THE EVOLUTION OF Lyα-EMITTING GALAXIES BETWEEN<i>z</i>= 2.1 AND<i>z</i>= 3.1

Ciardullo, Robin; Grönwall, C.; Wolf, Christopher A.; McCathran, Emily; Bond, Nicholas A.; Gawiser, Eric; Guaita, L.; Feldmeier, John J.; Treister, Ezequiel; Padilla, Nelson; Francke, Harold; Matkovic, Ana; Altmann, M.; Herrera, David

doi:10.1088/0004-637x/744/2/110

Cited by 118 publications

(221 citation statements)

References 66 publications

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“…These are the ideal samples to constrain any evolution (or lack thereof) between redshifts of z 3.1 and z 2.1. Ciardullo et al (2012) found z 3.1 LAEs with luminosities brighter than L(Lyα) > 10 42.4 erg s −1 had almost twice the number density of z 2.1 LAEs in the Extended Chandra Deep Field South. Also, the number of galaxies with EW(Lyα) > 100 Å at z 3.1 was almost twice the number at z 2.1.…”

Section: Introductionmentioning

confidence: 84%

Magellan/MMIRS near-infrared multi-object spectroscopy of nebular emission from star-forming galaxies at 2 <z< 3

Guaita¹,

Francke²,

Gawiser³

et al. 2013

A&A

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Aims. To investigate the ingredients, which allow star-forming galaxies to present Lyα line in emission, we studied the kinematics and gas phase metallicity of the interstellar medium. Methods. We used multi-object near-infrared spectroscopy with Magellan/MMIRS to study nebular emission from z 2−3 starforming galaxies discovered in three MUSYC fields. Results. We detected emission lines from four active galactic nuclei and 13 high-redshift star-forming galaxies, including Hα lines down to a flux of (4 ± 1)E-17 erg s −1 cm −2 . This yielded seven new redshifts. The most common emission line detected is [OIII]5007, which is sensitive to metallicity. We were able to measure metallicity (Z) for two galaxies and to set upper (lower) limits for another two (two). The metallicity values are consistent with 0.3 < Z/Z < 1.2, 12 + log (O/H) ∼ 8.2−8.8. Comparing the Lyα central wavelength with the systemic redshift, we find ∆v Lyα−[OIII]5007 = 70−270 km s −1 . Conclusions. High-redshift star-forming galaxies, Lyα emitting (LAE) galaxies, and Hα emitters appear to be located in the low mass, high star-formation rate (SFR) region of the SFR versus stellar mass diagram, confirming that they are experiencing burst episodes of star formation, which are building up their stellar mass. Their metallicities are consistent with the relation found for z ≤ 2.2 galaxies in the Z versus stellar mass plane. The measured ∆v Lyα−[OIII]5007 values imply that outflows of material, driven by star formation, could be present in the z ∼ 2−3 LAEs of our sample. Comparing with the literature, we note that galaxies with lower metallicity than ours are also characterized by similar ∆v Lyα−[OIII]5007 velocity offsets. Strong F([OIII]5007) is detected in many Lyα emitters. Therefore, we propose the F(Lyα)/F([OIII]5007) flux ratio as a tool for the study of high-redshift galaxies; while influenced by metallicity, ionization, and Lyα radiative transfer in the ISM, it may be possible to calibrate this ratio to primarily trace one of these effects.

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Section: Introductionmentioning

confidence: 84%

Magellan/MMIRS near-infrared multi-object spectroscopy of nebular emission from star-forming galaxies at 2 <z< 3

Guaita¹,

Francke²,

Gawiser³

et al. 2013

A&A

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“…To correct for these missing objects, one must estimate the total amount of emission associated with low-equivalent width galaxies. If the equivalent width distribution of such objects follows the exponential function defined by the higher EW LAEs, then our census may be missing between 20% and 30% of escaping Lyα photons (Ciardullo et al 2012;C. Gronwall et al 2014, in preparation).…”

Section: The Lyα Luminosity Function and F Lyα Escmentioning

confidence: 97%

“…To improve upon this situation, we have combined the data from four recent surveys: 3D-HST and AGHAST (Brammer et al 2012;Weiner & the AGHAST Team 2014), the Pilot Survey for HETDEX, the Hobby-Eberly Telescope Dark Energy Experiment (HPS; Adams et al 2011), and the 3727 Å narrowband observations of the Chandra Deep Field South (CDF-S; Guaita et al 2010;Ciardullo et al 2012). The first two of these studies unambiguously measures total Hβ fluxes in the redshift range 1.90 < z < 2.35 via Wide Field Camera 3 (WFC3) grism observations with the Hubble Space Telescope (HST); the latter two provide Lyα measurements (or upper limits) for many of these same galaxies via integral field spectroscopy and narrow-band imaging.…”

