Establishing the Galactic Centre distance using VVV Bulge RR Lyrae variables
This study’s objective was to exploit infrared VVV (VISTA Variables in the Via Lactea) photometry for high latitude RRab stars to establish an accurate Galactic Centre distance. RRab candidates were discovered and reaffirmed (n=4194n=4194n=4194) by matching KsKsK_{s} photometry with templates via χ2...
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| Main Authors: | , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
22 May 2018
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| In: |
Astrophysics and space science
Year: 2018, Volume: 363, Issue: 6 |
| ISSN: | 1572-946X |
| DOI: | 10.1007/s10509-018-3346-6 |
| Online Access: | Verlag, Volltext: http://dx.doi.org/10.1007/s10509-018-3346-6 Verlag, Volltext: https://doi.org/10.1007/s10509-018-3346-6 
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| Author Notes: | D. Majaess, I. Dékány, G. Hajdu, D. Minniti, D. Turner, W. Gieren |
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| 245 | 1 | 0 | |a Establishing the Galactic Centre distance using VVV Bulge RR Lyrae variables |c D. Majaess, I. Dékány, G. Hajdu, D. Minniti, D. Turner, W. Gieren |
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| 520 | |a This study’s objective was to exploit infrared VVV (VISTA Variables in the Via Lactea) photometry for high latitude RRab stars to establish an accurate Galactic Centre distance. RRab candidates were discovered and reaffirmed (n=4194n=4194n=4194) by matching KsKsK_{s} photometry with templates via χ2χ2\chi ^{2} minimization, and contaminants were reduced by ensuring targets adhered to a strict period-amplitude (ΔKsΔKs\Delta K_{s}) trend and passed the Elorietta et al. classifier. The distance to the Galactic Centre was determined from a high latitude Bulge subsample (|b|>4∘|b|>4∘|b|>4^{\circ}, RGC=8.30±0.36RGC=8.30±0.36R_{\mathit{GC}}=8.30 \pm 0.36 kpc, random uncertainty is relatively negligible), and importantly, the comparatively low color-excess and uncrowded location mitigated uncertainties tied to the extinction law, the magnitude-limited nature of the analysis, and photometric contamination. Circumventing those problems resulted in a key uncertainty being the MKsMKsM_{K_{s}} relation, which was derived using LMC RRab stars (MKs=−(2.66±0.06)logP−(1.03±0.06)MKs=−(2.66±0.06)logP−(1.03±0.06)M_{K_{s}}=-(2.66\pm 0.06) \log {P}-(1.03\pm 0.06), (J−Ks)0=(0.31±0.04)logP+(0.35±0.02)(J−Ks)0=(0.31±0.04)logP+(0.35±0.02)(J-K_{s})_{0}=(0.31\pm 0.04) \log {P} + (0.35\pm 0.02), assuming μ0,LMC=18.43μ0,LMC=18.43\mu _{0,\mathit{LMC}}=18.43). The Galactic Centre distance was not corrected for the cone-effect. Lastly, a new distance indicator emerged as brighter overdensities in the period-magnitude-amplitude diagrams analyzed, which arise from blended RRab and red clump stars. Blending may thrust faint extragalactic variables into the range of detectability. | ||
| 650 | 4 | |a Galaxy: center | |
| 650 | 4 | |a Stars: variables: RR Lyrae | |
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