Contact information

If you have any question or comment, please send an email to "cy-at-ahu.edu.cn".

Latest News

Gaia EDR3 filters added

November 20, 2020

Added Gaia EDR3 filters.

YBC paper on arXiv.org/astro-ph

October 22, 2019

The paper is available at arXiv:1910.09037. It is accepted for publication in A&A.

Non-uniform extinction for stars

October 21, 2019

Now you can supply different extinction value for different stars in your catalogue, by specifying the column number in section 4.

New extinction interpolation scheme and corrrections

May 23, 2019

Instead of using polynominal coefficients as in the last update, we now compute grids with Av=[0., 0.5, 1., 2., 5., 10., 20] and interpolate among them. Correct an error for AB+Vega mixed photometric systems.

Variable extinction implemented

April 24, 2019

Every spectrum used has been convlved with the extinction curve (Cardelli et al. (1989) + O'Donnell (1994) with RV=3.1.), therefore the spectral variation effect hass been considered. The non-lineararity as a function of Av amount has been also taken into account until the third order of the polynomial: Ai = a1*Av + a2*Av^2 + a3*Av^3.

YBC in PHP

February 22, 2019

Now website is changed from Python/Flask to PHP. Latest BC tables and interpolation code used now.
Read more

YBC on public domain

October 1st, 2018

This website is now on public domain.
Read more

YBC Web interface Launched

September 17th, 2018

The first time this website is on-line for internal test. It provides you the bolometric corrections given the stellar parameters.
Read more

Useful Links

Welcome to the database of stellar bolometric corrections

This database provides you with absolute magnitudes in any selected filter set, provided with stellar parameters. You can either input stellar parameters manually for single star, or upload a file containing a large number of stars. We appreciate your citation to our paper (A&A, 632 (2019) A105), if it is useful to your work.

Five steps to obtain BCs for your stars:

More information about the filters can be found Here (to be updated).
If you need results in other filter sets, please tell the names or send us the transmission files

2. Choose the spectral libraries to use

a) Library for low-intermediate Teff stars:

ATLAS9 & Phoenix & COMARCS (COMARCS used for Teff < 4850K and log g > 1.5, eg. TP-AGB)
Transition Teff from (low) K to (high) K

ATLAS9 & Phoenix (also for TP-AGB)
Transition Teff from (low) K to (high) K

ATLAS9 only

Phoenix only

ATLAS12 models with two 47Tuc metal contents & Phoenix (COMARCS for TP-AGB)
Transition Teff from (low) K to (high) K

ATLAS12 models with two 47Tuc metal contents & Phoenix (also for TP-AGB) only
Transition Teff from (low) K to (high) K

ATLAS12 models with two 47Tuc metal contents

b) Library for high Teff stars:

ATLAS9 & WMbasic & PoWR

ATLAS9 only

Phoenix only

ATLAS12 models with two 47Tuc metal contents

c) Library for AGB stars:

COMARCS

3. Interstellar extinction

Av = (Extinction curve: Cardelli et al. (1989) + O'Donnell (1994) with RV=3.1)
(Specify the extinction column in sec. 4, if your stars have different extinctions)

The variation of extinction within the filter window, the effect of spectral type, and the non-lineararity as a function of Av amount have been taking into account.
Circumstellar dust for RGB, RSG and TP-AGB are not included yet.

4. Stellar parameters of stars

Specify the stellar parameters:

log10(L(☉)): Teff(K) or log10(Teff/K):
log10(g)(cgs, put -100 if mass set):
mass(☉, put -100 if logg set):

Metallicity/abundance:

Z(-100 if not set):
Or
[FeH](-100 if not set):
Or
X(H mass fraction, -100 if not set):
Y(He mass fraction, -100 if not set):
Xc(C mass fraction, optional, -100 if not set):
Xn(N mass fraction, optional, -100 if not set):
Xo(O mass fraction, optional, -100 if not set):

Mdot(optinal): Vinf(optinal):

a) Upload your file:

An example file can be found Here (with corresponding columns given below in default).

b) Specify indices of the columns (starting from 1) for the following parameters:

The number and order of the columns is not a matter. The first line is considered to be the header. Header and auxiliary information lines should start with '#'.
log10(L(☉)): (column number!)
Teff(K) or log10(Teff/K): (column number!)
log10(g)(cgs, put -100 if mass set): (column number!)
mass(☉, put -100 if logg set): (column number!)

Metallicity/abundance:

Z(-100 if not set): (column number!)
Or
[Fe/H](-100 if not set): (column number!)
Or
X(H mass fraction, -100 if not set): (column number!)
Y(He mass fraction, -100 if not set): (column number!)
Xc(C mass fraction, -100 if not set): (column number!)
Xn(N mass fraction, -100 if not set): (column number!)
Xo(O mass fraction, -100 if not set): (column number!)

Mdot(optinal): (column number!)
Vinf(optinal): (column number!)

Av(extinction, optional, -100 if not present): (column number!)


a) Upload your file:

An example with Av=1.0 can be found at Here (with corresponding columns given below in default. It is downloaded from CMD). We are still investigating why the outputed magnitudes are not identical, but with some difference partly due to numerial rounding.

b) Specify indices of the columns (starting from 1) for the following parameters:

The number and order of the columns is not a matter. The first line is considered to be the header. Header and auxiliary information lines should start with '#'.
log10(L(☉)): (column number!)
Teff(K) or log10(Teff/K): (column number!)
log10(g)(cgs, put -100 if mass set): (column number!)
mass(☉, put -100 if logg set): (column number!)

Metallicity/abundance:

Z(-100 if not set): (column number!)
Or
[Fe/H](-100 if not set): (column number!)
Or
X(H mass fraction, -100 if not set): (column number!)
Y(He mass fraction, -100 if not set): (column number!)
Xc(C mass fraction, -100 if not set): (column number!)
Xn(N mass fraction, -100 if not set): (column number!)
Xo(O mass fraction, -100 if not set): (column number!)

Mdot(optinal): (column number!)
Vinf(optinal): (column number!)

Av(extinction, optional, -100 if not present): (column number!)

5.

(Absolute magnitudes are appended to your catalouge)