3. The library

As in Paper I, the stars included in the library have been selected as stars with low levels of chromospheric activity, that is to say, stars that do not present any evidence of emission in the core of Ca II H & K lines in our spectra (Montes et al. 1995c, 1996a), stars with the lower Ca II H & K spectrophometric index S (Baliunas et al. 1995), or stars known to be inactive and slowly rotating stars from other sources (see Strassmeier et al. 1990; Strassmeier & Fekel 1990; Hall & Ramsey 1992). In addition, we provide spectra of some active stars of late and very-late spectral types.

 

HD HR GJ Name MK [Fe/H] v sini S Obs. Pap. I

(dex) (days) (km s^-1) F stars

33256 1673 189.2 68 Eri F2V -0.49 - 0 - 3

6406 F3/F5IV/V - - - - 3

84937 BD+14 2151 F5VI -1.86 - - - 2

BD+18 3423 F6V - - - - 1

78154 3616 F6IV - - 0 0.142 6

9826 458 61 50 And F8V MK -0.14 - 8 0.154 1

142373 5914 602 F8V -0.431 - 10.0 0.147 5 *

144284 5986 609.1 F8IV (SB1) 0.23 - 27.7 0.203 6

98230 4374 423B F8.5V MK -0.12 - 3 - 5

114762 BD+18 2700 F9V -0.87 - - - 3

79028 3648 337.1 16 UMa F9V (SB1) - - 0 - 5, 6

114710 4983 502 F9.5V MK 0.135 12.35 4.3F 0.201 3 *

160269 6573 26 Dra G0IV-V (MK) (SB1) MK - - 41 - 1

15335 720 99.1 13 Tri G0V - - < 6 - 4

39587 2047 222B G0V (SB1) MK -0.084 5.36 8.6F 0.325 3 *

98231 A 4375 423A G0V (SB1) -0.352 - < 15 - 5 *

84737 3881 15 LMi G0.5V MK -0.04 - 3 0.145 5

10307 483 67 BD+41 328 G1.5V (SB1) MK 0.14 - 2.1 0.152 2

42807 2208 230 BD+10 1050 G2V - - - 0.352 4

153631 650 BD-13 4528 G2V (SB1) - - - - 3

186427 7504 765.1B 16 Cyg B G3V MK -0.002 - 0.4 0.145 1 *

86728 3951 376 20 LMi G3V MK -0.11 - 3 0.156 6

115617 5019 506 61 Vir G5V 0.032 - 0.4 0.162 3 *

178428 7260 746 BD+16 3752 G5V (SB1) - - - 0.154 3, 6

33802 B BD-12 1095B G5Ve - - - - 3

149414 629.2A BD-03 3968 G5V (SB1) -1.14 - - - 3, 5, 6

20630 996 137 G5V MK 0.133 9.24 3.9 0.366 2 *

31966 182.1 BD+14 804 G5V - - - - 4

108754 469.1 BD-02 3528 G7V (SB1) - - - - 3, 5

131156 A 5544 A 566A G8V MK -0.151 6.31 3.2 0.461 5 *

44867 2302 BD+16 1135 G8IV (G9III) - - - - 4

195987 793.1 BD+41 3799 G9V (SB1) - - - - 3

10780 511 75 BD+63 238 K0V 0.36 - 0.6 0.280 4

185144 7462 764 K0V MK -0.045 - 0.6 0.215 1 *

18972 BD+13 494 K0IV - - - - 4

48432 2477 13 Lyn K0III - - < 19 0.120 2

9546 59.3 ADS 1233 A K1V - - - - 4

10476 493 68 107 Psc K1V MK -0.123 35.2 0. 0.198 2 *

76291 3545 BD+46 1459 K1IV - - - - 2

6027 50.1 BD+58 155 K2V (K3III) - - - - 4

101177 B 4486 B 433.2 B ADS 8250 A K2V (SB) - - - 0.144 3, 6

38392 1982 216B K2V 0.02 - - - 3

136713 1191 BD-10 4088 K2V - - - - 3

223778 9038 909 A BD+74 1047 K3V - - - - 1

219134 8832 892 BD+56 2966 K3V MK -9.000 - - 0.230 2 *

16160 A 753 105A BD+06 398 K3V MK -0.297 48.0 - 0.226 4 *

98800 2084A ADS 8141 A K4V - - - - 3, 5

131156 B 5544 B 566B K4V 0.19 12.28 20 1.381 5 *

12208 83.3 V598 Cas K5V - - - - 4

154363 653 BD-04 4225 K5V - - - - 3

201091 8085 820 A 61 Cyg A K5V MK -0.06 35.37 0.6 0.658 2, 6 *

