skip to main content
Language:
Search Limited to: Search Limited to: Resource type Show Results with: Show Results with: Search type Index

Ultraviolet emission lines in young low-mass galaxies at z ≃ 2: physical properties and implications for studies at z > 7

Monthly notices of the Royal Astronomical Society, 2014-12, Vol.445 (3), p.3200-3220 [Peer Reviewed Journal]

2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society 2014 ;Copyright Oxford University Press, UK Dec 11, 2014 ;Distributed under a Creative Commons Attribution 4.0 International License ;ISSN: 0035-8711 ;EISSN: 1365-2966 ;DOI: 10.1093/mnras/stu1618

Digital Resources/Online E-Resources

Citations Cited by
  • Title:
    Ultraviolet emission lines in young low-mass galaxies at z ≃ 2: physical properties and implications for studies at z > 7
  • Author: Stark, Daniel P ; Richard, Johan ; Siana, Brian ; Charlot, Stéphane ; Freeman, William R ; Gutkin, Julia ; Wofford, Aida ; Robertson, Brant ; Amanullah, Rahman ; Watson, Darach ; Milvang-Jensen, Bo
  • Subjects: Astronomy ; Astrophysics ; Cosmology and Extra-Galactic Astrophysics ; Emission ; Emission spectroscopy ; Emitters ; Equivalence ; Galaxies ; Luminosity ; Photoionization ; Physical properties ; Pollution sources ; Red shift ; Sciences of the Universe ; Space telescopes ; Spectrum analysis ; Star formation ; Stars & galaxies ; Ultraviolet radiation
  • Is Part Of: Monthly notices of the Royal Astronomical Society, 2014-12, Vol.445 (3), p.3200-3220
  • Description: We present deep spectroscopy of 17 very low mass (M ⋆ ≃ 2.0 × 106–1.4 × 109 M⊙) and low luminosity (M UV ≃ −13.7 to −19.9) gravitationally lensed galaxies in the redshift range z ≃ 1.5-3.0. Deep rest-frame ultraviolet spectra reveal large equivalent width emission from numerous emission lines (N iv], O iii], C iv, Si iii], C iii]) which are rarely seen in individual spectra of more massive star-forming galaxies. C iii] is detected in 16 of 17 low-mass star-forming systems with rest-frame equivalent widths as large as 13.5 Å. Nebular C iv emission is present in the most extreme C iii] emitters, requiring an ionizing source capable of producing a substantial component of photons with energies in excess of 47.9 eV. Photoionization models support a picture whereby the large equivalent widths are driven by the increased electron temperature and enhanced ionizing output arising from metal-poor gas and stars (0.04–0.13 Z⊙), young stellar populations (6–50 Myr), and large ionization parameters (log U = −2.16 to −1.84). The young ages implied by the emission lines and continuum spectral energy distributions (SEDs) indicate that the extreme line emitters in our sample are in the midst of a significant upturn in their star formation activity. The low stellar masses, blue UV colours, and large specific star formation rates of our sample are similar to those of typical z ≳ 6 galaxies. Given the strong attenuation of Lyα in z ≳ 6 galaxies, we suggest that C iii] is likely to provide our best probe of early star-forming galaxies with ground-based spectrographs and one off the most efficient means of confirming z ≳ 10 galaxies with the James Webb Space Telescope.
  • Publisher: London: Oxford University Press
  • Language: English
  • Identifier: ISSN: 0035-8711
    EISSN: 1365-2966
    DOI: 10.1093/mnras/stu1618
  • Source: Hyper Article en Ligne (HAL) (Open Access)
Back to results list
INSPIRE LIBRARY - TON DUC THANG UNIVERSITY (84-028) 37 755 057 Feedback
19 Nguyen Huu Tho St. Dist.7, HCM thuvien@tdtu.edu.vn

Copyright © 2017 INSPIRE LIBRARY - TON DUC THANG UNIVERSITY

Searching Remote Databases, Please Wait