photometric parallax estimation using the miles catalog and basel models
DESCRIPTION
Photometric parallax estimation using the MILES catalog and BaSeL models. István Csabai László Dobos Márton Trencsényi Norbert Purger Géza Herczeg. Gyöngyi Kerekes MAGPOP Meeting , Malta 10 November 2014. Photometric parallax. Based on different distance measurements for stars : - PowerPoint PPT PresentationTRANSCRIPT
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EÖTVÖS UNIVERSITY BUDAPEST
Department of Physics of Complex Systems
Photometric parallax estimation using the MILES catalog and BaSeL models
Photometric parallax estimation using the MILES catalog and BaSeL models
István CsabaiLászló DobosMárton TrencsényiNorbert PurgerGéza Herczeg
István CsabaiLászló DobosMárton TrencsényiNorbert PurgerGéza Herczeg
GYÖNGYI KEREKES
MAGPOP MEETING, MALTA
April 20, 2023
GYÖNGYI KEREKES
MAGPOP MEETING, MALTA
April 20, 2023
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PHOTOMETRIC PARALLAX
• Based on different distance measurements for stars:o Trigonometric parallax (nearest stars)o Main sequence fitting (open clusters)o Cepheid variable stars (globular clusters), etc.
• Calculation of absolute magnitudes• Color-magnitude diagram• Main sequence fitting with a function
• If we know the color index of a star, we can estimate the distance.
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PHOTOMETRIC PARALLAX
Problems:• We can only estimate for main sequence stars• Color indices are metallicity-dependent (especially
B, V)• We need continuous parameters• Hawley, 2002
(spectroscopic parallax)
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PHOTOMETRIC PARALLAX ESTIMATIONS
Juric et al, 2005 THE MILKY WAY TOMOGRAPHY WITH SDSS
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OUR CONCEPTION
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MILES DATABASE
• 985 stars • Wavelength range: 3525 – 7500 Å
at 2.3 Å spectral resolution• Atmospheric data estimated using CEN01b
(Teff, log g, [Fe/H])
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MILES DATABASE
Teff vs log g
Large range of atmospheric parameters: from metal-rich, cool stars to hot, metal-poor stars.
Cenarro et al, 2006
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HIPPARCOS
• Trigonometric parallax• About 130.000 stars• Error: 0.7-0.9 mas for stars brighter than
9 mag
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MILES – HIPPARCOS CROSSMATCH
• Based on coordinates (40 arcsec) 614 stars
• HRD[V>10]
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MILES – HIPPARCOS CROSSMATCH
• CMD
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BASEL MODEL
• Used for fitting: 2 735 spectra• Method: least χ2 • Spectra fitted:
χ2=0.344
χ2=3.578
χ2=11.886
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SPECTRA FITTING
• Cut at χ2 = 3• Result:
562 stars
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SPECTRA FITTING
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SYNTHETIC MAGNITUDES
• u’, g’, r’, i’, z’ (Sloan filters)
[Fukugita et al, 1996]
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SYNTHETIC MAGNITUDES
Jester et al. 2005 filter transformation equations:
g=V+0.64(B-V)-0.13
r=V-0.46(B-V)+0.11
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COLOR-COLOR DIAGRAMS
g – r vs r – i for 100 000 Sloan stars (red dots) and for MILES stars (green crosses)
r – i
g –
r
SDSS stars selection:
Relative error in magnitudes < 0.04%
Magnitudes in range [14;17]
Upper CCD from Michael Richmond
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COLOR-COLOR DIAGRAMS
u-g vs g-r for 100 000 Sloan stars (red dots) and for MILES stars (green crosses)
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OUR ESTIMATION
• We have code for nonparametric estimation (multidimensional indexing integrated with databases)
• It was created for photometric redshift calculation and estimation of physical parameters of galaxies
• This code can be adapted for photometric parallax estimation: 5-D (4 CI & M) spaces nearest neighbour searching absolute manitude & parallax estimation
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FUTURE TASKS