An ultraviolet ultra-luminous lyman break galaxy at Z = 2.78 in NDWFS boötes field

Fuyan Bian, Xiaohui Fan, Linhua Jiang, Arjun Dey, Richard F. Green, Roberto Maiolino, Fabian Walter, Ian McGreer, Ran Wang, Yen Ting Lin

Research output: Contribution to journalArticle

7 Citations (Scopus)

Abstract

We present one of the most ultraviolet (UV) luminous Lyman break galaxies (LBGs; J1432+3358) at z = 2.78, discovered in the NOAO Deep Wide-Field Survey Boötes field. The R-band magnitude of J1432+3358 is 22.29AB, more than two magnitudes brighter than typical L* LBGs at this redshift. The deep z-band image reveals two components of J1432+3358 separated by 10 with a flux ratio of 3:1. The high signal-to-noise ratio rest-frame UV spectrum shows Lyα emission line and interstellar medium absorption lines. The absence of N V and C IV emission lines, and the non-detection in X-ray and radio wavelengths and mid-infrared (MIR) colors indicates weak or no active galactic nuclei (<10%) in this galaxy. The galaxy shows a broader line profile, with a FWHM of about 1000kms-1 and a larger outflow velocity (500kms-1) than those of typical z 3 LBGs. The physical properties are derived by fitting the spectral energy distribution (SED) with stellar synthesis models. The dust extinction, E(B - V) = 0.12, is similar to that in normal LBGs. The star formation rates (SFRs) derived from the SED fitting and the dust-corrected UV flux are consistent with each other, 300 M yr-1, and the stellar mass is (1.3 ± 0.3) × 1011 M . The SFR and stellar mass in J1432+3358 are about an order of magnitude higher than those in normal LBGs. The SED-fitting results support that J1432+3358 has a continuous star formation history, with a star formation episode of 6.3 × 108yr. The morphology of J1432+3358 and its physical properties suggest that J1432+3358 is in an early phase of a 3:1 merger process. The unique properties and the low space number density (10 -7Mpc-3) are consistent with the interpretation that such galaxies are either found in a short unobscured phase of the star formation or that a small fraction of intensive star-forming galaxies are unobscured.

Original languageEnglish (US)
Article number139
JournalAstrophysical Journal
Volume757
Issue number2
DOIs
StatePublished - Oct 1 2012

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galaxies
spectral energy distribution
star formation
physical property
dust
energy
star formation rate
stellar mass
signal-to-noise ratio
merger
physical properties
field survey
outflow
extinction
radio
wavelength
ultraviolet spectra
active galactic nuclei
history
signal to noise ratios

Keywords

  • galaxies: high-redshift
  • galaxies: star formation

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

An ultraviolet ultra-luminous lyman break galaxy at Z = 2.78 in NDWFS boötes field. / Bian, Fuyan; Fan, Xiaohui; Jiang, Linhua; Dey, Arjun; Green, Richard F.; Maiolino, Roberto; Walter, Fabian; McGreer, Ian; Wang, Ran; Lin, Yen Ting.

In: Astrophysical Journal, Vol. 757, No. 2, 139, 01.10.2012.

Research output: Contribution to journalArticle

Bian, F, Fan, X, Jiang, L, Dey, A, Green, RF, Maiolino, R, Walter, F, McGreer, I, Wang, R & Lin, YT 2012, 'An ultraviolet ultra-luminous lyman break galaxy at Z = 2.78 in NDWFS boötes field', Astrophysical Journal, vol. 757, no. 2, 139. https://doi.org/10.1088/0004-637X/757/2/139
Bian, Fuyan ; Fan, Xiaohui ; Jiang, Linhua ; Dey, Arjun ; Green, Richard F. ; Maiolino, Roberto ; Walter, Fabian ; McGreer, Ian ; Wang, Ran ; Lin, Yen Ting. / An ultraviolet ultra-luminous lyman break galaxy at Z = 2.78 in NDWFS boötes field. In: Astrophysical Journal. 2012 ; Vol. 757, No. 2.
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abstract = "We present one of the most ultraviolet (UV) luminous Lyman break galaxies (LBGs; J1432+3358) at z = 2.78, discovered in the NOAO Deep Wide-Field Survey Bo{\"o}tes field. The R-band magnitude of J1432+3358 is 22.29AB, more than two magnitudes brighter than typical L* LBGs at this redshift. The deep z-band image reveals two components of J1432+3358 separated by 10 with a flux ratio of 3:1. The high signal-to-noise ratio rest-frame UV spectrum shows Lyα emission line and interstellar medium absorption lines. The absence of N V and C IV emission lines, and the non-detection in X-ray and radio wavelengths and mid-infrared (MIR) colors indicates weak or no active galactic nuclei (<10{\%}) in this galaxy. The galaxy shows a broader line profile, with a FWHM of about 1000kms-1 and a larger outflow velocity (500kms-1) than those of typical z 3 LBGs. The physical properties are derived by fitting the spectral energy distribution (SED) with stellar synthesis models. The dust extinction, E(B - V) = 0.12, is similar to that in normal LBGs. The star formation rates (SFRs) derived from the SED fitting and the dust-corrected UV flux are consistent with each other, 300 M ⊙yr-1, and the stellar mass is (1.3 ± 0.3) × 1011 M ⊙. The SFR and stellar mass in J1432+3358 are about an order of magnitude higher than those in normal LBGs. The SED-fitting results support that J1432+3358 has a continuous star formation history, with a star formation episode of 6.3 × 108yr. The morphology of J1432+3358 and its physical properties suggest that J1432+3358 is in an early phase of a 3:1 merger process. The unique properties and the low space number density (10 -7Mpc-3) are consistent with the interpretation that such galaxies are either found in a short unobscured phase of the star formation or that a small fraction of intensive star-forming galaxies are unobscured.",
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AU - Jiang, Linhua

