A High-Resolution Stellar Library for Evolutionary Population Synthesis.
(copy of paper accepted by MNRAS: PDF  2.4MB, DVI 100KB)

Lucimara P. Martins,  martins@stsci.edu, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 
Rosa M. González Delgado,  rosa@iaa.es, Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain 
Claus Leitherer,  leitherer@stsci.edu, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 
Miguel Cerviño,  mcs@iaa.es, Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain 
Peter H. Hauschildt,  yeti@hs.uni-hamburg.de, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany

Abstract

We present a library of 1654 high-resolution stellar spectra, with a sampling of 0.3 Å and covering the wavelength range from 3000 Å to 7000 Å. The library was computed with the latest improvements in stellar atmospheres, incorporating non-LTE line-blanketed models for hot, massive (Teff >= 27500 K) and line-blanketed models for cool (3000 K <= Teff <= 4500 K) stars. The total coverage of the grid is 3000 K <= Teff <= 55000 K and –0.5 <= log g <= 5.5, for four chemical abundance values: twice solar, solar, half solar and 1/10 solar. Evolutionary synthesis models using this library are presented in a companion paper. We tested the general behavior of the library by calculating and comparing equivalent widths of numerous H and HeI lines, and some of the commonly used metallic indices. We also compared the library with the empirical libraries STELIB and Indo-US. The full set of the synthetic stellar spectra is available here for retrieval, or on request from authors.


Evolutionary Stellar Population Synthesis at High Spectral Resolution: Optical Wavelengths.   
(copy of paper accepted by MNRAS: PDF  3.8MB, DVI 96 KB)
 
Rosa M. González Delgado,  rosa@iaa.es, Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain 
Miguel Cerviño,  mcs@iaa.es, Instituto de Astrofísica de Andalucía (CSIC), Apdo. 3004, 18080 Granada, Spain 
Lucimara P. Martins,  martins@stsci.edu, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 
Claus Leitherer,  leitherer@stsci.edu, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA 
Peter H. Hauschildt,  yeti@hs.uni-hamburg.de, Hamburger Sternwarte, Gojenbergsweg 112, 21029 Hamburg, Germany

Abstract

We present the single stellar population (SSP) synthesis results of our new synthetic stellar atmosphere models library with a spectral sampling of 0.3 Å, covering the wavelength range from 3000 Å to 7000Å for a wide range of metallicities (twice solar, solar, half and 1/10 solar).  The stellar library is composed of 1650 spectra computed with the latest improvements in stellar atmospheres. In particular it incorporates non-LTE line-blanketed models for hot (Teff >= 27500 K) and LTE line-blanketed models (Phoenix) for cool (3000 K <= Teff <= 4500 K) stars. Because of the high spectral resolution of this library, evolutionary synthesis models can be used to predict the strength of numerous weak absorption lines, and the evolution of the profiles of the strongest lines over a wide range of ages. The SSP results have been calculated for ages 1 Myr to 17 Gyr using the stellar evolutionary provided by the Geneva and Padova-tracks groups. For young stellar populations, our results have a very detailed coverage of high-temperature stars with similar results for Padova and Geneva isochrones. For intermediate and old stellar populations, our results, once degraded to a lower resolution, are similar to the ones obtained by other groups apart from limitations imposed by the stellar evolutionary physics. The limitations and advantages of our library for the analysis of integrated populations are described. The full set of the stellar library and the evolutionary models are available here for retrieval or on request from authors.


Stellar library

References that must be quoted:
High Resolution library from \cite{Martetal04,GDetal04} based on atmosphere models from PHOENIX \cite{HB99,Aetal01}, ATLAS9 \cite{K91} computed with SPECTRUM \cite{GC94}, ATLAS9 library computed with SYNSPEC \cite{HLJ95}, and TLUSTY \cite{LH03}.

