Texas Spectroscopic Search for Lyα Emission at the End of Reionization. II. The Deepest Near-infrared Spectroscopic Observation at z ≳ 7

Jung, Intae; Finkelstein, Steven L.; Dickinson, Mark; Hutchison, Taylor A.; Larson, Rebecca L.; Papovich, Casey; Pentericci, L.; Song, Mimi; Ferguson, Harry; Guo, Y.; Malhotra, Sangeeta; Mobasher, Bahram; Rhoads, James E.; Tilvi, Vithal; Wold, Isak

doi:10.3847/1538-4357/ab1bde

Cited by 26 publications

(35 citation statements)

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“…Along with this theoretical expectation, recent observational studies reveal this asymmetric shape of a Lyα emission line at z > 7 from their deep spectroscopic observations (Oesch et al 2015;Song et al 2016a;Jung et al 2019;Tilvi et al 2020) while Pentericci et al (2018a) report an asymmetric Lyα line profile from their stacked analysis of Lyα emission lines at z ∼ 7. However, the occurrence of double-peaked Lyα emission has been also reported at these redshifts up to z 6 (Hu et al 2016;Matthee et al 2018;Songaila et al 2018;Bosman et al 2020).…”

Section: Asymmetric Line Profile Of Lyα Emissionmentioning

confidence: 69%

“…Our spectroscopic data were obtained through a total of 18 nights of spectroscopic observations in the GOODS fields with Keck/DEIMOS (PI: R. Livermore, published in Jung et al 2018) and Keck/MOSFIRE (the majority awarded through the NASA/Keck allocation; PI: S. Finkelstein). The GOODS-S MOSFIRE observations were published in Song et al (2016a), and Jung et al (2019) published the deepest (>16hr) MOSFIRE dataset in GOODS-N.…”

Section: Texas Spectroscopic Search For Lyα Emission At the End Of Rementioning

confidence: 99%

“…25). The details of the observations are described in Table 1 of Jung et al (2019). Table 3 in the Appendix shows the list of the spectroscopic targets in our GOODS-N MOSFIRE observations.…”

Section: Mosfire Y -Band Observations In Goods-nmentioning

confidence: 99%

“…Thanks to our deep spectroscopic observations along with Song et al (2016a) and Jung et al (2019), the analysis of the Lyα line profile is feasible for multiple sources. In Table 1, we present the measured asymmetry (σ red /σ blue ) of the detected Lyα line profiles in the last column.…”

Section: Asymmetric Line Profile Of Lyα Emissionmentioning

confidence: 99%

“…Over the past decade, multi-object spectroscopic observations with large ground-based telescopes (e.g., Keck/DEIMOS, Keck/MOSFIRE, VLT/FORS2, VLT/KMOS, VLT/MUSE) have delivered a number of confirmed Lyα emitters at/around the end of reionization (e.g., Finkelstein et al 2013;Schenker et al 2014;Tilvi et al 2014;Oesch et al 2015;Zitrin et al 2015;Song et al 2016a;Herenz et al 2017;Hoag et al 2017;Laporte et al 2017;Stark et al 2017;Jung et al 2018Jung et al , 2019Pentericci et al 2018a;Mason et al 2019;Khusanova et al 2020). Initial studies of the simple "Lyα fraction" (= N LAE /N LBG ), where N LAE is the number of Lyα-detected objects and N LBG is the number of high-z candidate galaxies observed in spectroscopic observations, have found an apparent deficit of Lyα emission at z > 6.5 (e.g., Fontana et al 2010;Pentericci et al 2011Pentericci et al , 2018a, implying an increasing H I fraction in the IGM from z ∼ 6 → 7, although other Lyα systematics with galaxy evolutionary features need to be taken into account (e.g., Yang et al 2017a;Du et al 2020;Tang et al 2019;Trainor et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Texas Spectroscopic Search for Lyα Emission at the End of Reionization I. Constraining the Lyα Equivalent-width Distribution at 6.0 < z < 7.0

Jung

Finkelstein

Livermore

et al. 2018

ApJ

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The distribution of Lyα emission is an presently accessible method for studying the state of the intergalactic medium (IGM) into the reionization era. We carried out deep spectroscopic observations in order to search for Lyα emission from galaxies with photometric redshifts z = 5.5−8.3 selected from the Cosmic Assembly Nearinfrared Deep Extragalactic Legacy Survey (CANDELS). Utilizing data from the Keck/DEIMOS spectrograph, we explore a wavelength coverage of Lyα emission at z ∼ 5 − 7 with four nights of spectroscopic observations for 118 galaxies, detecting five emission lines with ∼ 5σ significance: three in the GOODS-N and two in the GOODS-S field. We constrain the equivalent width (EW) distribution of Lyα emission by comparing the number of detected objects with the expected number constructed from detailed simulations of mock emission lines that account for the observational conditions (e.g., exposure time, wavelength coverage, and sky emission) and galaxy photometric redshift probability distribution functions. The Lyα EW distribution is well described by an exponential form, dN/dEW ∝ exp(-EW/W 0 ), characterized by the e-folding scale (W 0 ) of ∼ 60 − 100Å at 0.3 < z < 6. By contrast, our measure of the Lyα EW distribution at 6.0 < z < 7.0 rejects a Lyα EW distribution with W 0 > 36.4Å (125.3Å) at 1σ (2σ) significance. This provides additional evidence that the EW distribution of Lyα declines at z > 6, suggesting an increasing fraction of neutral hydrogen in the IGM at that epoch.

