FIRST SPECTROSCOPIC MEASUREMENTS OF [O III] EMISSION FROM Lyα SELECTED FIELD GALAXIES AT<i>z</i>∼ 3.1

McLinden, Emily; Finkelstein, Steven L.; Rhoads, James E.; Malhotra, Sangeeta; Hibon, Pascale; Richardson, Mark L. A.; Cresci, G.; Quirrenbach, A.; Pasquali, A.; Bian, Fuyan; Fan, Xiaohui; Woodward, C. E.

doi:10.1088/0004-637x/730/2/136

Cited by 110 publications

(135 citation statements)

References 80 publications

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“…For the other three LAEs at z ∼ 2−3 (star symbols), the offsets are 70−270 km s −1 . These values are consistent with previous estimations from McLinden et al (2011) and updated by Chonis et al, priv. comm.).…”

Section: Lyα Emitter Ism Propertiessupporting

confidence: 93%

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: Lyα Emitter Ism Propertiessupporting

confidence: 93%

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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“…The ∆v Lyα,r value has been measured in more than 60 LAEs (McLinden et al 2011;Finkelstein et al 2011;Hashimoto et al 2013;Guaita et al 2013;Chonis et al 2013;Shibuya et al 2014b;Song et al 2014;Erb et al 2014). These studies have shown that LAEs at z ∼ 2 − 3 have a mean ∆v Lyα,r of ≃ 200 km s −1 , which is significantly smaller than that of LBGs at a similar redshift, ∆v Lyα,r ≃ 400 km s −1 (e.g., Steidel et al 2010;Rakic et al 2011;Kulas et al 2012).…”

Section: Lyα Main Red Peak Velocity Offsets ∆Vlyαrmentioning

confidence: 99%

A CLOSE COMPARISON BETWEEN OBSERVED AND MODELED LyαLINES FORz∼ 2.2 LyαEMITTERS

Hashimoto

Verhamme

Ouchi

et al. 2015

ApJ

115

137

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We present the results of a Lyα profile analysis of 12 Lyα emitters (LAEs) at z ∼ 2.2 with highresolution Lyα spectra. We find that all 12 objects have a Lyα profile with the main peak redward of the systemic redshift defined by nebular lines, and five have a weak, secondary peak blueward of the systemic redshift (blue bump). The average velocity offset of the red main peak (the blue bump, if any) with respect to the systemic redshift is ∆v Lyα,r = 174±19 km s −1 (∆v Lyα,b = −316±45 km s −1 ), which is smaller than (comparable to) that of Lyman-break galaxies (LBGs). The outflow velocities inferred from metal absorption lines in three individual and one stacked spectra are comparable to those of LBGs. The uniform expanding shell model constructed by Verhamme et al. (2006) reproduces not only the Lyα profiles but also other observed quantities including the outflow velocity and the FWHM of nebular lines for the non-blue bump objects. On the other hand, the model predicts too high FWHMs of nebular lines for the blue bump objects, although this discrepancy may disappear if we introduce additional Lyα photons produced by gravitational cooling. We show that the small ∆v Lyα,r values of our sample can be explained by low neutral-hydrogen column densities of log(N HI ) = 18.9 cm −2 on average. This value is more than one order of magnitude lower than those of LBGs but is consistent with recent findings that LAEs have high ionization parameters and low Hi gas masses. This result suggests that low N HI values, giving reduced numbers of resonant scattering of Lyα photons, are the key to the strong Lyα emission of LAEs.

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“…In starburst galaxies, the width of the intrinsic Lyα line is lower than 100 km s −1 (Teplitz et al 2000;Baker et al 2004;Erb et al 2003;McLinden et al 2011), which implies an expansion velocity v exp lower than 200 km s −1 in the ISM. We illustrate this limit in Fig.…”

Section: Physical Conditions Needed In the Ismmentioning

confidence: 99%

Lymanαline and continuum radiative transfer in a clumpy interstellar medium

Duval

Schaerer

Östlin

et al. 2014

A&A

108

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Aims. Studying the effects of an inhomogeneous interstellar medium (ISM) on the strength and the shape of the Lyman alpha (Lyα) line in starburst galaxies. Methods. Using our 3D Monte Carlo Lyα radiation transfer code, we study the radiative transfer of Lyα, UV and optical continuum photons in homogeneous and clumpy shells of neutral hydrogen and dust surrounding a central source. Our simulations predict the Lyα and continuum escape fraction, the Lyα equivalent width EW(Lyα), and the Lyα line profile, and their dependence on the geometry of the gas distribution and the main input physical parameters. Results. The ISM clumpiness is found to have a strong impact on the Lyα line radiative transfer, entailing a strong dependence of the emergent features of the Lyα line (escape fraction, EW(Lyα)) on the ISM morphology. Although a clumpy and dusty ISM appears more transparent to radiation (both line and continuum) compared to an equivalent homogeneous ISM of equal dust optical depth, we find that the Lyα photons are, in general, still more attenuated than UV continuum radiation. As a consequence, the observed equivalent width of the Lyα line (EW obs (Lyα)) is lower than the intrinsic one (EWint(Lyα)) for nearly all clumpy ISM configurations considered. There are, however, special conditions under which Lyα photons escape more easily than the continuum, resulting in an enhanced EW obs (Lyα). The requirement for this to happen is that the ISM is almost static (galactic outflows ≤ 200 km s −1 ), extremely clumpy (with density contrasts > 10 7 in HI between clumps and the interclump medium), and very dusty (E(B-V) > 0.30). When these conditions are fulfilled the emergent Lyα line profile generally shows no velocity shift and little asymmetry. Otherwise the Lyα line profile is very similar to that expected for homogeneous media. Conclusions. Given the asymmetry and velocity shifts generally observed in star-forming galaxies with Lyα emission, we therefore conclude that clumping is unlikely to significantly enhance their relative Lyα/UV transmission.

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FIRST SPECTROSCOPIC MEASUREMENTS OF [O III] EMISSION FROM Lyα SELECTED FIELD GALAXIES ATz∼ 3.1

Cited by 110 publications

References 80 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

A CLOSE COMPARISON BETWEEN OBSERVED AND MODELED LyαLINES FORz∼ 2.2 LyαEMITTERS

Lymanαline and continuum radiative transfer in a clumpy interstellar medium

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