\bibitem[Allar et al.(2001)]{Aetal01} Allard, F., Hauschildt, P.H., Alexander, D.R., Tamanai, A., \& Schweitzer, A. 2001, ApJ, 556, 357
\bibitem[Gonz\'alez Delgado et al.~(2004)]{GDetal04} Gonz\'alez Delgado, R., Cervi\~no, M., Martins, L.P., Leitherer, C., Hauschildt, P.H. 2004, MNRAS (accepted; please check ADS)
\bibitem[Gray \& Corbally(1994)]{GC94} Gray, R.O., Corbally, C.J. 1994, AJ, 107, 742 {\tt http://www1.appstate.edu/dept/physics/spectrum/spectrum.html}
\bibitem[Hauschildt \& Baron(1999)]{HB99} Hauschildt, P.H., \& Baron, E. 1999, Journal of Computational and Applied Mathematics, 102, 41
\bibitem[Kurucz(1991)]{K91} Kurucz, R.L. 1991, in {\it Stellar Atmospheres, Beyond Classical Limits}, Crivellari L., Hubeny I., Hummer D.G. eds., Kluwer, Dordrecht, p. 441 (ATLAS9) {\tt http//kurucz.harvard.edu/}
\bibitem[Lanz \& Hubeny(2003)]{LH03} Lanz, T., \& Hubeny, I. 2003, ApJ, 146, 417 {\tt http://tlusty.gsfc.nasa.gov/}
\bibitem[Martins et al.~(2004)]{Martetal04} Martins, L.P. et al. 2004 (accepted; please check ADS)


The Stellar library:
Note:The library is in the following units: erg/s/Å/cm2; it must be multiplied by 4 pi R([cm])2 to obtain the Luminosity [erg/s/Å]. Wavelengths are in the air reference system.
Z
 [Fe/H]
 file (gzipped ~13 Mb each)
download
full set
(gzipped tar file)  
  52.4 Mb
0.002
 -10
 HRESm10.vis
0.005/0.010
 -5 & -3
 HRESm05.vis
0.020
 0
 HRESp00.vis
0.040
 +3
 HRESp03.vis


Measured line indices1:

index
 view html  (by metallicity)
download
full set
 
  172kB
Balmer
 0.002   -  0.005/0.010   -  0.020   -  0.040
Rose
 0.002   -  0.010/0.005   -  0.020   -  0.040
Bica
 0.002   -  0.010/0.005   -  0.020   -  0.040





Synthesis results

References that must be quoted:
Model generated with Sed@.0 code\footnote{Sed@ is a synthesis code included in the {\it Legacy Tool project} of the {\it Violent Star Formation Network}; see {\it Sed@ Reference Manual} at {\tt http://www.iaa.es/$\sim$mcs/sed@} for more information} with the following inputs: IMF from \cite{Salpeter55} in the mass range 0.1-120 $M_\odot$; High Resolution library from \cite{Martetal04,GDetal04} based on atmosphere models from PHOENIX \cite{HB99,Aetal01}, ATLAS9 \cite{K91} computed with SPECTRUM \cite{GC94}, ATLAS9 library computed with SYNSPEC \cite{HLJ95}, and TLUSTY \cite{LH03}
Geneva: Isochrones computed with the isochrone program presented in \cite{Mey95} and following the prescriptions quoted in \cite{Cetal01} from the evolutionary tracks from

