EVOLUTION IN THE CONTINUUM MORPHOLOGICAL PROPERTIES OF Lyα-EMITTING GALAXIES FROM<i>z</i>= 3.1 TO<i>z</i>= 2.1

Bond, Nicholas A.; Gawiser, Eric; Guaita, L.; Padilla, Nelson; Grönwall, C.; Ciardullo, Robin; Lai, Kamson

doi:10.1088/0004-637x/753/2/95

Cited by 39 publications

(91 citation statements)

References 65 publications

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“…Their stellar mass tend to be larger than LAEs, consistent with LBAs and LBGs. However, there is an overlap in stellar mass between LARS-LAEs (M * < 10 10 M ) and the most massive LAEs in the sample of Bond et al (2012). Also, LARS galaxies are less massive than cSFGs.…”

Section: Lars Galaxies At Z ∼mentioning

confidence: 92%

“…As LARS Lyα and Hα(rest-UV and optical continua) images are in units of flux(flux density), the image depths are given in units of erg s −1 cm −2 (AB magnitudes). The MUSYC (Guaita et al 2010;Bond et al 2012) NB3727 survey implied a 10σ detection limit of F(Lyα) = 5E-17 erg s −1 cm −2 . MUSYC U,B (HUDF V606) 10σ detection limits were about 26(29.5).…”

Section: High-redshift Simulationmentioning

confidence: 99%

“…To choose reasonable ranges of detection limits (Table 1) to apply, we referred to the MUlti-wavelength Survey by Yale-Chile (MUSYC) NB3727 narrow band (Guaita et al 2010;Bond et al 2012), to the triple narrow band by Nakajima et al (2012), CANDELS/HUDF (McLure et al 2013) broad band, and to the dual narrow-band survey by Lee et al (2012).…”

Section: High-redshift Simulationmentioning

confidence: 99%

“…-Narrow-band selected Lyman alpha emitters at z 2.07 and z 3.1 (Bond et al 2009(Bond et al , 2012 belonging to the MUSYC survey. We considered the stack of the z ∼ 2.07 entire sample and of subsamples separated by photometric properties, UV-faint(UV-bright) with R > 25.5(<25.5), IRAC-faint(IRAC-bright) with f 3.6 μm < 0.57(>0.57) μJ, low-(high-)EW with EW(Lyα) < 66(>66) Å, red-(blue-)LAE with B − R > 0.5(<0.5) (Guaita et al 2011).…”

Section: Lars Galaxies At Z ∼mentioning

confidence: 99%

“…From the ground LAEs were observed to be compact in the rest-frame UV, but multiple components were identified in deep HST-resolution images (Bond et al 2009(Bond et al , 2012. There have also been a few attempts to quantify the morphology of the Lyα emission itself.…”

Section: Introductionmentioning

confidence: 99%

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The Lyman alpha reference sample

Guaita

Melinder

Hayes

et al. 2015

A&A

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Context. The transport of Lyα photons in galaxies is a complex process and the conditions under which Lyα photons manage to escape from certain galaxies is still under investigation. The Lyman alpha reference sample (LARS) is a sample of 14 local starforming galaxies, designed to study Lyα in detail and relate it to rest-frame UV and optical emission. Aims. With the aim of identifying rest-frame UV and optical properties, which are typical of Lyα emitters (LAEs, galaxies with EW(Lyα) > 20 Å) at both low and high redshift, we investigated the morphological properties of the LARS galaxies, in particular the ones that exhibit intense Lyα radiation. Methods. We measured sizes and morphological parameters in the continuum, Lyα, and Hα images. We studied morphology by using the Gini coefficient vs. M20 and asymmetry vs. concentration diagrams. We then simulated LARS galaxies at z ∼ 2 and 5.7, performing the same morphological measurements. We also investigated the detectability of LARS galaxies in current deep field observations. The subsample of LAEs within LARS (LARS-LAEs) was stacked to provide a comparison to stacking studies performed at high redshift. Results. LARS galaxies have continuum size, stellar mass, and rest-frame absolute magnitude typical of Lyman break analogues in the local Universe and also similar to 2 < z < 3 star-forming galaxies and massive LAEs. LARS optical morphology is consistent with the one of merging systems, and irregular or starburst galaxies. For the first time we quantify the morphology in Lyα images: even if a variety of intrinsic conditions of the interstellar medium can favour the escape of Lyα photons, LARS-LAEs appear small in the continuum, and their Lyα is compact. LARS galaxies tend to be more extended in Lyα than in the rest-frame UV. It means that Lyα photons escape by forming haloes around HII regions of LARS galaxies. Conclusions. The stack of LARS-LAE Lyα images is peaked in the centre, indicating that the conditions, which make a galaxy an LAE, tend to produce a concentrated surface brightness profile. On the other hand, the stack of all LARS galaxies is shallower and more extended. This can be caused by the variety of dust and HI amount and distribution, which produces a more complex, patchy, and extended profile, like the one observed for Lyman break galaxies that can contribute to the stack. We cannot identify a single morphological property that controls whether a galaxy emits a net positive Lyα flux. However, the LARS-LAEs have continuum properties consistent with merging systems.