AU - Dey, Arjun

AU - Green, Richard F.

AU - Maiolino, Roberto

AU - Walter, Fabian

AU - McGreer, Ian

AU - Wang, Ran

AU - Lin, Yen Ting

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N2 - We present one of the most ultraviolet (UV) luminous Lyman break galaxies (LBGs; J1432+3358) at z = 2.78, discovered in the NOAO Deep Wide-Field Survey Boötes field. The R-band magnitude of J1432+3358 is 22.29AB, more than two magnitudes brighter than typical L* LBGs at this redshift. The deep z-band image reveals two components of J1432+3358 separated by 10 with a flux ratio of 3:1. The high signal-to-noise ratio rest-frame UV spectrum shows Lyα emission line and interstellar medium absorption lines. The absence of N V and C IV emission lines, and the non-detection in X-ray and radio wavelengths and mid-infrared (MIR) colors indicates weak or no active galactic nuclei (<10%) in this galaxy. The galaxy shows a broader line profile, with a FWHM of about 1000kms-1 and a larger outflow velocity (500kms-1) than those of typical z 3 LBGs. The physical properties are derived by fitting the spectral energy distribution (SED) with stellar synthesis models. The dust extinction, E(B - V) = 0.12, is similar to that in normal LBGs. The star formation rates (SFRs) derived from the SED fitting and the dust-corrected UV flux are consistent with each other, 300 M ⊙yr-1, and the stellar mass is (1.3 ± 0.3) × 1011 M ⊙. The SFR and stellar mass in J1432+3358 are about an order of magnitude higher than those in normal LBGs. The SED-fitting results support that J1432+3358 has a continuous star formation history, with a star formation episode of 6.3 × 108yr. The morphology of J1432+3358 and its physical properties suggest that J1432+3358 is in an early phase of a 3:1 merger process. The unique properties and the low space number density (10 -7Mpc-3) are consistent with the interpretation that such galaxies are either found in a short unobscured phase of the star formation or that a small fraction of intensive star-forming galaxies are unobscured.

AB - We present one of the most ultraviolet (UV) luminous Lyman break galaxies (LBGs; J1432+3358) at z = 2.78, discovered in the NOAO Deep Wide-Field Survey Boötes field. The R-band magnitude of J1432+3358 is 22.29AB, more than two magnitudes brighter than typical L* LBGs at this redshift. The deep z-band image reveals two components of J1432+3358 separated by 10 with a flux ratio of 3:1. The high signal-to-noise ratio rest-frame UV spectrum shows Lyα emission line and interstellar medium absorption lines. The absence of N V and C IV emission lines, and the non-detection in X-ray and radio wavelengths and mid-infrared (MIR) colors indicates weak or no active galactic nuclei (<10%) in this galaxy. The galaxy shows a broader line profile, with a FWHM of about 1000kms-1 and a larger outflow velocity (500kms-1) than those of typical z 3 LBGs. The physical properties are derived by fitting the spectral energy distribution (SED) with stellar synthesis models. The dust extinction, E(B - V) = 0.12, is similar to that in normal LBGs. The star formation rates (SFRs) derived from the SED fitting and the dust-corrected UV flux are consistent with each other, 300 M ⊙yr-1, and the stellar mass is (1.3 ± 0.3) × 1011 M ⊙. The SFR and stellar mass in J1432+3358 are about an order of magnitude higher than those in normal LBGs. The SED-fitting results support that J1432+3358 has a continuous star formation history, with a star formation episode of 6.3 × 108yr. The morphology of J1432+3358 and its physical properties suggest that J1432+3358 is in an early phase of a 3:1 merger process. The unique properties and the low space number density (10 -7Mpc-3) are consistent with the interpretation that such galaxies are either found in a short unobscured phase of the star formation or that a small fraction of intensive star-forming galaxies are unobscured.

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KW - galaxies: star formation

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