AN ATLAS OF<i>z</i>= 5.7 AND<i>z</i>= 6.5 Lyα EMITTERS,

Hu, E. M.; Cowie, L. L.; Barger, A. J.; Capak, P.; Kakazu, Y.; Trouille, Laura

doi:10.1088/0004-637x/725/1/394

Cited by 220 publications

(393 citation statements)

References 49 publications

Supporting

Mentioning

346

Contrasting

Unclassified

Order By: Relevance

“…The redshifts of the galaxies shown in the left panel of Figure 3 have been compiled from a number of published spectroscopic surveys of the GOODS-N region 20,[31][32][33][34][35][36][37][38] and include new data from ongoing surveys (Stark et al in prep., Stern et al in prep). The redshifts shown in the histogram have primarily been derived from the red-shifted Lyman-Alpha emission line (typically, asymmetric line profiles are seen in the spectra, which add confidence to their high redshift).…”

Section: Supplementary Informationmentioning

confidence: 99%

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Walter

Decarli

Carilli

et al. 2012

Nature

282

348

View full text Add to dashboard Cite

The Hubble Deep Field (HDF) is a region in the sky that provides one of the deepest multi-wavelength views of the distant universe and has led to the detection of thousands of galaxies seen throughout cosmic time 1 . An early map of the HDF at a wavelength of 850 microns that is sensitive to dust emission powered by star formation revealed the brightest source in the field, dubbed HDF850.1 2 . For more than a decade, this source remained elusive and, despite significant efforts, no counterpart at shorter wavelengths, and thus no redshift, size or mass, could be identified 3-7 . Here we report, using a millimeter wave molecular line scan, an unambiguous redshift determination for HDF850.1 of z=5.183. This places HDF850.1 in a galaxy overdensity at z~5.2 in the HDF, corresponding to a cosmic age of only 1.1 Gyr after the Big Bang. This redshift is significantly higher than earlier estimates 3,4,6,8 and higher than most of the >100 sub-millimeter bright galaxies identified to date. The source has a star formation rate of 850 M sun yr -1 and is spatially resolved on scales of 5 kpc, with an implied dynamical mass of ~1.3x10 11 M sun , a significant fraction of which is present in the form of molecular gas. Despite our accurate redshift and position, a counterpart arising from starlight remains elusive.We have obtained a full frequency scan of the 3 mm band towards the HDF using the IRAM Plateau de Bure Interferometer (PdBI). The observations covered the frequency range from 80-115 GHz in 10 frequency settings at uniform sensitivity and at a resolution (~2.3") that is a good match to galaxy sizes at high redshift. They resulted in the detection of two lines of Carbon Monoxide (CO), the most common tracer for molecular gas at high redshift 9 , at 93.20 GHz and 111.84 GHz at the position of HDF850.1. Identifying these lines with the J=5 and J=6 rotational transitions of CO gives a redshift for HDF850.1 of z=5.183. This redshift was then unambiguously confirmed by the PdBI detection of the 158 μm line of ionized carbon ([CII], redshifted to 307.38 GHz), one of the main cooling lines of the star-forming interstellar medium. Stacking of other molecules covered by our frequency scan that trace higher volume densities did not lead to a detection (see Supplementary Information). Subsequently, the J=2 line of CO has also been detected using the NRAO Jansky Very Large Array (Jansky VLA) at 37.29 GHz. The observed [CII] and CO spectra towards HDF850.1 are shown in Fig. 1.The beamsize of our CO observations (~2.3", 15 kpc at z=5.183) is too large to spatially resolve the molecular gas emission in HDF850.1. However the [CII] and underlying continuum observations (~1.2" x 0.8") show that the source is extended (hitherto, the interstellar medium has been spatially resolved only in extremely rare quasar host galaxies at such high redshift 10 ). A single Gaussian fit yields a deconvolved size of 0.9±0.3", or 5.7±1.9 kpc at the redshift of the source. Fig. 2 shows the maps of total [CII] emission (left) as well as the red-and blue-...

show abstract

Section: Supplementary Informationmentioning

confidence: 99%

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Walter

Decarli

Carilli

et al. 2012

Nature

282

348

View full text Add to dashboard Cite

show abstract

“…In addition, Lyα emitters were selected using the IA624, NB711, and NB816 bands following previous studies (C. Scarlata et al 2012, in preparation;Shioya et al 2009;Murayama et al 2007), with the modification that a fixed color cut was used to the faintest magnitudes as done in Hu et al (2010) instead of a noise adjusted cut. To the NB711 sources selected by the Shioya et al (2009) criteria, sources were also added with 0.3 mag excess between the NB711 and the interpolated r + i + photometry, and also sources with a 0.3 mag excess between the NB711 and interpolated IA707 and IA738 magnitudes in order to add sources possibly having lower Lyα equivalent widths (EWs) than the Shioya et al (2009) selection criteria.…”

Section: Source Selectionmentioning

confidence: 99%

“…The Lyα luminosity function of these sources increases with redshift, indicating that galaxies with Lyα emission are more common at higher redshifts. Hu et al (2010) presented an atlas of 88 z ∼ 5.7 and 30 z ∼ 6.5 spectroscopically confirmed LAEs. Ouchi et al (2010) presented spectra of LAEs at z ∼ 6.6 examining the Lyα line profiles, the luminosity function, and clustering properties of the sources.…”

