Help FAQ Papers People History

Pointing parameters Using Epoch 2000, decimal numbers: Galactic coordinates centered on l = deg, b = deg Equatorial coordinates centered on α = h, δ = deg Total field area = deg² (max=10 deg²)Photometric system Bolometric corrections are computed as in Girardi et al. 2002. Available systems:
2MASS + Spitzer (IRAC+MIPS)
2MASS + Spitzer (IRAC+MIPS) + WISE
2MASS JHKs
OGLE + 2MASS + Spitzer (IRAC+MIPS)
2MASS+Spitzer+WISE+Washington+DDO51
UBVRIJHK (cf. Maiz-Apellaniz 2006 + Bessell 1990)
UBVRIJHKLMN (cf. Bessell 1990 + Bessell & Brett 1988)
AKARI
BATC
CFHT Megacam + Wircam (all ABmags)
CFHT Wircam
CFHT/Megacam u*g'r'i'z'
CIBER
DECAM (ABmags)
DECAM ugrizY (ABmags) + VISTA ZYJHKs (Vegamags)
DENIS
DMC 14 filters
DMC 15 filters
ESO/EIS (WFI UBVRIZ + SOFI JHK)
ESO/WFI
ESO/WFI2
Euclid/NISP (ABmags)
GALEX FUV+NUV (Vegamag) + SDSS ugriz (ABmags)
GALEX FUV+NUV + Johnson's UBV (Maiz-Apellaniz version), all Vegamags
Gaia DR1 + Tycho2 + 2MASS (all Vegamags)
Gaia DR2 + Tycho2 + 2MASS (all Vegamags, Gaia passbands from Evans et al. 2018)
Gaia DR2 + Tycho2 + 2MASS (all Vegamags, Gaia passbands from Weiler 2018)
Gaia's DR1 G, G_BP and G_RP (Vegamags)
Gaia's DR2 G, G_BP and G_RP (Vegamags, Gaia passbands from Evans et al. 2018)
Gaia's DR2 G, G_BP and G_RP (Vegamags, Gaia passbands from Maiz-Apellaniz and Weiler 2018)
Gaia's DR2 G, G_BP and G_RP (Vegamags, Gaia passbands from Weiler 2018)
HST+GALEX+Swift/UVOT UV filters
HST/ACS HRC
HST/ACS WFC
HST/NICMOS AB
HST/NICMOS Vega
HST/STIS imaging mode, Vegamag
HST/WFC3 all W+LP+X filters (UVIS1+IR, final throughputs)
HST/WFC3 long-pass and extremely wide filters (UVIS1, final throughputs)
HST/WFC3 medium filters (UVIS1+IR, final throughputs)
HST/WFC3 wide filters (UVIS1+IR, final throughputs)
HST/WFPC2 (Vegamag, cf. Holtzman et al. 1995)
INT/WFC (Vegamag)
IPHAS
JWST MIRI wide filters, Vegamags
JWST NIRCam wide+verywide filters, Vegamags
JWST NIRCam wide+verywide+medium filters, Vegamags
JWST Nirspec filters, Vegamags
Kepler + SDSS griz + DDO51 (in ABmags)
Kepler + SDSS griz + DDO51 (in ABmags) + 2MASS (~Vegamag)
LBT/LBC (Vegamag)
LSST (ABmags) + WFIRST proposed filters (Vegamags)
LSST ugrizY, March 2012 total filter throughputs (all ABmags)
NOAO/CTIO/MOSAIC2 (Vegamag)
OGLE-II
Pan-STARRS1
S-PLUS (Vegamags), revised on Nov. 2017
SDSS ugriz
SDSS ugriz + 2MASS JHKs
SDSS ugriz + UKIDSS ZYJHK
SWIFT/UVOT UVW2, UVM2, UVW1,u (Vegamag)
SkyMapper (ABmags)
Spitzer IRAC+MIPS
Stroemgren-Crawford
Subaru/Suprime-Cam (ABmags)
TESS + 2MASS (Vegamags)
TESS + 2MASS (Vegamags) + Kepler + SDSS griz + DDO51 (in ABmags)
UKIDSS ZYJHK (Vegamag)
UVIT (all ABmags)
VISIR
VISTA ZYJHKs (Vegamag)
VPHAS+ (ABmags)
VST/OMEGACAM (ABmag)
Vilnius
WFIRST proposed filters, Vegamags
Washington CMT1T2 + DDO51
deltaa (Paunzen) + UBV (Maiz-Apellaniz), in Vegamags
Limiting magnitude in ^{th} filter is set to mag (max=32 mag) Distance modulus resolution of Galaxy components is mag (min=0.05 mag)IMF and binaries IMF for single stars:
Salpeter with cutoff at 0.01 M☉
Chabrier exponential
Chabrier lognormal (see paper)
Chabrier lognormal + Salpeter for M>1M☉
Kroupa (corrected for binaries)
Kroupa (non corrected for binaries)
Turn binaries on off Binary fraction = with mass ratios between and