\cite{Schetal92} at Z=0.001/Z=0.020

\cite{Charetal93} at Z=0.004

\cite{Schetal93} at Z=0.008

\cite{Schetal93b} at Z=0.040
Padova: Isochrones presented in \cite{Gietal02}\footnote{Available at {\tt http://pleiadi.pd.astro.it/}} based on the (solar scaled mixture) tracks from \cite{Gi00,Be94} that includes overshooting and a simple synthetic evolution of TP-AGB \cite{GB98} . :
\bibitem[Allar et al.(2001)]{Aetal01} Allard, F., Hauschildt, P.H., Alexander, D.R., Tamanai, A., \& Schweitzer, A. 2001, ApJ, 556, 357
\bibitem[Bertelli et al.(1994)]{Be94} Bertelli, G., Bressan, A., Chiosi, C., Fagotto, F., \& Nasi, E.\ 1994, \aaps, 106, 275
\bibitem[Cervi{\~ n}o et al.(2001)]{Cetal01} Cervi{\~ n}o, M., G{\' o}mez-Flechoso, M.~A., Castander, F.~J., et al.\ 2001 \aap, 376, 422
\bibitem[Charbonnel et al.(1993)]{Charetal93} Charbonnel, C., Meynet, G., Maeder, A., Schaller, G., \& Schaerer, D.\ 1993, \aaps, 101, 415
\bibitem[Girardi \& Bertelli(1998)]{GB98} Girardi, L., \& Bertelli, G.\ 1998, \mnras, 300, 533
\bibitem[Girardi et al.(2002)]{Gietal02} Girardi, L., Bertelli, G., Bressan, A., Chiosi, C., Groenewegen, M.~A.~T., Marigo, P., Salasnich, B., \& Weiss, A.\ 2002, \aap, 391, 195
\bibitem[Girardi, Bressan, Bertelli, \& Chiosi(2000)]{Gi00} Girardi , L., Bressan, A., Bertelli, G., \& Chiosi, C.\ 2000, \aaps, 141, 371
\bibitem[Gonz\'alez Delgado et al.~(2004)]{GDetal04} Gonz\'alez Delgado, R., Cervi\~no, M., Martins, L.P., Leitherer, C., Hauschildt,P.H. 2004, MNRAS (accepted; please check ADS)
\bibitem[Gray \& Corbally(1994)]{GC94} Gray, R.O., Corbally, C.J. 1994, AJ, 107, 742 {\tt http://www1.appstate.edu/dept/physics/spectrum/spectrum.html}
\bibitem[Hauschildt \& Baron(1999)]{HB99}Hauschildt, P.H., \& Baron, E. 1999, Journal of Computational and Applied Mathematics, 102, 41
\bibitem[Kurucz(1991)]{K91} Kurucz, R.L. 1991, in {\it Stellar Atmospheres, Beyond Clasical Limits},Crivellari L., Hubeny I., Hummer D.G. eds.,Klu wer, Dordrecht, p. 441 (ATLAS9) {\tt http//kurucz.harvard.edu/}
\bibitem[Lanz \& Hubeny(2003)]{LH03} Lanz, T., \& Hubeny, I. 2003, ApJ, 146, 417 {\tt http://tlusty.gsfc.nasa.gov/}
\bibitem[Martins et al.~(2004)]{Martetal04} Martins, L.P. et al. 2004 (accepted; please check ADS)
\bibitem[Meynet(1995)]{Mey95} Meynet, G. 1995, A\&A 298, 767
\bibitem[Salpeter~(1955)]{Salpeter55} Salpeter, E. E. 1955, \apj, ~121, 161
\bibitem[Schaerer et al.(1993a)]{Schetal93} Schaerer, D., Charbonnel, C., Meynet, G., Maeder, A., \& Schaller, G.\ 1993a, \aaps, 102, 339
\bibitem[Schaerer et al.(1993b)]{Schetal93b} Schaerer, D., Meynet, G., Maeder, A., \& Schaller, G.\ 1993b, \aaps, 98, 523
\bibitem[Schaller et al.(1992)]{Schetal92} Schaller, G., Schaerer, D., Meynet, G. \& Maeder, A.\ 1992,\aaps, 96, 269
Full output from SED@:
one file for each metallicity, which contains a header and the following columns: (wavelength, Li1 Li2 Li3, ...), where Li1 is the luminosity in (erg/s/Å/Msun), Li2 is the effective number of stars (Neff/Mo quoted in Buzzoni 1989 and Cerviño et al. 2002), and Li3 is the Lowest Luminosity Limit, Lmin[erg/s/Å] for the use of synthesis models at the given wavelength (Cerviño & Luridiana 2004). The three luminosity values are sequentially written for all 'i' ages, one line per wavelength. Information about references, etc., in the header of the files.
\bibitem[Buzzoni~(1989)]{Buzz89]Buzzoni, A. 1989, \apjs, 71, 817
\bibitem[Cervi{\~ n}o et al.~(2002)]{CVGLMH02} Cervi{\~n}o, M., Valls-Gabaud, D., Luridiana, V., \& Mas-Hesse, J.~M.\ 2002, \aap, 381, 51
\bibitem[Cervi{\~ n}o \& Luridiana(2004)]{CL04} Cervi{\~n}o, M.,~\& Luridiana, V.\ 2004, \aap, 413, 145
Geneva models are computed at these ages, in million years:
1,2,3,4,5,6,7,8,9,10,15,20,25,30,35,40,45,50,55,60,65,70,75,80,85,90,95,100,200,300,400,500,600,700,800,900,1000,2000,3000,4000,5000,6000,7000,8000,9000,10000.

Padova models are computed at these ages, in million years:
3.981, 4.467, 5.012, 5.623, 6.310, 7.079, 7.943, 8.913, 10.00, 11.22, 12.59, 14.13, 15.85, 17.78, 19.95, 22.39, 25.12, 28.18, 31.62, 35.48, 39.81, 44.67, 50.12, 56.23, 63.10, 70.80, 79.43, 89.13, 100.0, 112.2, 125.9, 141.3, 158.5, 177.8, 199.5, 223.9, 251.2, 281.8, 316.2, 354.8, 398.1, 446.7, 501.2, 562.4, 631.0, 708.0, 794.3, 891.3, 1000., 1122., 1259., 1413., 1585., 1778., 1995., 2239., 2512., 2818., 3162., 3548., 3981., 4467., 5012., 5624., 6310., 7080., 7944., 8913., 10000., 11220., 12590., 14130, 15850, 17780.
Note 1: The atmosphere model asignation during WR phases in Geneva isochrones has been performed using the T* values in the isochrone, instead Teff values. This produces some diferences with respect to the results of other isochrones at the corresponding ages.
Note 2: Wavelengths are quoted in air (not in vacuum), note that some surveys, like SLOAN, are calibrated in vacuum wavelengths.

