General Instructions for IA2 - BaSTI Database Server

This form allows the user to download ascii files creating using FRANEC code described in Pietrinferni, Cassisi, Salaris & Castelli (2004, ApJ, 612, 168).

Descriptions of individual fields on this form follow:

Filename

This string gives the name of the file contained into the Database, it is unique.

Data type

The available theoretical predictions are:

TRACK:

the evolution of a stellar model followed from the Main-Sequece to the first thermal pulse.

TRACK HB:

the evolution of a stellar model followed from the Zero Age Horizontal Branch (ZAHB) to the first thermal pulse.

ISOCHRON:

the locus of H-R diagram (or CMD) populated by structures with the same age and initial chemical composition but different mass.

Tab. ZAHB:

the locus of H-R diagram (or CMd) populated by structures with the same Helium core mass and chemical composition, but different total mass taken at the ZAHB phase.

Tab. End He:

the locus of H-R diagram (or CMd) populated by structures with the same Helium core mass and chemical composition, but different total mass taken at the end of central Helium burning phase.

Summary Tab.:

table with same important quantities taken at different evolutionary phases.

Scenario

CANONICAL:

the models do not include gravitational settling, radiative acceleration, convective overshooting, rotational mixing.

OVERSHOOTING:

the models do not include gravitational settling, radiative acceleration, rotational mixing, but account for core convective overshooting during the H-burning phase. The value adopted for the overshoot from the classical Schwarzschild convective boundary is equal to λ_OV·H_p where λ_OV=0.2 and H_p is the local pressure scale.

DIFFUSION:

not yet available.

ROTATION:

not yet available.

Age

It represents the age (in Gyr) of an isochron; the minimum value is 0.03 Gyr, while the maximum value depends from the adopted Mass loss (η) and Overshooting (λ_OV) parameters as summarized in the table:

η	λ_OV	Age max
0.2	0.0	19
0.2	0.2	9.5
0.4	0.0	15
0.4	0.2	9.5

Mass

It is the mass (in Solar Unit) of the structure. Its minimum and maximum values depend from the adopted Mass loss (η) and Overshooting (λ_OV) parameters as summarized in the table:

η	λ_OV	Mass min	Mass max
0.2	0.0	0.5	2.5
0.2	0.2	1.1	2.5
0.4	0.0	0.5	10
0.4	0.2	1.1	10

Z

The mass fraction of the initial heavy elements abundance; the range covered is: 0.0001 ≤ Z ≤ 0.04

Y

The mass fraction of the initial helium abundance; the range covered is: 0.245 ≤ Y ≤ 0.303
Actually, for each Z models have been computed by adopting a unique Y value given by: Y=1.44·(Z-0.0001)

[Fe/H]

The iron abundance in the spectroscopic formalism:

[Fe/H]= log₁₀(Fe_∗/H_∗) - log₁₀(Fe_sun/H_sun) the range covered is: -2.62 ≤ [Fe/H] ≤ 0.40

[M/H]

The metal abundance in the spectroscopic formalism:

[Z/H]= log₁₀(Z_∗/H_∗) - log₁₀(Z_sun/H_sun) the range covered is: -2.27 ≤ [Fe/H] ≤ 0.40

Type

NORMAL:

the evolution tracks and isochrones have been followed until the first thermal pulse.

AGBEXTENDED:

both stellar evolution models and isochrones have been extended along the Asimptotic Giant Branch (AGB) stage to cover the full thermal pulses phase, using the synthetic AGB tecnique (Iben & Truran 1978, ApJ, 220, 980)

Mass loss

All models include mass loss according to the Reimers (1975) low:

dM/dt = -4 · 10-13 η ·(L/gR) (M_sun/yr) (where L, g and R are the stellar luminosity, surface gravity and radius respectively) with the free parameter η set to 0.2 and 0.4.

Photometric system

All the theoretical predictions has been transferred from the theoretical to different photometric system:

ACS: Advanced Camera for Survey - on board of HST - Vega mag (Bedin et al. 2005, MNRAS, 357, 1038)

F435W	F475W	F555W	F606W	F625W	F775W	F814W

SLOAN: Sloan system (Marconi et al. 2005, MNRAS, 371, 1503)

Mg	(u-g)	(g-r)	(r-i)	(i-z)

JOHNSON CASTELLI: Johnson-Cousins system (Pietrinferni et al. 2004, ApJ, 612, 168)

M_V	(B-V)	(U-B)	(V-I)	(V-R)	(V-J)	(V-K)	(V-L)	(H-K)

STROEMGREN CASTELLI: Stroemgren system (Pietrinferni et al. 2006, ApJ, 642, 797)

M_y	(u-b)	(u₀-b)	(b-y)	(m₁)	(c₁)	(c_{1_0})	(Hβ)	(hk)

WALRAVEN : Walraven system

M_V	(V-B)	(B-U)	(U-W)	(B-L)	(L-U)

WFC2 HST: Wide Field Planetary Camera 2 system - on board of HST

F122W	F130lp	F160W	F165lp	F170W	F185W	F218W	F255W	F300W	F336W	F380W	F439W	F450W	F555W	F606W	F622W	F675W	F702W	F791W	F814W	F850lp

WFC3 (UVIS) HST: Wide Field Camera 3 (UVIS) system - on board of HST

F218W	F225W	F275W	F336W	F390W	F438W	F475W	F555W	F606W	F625W	F775W	F814W

Mixture

All the theoretical predictions have been computed adopting two different distributions for the heavy elements:

SCALED SOLAR
(Grevesse & Noel 1993)

ALPHA ENHANCED
(Weiss 1995)

N¹⁴

O¹⁶

Ar⁴⁰

Ca⁴⁰

Ti⁴⁸

Mn⁵⁵

Fe⁵⁶

Ni⁵⁹

Code version

The stellar evolutionary codes adopted in this work are the FRANEC (Frascati Raphson-Newton Evolutionary Code), i.e. the same used by Cassisi & Salaris (1997) and Salris & Cassisi (1998), with various updates:

Physical inputs	2003	2007
Equation of State	Irwin 2003	Irwin 2003
Low-T radiative opacity	Alexander & Ferguson 1994	Ferguson et al. 2005
High-T radiative opacity	Iglesias & Rogers 1996	Iglesias & Rogers 1996
Conductive opacity	Potekhin 1999	Potekhin 1999
Nuclear reaction	NACRE (Angulo et al. 1999)	NACRE (Angulo et al. 1999)
Plasma neutrino	Haft et al. 1994	Haft et al. 1994
Boundary Condition	Krishna-Swamy 1966	Krishna-Swamy 1966
Mixing length	1.913	2.013
Atomic Diffusion	NO	NO
Mass loss	Reimers 1975	Reimers 1975

Rad opacity

This field indicates the prescription followed to include the low temperature radiative opacity:

Alexander & Ferguson 1994 ⇒ Alexander D. R., & Ferguson J. W., 1994, ApJ, 437, 879

Ferguson 2005 ⇒ Ferguson et al. 2005, ApJ, 623, 585

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