THE HETDEX PILOT SURVEY. II. THE EVOLUTION OF THE Lyα ESCAPE FRACTION FROM THE ULTRAVIOLET SLOPE AND LUMINOSITY FUNCTION OF 1.9 &lt;<i>z</i>&lt; 3.8 LAEs

Blanc, Guillermo A.; Adams, Joshua J.; Gebhardt, Karl; Hill, Gary J.; Drory, Niv; Hao, Lei; Bender, Ralf; Ciardullo, Robin; Finkelstein, Steven L.; Fry, Alexander B.; Gawiser, Eric; Grönwall, C.; Hopp, U.; Jeong, Donghui; Kelzenberg, Ralf; Komatsu, Eiichiro; MacQueen, Phillip J.; Murphy, J.H.; Roth, Martin; Schneider, Donald P.; Tufts, Joseph R.

doi:10.1088/0004-637x/736/1/31

Cited by 173 publications

(288 citation statements)

References 101 publications

(131 reference statements)

Supporting

Mentioning

233

Contrasting

Order By: Relevance

“…As extinction increases the range of the escape fraction decreases. This is similar to the trend seen for Lyα sources at z ∼ 0.1 (Scarlata et al 2009;Atek et al 2009) and z ∼ 3 (Blanc et al 2011). This may indicate that the same physical conditions/processes (such as gas kinematics, H i covering fraction, and/or galaxy morphology) that inhibit and allow for the escape of Lyα photons at low redshift are similarly occurring in high-redshift galaxies too.…”

Section: Estimating the Escape Fractionsupporting

confidence: 88%

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

Section: Estimating the Escape Fractionsupporting

confidence: 88%

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Mallery

Mobasher

Capak

et al. 2012

ApJ

View full text Add to dashboard Cite

show abstract

“…The extinction is likely to be low, however, since it is known to decrease with both decreasing luminosity (Bouwens et al 2009) and increasing Lyα emission Verhamme et al 2008;Hayes et al 2010;Kornei et al 2010;Pentericci et al 2010;Blanc et al 2011).…”

Section: Star Formation Ratesmentioning

confidence: 99%

THE Lyα PROPERTIES OF FAINT GALAXIES ATz∼ 2-3 WITH SYSTEMIC REDSHIFTS AND VELOCITY DISPERSIONS FROM KECK-MOSFIRE

Erb

Steidel

Trainor

et al. 2014

ApJ

190

236

View full text Add to dashboard Cite

We study the Lyα profiles of 36 spectroscopically detected Lyα-emitters (LAEs) at z ∼ 2-3, using Keck MOSFIRE to measure systemic redshifts and velocity dispersions from rest-frame optical nebular emission lines. The sample has a median optical magnitude R = 26.0, and ranges from R 23 to R > 27, corresponding to rest-frame UV absolute magnitudes M UV −22 to M UV > −18.2. Dynamical masses range from M dyn < 1.3 × 10 8 M to M dyn = 6.8 × 10 9 M , with a median value of M dyn = 6.3 × 10 8 M . Thirty of the 36 Lyα emission lines are redshifted with respect to the systemic velocity with at least 1σ significance, and the velocity offset with respect to systemic Δv Lyα is correlated with the R-band magnitude, M UV , and the velocity dispersion measured from nebular emission lines with >3σ significance: brighter galaxies with larger velocity dispersions tend to have larger values of Δv Lyα . We also make use of a comparison sample of 122 UV-color-selected R < 25.5 galaxies at z ∼ 2, all with Lyα emission and systemic redshifts measured from nebular emission lines. Using the combined LAE and comparison samples for a total of 158 individual galaxies, we find that Δv Lyα is anti-correlated with the Lyα equivalent width with 7σ significance. Our results are consistent with a scenario in which the Lyα profile is determined primarily by the properties of the gas near the systemic redshift; in such a scenario, the opacity to Lyα photons in lower mass galaxies may be reduced if large gaseous disks have not yet developed and if the gas is ionized by the harder spectrum of young, low metallicity stars.

show abstract

“…Within the options discussed in this paper, this choice best describes the trend of increasing strength of Lyα with redshift as observed from spectroscopic surveys (e.g. Ando et al 2006;Ouchi et al 2008;Stark et al 2010), other studies (Blanc et al 2011;Hayes et al 2011), and our models that allow for varying Lyα strength ).…”

Section: Evolution Of the Physical Properties From Z ∼ 3 To Z ∼mentioning

confidence: 99%

Properties ofz~ 3–6 Lyman break galaxies

Barros

Schaerer

Stark

2014

A&A

152

205

View full text Add to dashboard Cite

Context. To gain insight on the mass assembly and place constraints on the star formation history (SFH) of Lyman break galaxies (LBGs), it is important to accurately determine their properties. Aims. We estimate how nebular emission and different SFHs affect parameter estimation of LBGs.Methods. We present a homogeneous, detailed analysis of the spectral energy distribution (SED) of ∼1700 LBGs from the GOODS-MUSIC catalogue with deep multi-wavelength photometry from the U band to 8 μm to determine stellar mass, age, dust attenuation, and star formation rate. Using our SED fitting tool, which takes into account nebular emission, we explore a wide parameter space. We also explore a set of different star formation histories. Results. Nebular emission is found to significantly affect the determination of the physical parameters for the majority of z ∼ 3−6 LBGs. We identify two populations of galaxies by determining the importance of the contribution of emission lines to broadband fluxes. We find that ∼65% of LBGs show detectable signs of emission lines, whereas ∼35% show weak or no emission lines. This distribution is found over the entire redshift range. We interpret these groups as actively star-forming and more quiescent LBGs, respectively. We find that it is necessary to considerer SED fits with very young ages (<50 Myr) to reproduce some colours affected by strong emission lines. Other arguments favouring episodic star formation and relatively short star formation timescales are also discussed. Considering nebular emission generally leads to a younger age, lower stellar mass, higher dust attenuation, higher star formation rate, and a large scatter in the SFR-M relation. Our analysis yields a trend of increasing specific star formation rate with redshift, as predicted by recent galaxy evolution models. Conclusions. The physical parameters of approximately two thirds of high redshift galaxies are significantly modified when we account for nebular emission. The SED models, which include nebular emission shed new light on the properties of LBGs with numerous important implications.

show abstract

THE HETDEX PILOT SURVEY. II. THE EVOLUTION OF THE Lyα ESCAPE FRACTION FROM THE ULTRAVIOLET SLOPE AND LUMINOSITY FUNCTION OF 1.9 <z< 3.8 LAEs

Cited by 173 publications

References 101 publications

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

Lyα EMISSION FROM HIGH-REDSHIFT SOURCES IN COSMOS

THE Lyα PROPERTIES OF FAINT GALAXIES ATz∼ 2-3 WITH SYSTEMIC REDSHIFTS AND VELOCITY DISPERSIONS FROM KECK-MOSFIRE

Properties ofz~ 3–6 Lyman break galaxies

Contact Info

Product

Resources

About