Section: Introductionmentioning

confidence: 99%

HUBBLE SPACE TELESCOPEEMISSION LINE GALAXIES ATz∼ 2: THE Lyα ESCAPE FRACTION

Ciardullo

Zeimann

Grönwall

et al. 2014

ApJ

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We compare the Hβ line strengths of 1.90 < z < 2.35 star-forming galaxies observed with the near-IR grism of the Hubble Space Telescope with ground-based measurements of Lyα from the HETDEX Pilot Survey and narrow-band imaging. By examining the line ratios of 73 galaxies, we show that most star-forming systems at this epoch have a Lyα escape fraction below ∼6%. We confirm this result by using stellar reddening to estimate the effective logarithmic extinction of the Hβ emission line (c Hβ = 0.5) and measuring both the Hβ and Lyα luminosity functions in a ∼100,000 Mpc 3 volume of space. We show that in our redshift window, the volumetric Lyα escape fraction is at most 4.4 +2.1 −1.2 %, with an additional systematic ∼25% uncertainty associated with our estimate of extinction. Finally, we demonstrate that the bulk of the epoch's star-forming galaxies have Lyα emission line optical depths that are significantly greater than that for the underlying UV continuum. In our predominantly [O iii] λ5007-selected sample of galaxies, resonant scattering must be important for the escape of Lyα photons.

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“…In addition, the depth of the narrowband (NB) imaging should reach NB ∼ 25 ( ( ) ( ) * a ã L L Ly Ly ) at z∼3 (Ciardullo et al 2012). Ideally, sufficiently wide field cameras with fields of view of 30′ are preferred for conducting the imaging observations to quantify the galaxy overdensity on 20 h −1 Mpc.…”

Section: A4 Requirements For Imaging Follow-up Cosla Candidatesmentioning

confidence: 99%

Mapping the Most Massive Overdensity Through Hydrogen (Mammoth). I. Methodology

Cai

Fan

Peirani

et al. 2016

ApJ

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Modern cosmology predicts that a galaxy overdensity (e.g., protocluster) will be associated with a large intergalactic medium gas reservoir, which can be traced by Lyα forest absorption. We have undertaken a systematic study of the relation between Coherently Strong intergalactic Lyα Absorption systems (CoSLAs), which have the highest optical depth (τ) in the τ distribution, and mass overdensities on the scales of ∼10-20 h −1 comoving Mpc. On such large scales, our cosmological simulations show a strong correlation between the effective optical depth (τ eff ) of the CoSLAs and the three-dimensional mass overdensity. In spectra with moderate signal-tonoise ratio, however, the profiles of CoSLAs can be confused with individual high column density absorbers. For z>2.6, where the corresponding Lyβ is redshifted to the optical, we have developed a selection technique to distinguish between these two alternatives. We have applied this technique to ∼6000 sight lines provided by Sloan Digital Sky Survey III quasar survey at z = 2.6-3.3 with a continuum-to-noise ratio greater than 8, and we present a sample of five CoSLA candidates with τ eff on 15 h −1 Mpc greater than 4.5× the mean optical depth. At lower redshifts of z<2.6, where the background quasar density is higher, the overdensity can be traced by intergalactic absorption groups using multiple sight lines with small angular separations. Our overdensity searches fully use the current and next generation of Lyα forest surveys, which cover a survey volume of >1 (h −1 Gpc) 3 . Systems traced by CoSLAs will yield a uniform sample of the most massive overdensities at z>2 to provide stringent constraints to models of structure formation.

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THE EVOLUTION OF Lyα-EMITTING GALAXIES BETWEENz= 2.1 ANDz= 3.1

Cited by 118 publications

References 66 publications

Magellan/MMIRS near-infrared multi-object spectroscopy of nebular emission from star-forming galaxies at 2 <z< 3

Magellan/MMIRS near-infrared multi-object spectroscopy of nebular emission from star-forming galaxies at 2 <z< 3

HUBBLE SPACE TELESCOPEEMISSION LINE GALAXIES ATz∼ 2: THE Lyα ESCAPE FRACTION

Mapping the Most Massive Overdensity Through Hydrogen (Mammoth). I. Methodology

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