Constraining C III] Emission in a Sample of Five Luminous z = 5.7 Galaxies

Jiani Ding, Zheng Cai, Xiaohui Fan, Daniel P Stark, Fuyan Bian, Linhua Jiang, Ian D. McGreer, Brant E Robertson, Brian Siana

Research output: Contribution to journalArticle

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Abstract

Recent observations have suggested that the C iii] emission lines could be alternative diagnostic lines for galaxies in the reionization epoch. We use the F128N narrowband filter on the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) to search for C iii] emission in a sample of five galaxies at z = 5.7 in the Subaru Deep Field and the Subaru/XMM-Newton Deep Field. Using the F128N narrowband imaging, together with the broadband imaging, we do not detect C iii] emission for the five galaxies with ranging from 24.10 to 27.00 in our sample. For the brightest galaxy J132416.13+274411.6 in our sample (z = 5.70,JAB= 24.10), which has a significantly higher signal to noise, we report a C iii] flux of 3.34 ± 1.81 × 10-18 erg s-1 cm-2 flux of , which places a stringent 3σ upper limit of on C iii] flux and 6.57 Å on the C iii] 2.55 × 10-18 erg s-1 cm-2 equivalent width. Using the stacked image, we put a 3σ upper limit on the mean C iii] flux of and a 3σ upper limit on the mean C iii] equivalent width of 4.20 Å for this sample of galaxies at z = 5.70. Combined with strong C iii] detection reported among high-z galaxies in the literature, our observations suggest that the equivalent widths of C iii] from galaxies at z > 5.70 exhibit a wide range of distribution. Our strong limits on C iii] emission could be used as a guide for future observations in the reionization epoch.

Original languageEnglish (US)
Article numberL22
JournalAstrophysical Journal Letters
Volume838
Issue number2
DOIs
StatePublished - Apr 1 2017

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galaxies
erg
narrowband
time measurement
filter
XMM-Newton telescope
Hubble Space Telescope
newton
cameras
broadband
filters
distribution
detection

Keywords

  • dark ages
  • first stars-galaxies: high-redshift
  • reionization

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Constraining C III] Emission in a Sample of Five Luminous z = 5.7 Galaxies. / Ding, Jiani; Cai, Zheng; Fan, Xiaohui; Stark, Daniel P; Bian, Fuyan; Jiang, Linhua; McGreer, Ian D.; Robertson, Brant E; Siana, Brian.

In: Astrophysical Journal Letters, Vol. 838, No. 2, L22, 01.04.2017.

Research output: Contribution to journalArticle

Ding, Jiani ; Cai, Zheng ; Fan, Xiaohui ; Stark, Daniel P ; Bian, Fuyan ; Jiang, Linhua ; McGreer, Ian D. ; Robertson, Brant E ; Siana, Brian. / Constraining C III] Emission in a Sample of Five Luminous z = 5.7 Galaxies. In: Astrophysical Journal Letters. 2017 ; Vol. 838, No. 2.
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title = "Constraining C III] Emission in a Sample of Five Luminous z = 5.7 Galaxies",
abstract = "Recent observations have suggested that the C iii] emission lines could be alternative diagnostic lines for galaxies in the reionization epoch. We use the F128N narrowband filter on the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) to search for C iii] emission in a sample of five galaxies at z = 5.7 in the Subaru Deep Field and the Subaru/XMM-Newton Deep Field. Using the F128N narrowband imaging, together with the broadband imaging, we do not detect C iii] emission for the five galaxies with ranging from 24.10 to 27.00 in our sample. For the brightest galaxy J132416.13+274411.6 in our sample (z = 5.70,JAB= 24.10), which has a significantly higher signal to noise, we report a C iii] flux of 3.34 ± 1.81 × 10-18 erg s-1 cm-2 flux of , which places a stringent 3σ upper limit of on C iii] flux and 6.57 {\AA} on the C iii] 2.55 × 10-18 erg s-1 cm-2 equivalent width. Using the stacked image, we put a 3σ upper limit on the mean C iii] flux of and a 3σ upper limit on the mean C iii] equivalent width of 4.20 {\AA} for this sample of galaxies at z = 5.70. Combined with strong C iii] detection reported among high-z galaxies in the literature, our observations suggest that the equivalent widths of C iii] from galaxies at z > 5.70 exhibit a wide range of distribution. Our strong limits on C iii] emission could be used as a guide for future observations in the reionization epoch.",
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AU - Bian, Fuyan

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N2 - Recent observations have suggested that the C iii] emission lines could be alternative diagnostic lines for galaxies in the reionization epoch. We use the F128N narrowband filter on the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) to search for C iii] emission in a sample of five galaxies at z = 5.7 in the Subaru Deep Field and the Subaru/XMM-Newton Deep Field. Using the F128N narrowband imaging, together with the broadband imaging, we do not detect C iii] emission for the five galaxies with ranging from 24.10 to 27.00 in our sample. For the brightest galaxy J132416.13+274411.6 in our sample (z = 5.70,JAB= 24.10), which has a significantly higher signal to noise, we report a C iii] flux of 3.34 ± 1.81 × 10-18 erg s-1 cm-2 flux of , which places a stringent 3σ upper limit of on C iii] flux and 6.57 Å on the C iii] 2.55 × 10-18 erg s-1 cm-2 equivalent width. Using the stacked image, we put a 3σ upper limit on the mean C iii] flux of and a 3σ upper limit on the mean C iii] equivalent width of 4.20 Å for this sample of galaxies at z = 5.70. Combined with strong C iii] detection reported among high-z galaxies in the literature, our observations suggest that the equivalent widths of C iii] from galaxies at z > 5.70 exhibit a wide range of distribution. Our strong limits on C iii] emission could be used as a guide for future observations in the reionization epoch.

AB - Recent observations have suggested that the C iii] emission lines could be alternative diagnostic lines for galaxies in the reionization epoch. We use the F128N narrowband filter on the Hubble Space Telescope's (HST) Wide Field Camera 3 (WFC3) to search for C iii] emission in a sample of five galaxies at z = 5.7 in the Subaru Deep Field and the Subaru/XMM-Newton Deep Field. Using the F128N narrowband imaging, together with the broadband imaging, we do not detect C iii] emission for the five galaxies with ranging from 24.10 to 27.00 in our sample. For the brightest galaxy J132416.13+274411.6 in our sample (z = 5.70,JAB= 24.10), which has a significantly higher signal to noise, we report a C iii] flux of 3.34 ± 1.81 × 10-18 erg s-1 cm-2 flux of , which places a stringent 3σ upper limit of on C iii] flux and 6.57 Å on the C iii] 2.55 × 10-18 erg s-1 cm-2 equivalent width. Using the stacked image, we put a 3σ upper limit on the mean C iii] flux of and a 3σ upper limit on the mean C iii] equivalent width of 4.20 Å for this sample of galaxies at z = 5.70. Combined with strong C iii] detection reported among high-z galaxies in the literature, our observations suggest that the equivalent widths of C iii] from galaxies at z > 5.70 exhibit a wide range of distribution. Our strong limits on C iii] emission could be used as a guide for future observations in the reionization epoch.

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