Print binary components as a single entry separately

Extinction No dust extinction or Exponential disk exp(-|z |/h_{z} _{,dust} )×exp(-R /h_{R} _{,dust} ) with scale heigth h_{z} _{,dust} = pc and scale length h_{R} _{,dust} = pc Local calibration: dA_{V} /dr (☉)= mag/pc Calibration at infinity: A_{V} (∞)= mag

1σ dispersion= times the total extinction (max=0.3)

Solar position Sun's Galactocentric radius R ☉= pc, height above disk z ☉= pc Thin disc No thin disc or Along z: Exponential: exp(-|z |/h_{z} _{,d} ) Squared hyperbolic secant: sech²(0.5z /h_{z} _{,d} ) with scale height h_{z} _{,d} increasing with age t cf. h_{z} _{,d} =z _{0} (1+t/t _{0} )^{α} z _{0} = pc, t _{0} = yr, α= .

Along R : Exponential disc: exp(-R /h_{R} _{,d} ) with scale length h_{R} _{,d} = pc, and inner/outer cutoffs at R = pc and pc.

Local calibration: Σ_{d} (☉)= M☉/pc²

SFR and AMR given by
const. SFR + Fuhrman's AMR + α-enh.
2-step SFR + Fuhrman's AMR + α-enh. (see paper)
with age(yr)= ×t + .

Thick disc No thick disc or Along z: Exponential: exp(-|z |/h_{z} _{,td} ) Squared hyperbolic secant: sech²(0.5z /h_{z} _{,td} ) with scale height h_{z} _{,td} = pc

Along R : Exponential disc: exp(-R /h_{R} _{,td} ) with scale length h_{R} _{,td} = pc, and inner/outer cutoffs at R = pc and pc.

Local calibration: Ω_{td} (☉)= M☉/pc³

SFR and AMR given by
11-12 Gyr const. SFR + Z=0.008 with σ[M/H]=0.1 dex
with age(yr)= ×t + .

Halo No halo or r ¼ Spheroid Oblate r ¼ Spheroid Effective radius r _{h} = pc (at major axis), oblateness q _{h} =

Local calibration: Ω_{h} (☉)= M☉/pc³

SFR and AMR given by
12-13 Gyr + Ryan & Norris [M/H] distribution
12-13 Gyr + Z=0.0095 with σ[M/H]=1.0 dex
with age(yr)= ×t + .

Bulge See Vanhollebeke et al. (2009) for details. No bulge or Triaxial bulge Scale length a_{m} = pc, truncation scale length a _{0} = pc, y/x axial ratio η= z/x axial ratio ξ= Sun-GC-bar angle φ_{0} = °Central calibration: Ω_{b} (GC)= M☉/pc³

SFR and AMR given by
10 Gyr, Zoccali et al. 2003 [M/H]
10 Gyr, Zoccali et al.2003 [M/H] + 0.3 dex
with age(yr)= ×t + .

Additional object The addition of star clusters and galaxies is being planned. It requires a major upgrade of the web forms.

This service is mantained by Léo Girardi at the Osservatorio Astronomico di Padova . Questions, comments and special requests should be directed to leo.girardi@oapd·inaf·it . Last modified: Thu Jan 30 15:24:21 2020