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J/MNRAS/404/1639    MILES base models & new line index system  (Vazdekis+, 2010)

Evolutionary stellar population synthesis with MILES. I. The base models and a new line index system. Vazdekis A., Sanchez-Blazquez P., Falcon-Barroso J., Cenarro A.J., Beasley M.A., Cardiel N., Gorgas J., Peletier R.F. <Mon. Not. R. Astron. Soc., 404, 1639-1671 (2010)> =2010MNRAS.404.1639V
ADC_Keywords: Models ; Spectroscopy ; Energy distributions ; Clusters, globular ; Galaxies, spectra Keywords: globular clusters: general - galaxies: abundances - galaxies: elliptical and lenticular, cD - galaxies: stellar content Abstract: We present synthetic spectral energy distributions (SEDs) for single-age, single-metallicity stellar populations (SSPs) covering the full optical spectral range at moderately high resolution [full width at half-maximum (FWHM)=2.3Å]. These SEDs constitute our base models, as they combine scaled-solar isochrones with an empirical stellar spectral library [Medium resolution INT Library of Empirical Spectra (MILES)], which follows the chemical evolution pattern of the solar neighbourhood. The models rely as much as possible on empirical ingredients, not just on the stellar spectra, but also on extensive photometric libraries, which are used to determine the transformations from the theoretical parameters of the isochrones to observational quantities. The unprecedented stellar parameter coverage of the MILES stellar library allowed us to safely extend our optical SSP SED predictions from intermediate- to very-old-age regimes and the metallicity coverage of the SSPs from super-solar to [M/H]=-2.3. SSPs with such low metallicities are particularly useful for globular cluster studies. We have computed SSP SEDs for a suite of initial mass function shapes and slopes. We provide a quantitative analysis of the dependence of the synthesized SSP SEDs on the (in)complete coverage of the stellar parameter space in the input library that not only shows that our models are of higher quality than those of other works, but also in which range of SSP parameters our models are reliable. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 377 489 Lick indices measured in the Line Index System (LIS) for glubulars and galaxies from selected references
See also: J/MNRAS/371/703 : MILES library of empirical spectra (Sanchez-Blazquez+, 2006) J/MNRAS/374/664 : Stellar atmospheric param. in MILES library (Cenarro+, 2007) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1 A1 --- Ref [A-J] Reference code (1) 3- 14 A12 --- Name Globular cluster or galaxy name 16- 22 F7.4 0.1nm HdA ?=- HdA line-strength index 24- 30 F7.4 0.1nm HdF ?=- HdF line-strength index 32- 38 F7.4 mag CN1 ?=- CN1 line-strength index 40- 46 F7.4 mag CN2 ?=- CN2 line-strength index 48- 53 F6.4 0.1nm Ca4227 ?=- Ca4227 line-strength index 55- 60 F6.4 0.1nm G4300 ?=- G4300 line-strength index 62- 68 F7.4 0.1nm HgA ?=- HgA line-strength index 70- 76 F7.4 0.1nm HgF ?=- HgF line-strength index 78- 83 F6.4 0.1nm Fe4383 ?=- Fe4383 line-strength index 85- 90 F6.4 0.1nm Ca4455 ?=- Ca4455 line-strength index 92- 97 F6.4 0.1nm Fe4531 ?=- Fe4531 line-strength index 99-105 F7.4 0.1nm C4668 ?=- C4668 line-strength index 107-112 F6.4 0.1nm Hb ?=- Hb line-strength index 114-119 F6.4 0.1nm Fe5015 ?=- Fe5015 line-strength index 121-127 F7.4 mag Mg1 ?=- Mg1 line-strength index 129-134 F6.4 mag Mg2 ?=- Mg2 line-strength index 136-141 F6.4 0.1nm Mgb ?=- Mgb line-strength index 143-148 F6.4 0.1nm Fe5270 ?=- Fe5270 line-strength index 150-155 F6.4 0.1nm Fe5335 ?=- Fe5335 line-strength index 157-162 F6.4 0.1nm Fe5406 ?=- Fe5406 line-strength index 164-170 F7.4 0.1nm Fe5709 ?=- Fe5709 line-strength index 172-178 F7.4 0.1nm Fe5782 ?=- Fe5782 line-strength index 180-186 F7.4 0.1nm NaD ?=- NaD line-strength index 188-194 F7.4 mag TiO1 ?=- TiO1 line-strength index 196-202 F7.4 mag TiO2 ?=- TiO2 line-strength index 204-209 F6.4 0.1nm e_HdA ?=- Error on HdA 211-216 F6.4 0.1nm e_HdF ?=- Error on HdF 218-223 F6.4 mag e_CN1 ?=- Error on CN1 225-230 F6.4 mag e_CN2 ?=- Error on CN2 232-237 F6.4 0.1nm e_Ca4227 ?=- Error on Ca4227 239-244 F6.4 0.1nm e_G4300 ?=- Error on G4300 246-251 F6.4 0.1nm e_HgA ?=- Error on HgA 253-258 F6.4 0.1nm e_HgF ?=- Error on HgF 260-265 F6.4 0.1nm e_Fe4383 ?=- Error on Fe4383 267-272 F6.4 0.1nm e_Ca4455 ?=- Error on Ca4455 274-279 F6.4 0.1nm e_Fe4531 ?=- Error on Fe4531 281-286 F6.4 0.1nm e_C4668 ?=- Error on C4668 288-293 F6.4 0.1nm e_Hb ?=- Error on Hb 295-300 F6.4 0.1nm e_Fe5015 ?=- Error on Fe5015 302-307 F6.4 mag e_Mg1 ?=- Error on Mg1 309-314 F6.4 mag e_Mg2 ?=- Error on Mg2 316-321 F6.4 0.1nm e_Mgb ?=- Error on Mgb 323-328 F6.4 0.1nm e_Fe5270 ?=- Error on Fe5270 330-335 F6.4 0.1nm e_Fe5335 ?=- Error on Fe5335 337-342 F6.4 0.1nm e_Fe5406 ?=- Error on Fe5406 344-349 F6.4 0.1nm e_Fe5709 ?=- Error on Fe5709 351-356 F6.4 0.1nm e_Fe5782 ?=- Error on Fe5782 358-363 F6.4 0.1nm e_NaD ?=- Error on NaD 365-370 F6.4 mag e_TiO1 ?=- Error on TiO1 372-377 F6.4 mag e_TiO2 ?=- Error on TiO2
Note (1): References as follows: A = Puzia et al. (2002A&A...395...45P) [LIS-5.0A] B = Schiavon et al. (2005ApJS..160..163S) [LIS-5.0A] C = Trager et al. (2000AJ....119.1645T) [LIS-8.4A] D = Trager et al. (2000AJ....119.1645T) [LIS-14.0A] E = Sanchez-Blazquez et al. (2006MNRAS.371..703S) [LIS-8.4A] F = Sanchez-Blazquez et al. (2006MNRAS.371..703S) [LIS-14.0A] G = Yamada et al. (2006ApJ...637..200Y) [LIS-8.4A] H = Yamada et al. (2006ApJ...637..200Y) [LIS-14.0A] I = Kuntschner et al. (2006MNRAS.369..497K) [LIS-8.4A] J = Kuntschner et al. (2006MNRAS.369..497K) [LIS-14.0A] [LIS refers to the new line index system, i.e., LIS-5.0A for globular cluster, LIS-8.4A for dwarf and intermediate-mass galaxies, LIS-14.0A for massive galaxies. See paper for definitions, tables A1-A3]
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 08-Nov-2010
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