Note3: c Spectral type from Kirkpatrick et al, 1995, AJ, 109, 797 d Strong CaH - probable metal-poor disk dwarf or halo subdwarf f 1752: Leggett & Hawkins (1988, MNRAS, 234, 1065) suggest, on the basis of JHK colours, that this star might be a giant, but our spectra are consistent with classification as a dwarf. Note that the V magnitude listed by LH88 is 8.07, while the CNS3 magnitude is 11.4 (photometric estimate). The authors observed a star of the latter magnitude. There is a nearby 8th magnitude SAO star (SAO 7382) - listed as K5, luminosity class unknown but Mu ~ 0 arcsec/yr which Leggett & Hawkins may have observed by mistake. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1b.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Star Star number 5 1X --- --- Blank 6-17 A12 --- Name Star name, references same as Table 1A 18-19 A2 --- Note1 *Note flags 20-22 I3 h RAh Right ascension, 2000 23-25 I3 min RAm R.A. 26-30 F5.1 s RAs R.A. 31 1X --- --- Blank 32 A1 --- DE- Declination sign 33-34 I2 deg DEd Declination, 2000 35-37 I3 arcmin DEm Dec. 38-40 I3 arcsec DEs Dec. 41-42 2X --- --- Blank 43-45 A3 --- Src Source of positional data, as in Table 1A 46-51 F6.1 mag M_V *Absolute V magnitude 52 A1 --- Note2 *Note flag 53-57 F5.1 pc r *Distance 58-60 I3 % e_r *Distance uncertainty 61-66 F6.1 mag V_P Magnitude of primary star inthe system 67-72 F6.1 mag dV Magnitude difference 73-78 F6.1 arcsec dP Separation -------------------------------------------------------------------------------- Notes for file: table1b.dat -------------------------------------------------------------------------------- Note1: c 377: The CNS3 notes that this star is not listed as a companion to Gl 84.2A in any of the Luyten proper motion catalogues d Gl 171.1A, or ADS 3321 A, is Alp Tau e Gl 452B (1863) is listed as an f-type companion to Gl 452A, 7.5 magnitudes fainter and ~15 arcseconds distant. The authors were unable to locate this star on the TV guider (r_lim ~ 21) of the Keck telescope f The companion to LHS 2789 (2172) is listed in the LTT, but not in the LHS and may not exist g Known VLM companion - Forrest, Skrutskie & Shure, 1987, ApJ, 330, L119 h Eggen (1980, ApJS, 43, 457) noted that the primary star appeared double in good seeing, but there is no strong evidence for a binary companion n These stars are not listed separately in the CNS3 M_V: Absolute magnitudes have been calculated using the magnitudes listed in the CNS3 and the distance estimate to the primary star (either from CNS3 or Table 1A) Note2: a CNS3 lists a photographic magnitude b CNS3 lists a 'photometric' magnitude estimate r, e_r: Distance and estimated uncertainty (%) from the authors' data, using a weighted combination of trigonometric and spectroscopic parallaxes. -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1c.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Star Star number 5 1X --- --- Blank 6-19 A14 --- Name Star name, references same as Table 1A 20 A1 --- Bin *[ps] Primary or secondary binary comp. 21 1X --- --- Blank 22-24 I3 h RAh Right ascension, 2000 25-27 I3 min RAm R.A. 28-32 F5.1 s RAs R.A. 33 1X --- --- Blank 34 A1 --- DE- Declination sign 35-36 I2 deg DEd Declination, 2000 37-39 I3 arcmin DEm Dec. 40-42 I3 arcsec DEs Dec. 43-44 2X --- --- Blank 45-47 A3 --- Src Source of positional data, as in Table 1A 48-53 F6.2 mag V V magnitude from the CNS3 54-59 F6.1 mag M_V *Absolute V magnitude 60-65 I6 pc r Distance 66 A1 --- Note1 *Note flag 67 1X --- --- Blank 68-73 A6 --- Sp Spectral type 74 A1 --- Note2 *Note flag -------------------------------------------------------------------------------- Notes for file: table1c.dat -------------------------------------------------------------------------------- Bin: Components in a binary system are identified as p (primary) or s (secondary, tertiary). M_V: Absolute magnitudes are derived using Reid & Murray's (1992, AJ 103, 514) (M_V, (B-V)) relation unless otherwise indicated. Note1: a distance from CNS3 b distance estimated from the spectral type c distance estimated from companion star e FS Comae - distance based on Jura & Kleinmann's (1992, ApJS, 83, 329) M_K f distance from McCook & Sion (1987, ApJS, 65, 603) (M_V, B-V) relations Note2: d 757: foreground reddening probably present -------------------------------------------------------------------------------- Byte-by-byte Description of file: table1d.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1-12 A12 --- Name Star name 13 1X --- --- Blank 14 A1 --- Note1 *Note flag 15 1X --- --- Blank 16-18 I3 h RAh Right ascension, 2000 19-21 I3 min RAm R.A. 22-26 F5.1 s RAs R.A. 27 1X --- --- Blank 28 A1 --- DE- Declination sign 29-30 I2 deg DEd Declination, 2000 31-33 I3 arcmin DEm Dec. 34-36 I3 arcsec DEs Dec. 37-38 2X --- --- Blank 39-41 A3 --- Src Source of positional data, as in Table 1A 42-47 F6.2 mag M_V Absolute V magnitude 48-53 F6.1 pc r Distance 54-56 I3 % e_r Distance uncertainty 57 1X --- --- Blank 58-59 A2 --- Dist *Method of distance determination 60-66 F7.1 km/s V_r Radial vel. from authors' spectroscopy 67 1X --- --- Blank 68-72 A5 --- Sp Spectral type 73 1X --- --- Blank 74 A1 --- Note2 *Note flag -------------------------------------------------------------------------------- Notes for file: table1c.dat -------------------------------------------------------------------------------- Note1: d From Brosch & Goldberg 1994, MNRAS, 268, L27 e From Irwin et al. 1991, MNRAS, 252, 61P Dist: Sp Distance estimate is based on the authors' spectrocopic data Pi Distance estimate is based on trigonometric parallax Note2: c Strong CaH - probable halo subdwarf f Spectral type from Kirkpatrick et al. 1995, AJ, 109, 797 -------------------------------------------------------------------------------- Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Star Star number 5-10 F6.2 --- TiO1 []? TiO1 bandstrength ratio 11-16 F6.2 --- TiO2 []? TiO2 bandstrength ratio 17-22 F6.2 --- TiO3 []? TiO3 bandstrength ratio 23-28 F6.2 --- TiO4 []? TiO4 bandstrength ratio 29-34 F6.2 --- TiO5 []? TiO5 bandstrength ratio 35-40 F6.2 --- CaH1 []? CaH1 bandstrength ratio 41-46 F6.2 --- CaH2 []? CaH2 bandstrength ratio 47-52 F6.2 --- CaH3 []? CaH3 bandstrength ratio 53-58 F6.2 --- CaOH []? CaOH bandstrength ratio 59-64 F6.2 --- Halp []? H alpha equivalent width -------------------------------------------------------------------------------- Byte-by-byte Description of file: table5.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 4 I4 --- Star Star number 5-11 F7.3 arcsec/yr pmRA Proper motion in R.A., from CNS3 12-18 F7.3 arcsec/yr pmDE Proper motion in Dec., from CNS3 19-25 F7.1 km/s V_rad Radial velocity 26 A1 --- Note [*] If no proper motions are available 27-31 I5 km/s U U space velocity 32-36 I5 km/s V V space velocity 37-41 I5 km/s W W space velocity 42-48 F7.2 mag M_V Absolute V magnitude -------------------------------------------------------------------------------- ================================================================================ (End) Lee Brotzman [ADS] 02-Nov-1995