SED@ Evolutionary Synthesis Models

Observable			Reference paper
Continuum and nebular emission lines	Stellar populations	Contribution to the continuum	(1)
X-ray emission and kinetic energy	Nebular emission lines with X-rays	Complete SED (X-ray to NIR)	(2)
Effective rate of ionizing photons (mean, dispersion, LLL and correlation matrix)			(3)
Ref 1: Cerviño, M., Valls-Gabaud, D., Luridiana, V. & Mas-Hesse, J.M., 2002, A&A 381, 51 Ref 2: Cerviño, Mas-Hesse and Kunth, 2002, A&A, 392, 19 Ref 3: Cerviño, Luridiana, Pérez, Vílchez and Valls-Gabaud, 2003, A&A, (accepted A&A, astro-ph/0304062)

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What observable do you want to see?
(it will appear in companion window for all the metallicities)

Important Note:

• the models presented here assumes NO extinction,
• only a fraction of 0.7 of the ionizing flux produces the nebular emission lines.

 
• Continuum and nebular emission lines
  

  X-ray and kinetic energy and momentum outputs are bellow
  gamma-ray outputs are in a separate page
  

  Monocromatic luminosities (1285 - 36000 A):
  Standard Mdot 2 x Mdot L_1285 L_1362 L_1400 L_1440 L_1550 L_1635 L_1762 L_1930 L_2175 L_2450 L_3000 L_3640 L_3650 L_4400 L_4471 L_4686 L_4861 L_5500 L_5808 L_6563 L_7000 L_9000 L_12500 L_22200 L_36000 L_Bol
  Colors (only CMHK colors have the dispersion computed at this moment)
  Standard Mdot 2 x Mdot log (L(1285)/L(1930)) log (L(1400)/L(1930)) log (L(1285)/L(3000)) log (L(1930)/L(3000)) log (L(2450)/L(3000)) 130 - V 210 - V U - B U - B (CMHK) B - V B - V (CMHK) V - R V - I R - I V - J V - H V - K V - K (CMHK) V - L J - K (CMHK)
  Si IV, C IV, SN and Radio continua:
  Standard Mdot 2 x Mdot W(Si IV abs.) [A] W(Si IV em.) [A] W(C IV abs.) [A] W(C IV em.) [A] W(Si IV)/W(C IV) SNr [yr-1 Mo-1] log L_SNr (6 cm) Jy Kpc^2 log L (6cm) log L (20cm) radio index (6-20 cm)
  Ionizing fluxes and nebular emission lines Q(He++)... W(Hb)...         (see also X-ray outputs)
  Standard Mdot 2 x Mdot log Q(He+) log Q(He0) log Q(H0) log Q(Ly) log L(Hb) EW(Hb) [A] log L(Ha) EW(Ha) [A] log L(th)(6cm) log L(He I) W(He I) [A] L(He I)/L(Hb) log L(He II) W(He II) [A] L(He II)/L(Hb) log Q(H_2) B=log(NLyc /L(1400)) Teff [K]

   
• Stellar populations:

  By Luminosity Class:
  Standard Mdot 2 x Mdot Fraction by number of V Fraction by number of Blue V Fraction by number of Yellow V Fraction by number of Red V Fraction by number of III Fraction by number of Blue III Fraction by number of Yellow III Fraction by number of Red III Fraction by number of I Fraction by number of Blue I Fraction by number of Yellow I Fraction by number of Red I
  OB Stars:
  Standard Mdot 2 x Mdot Fraction by number of O3 Fraction by number of O4 Fraction by number of O5 Fraction by number of O6 Fraction by number of O7 Fraction by number of O8 Fraction by number of O9 Fraction by number of B0 Fraction by number of B1 Fraction by number of B2 Fraction by number of B3 Fraction by number of B4 Fraction by number of B5 Fraction by number of B6 Fraction by number of B7 Fraction by number of B8 Fraction by number of B9
  WR and PMS Stars:
  	WR and PMS numbers and ratios
  	Standard Mdot 2 x Mdot WR / (WR + O) WN / (WR + O) WNL / (WR + O) WNE / (WR + O) WC / (WR + O) WRb / (WR + O) WNb / (WR + O) WNLb / (WR + O) WNEb / (WR + O) WCb / (WR + O) WC/WR Total number of WR Total number of WN Total number of WNL Total number of WNE Total number of WC Total number of Of WR/(RSG+WR) Total number of O Total number of RSG Total number of PMS
  	WR emission lines
  	Standard Mdot 2 x Mdot log L (He II WR bump) EW(WR bump) [A] L(WR bump)/L(Hb) log L (C IV WCbump) EW(WC bump) [A] L(WC bump)/L(Hb) log L (He I 1640 WR) EW(He I 1640 WR) [A] L(He I 1640 WR)/L(Hb) log L (N III 4640 WR) EW(N III 4640 WR) [A] L(N III 4640 WR)/L(Hb) log L (C IV 4650 WR) EW(C IV 4650 WR) [A] L(C IV 4650 WR)/L(Hb) log L (He II 4686 WR) EW(He II 4686 WR) [A] L(He II 4686 WR)/L(Hb) log L (Hb WR) EW(Hb WR) [A] L(Hb WR)/L(Hb) log L (C III 5689 WR) EW(C III 5689 WR) [A] L(C III 5689 WR)/L(Hb) log L (C IV 5808 WR) EW(C IV 5808 WR) [A] L(C IV 5808 WR)/L(Hb) log L (Ha WR) EW(Ha WR) [A] L(Ha WR)/L(Hb) log L (He II 5411 WR) EW(He II 5411 WR) [A] L(He II 5411 WR)/L(Hb)
  	WR ionizing flux
  	Standard Mdot 2 x Mdot log Q(He+) by WR log Q(He0) by WR log Q(H0) by WR log Q(Ly) by WR log Q(He+) by WN log Q(He0) by WN log Q(H0) by WN log Q(Ly) by WN log Q(He+) by WNL log Q(He0) by WNL log Q(H0) by WNL log Q(Ly) by WNL log Q(He+) by WNE log Q(He0) by WNE log Q(H0) by WNE log Q(Ly) by WNE log Q(He+) by WC log Q(He0) by WC log Q(H0) by WC log Q(Ly) by WC log Q(H0) by OB log Q(H0) by RSG

