Investigation of Metallicity Gradient with GALAH and Gaia Data in the Milky Way

Abstract

In this study, metallicity abundance gradients for the thin disk population of the Milky Way were investigated using the metal abundances, Galactic orbital parameters and space velocities of 66,220 main sequence stars selected from the high-sensitivity data from the GALAH DR3 and Gaia EDR3 sky survey programs. The metallicity abundance gradients calculated in the $R_{\rm GC}$, $R_{\rm Rehber}$, $Z_{\rm max}$ planes according to the iron abundances of thin disk stars are $d[{\rm Fe/H}]/dR_{\rm GC}=-0.068\pm 0.014$, $d[{\rm Fe/H}]/dR_{\rm Rehber}=-0.074\pm 0.005$ ve $d[{\rm Fe/H}]/dZ_{\rm max}=-0.160\pm 0.008$ dex/kpc. Alpha element abundance gradients in the same planes were calculated as $d[\alpha/{\rm Fe}]/dR_{GC}=+0.001\pm 0.003$, $d[\alpha/{\rm Fe}]/dR_{Rehber}=-0.005\pm 0.001$ dex/kpc ve $d[\alpha/{\rm Fe}]/dZ_{\rm max}=0.034\pm 0.002$ dex/kpc. As a result, the findings obtained in the study support the two-infall model.

Keywords

• Galaxy: abundances
• Galaxy: disc
• solar neighbourhood

GALAH ve Gaia Verileriyle Samanyolu'nda Metal Bolluğu Gradyent Araştırması

Öz

Bu çalışmada GALAH DR3 ve Gaia EDR3 gökyüzü tarama programlarından duyarlılığı yüksek veriler arasından seçilen 66,220 anakol yıldızının metal bollukları, Galaktik yörünge parametreleri ve uzay hızları kullanılarak Samanyolu'nun ince disk popülasyonu için metal bolluğu gradyentleri araştırılmıştır. İnce disk yıldızlarının demir bolluklarına göre $R_{\rm GC}$, $R_{\rm Rehber}$, $Z_{\rm max}$ düzlemlerinde hesaplanan metal bolluğu gradyentleri $d[{\rm Fe/H}]/dR_{\rm GC}=-0.068\pm 0.014$, $d[{\rm Fe/H}]/dR_{\rm Rehber}=-0.074\pm 0.005$ ve $d[{\rm Fe/H}]/dZ_{\rm max}=-0.160\pm 0.008$ dex/kpc'dir, alfa element bolluk gradyentleri de $d[\alpha/{\rm Fe}]/dR_{GC}=+0.001\pm 0.003$, $d[\alpha/{\rm Fe}]/dR_{Rehber}=-0.005\pm 0.001$ dex/kpc ve $d[\alpha/{\rm Fe}]/dZ_{\rm max}=0.034\pm 0.002$ dex/kpc’dir. Bulunan sonuçlar Samanyolu'nun içten dışa çökme senaryoları ile uyum içerisindedir.

Anahtar Kelimeler

• Galaxy: abundances
• Galaxy: disc
• solar neighbourhood

Kaynakça

1. Bensby T., Feltzing S., 2010, in Cunha K., Spite M., Barbut B., eds, Vol. 265, Chemical Abundances in the Universe: Connect-ing First Stars to Planets. pp 300-303. (arXiv:0908.3807), doi:10.1017/S1743921310000773.
2. Bressan A., Marigo P., Girardi L., Salasnich B., Dal Cero C., Rubele S., Nanni A., 2012, MNRAS, 427, 127.
3. Gaia Collaboration 2020, VizieR Online Data Catalog, p. I/350, ADS.
4. Marsakov V. A., Koval V. V., Borkova T. V., Shapovalov M. V., 2011, Astronomy Reports, 55, 667.
5. Nissen P. E., 2004, in McWilliam A., Rauch M., eds, Origin and Evolution of the Elements. p. 154 (arXiv:astro-ph/0310326)
6. Plevne O., Önal Taş Ö., Bilir S., Seabroke G. M., 2020, ApJ, 893,108.
7. Sharma S., et al., 2017, Monthly Notices of the Royal Astronomical Society, 473, 2004.
8. Sharma S., Hayden M. R., Bland-Hawthorn J., 2021, MNRAS, 507, 5882.