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| SMSS J173823.36-145701.0 , the SIMBAD biblio (9 results) | C.D.S. - SIMBAD4 rel 1.8 - 2026.10.18CEST18:15:30 |
| Bibcode/DOI | Score |
in Title|Abstract| Keywords |
in a table | in teXt, Caption, ... | Nb occurence | Nb objects in ref |
Citations (from ADS) |
Title | First 3 Authors |
|---|---|---|---|---|---|---|---|---|---|
|
2015ApJ...807..171J |
16 | D | 1 | 131 | 106 | High-resolution spectroscopic study of extremely metal-poor star candidates from the SkyMapper survey. | JACOBSON H.R., KELLER S., FREBEL A., et al. | ||
| 2015Natur.527..484H | 17 | D | 1 | 28 | 93 | Extremely metal-poor stars from the cosmic dawn in the bulge of the Milky Way. | HOWES L.M., CASEY A.R., ASPLUND M., et al. | ||
|
2016ApJ...833...20Y |
16 | D | 1 | 304 | 147 | Observational constraints on first-star nucleosynthesis. I. Evidence for multiple progenitors of CEMP-no stars. | YOON J., BEERS T.C., PLACCO V.M., et al. | ||
|
2018ApJ...857...46I |
16 | D | 1 | 205 | 88 | The initial mass function of the first stars inferred from extremely metal-poor stars. | ISHIGAKI M.N., TOMINAGA N., KOBAYASHI C., et al. | ||
|
2019A&A...621A.108A |
97 | D | X | 3 | 59 | 49 | Binarity among CEMP-no stars: an indication of multiple formation pathways? | ARENTSEN A., STARKENBURG E., SHETRONE M.D., et al. | |
| 2019A&A...632A..62C | 81 | C | 2 | 261 | ~ | Inferring the velocity of early massive stars from the abundances of extremely metal-poor stars. | CHOPLIN A., TOMINAGA N. and ISHIGAKI M.N. | ||
|
2021MNRAS.503.2539C |
17 | D | 1 | 478 | 34 | Exploring the Galaxy's halo and very metal-weak thick disc with SkyMapper and Gaia DR2. | CORDONI G., DA COSTA G.S., YONG D., et al. | ||
|
2023ApJ...947...23Z |
17 | D | 1 | 647 | 14 | Chemodynamically Tagged Groups of CEMP Stars in the Halo of the Milky Way. I. Untangling the Origins of CEMP-s and CEMP-no Stars. | ZEPEDA J., BEERS T.C., PLACCO V.M., et al. | ||
| 2024ApJS..270...28R | 18 | D | 1 | 54 | ~ | Zero and Extremely Low-metallicity Rotating Massive Stars: Evolution, Explosion, and Nucleosynthesis Up to the Heaviest Nuclei. | ROBERTI L., LIMONGI M. and CHIEFFI A. |