   
• Contribution to the continuum:

  Nebular contribution:
  Standard Mdot 2 x Mdot Fraction L_1285 nebular Fraction L_1362 nebular Fraction L_1400 nebular Fraction L_1440 nebular Fraction L_1550 nebular Fraction L_1635 nebular Fraction L_1762 nebular Fraction L_1930 nebular Fraction L_2175 nebular Fraction L_2450 nebular Fraction L_3000 nebular Fraction L_3640 nebular Fraction L_3650 nebular Fraction L_4400 nebular Fraction L_4471 nebular Fraction L_4686 nebular Fraction L_4861 nebular Fraction L_5500 nebular Fraction L_5808 nebular Fraction L_6563 nebular Fraction L_7000 nebular Fraction L_9000 nebular Fraction L_12500 nebular Fraction L_22200 nebular Fraction L_36000 nebular Fraction L_bol nebular
  WR contribution:
  Standard Mdot 2 x Mdot Fraction L_1285 WR Fraction L_1362 WR Fraction L_1400 WR Fraction L_1440 WR Fraction L_1550 WR Fraction L_1635 WR Fraction L_1762 WR Fraction L_1930 WR Fraction L_2175 WR Fraction L_2450 WR Fraction L_3000 WR Fraction L_3640 WR Fraction L_3650 WR Fraction L_4400 WR Fraction L_4471 WR Fraction L_4686 WR Fraction L_4861 WR Fraction L_5500 WR Fraction L_5808 WR Fraction L_6563 WR Fraction L_7000 WR Fraction L_9000 WR Fraction L_12500 WR Fraction L_22200 WR Fraction L_36000 WR Fraction L_bol WR
  OB contribution:
  Standard Mdot 2 x Mdot Fraction L_1285 OB Fraction L_1362 OB Fraction L_1400 OB Fraction L_1440 OB Fraction L_1550 OB Fraction L_1635 OB Fraction L_1762 OB Fraction L_1930 OB Fraction L_2175 OB Fraction L_2450 OB Fraction L_3000 OB Fraction L_3640 OB Fraction L_3650 OB Fraction L_4400 OB Fraction L_4471 OB Fraction L_4686 OB Fraction L_4861 OB Fraction L_5500 OB Fraction L_5808 OB Fraction L_6563 OB Fraction L_7000 OB Fraction L_9000 OB Fraction L_12500 OB Fraction L_22200 OB Fraction L_36000 OB Fraction L_bol OB
  RSG contribution:
  Standard Mdot 2 x Mdot Fraction L_1285 RSG Fraction L_1362 RSG Fraction L_1400 RSG Fraction L_1440 RSG Fraction L_1550 RSG Fraction L_1635 RSG Fraction L_1762 RSG Fraction L_1930 RSG Fraction L_2175 RSG Fraction L_2450 RSG Fraction L_3000 RSG Fraction L_3640 RSG Fraction L_3650 RSG Fraction L_4400 RSG Fraction L_4471 RSG Fraction L_4686 RSG Fraction L_4861 RSG Fraction L_5500 RSG Fraction L_5808 RSG Fraction L_6563 RSG Fraction L_7000 RSG Fraction L_9000 RSG Fraction L_12500 RSG Fraction L_22200 RSG Fraction L_36000 RSG Fraction L_bol RSG
  Post Main Sequence (PMS) contribution:
  Standard Mdot 2 x Mdot Fraction L_1285 PMS Fraction L_1362 PMS Fraction L_1400 PMS Fraction L_1440 PMS Fraction L_1550 PMS Fraction L_1635 PMS Fraction L_1762 PMS Fraction L_1930 PMS Fraction L_2175 PMS Fraction L_2450 PMS Fraction L_3000 PMS Fraction L_3640 PMS Fraction L_3650 PMS Fraction L_4400 PMS Fraction L_4471 PMS Fraction L_4686 PMS Fraction L_4861 PMS Fraction L_5500 PMS Fraction L_5808 PMS Fraction L_6563 PMS Fraction L_7000 PMS Fraction L_9000 PMS Fraction L_12500 PMS Fraction L_22200 PMS Fraction L_36000 PMS Fraction L_bol PMS

