J-PLUS: Systematic impact of metallicity on photometric calibration with the stellar locus

López-Sanjuan, C.; Yuan, Haibo; Ramió, H. Vázquez; Varela, J.; Cristóbal-Hornillos, D.; Tremblay, Pier-Emmanuel; Marín-Franch, A.; Cenarro, A. J.; Ederoclite, A.; Alfaro, E. J.; Álvarez-Candal, A.; Daflon, S.; Hernán-Caballero, A.; Hernández-Monteagudo, C.; Jiménez-Esteban, F.; Placco, Vinicius M.; Tempel, Elmo; Alcaniz, J. S.; Angulo, Raúl E.; Dupke, Renato A.; Moles, M.; Sodré, L.

doi:10.1051/0004-6361/202140444

Cited by 23 publications

(15 citation statements)

References 62 publications

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“…Using the stellar color regression method (SCR; Yuan et al 2015a, Huang et al 2021b, Niu et al 2021a, Niu et al 2021b, Huang & Yuan 2021, by combining the LAMOST DR5 spectroscopy and Gaia DR2 photometry, we have re-calibrated the J-PLUS DR1 data and achieved an accuracy of about 0.5 per cent or better for all the J-PLUS filters (Yuan et al in preparation). Strongly correlated calibration errors are found in the previous calibration, due to the strong metallicity-dependence of stellar loci for blue filters (e.g., Yuan et al 2015b, López-Sanjuan et al 2021) and errors in the 3D dust map and reddening coefficients used (Yuan et al in preparation). In order to make the best use of the full power of J-PLUS filters, the re-calibrated J-PLUS DR1 data are used in this work.…”

Section: Stellar Colorsmentioning

confidence: 91%

J-PLUS: Stellar Parameters, C, N, Mg, Ca and [α/Fe] Abundances for Two Million Stars from DR1

Yang,

Yuan,

Xiang

et al. 2021

Preprint

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Context. The Javalambre Photometric Local Universe Survey (J-PLUS) has obtained precise photometry in twelve specially designed filters for large numbers of Galactic stars. Deriving their precise stellar atmospheric parameters and individual elemental abundances is crucial for studies of Galactic structure, and the assembly history and chemical evolution of our Galaxy. Aims. Our goal is to estimate not only stellar parameters (effective temperature, T eff , surface gravity, log g, and metallicity, [Fe/H]), but also [α/Fe] and four elemental abundances ([C/Fe], [N/Fe], [Mg/Fe], and [Ca/Fe]) using data from J-PLUS DR1. Methods. By combining recalibrated photometric data from J-PLUS DR1, Gaia DR2, and spectroscopic labels from LAMOST, we design and train a set of cost-sensitive neural networks, the CSNet, to learn the non-linear mapping from stellar colors to their labels. Special attention is paid to the poorly populated regions of the label space by giving different weights according to their density distribution.Results. We have achieved precisions of δ T eff ∼ 55 K, δ log g ∼ 0.15 dex, and δ [Fe/H] ∼ 0.07 dex, respectively, over a wide range of temperature, surface gravity, and metallicity. The uncertainties of the abundance estimates for [α/Fe] and the four individual elements are in the range 0.04-0.08 dex. We compare our parameter and abundance estimates with those from other spectroscopic catalogs such as APOGEE and GALAH, and find an overall good agreement. Conclusions. Our results demonstrate the potential of well-designed, high-quality photometric data for determinations of stellar parameters as well as individual elemental abundances. Applying the method to J-PLUS DR1, we have obtained the aforementioned parameters for about two million stars, providing an outstanding data set for chemo-dynamic analyses of the Milky Way. The catalog of the estimated parameters is publicly accessible.

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Section: Stellar Colorsmentioning

confidence: 91%

J-PLUS: Stellar Parameters, C, N, Mg, Ca and [α/Fe] Abundances for Two Million Stars from DR1

Yang,

Yuan,

Xiang

et al. 2021

Preprint

View full text Add to dashboard Cite

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“…Using the stellar colour regression method (SCR; Yuan et al 2015a, Huang et al 2021b, Niu et al 2021a, Niu et al 2021b, Huang & Yuan 2021 and by combining the LAMOST DR5 spectroscopy and Gaia DR2 photometry, we recalibrated the J-PLUS DR1 data and achieved an accuracy of about 0.5 per cent or better for all the J-PLUS filters (Yuan et al in preparation). Strongly correlated calibration errors are found in the previous calibration due to the strong metallicity-dependence of stellar loci for blue filters (e.g., Yuan et al 2015b, López-Sanjuan et al 2021 and errors in the 3D dust map and reddening coefficients used (Yuan et al in preparation). In order to make the best use of the full power of J-PLUS filters, the recalibrated J-PLUS DR1 data were used in this work.…”

Section: Stellar Coloursmentioning

confidence: 92%

J-PLUS: Stellar parameters, C, N, Mg, Ca, and [α/Fe] abundances for two million stars from DR1