201092 8086 820 B 61 Cyg B K7V MK -0.10 37.84 1.4 0.986 2, 6 *

52 BD +63 137 K7V - - - - 4

157881 673 BD+02 3312 K7V 0.40 - 3.9 1.464 1

88230 380 BD+50 1725 K7V(1) (K6V MK) MK 0.28 - 3.1 1.617 3

151877 639 BD+37 2804 K7V - - - 0.197 3

151288 638 BD+33 2777 K7.5Ve MK - - - 1.380 3, 6

 

HD HR GJ Name MK [Fe/H] v sini S Obs. Pap. I

(dex) (days) (km s^-1)

16 M0V - - - - 1

79210 338A ADS 7251 A M0Ve (1) - - - 2.113 3 *

572 BD+45 2247 M0V - - - - 3, 5

232979 172 BD+52 857 M0.5V MK - - - 1.909 4

1326 A 15A GX And M1.5V (1) (M2V MK) MK - - - - 4

36395 205 BD-03 1123 M1.5V (1) MK 0.60 - - - 4

95735 411 BD+36 2147 M2V MK -0.20 - - 0.424 3

623AB LHS 417 M2.5V (1) - - - - 3, 5, 6

813 LHS 3605 M3V - - - - 1

173739 A 725A ADS 11632 A M3V (1) - - - 0.534 3, 5

180617 752A LHS 473 M3 V (1) MK - - - 1.252 6

273 BD+05 1668 M3.5V (1) - - - - 3

16160 B 105B BD+06 398 B M3.5V (1) (3) - - - - 1

699 Barnard's star M4V (1) - - - - 3

13124 748 Wolf 1062 M4V (M3.5V (4)) - - - - 3, 5, 6

447 FI Vir, LHS 315 M4V (1) (3) - - - - 6

12025 U Per M4III (M6e) - - - - 4

234AB LHS 1849/50 M4.5V (1) e - - < 10 - 3, 5

831AB LHS 511 M4.5V (1) e - - < 10 - 6

473AB FL Vir, LHS 333 M5.5V (1) e - - - - 3, 5, 6

1245A V1581 Cyg M5.5V e - - - - 6

1245B LHS 3495 M5.5V e - - - - 6

406 LHS 36 M6V (1) e - - < 3 - 3 *

1111 DX Cnc, LHS 248 M6.5V - - 11 - 3, 5 *

644C VB 8, LHS 429 M7V (2) - 0.14 8 - 3, 5, 6

752B VB 10, V1298 Aql M8V (1) e - - < 5 - 6

(1): Henry et al. (1994)

(2): Kirkpatrick et al. (1995)

(3): "Zero H star", Byrne (1993)

(4): Kirkpatrick et al. (1991)

MK: "A List of MK Standard Stars", Garcıa (1989)

SB: Spectroscopic Binary (Duquennoy & Mayor 1991; Mazeh et al. 1997).

Table 6 (click here) presents information about the observed stars. In this table we give the HD, HR and GJ numbers, name, spectral type and luminosity class , from the Bright Star Catalogue (Hoffleit & Jaschek 1982; Hoffleit & Warren 1991) and the Catalogue of Nearby Stars (Gliese & Jahreiss 1991), except for some M dwarfs for which we list the more recent spectral type determination given by Henry et al. (1994) and Kirkpatrick et al. (1995). In Col. (6) MK indicates if the star is included in the list of Morgan and Keenan (MK) Standard Stars compiled by García (1989). Column (7) give the metallicity [Fe/H] from Taylor (1994; 1995) or Cayrel de Strobel (1992; 1997) and Col. (8) rotational period and v sini from Donahue (1993); Baliunas et al. (1995); Strassmeier & Fekel (1990); Fekel (1997); Stauffer & Hartmann (1986); Martın et al. (1996), and Basri & Marcy (1995; 1996). We also give, in Col. (9), the Ca II H & K spectrophometric index S from Baliunas et al. (1995) and Duncan et al. (1991). In
Col. (10) we list information about the observing run in which each star have been observed, using a code given in the first column of Table 1 (click here), and the last column indicate if the star was also included in Paper I.