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Section: Asymmetric Line Profile Of Lyα Emissionmentioning

confidence: 69%

Section: Texas Spectroscopic Search For Lyα Emission At the End Of Rementioning

confidence: 99%

Section: Mosfire Y -Band Observations In Goods-nmentioning

confidence: 99%

Section: Asymmetric Line Profile Of Lyα Emissionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Texas Spectroscopic Search for Lyα Emission at the End of Reionization I. Constraining the Lyα Equivalent-width Distribution at 6.0 < z < 7.0

Jung

Finkelstein

Livermore

et al. 2018

ApJ

Self Cite

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Exploration of the high-redshift universe enabled by THESEUS

et al. 2021

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At peak, long-duration gamma-ray bursts are the most luminous sources of electromagnetic radiation known. Since their progenitors are massive stars, they provide a tracer of star formation and star-forming galaxies over the whole of cosmic history. Their bright power-law afterglows provide ideal backlights for absorption studies of the interstellar and intergalactic medium back to the reionization era. The proposed THESEUS mission is designed to detect large samples of GRBs at z > 6 in the 2030s, at a time when supporting observations with major next generation facilities will be possible, thus enabling a range of transformative science. THESEUS will allow us to explore the faint end of the luminosity function of galaxies and the star formation rate density to high redshifts; constrain the progress of re-ionisation beyond $z\gtrsim 6$ z ≳ 6 ; study in detail early chemical enrichment from stellar explosions, including signatures of Population III stars; and potentially characterize the dark energy equation of state at the highest redshifts.

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Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy

Álvarez-Márquez

Colina

Marques-Chaves

et al. 2019

A&A

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The James Webb Space Telescope (JWST) will provide deep imaging and spectroscopy for sources at redshifts above 6, covering the entire Epoch of Reionization (EoR, 6< z <10), and enabling the detailed exploration of the nature of the different sources during the first 1 Gyr of the history of the Universe. The Medium Resolution Spectrograph (MRS) of the mid-IR Instrument (MIRI) will be the only instrument on board JWST able to observe the brightest optical emission lines Hα and [OIII]0.5007µm at redshifts above 7 and 9, respectively, providing key insights into the physical properties of sources during the early phases of the EoR. This paper presents a study of the Hα fluxes predicted by state-of-the-art FIRSTLIGHT cosmological simulations for galaxies at redshifts of 6.5 to 10.5, and its detectability with MIRI. Deep (40 ksec) spectroscopic integrations with MRS will be able to detect (S/N > 5) EoR sources at redshifts above 7 with intrinsic star formation rates (SFR) of more than 2 M yr −1 , and stellar masses above 4-9 × 10 7 M . These limits cover the upper end of the SFR and stellar mass distribution at those redshifts, representing ∼ 6% and ∼1% of the predicted FIRSTLIGHT population at the 6.5-7.5 and 7.5-8.5 redshift ranges, respectively. In addition, the paper presents realistic MRS simulated observations of the expected rest-frame optical and near-infrared spectra for some spectroscopically confirmed EoR sources recently detected by ALMA as [OIII]88µm emitters. The MRS simulated spectra cover a wide range of low metallicities from about 0.2 to 0.02 Z , and different [OIII]88µm/[OIII]0.5007µm line ratios. The simulated 10ks MRS spectra show S/N in the range of 5 to 90 for Hβ, [OIII]0.4959,0.5007 µm, Hα and HeI1.083µm emission lines of the currently highest spectroscopically confirmed EoR (lensed) source MACS1149-JD1 at a redshift of 9.11, independent of metallicity. In addition, deep 40 ksec simulated spectra of the luminous merger candidate B14-65666 at 7.15 shows the MRS capabilities of detecting, or putting strong upper limits on, the weak [NII]0.6584µm, [SII]0.6717,0.6731µm, and [SIII]0.9069,0.9532µm emission lines. These observations will provide the opportunity of deriving accurate metallicities in bright EoR sources using the full range of rest-frame optical emission lines up to 1µm. In summary, MRS will enable the detailed study of key physical properties such as internal extinction, instantaneous star formation, hardness of the ionizing continuum, and metallicity in bright (intrinsic or lensed) EoR sources.

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Texas Spectroscopic Search for Lyα Emission at the End of Reionization. II. The Deepest Near-infrared Spectroscopic Observation at z ≳ 7

Cited by 26 publications

References 100 publications

Texas Spectroscopic Search for Lyα Emission at the End of Reionization I. Constraining the Lyα Equivalent-width Distribution at 6.0 < z < 7.0

Texas Spectroscopic Search for Lyα Emission at the End of Reionization I. Constraining the Lyα Equivalent-width Distribution at 6.0 < z < 7.0

Exploration of the high-redshift universe enabled by THESEUS

Investigating the physical properties of galaxies in the Epoch of Reionization with MIRI/JWST spectroscopy

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