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1. The DEIMOS 10k spectroscopic survey catalog of the COSMOS field

2. Rest-UV Absorption Lines as Metallicity Estimator: the Metal Content of Star-Forming Galaxies at z~5

3. Unveiling a population of galaxies harboring low-mass black holes with X-rays

4. Dissecting Photometric redshift for Active Galactic Nuclei using XMM- and Chandra-COSMOS samples

5. The Population of High Redshift AGNs in the Chandra COSMOS survey

6. Probing the faint end of the quasar luminosity function at z ~ 4 in the COSMOS field

7. An Atlas of z=5.7 and z=6.5 Ly alpha Emitters

8. Evidence for Supernova-Synthesised Dust from the Rising Afterglow of GRB 071025 at z~5

9. The stellar content of the COSMOS field as derived from morphological and SED based gtar/galaxy Separation

10. The Discovery of a Very Narrow-Line Star Forming Obat a Redshift of 5.66ject

11. A New High-Redshift Lyman alpha Emitter: Possible Superwind Galaxy at z = 5.69

12. Mineralogy, Three Dimensional Structure, and Oxygen Isotope Ratios of Four Crystalline Particles from Comet 81P/Wild 2

14. The DEIMOS 10K Spectroscopic Survey Catalog of the COSMOS Field

16. Bulk oxygen isotopic composition of ultra-carbonaceous antarctic micrometeorites with the Nanosims

17. REST-UV ABSORPTION LINES AS METALLICITY ESTIMATOR: THE METAL CONTENT OF STAR-FORMING GALAXIES ATz∼ 5

18. Early evolution of CV reduced-type parent body

19. An atlas of z = 5.7 and z = 6.5 Lyα emitters

20. Visible-IR and Raman microspectroscopic investigation of three Itokawa particles collected by Hayabusa: Mineralogy and degree of space weathering based on nondestructive analyses

26. DISSECTING PHOTOMETRIC REDSHIFT FOR ACTIVE GALACTIC NUCLEUS USINGXMM- ANDCHANDRA-COSMOS SAMPLES

27. THE POPULATION OF HIGH-REDSHIFT ACTIVE GALACTIC NUCLEI IN THECHANDRA-COSMOS SURVEY

28. PROBING THE FAINT END OF THE QUASAR LUMINOSITY FUNCTION AT z ∼ 4 IN THE COSMOS FIELD

30. Evidence for supernova-synthesized dust from the rising afterglow of GRB 071025 at z∼ 5

31. The Stellar Content of the COSMOS Field as Derived from Morphological and SED‐based Star/Galaxy Separation

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