In Fig. 1 (click here) we have plotted for a K1V star representative spectral orders, with the line identification marked. The two first orders (H and Mg I b lines) correspond to the K1V star HD 10476 from the Dec-93 observing run and the following orders correspond to K1V star HD 9546 from the the Nov.-94 run.

 
Figure 1: Representative spectral orders for the Dec.-93 and Nov.-94 observing runs of a K1V star, with the line identification marked (published only electronically at CDS)  

Representative spectra (from F to M stars) in different spectral regions are plotted in Figs. 2 (click here) to 6 (click here) in order to show the behaviour of the more remarkable spectroscopic features with the spectral type. In order of increasing wavelength we have plotted the following line regions: H (Fig. 2 (click here)), Mg I b triplet (Fig. 3 (click here)) Na I D₁, D₂ (Fig. 4 (click here)) and He I D₃) (Fig. 4 (click here)), H (Fig. 5 (click here)),and Ca II IRT 8498, 8542, 8662 (Fig. 6 (click here)).

 
Figure 2: Spectra in the H line region  

 
Figure 3: Spectra in the Mg I b triplet lines region  

 
Figure 4: Spectra in the Na I D₁, D₂ and He I D₃ lines region  

 
Figure 5: Spectra in the H line region  

 
Figure 6: Spectra in the Ca II IRT 8498, 8542, 8662 lines region  

In the following, we describe the behaviour of some interesting spectral lines and molecular bands present in the spectral range covered by the spectra (from 4800 to 10600 ). We list the spectroscopic features in order of increasing wavelength, and the echelle order in which they appear in each observing run can be found in Tables 2 (click here) to 5 (click here).