Geneva
 by metallicity:    0.001 0.004 0.008 0.020 0.040 (gzipped files, ~6.5 MB each)
full set  (gzipped tar file, 32.7 MB, contains the above five files)

Padova
 by metallicity:    0.004 0.008 0.019 (gzipped files, 10.8 MB each)
full set  (gzipped tar file, 29.5 MB, contains the above three files)

 
Measured line indices1:

index
view html  (by metallicity)



download
full set

31 kB

Balmer
 Geneva
 0.001 - 0.004 - 0.008 - 0.020 - 0.040
Padova
 0.004 - 0.008 - 0.019

Rose
 Geneva
 0.001 - 0.004 - 0.008 - 0.020 - 0.040
Padova
  0.004 - 0.008 - 0.019

Balogh
 Geneva
 0.001 - 0.004 - 0.008 - 0.020 - 0.040
Padova
 0.004 - 0.008 - 0.019
 

Index definitions:
Balmer
Line BD(Rose) HeI4026 Hdelta(1) Hdelta(2) Hdelta(3) Hgamma(1) Hgamma(2) Hgamma(3) HeI4471 HeII4686 Hbeta(1) Hbeta(2) Hbeta(3) HeI5876 Halpha(1) Halpha(2)
Type ratio EW EW EW EW EW EW EW EW EW EW EW EW EW EW EW
Line window
4020-4031 4092-4112 4087-4117 4070-4130 4330-4350 4325-4355 4310-4370 4464-4478 4681-4691 4852-4872 4847-4877 4832-4892 5871-5880 6553-6573 6548-6578
Continuum window (blue) 3525-3600 4012-4020 4262-4270 4445-4453 4665-4675 4770-4782 5835-5845 6506-6514
Continuum window (red) 3700-3825 4158-4169 4445-4453 4493-4503 4725-4735 4942-4954 5904-5912 6612-6620



Balogh
Index D4000 (Balogh) Hdelta
Type I EW
Line window
4082-4122
Continuum window (blue) 3850-4000 4082-4101
Continuum window (red) 4000-4100 4122-4170


Bica
Index C4020/C3660 (Bica) C3816 B-H9 H8 CaIIK CaIIH+He Hdelta Banda G Hgamma Hbeta Mg II
Type I EW EW EW EW EW EW EW EW EW EW
Line window
3810-3822 3822-3860 3860-3908 3908-3952 3952-3988 4082-4124 4284-4318 4318-4364 4846-4884 5156-5196
Continuum window (blue) 3650-3670 3778-3789 3775-3785 4012-4023 4609-4627
Continuum window (red) 4000-4020 4009-4020 4512-4523 5307-5317


Rose
Index BD(Rose) CaII+He(3968.6o3969.8)/CaIIK(3933.5) Hdelta(4101.7)/FeI(4045.6) D4000(Balogh) Hdelta Hdelta(WO97) CaIIK
Type I M M I E E E
Line window



4082-4122 4083.5-4122.25 3908-3952
Continuum window (blue) 3525-3600 3932.9-3934.9 4045.1-4046.1 3850-3950 4030-4082 4041.6-4079.75 3775-3785
Continuum window (red) 3700-3825 3967.9-3970.9 4101.2-4102.2 4000-4100 4122-4170 4128.5-4161 4009-4020



\bibitem[Balogh et al.~(1999)]{Betal99}Balogh, M.L., Morris, S.L., Yee, H.K.C., Carlberg, R.G., \& Ellingson, E. 1999 \apj, 527, 54
\bibitem[Bica \& Aloin~(1986)]{BA86}Bica, E., \& Alloin, D. 1986, \aap, 166, 83
\bibitem[Rose~(1984)]{Rose84}Rose, J.A. 1984, \aj, 89, 1238
\bibitem[Rose~(1984)]{Rose84}Rose, J.A. 1985, \aj, 90, 1927