Yang

Yuan

Xiang

et al. 2022

A&A

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Context. The Javalambre Photometric Local Universe Survey (J-PLUS) has obtained precise photometry in 12 specially designed filters for large numbers of Galactic stars. Deriving their precise stellar atmospheric parameters and individual elemental abundances is crucial for studies of Galactic structure and the assembly history and chemical evolution of our Galaxy. Aims. Our goal is to estimate not only stellar parameters (effective temperature, T eff , surface gravity, log g, and metallicity, [Fe/H]), but also [α/Fe] and four elemental abundances ([C/Fe], [N/Fe], [Mg/Fe], and [Ca/Fe]) using data from the first data release (DR1) of J-PLUS. Methods. By combining recalibrated photometric data from J-PLUS DR1, Gaia DR2, and spectroscopic labels from the Large sky Area Multi-Object fiber Spectroscopic Telescope (LAMOST), we designed and trained a set of cost-sensitive neural networks, the CSNet, to learn the nonlinear mapping from stellar colours to their labels. Special attention was paid to the poorly populated regions of the label space by giving different weights according to their density distribution. Results. We achieved precisions of δ T eff ∼ 55 K, δ log g ∼ 0.15 dex, and δ [Fe/H] ∼ 0.07 dex, respectively, over a wide range of temperatures, surface gravities, and metallicities. The uncertainties of the abundance estimates for [α/Fe] and the four individual elements are in the 0.04-0.08 dex range. We compare our parameter and abundance estimates with those from other spectroscopic catalogs such as the Apache Point Observatory for Galactic Evolution Experiment (APOGEE) and the Galactic Archaeology with High Efficiency and Resolution Multi-Element Spectrograph (GALAH) and find an overall good agreement. Conclusions. Our results demonstrate the potential of well-designed, high-quality photometric data for determinations of stellar parameters as well as individual elemental abundances. Applying the method to J-PLUS DR1, we obtained the aforementioned parameters for about two million stars, providing an outstanding dataset for chemo-dynamic analyses of the Milky Way. The catalog of the estimated parameters is publicly accessible.

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“…2021; López-Sanjuan et al 2021). The limiting magnitudes (5σ, 3 arsec aperture) of the DR2 are ∼ 22 mag in g and r passbands, and ∼ 21 mag in the other ten bands.…”

Section: -8895mentioning

confidence: 91%

“…The observed fluxes were stored in the vector f = { f j }, and their errors in the vector σ f = {σ j }, where the index j runs the J-PLUS passbands. The error vector includes the uncertainties from photon counting, sky background, and photometric calibration (López-Sanjuan et al 2021).…”

Section: -8895mentioning

confidence: 99%

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J-PLUS: Spectral evolution of white dwarfs by PDF analysis

López-Sanjuan,

Tremblay,

Ederoclite

et al. 2021

Preprint

Self Cite

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Aims. We estimated the spectral evolution of white dwarfs with effective temperature using the Javalambre Photometric Local Universe Survey (J-PLUS) second data release (DR2), that provides twelve photometric optical passbands over 2 176 deg 2 . Methods. We analysed 5 926 white dwarfs with r ≤ 19.5 mag in common between a white dwarf catalog defined from Gaia EDR3 and J-PLUS DR2. We performed a Bayesian analysis by comparing the observed J-PLUS photometry with theoretical models of hydrogen (H) and helium (He) dominated atmospheres. We estimated the probability distribution functions for effective temperature (T eff ), surface gravity, parallax, and composition; and the probability of having a H-dominated atmosphere (p H ) for each source. We applied a prior in parallax, using Gaia EDR3 measurements as reference, and derived a self-consistent prior for the atmospheric composition as a function of T eff . Results. We described the fraction of He-dominated atmosphere white dwarfs ( f He ) with a linear function of the effective temperature at 5 000 < T eff < 30 000 K. We found f He = 0.24 ± 0.01 at T eff = 10 000 K, a change rate along the cooling sequence of 0.14 ± 0.02 per 10 kK, and a minimum He-dominated fraction of 0.08 ± 0.02 at the high-temperature end. We tested the obtained p H by comparison with spectroscopic classifications, finding that it is reliable. We estimated the mass distribution for the 351 sources with distance d < 100 pc, mass M > 0.45 M , and T eff > 6 000 K. The result for H-dominated white dwarfs agrees with previous work, with a dominant M = 0.59 M peak and the presence of an excess at M ∼ 0.8 M . This high-mass excess is absent in the He-dominated distribution, which presents a single peak. Conclusions. The J-PLUS optical data provides a reliable statistical classification of white dwarfs into H-and He-dominated atmospheres. We find a 21 ± 3% increase in the fraction of He-dominated white dwarfs from T eff = 20 000 K to T eff = 5 000 K.

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J-PLUS: Systematic impact of metallicity on photometric calibration with the stellar locus

Cited by 23 publications

References 62 publications

J-PLUS: Stellar Parameters, C, N, Mg, Ca and [α/Fe] Abundances for Two Million Stars from DR1

J-PLUS: Stellar Parameters, C, N, Mg, Ca and [α/Fe] Abundances for Two Million Stars from DR1

J-PLUS: Stellar parameters, C, N, Mg, Ca, and [α/Fe] abundances for two million stars from DR1

J-PLUS: Spectral evolution of white dwarfs by PDF analysis

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