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Section: Lars Galaxies At Z ∼mentioning

confidence: 92%

Section: High-redshift Simulationmentioning

confidence: 99%

Section: High-redshift Simulationmentioning

confidence: 99%

Section: Lars Galaxies At Z ∼mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Lyman alpha reference sample

Guaita

Melinder

Hayes

et al. 2015

A&A

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The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

Grazian

Castellano

Fontana

et al. 2012

A&A

102

157

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Context. The exploration of the relation between galaxy sizes and other physical parameters (luminosity, mass, star formation rate) has provided important clues for understanding galaxy formation, but such exploration has until recently been limited to intermediate redshift objects. Aims. We use the currently available CANDELS Deep+Wide surveys in the GOODS-South, UDS and EGS fields, complemented by data from the HUDF09 program, to address the relation between size and luminosity at z ∼ 7. Methods. The six different fields used for this study are characterized by a wide combination of depth and areal coverage, well suited for reducing the biases on the observed size-magnitude plane. From these fields, we select 153 z-band dropout galaxies. Detailed simulations have been carried out for each of these six fields, inserting simulated galaxies at different magnitudes and half light radius in the two dimensional images for all the Hubble Space Telescope (HST) bands available and recovering them as carried out for the real galaxies. These simulations allow us to derive precisely the completeness as a function of size and magnitude and to quantify measurements errors/biases, under the assumption that the 2D profile of z = 7 galaxies is well represented by an exponential disk function. Results. We find in a rather robust way that the half light radius distribution function of z ∼ 7 galaxies fainter than J = 26.6 is peaked at ≤0.1 arcsec (or equivalently 0.5 kpc proper), while at brighter magnitudes high-z galaxies are typically larger than ∼0.15 arcsec. We also find a well defined size-luminosity relation, Rh ∝ L 1/2 . We compute the luminosity function (LF) in the HUDF and P12HUDF fields, finding large spatial variation on the number density of faint galaxies. Adopting the size distribution and the size-luminosity relation found for faint galaxies at z = 7, we derive a mean slope of −1.7 ± 0.1 for the LF of LBGs at this redshift. Conclusions. Using this LF, we find that the number of ionizing photons emitted from galaxies at z ∼ 7 cannot keep the Universe re-ionized if the IGM is clumpy (C HII ≥ 3) and the Lyman continuum escape fraction of high-z LBGs is relatively low ( f esc ≤ 0.3). If these results are confirmed and strengthened by future CANDELS data, in particular by the forthcoming deep observations in GOODS-South and North and the wide field COSMOS, we can put severe limits to the role of galaxies in the reionization of the Universe.

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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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EVOLUTION IN THE CONTINUUM MORPHOLOGICAL PROPERTIES OF Lyα-EMITTING GALAXIES FROMz= 3.1 TOz= 2.1

Abstract: We present a rest-frame ultraviolet morphological analysis of 108 z ≃ 2.

Cited by 39 publications

References 65 publications

The Lyman alpha reference sample

The Lyman alpha reference sample

The size-luminosity relation atz = 7 in CANDELS and its implication on reionization

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

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