 

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• X-ray emission and kinetic energy

  Important Note:

  • the models presented in the following tables assumes X-ray emission from SN remnants (besides the reprocessing of kinetic power),
  • NO extinction has been considered,
  • only a fraction of 0.7 of the ionizing flux (including the one due to the X-rays) produces the nebular emission lines.

  Kinetic energy and X-ray emission
  Standard Mdot 2 x Mdot Ek Lk Ek (eff) Lk (eff) L(0.07-0.41 keV) L(0.41-2.4 keV) L(0.41-1.0 keV) L(1.0-2.4 keV) L(ROSAT 0.07-2.4 keV) L(EINSTEIN 0.1-3.4 keV) L(0.01-10 keV) L(2 keV) L(EINSTEIN)/nuLnu(1400 A)
  vary fX for a fixed metallicity vary metallicity for a fixed fX	Z=0.001 Z=0.004 Z=0.008 Z=0.020 Z=0.040 fx=0.00 fx=0.05 fx=0.20 fx=0.50 fx=0.80 fx=1.00
  Ionizing fluxes and nebular emission lines with X-rays: Q(He++)... W(Hb)...
  Standard Mdot 2 x Mdot log Q(He+) log Q(He0) log Q(H0) log Q(Ly) log L(Hb) EW(Hb) [A] log L(Ha) EW(Ha) [A] log L(th)(6cm) log L(He I) W(He I) [A] L(He I)/L(Hb) log L(He II) W(He II) [A] L(He II)/L(Hb) log Q(H_2) B=log(NLyc /L(1400)) Teff [K]
  vary fX for a fixed metallicity vary metallicity for a fixed fX	Z=0.001 Z=0.004 Z=0.008 Z=0.020 Z=0.040 fx=0.00 fx=0.05 fx=0.20 fx=0.50 fx=0.80 fx=1.00

 

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• Tables with the complete stellar energy distribution from X-rays to NIR tables (0.1-10 Myr)

  It includes only stellar emission. X-ray emission is included with different values of the kinetic energy to X-ray conversion (do not include nebular or extinction or dust):

  Stellar component alone (typical output of other synthesis codes)

  Stellar component and X-Rays from SN remants alone

  Stellar component, X-Rays from SN remants and additional X-rays due to release of kinetic energy following different efficiencies

  The tables can be used for photoionization codes, obtain colors etc... It includes the corresponding N_eff at each wavelength for the evaluation of statistical effects. Data normalized to a Salpeter IMF in the mass range 0.1-120 Mo. More details in the header of each table. Note: each table have a size about 4Mb (once ungzippez). For any question related with the use of the tables, question about additional outputs (like the results for other set of tracks or IMF assumptions), or if you find any problem with the tables, please, contact mcs@laeff.esa.es.
  The tables are only for standard Mdot.
  Additionally, for Cloudy users, here there is an ANSI C program that extracts the spectrum from the data file and produce a file with the continuum in an adecuate format for a direct use in Cloudy. Click here to get it. The program is self-explicative (see the header). Any question/comment, please, contanct me (mcs@laeff.inta.es or mcs@iaa.es).

  Standard Mdot      Z=0.001 Z=0.004 Z=0.008 Z=0.020 Z=0.040      fx=0.00 (and NO SNR) fx=0.00 (only SNR) fx=0.05 fx=0.20 fx=0.50 fx=1.00

  
  
  

 

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• Tables with the Effective rate of ionizing photons (mean, dispersion LLL and correlation matrix) (0.1-10 Myr)

  It includes only stellar emission NO X-ray emission. The tables includes the effective rate of ionizing photons for H⁰, He⁰, He⁺, C⁰, N⁰, N⁺, N⁺⁺, O⁰, O⁺, O⁺⁺, Ne⁰, Ne⁺, S⁰, S⁺, S⁺⁺, Ar⁰, Ar⁺ and Ar⁺⁺. The correlation coefficient matrix between the effective rate of ionizing photons for all the ions is also included. For any question related with the use of the tables, question about additional outputs or if you find any problem with the tables, please, contact mcs@laeff.esa.es.
  

  
  
  

  Standard Mdot 2 x Mdot      Z=0.001 Z=0.004 Z=0.008 Z=0.020 Z=0.040      Mean value Neff Lowest Luminosity Limit Correlation matrix

  
  
  

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Justicia, no venganza Justice, not revenge

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Miguel Cerviño, May 2003