Section: Introductionmentioning

confidence: 99%

“…The study of the high-redshift universe and the early evolution of galaxies has primarily relied on two techniques to obtain large samples of high-redshift galaxies, the Lyman break technique (LBGs; Steidel et al 1999;Ouchi et al 2004;Bouwens & Illingworth 2006, and references therein) and narrowband surveys targeting Lyα emitting galaxies (LAEs; Hu & McMahon 1996;Rhoads & Malhotra 2001;Ajiki et al 2003;Hu et al 2004Hu et al , 2010Taniguchi et al 2005;Murayama et al 2007;Gronwall et al 2007;Ouchi et al 2008, and references therein). Studying the difference in the nature and properties of the two populations, selected by these two techniques, helps to understand early stages of galaxy formation and provides constraints on reionization.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Mallery

Mobasher

Capak

et al. 2012

ApJ

View full text Add to dashboard Cite

We investigate spectroscopically measured Lyα equivalent widths (EWs) and escape fractions of 244 sources of which 95 are Lyman break galaxies (LBGs) and 106 Lyman alpha emitters (LAEs) at z ∼ 4.2, z ∼ 4.8, and z ∼ 5.6 selected from intermediate and narrowband observations. The sources were selected from the Cosmic Evolution Survey and observed with the DEIMOS spectrograph. We find that the distribution of EWs shows no evolution with redshift for both the LBG selected sources and the intermediate/narrowband LAEs. We also find that the Lyα escape fraction of intermediate/narrowband LAEs is on average higher and has a larger variation than the escape fraction of LBG selected sources. The escape fraction does not show a dependence with redshift. Similar to what has been found for LAEs at low redshifts, the sources with the highest extinctions show the lowest escape fractions. The range of escape fractions increases with decreasing extinction. This is evidence that the dust extinction is the most important factor affecting the escape of Lyα photons, but at low extinctions other factors, such as the H i covering fraction and gas kinematics, can be just as effective at inhibiting the escape of Lyα photons.

show abstract

“…As seen from this equation, even a neutral hydrogen fraction as low as 10 −5 can lead to a significant attenuation of Lyα photons at high-z , making them extremely sensitive probes of H I in the IGM. As a result, a class of high-z galaxies called Lyman Alpha Emitters (LAEs), detected by means of their Lyα line (at 1216Å in the rest frame), have become popular probes of reionization, with statistically significant samples available in the reionization epoch, at z 5.7 and 6.6 (Malhotra et al 2005;Taniguchi et al 2005;Shimasaku et al 2006;Hu et al 2010;Kashikawa et al 2006;Ouchi et al 2010;Kashikawa et al 2011). Indeed, a number of theoretical papers have used semi-analytic (e.g.…”

Section: Introductionmentioning

confidence: 99%

Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

Hutter

Dayal

Müller

2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We calculate Lyman Alpha Emitter (LAE) angular correlation functions (ACFs) at z 6.6 and the fraction of lifetime (for the 100 Myrs preceding z 6.6) galaxies spend as Lyman Break Galaxies (LBGs) or as LBGs with Lyman Alpha (Lyα) emission using a model that combines SPH cosmological simulations (GADGET-2), dust attenuation and a radiative transfer code (pCRASH). The ACFs are a powerful tool that significantly narrows the 3D parameter space allowed by LAE Lyα and UV luminosity functions (LFs) alone. With this work, we simultaneously constrain the escape fraction of ionizing photons f esc = 0.05 − 0.5, the mean fraction of neutral hydrogen in the intergalactic medium (IGM) χ HI < ∼ 0.01 and the dust-dependent ratio of the escape fractions of Lyα and UV continuum photons f α /f c = 0.6 − 1.2. Our results show that reionization has the largest impact on the amplitude of the ACFs, and its imprints are clearly distinguishable from those of f esc and f α /f c . We also show that galaxies with a critical stellar mass of M * = 10 8.5 (10 9.5 )M produce enough luminosity to stay visible as LBGs (LAEs). Finally, the fraction of time during the past 100 Myrs prior to z = 6.6 a galaxy spends as a LBG or as a LBG with Lyα emission increases with the UV magnitude (and the stellar mass M * ): considering observed (dust and IGM attenuated) luminosities, the fraction of time a galaxy spends as a LBG (LAE) increases from 65% to 100% ( 0 − 100%) as M U V decreases from M U V = −18.0 to −23.5 (M * increases from 10 8 − 10 10.5 M ). Thus in our model the brightest (most massive) LBGs most often show Lyα emission.

show abstract

AN ATLAS OFz= 5.7 ANDz= 6.5 Lyα EMITTERS,

Cited by 220 publications

References 49 publications

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

The intense starburst HDF 850.1 in a galaxy overdensity at z ≈ 5.2 in the Hubble Deep Field

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Clustering and lifetime of Lyman Alpha Emitters in the Epoch of Reionization

Contact Info

Product

Resources

About