• The H 4861.3 line (Fig. 2 (click here)) is a well know chromospherically activity indicator (emission or filled-in).
• The Mg I b triplet 5167, 5172, 5183 (Fig. 3 (click here)) is luminosity sensitive in the range G8-K5. These strong neutral metal lines are formed in the lower chromosphere and the region of temperature minimum and they are good diagnostics of activity (Basri et al. 1989;
  Gunn & Doyle 1997; Gunn et al. 1997; Montes et al. 1998b).
• The He I D₃ 5876 absorption line is another important indicator of stellar activity in the upper chromosphere (Garcıa López et al. 1993; Montes et al. 1997b, 1998a; Saar et al. 1997) and also could be in emission during stellar flares (Huenemoerder & Ramsey 1987; Montes et al. 1996b, 1997b, 1998b).
• The Na I D₁ 5895.92 and D₂ 5889.95 lines (Fig. 4 (click here)) are well known temperature and luminosity discriminant. These resonance lines are collisionally-controlled in the atmospheres of late-type stars and then provide information about chromospheric activity see Montes et al. (1996b, 1997b, 1998a) and the recent models of these lines for M dwarfs stars by Andretta et al. (1997).
• The wings of the Ca I triplet 6102, 6122, 6162 lines can be used as luminosity indicators (Cayrel et al. 1996). These lines are very weak at spectral type F and increase in strength with decreasing temperature.
• The V I 6251.83 and Fe I 6252.57 line-depth ratio can be used to determine stellar temperatures (Gray & Johanson 1991; Gray 1994).
• The line ratio Fe II 6432.65/Fe I 6430.85 is useful for spectral-class/temperature classification for F to M stars. Other spectral class indicators are the ratios of V I 6452/Ca I 6456 (for F, and G stars), Co I 6455/Ca I 6456 and Fe II 6457/Ca I 6456 (for F to K stars) (Strassmeier & Fekel 1990).
• The Fe I 6411.66 , Fe I 6430.85 , and Ca I 6439.08  lines normally used for the application of the Doppler imaging technique.
• The emission or filled-in of the Å ) (Fig. 5 (click here)) line is one the primary optical indicators of chromospheric activity in late-type stars, together with the Ca II H & K emission lines.
• The Li I resonance line at 6707.8  and the subordinate lines at 6103  and Å (Pavlenko et al. 1995; Carlsson et al. 1994).
• The K I 7664.91, 7698.98 doublet is a resonance transition and thus will be influenced by chromospheric activity, particularly in M dwarf stars (see Basri & Marcy 1995; Schweitzer et al. 1996).
• The Rb I resonance line at 7947.63  is strong in very late-type stars, and it seems to be a good temperature diagnostic (Basri & Marcy 1995).
• The Na I doublet 8183.26, 8194.8 lines are subordinate transitions and therefore, form mainly in the photosphere and should not be significantly affected by the chromosphere. These lines can be used as a dwarf/giant indicator (Schiavon et al. 1997).
• The Ti I lines for multiplet 33 (specially the 8382.54, 8382.82 lines) and other Ti I lines. can be used as a luminosity classification criterium because they present a positive luminosity effect (Keenan & Hynek 1945; Ginestet et al. 1994; Jashek & Jashek 1995; Montes et al. 1998a).
• The Ca II infrared triplet (IRT) 8498, 8542, and 8662 lines (Fig. 6 (click here)) formed in the lower chromosphere and are also important activity indicators (Linsky et al. 1979; Foing et al. 1989; Dempsey et al. 1993; Montes et al. 1998a). These lines have been also used by several authors as a gravity sensitive index. In this spectral region the Paschen lines P12 (8750) and P14 (8598) are also visible in F stars (Carquillat et al. 1997).
• From mid K through M stars we can also see a number of titanium oxide (TiO) molecular bands such as (5847-6058), (6080-6390), (6322-6512), (6569-6649), (6651-6852), (7053-7270), (76667861), (8206-8569), (8432-8452), and (8859-8937), useful in classifying early M dwarfs, and a number of vanadium oxide (VO) bands such as (7400-7510), (7851-7973), and (8521-8668), useful in classifying late M dwarfs. CaH bands at (6346, 6382, 6389) and (6750-7050) are also present in these stars.
• Other strong features that appear in the spectra are the telluric O₂ A and B bands at 6867  7600  and several telluric H₂O bands at (7186-7273), (8164-8177), 8227, 8282, (8952-8972), and (8980-8992).

A more detailed description of the H, H, Na I D₁, D₂ and He I D₃ lines and the corresponding photospheric features included in these spectral regions, can be found in Paper I. An extensive list of features identifiable in late-K to late-M spectra from 6300 to 9000  can be found in Kirkpatrick et al. (1991). A description of the spectroscopic characteristics of very cool dwarfs and substellar candidates is given by Martın et al. (1996). For more information about spectral classification of stars and the behaviour of chemical elements in stars the reader is referred to Jaschek & Jaschek (1990; 1995).

In order to enable other investigators to make use of the spectra of this library, all the multidimensional spectra containing all the echelle orders of the stars listed in Table 6 (click here) are available as FITS format files at the CDS in Strasbourg, France, via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5). They are also available via the World Wide Web at:
http://www.ucm.es/OTROS/Astrof/fgkmsl/UESfgkmsl.html.

In order to facilitate the use of this library the onedimensional normalized and wavelength-shifted spectra, resulting for the extraction of the orders containing the more remarkable spectroscopic features (the spectral regions plotted in Figs. 2 (click here) to 6 (click here)), are also available as separate FITS format files.

The extension of this library including stars of higher luminosity class, as well as the use of these spectra to analyse temperature sensitive lines in order to improve the actual line-depth ratio temperature calibrations (Gray & Johanson 1991; Gray 1994) and spectral-class/temperature classifications (Strassmeier & Fekel 1990), will be the subject of forthcoming papers.

Acknowledgements

We thank J. Sanz-Forcada for help in the reduction of some of the echelle spectra. This research has made use the La Palma Archive and of the SIMBAD data base, operated at CDS, Strasbourg, France. This work has been supported by the Universidad Complutense de Madrid and the Spanish Dirección General de Investigación Cientıfica y Técnica (DGICYT) under grants PB94-0263 and PB95-1132-C02-01.