Spectroscopic Confirmation of Faint Lyman Break Galaxies Near Redshift Five in the Hubble Ultra Deep Field

Rhoads, James E.; Malhotra, Sangeeta; Pirzkal, Norbert; Dickinson, Mark; Cohen, Seth H.; Grogin, Norman A.; Hathi, N. P.; Xu, Chun; Ferreras, Ignacio; Grönwall, C.; Koekemoer, Anton M.; Kümmel, M.; Meurer, G. R.; Panagia, N.; Pasquali, A.; Ryan, Russell E.; Straughn, Amber N.; Walsh, J. R.; Windhorst, Rogier A.; Yan, Hao

doi:10.1088/0004-637x/697/1/942

Cited by 35 publications

(19 citation statements)

References 36 publications

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“…They concluded that these objects have Lyα half-light radii < 1.5 kpc, similar to their rest-frame UV sizes, with the Lyα emission coincident within 0.5 kpc of the rest-frame UV emission. Rhoads et al (2009) also examined the relative sizes of LAEs in Lyα and the UV continuum using ACS grism spectroscopic data from the PEARS survey by examining the sizes of the objects in the spatial dimension. They did not find evidence of an extended Lyα halo in a stack of the spectra from all 39 z ∼ 5 galaxies in their sample.…”

Section: Previous Resultsmentioning

confidence: 99%

HUBBLE SPACE TELESCOPEIMAGING OF Lyα EMISSION ATz≈ 4.4

Finkelstein¹,

Cohen²,

Windhorst³

et al. 2011

ApJ

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We present the highest redshift detections of resolved Lyα emission, using Hubble Space Telescope (HST)/Advanced Camera for Surveys F658N narrowband-imaging data taken in parallel with the Wide Field Camera 3 Early Release Science program in the GOODS Chandra Deep Field-South. We detect Lyα emission from three spectroscopically confirmed z = 4.4 Lyα emitting galaxies (LAEs), more than doubling the sample of LAEs with resolved Lyα emission. Comparing the light distribution between the rest-frame ultraviolet continuum and narrowband images, we investigate the escape of Lyα photons at high redshift. While our data do not support a positional offset between the Lyα and rest-frame ultraviolet (UV) continuum emission, the half-light radius in one out of the three galaxies is significantly (>1σ ) larger in Lyα than in the rest-frame UV continuum. Stacking the three LAEs in both the narrowband and UV continuum images, we find that the Lyα light appears larger than the rest-frame UV at 4.2σ significance. This Lyα flux detected with HST is a factor of 4-10 less than observed in similar filters from the ground. These results together imply that the Lyα emission is not strictly confined to its indigenous star-forming regions. Rather, for at least one object the Lyα emission is more extended, with the missing HST flux possibly existing in a diffuse outer halo. This suggests that the radiative transfer of Lyα photons in high-redshift LAEs is complicated, with the interstellar-medium geometry and/or outflows playing a significant role in galaxies at these redshifts.

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Section: Previous Resultsmentioning

confidence: 99%

HUBBLE SPACE TELESCOPEIMAGING OF Lyα EMISSION ATz≈ 4.4

Finkelstein¹,

Cohen²,

Windhorst³

et al. 2011

ApJ

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“…The Lyman-α galaxies may show a different size in line emission: larger, if the resonant scattering of Lyman-α photons to escape from the galaxy is important; and smaller if the Lyman-α comes from an active nucleus. Rhoads et al (2009) examined the sizes of galaxies in the Lyman-α line and the adjoining continuum using data from slitless spectroscopy, and found no significant difference in FWHM in the line and continuum. HST imaging in narrow bandpass dominated by the Lyman-α line flux also exists for a few cases (Bond et al 2010, Finkelstein et al 2010b.…”

Section: Discussionmentioning

confidence: 99%

SIZING UP Lyα AND LYMAN BREAK GALAXIES

Malhotra

Rhoads

Finkelstein

et al. 2012

ApJ

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102

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We show that populations of high redshift galaxies grow more luminous as they grow in linear size. This is because the brightness per unit area has a distinct upper limit due to the self-regulating nature of star-formation. As a corollary, we show that the observed increase in characteristic luminosity of Lyman Break Galaxies (L * ) with time can be explained by their increase in size, which scales as H(z) −1 . In contrast, Lyman-α selected galaxies have a characteristic, constant, small size between redshift z = 2.25 and 6.5. Coupled with a characteristic surface brightness, this can explain their non-evolving ultraviolet continuum luminosity function. This compact physical size seems to be a critical determining factor in whether a galaxy will show Lyman-α emission. We base these conclusions on new size measurements for a sample of about 170 Lyman-α selected galaxies with Hubble Space Telescope broad band imaging, over the redshift range 2.25 < z < 6. We combine these with a similar number of Lyman-α selected galaxies with half-light radii from the literature, and derive surface brightnesses for the entire combined sample.

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“…Available data include Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) and Wide Field Camera 3 IR data from the HUDF09, HUDF12, and Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) programs, as well as public photometric and spectroscopic catalogs (Coe et al 2006;Xu et al 2007;Rhoads et al 2009;McLure et al 2013;Schenker et al 2013;Bouwens et al 2014;Skelton et al 2014;Momcheva et al 2016;Morris et al 2015). In this study, we make use of this optical and infrared coverage of the XDF, including the photometric and spectroscopic redshift information available from Skelton et al (2014).…”

Section: Multiwavelength Datamentioning

confidence: 99%

THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR-FORMING GALAXIES

Aravena

Decarli

Walter

et al. 2016

ApJ

127

118

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We present an analysis of a deep (1σ=13 μJy) cosmological 1.2 mm continuum map based on ASPECS, the ALMA Spectroscopic Survey in the Hubble Ultra Deep Field. In the 1 arcmin 2 covered by ASPECS we detect nine sources at s >3.5 significance at 1.2 mm. Our ALMA-selected sample has a median redshift of =  z 1.6 0.4, with only one galaxy detected at z>2 within the survey area. This value is significantly lower than that found in millimeter samples selected at a higher flux density cutoff and similar frequencies. Most galaxies have specific star formation rates (SFRs) similar to that of main-sequence galaxies at the same epoch, and we find median values of stellar mass and SFRs of , respectively. Using the dust emission as a tracer for the interstellar medium (ISM) mass, we derive depletion times that are typically longer than 300 Myr, and we find molecular gas fractions ranging from ∼0.1 to 1.0. As noted by previous studies, these values are lower than those using CO-based ISM estimates by a factor of ∼2. The 1 mm number counts (corrected for fidelity and completeness) are in agreement with previous studies that were typically restricted to brighter sources. With our individual detections only, we recover 55%±4% of the extragalactic background light (EBL) at 1.2 mm measured by the Planck satellite, and we recover 80% ±7% of this EBL if we include the bright end of the number counts and additional detections from stacking. The stacked contribution is dominated by galaxies at -z 1 2, with stellar masses of (1-3)×10 10 M  . For the first time, we are able to characterize the population of galaxies that dominate the EBL at 1.2 mm.

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Spectroscopic Confirmation of Faint Lyman Break Galaxies Near Redshift Five in the Hubble Ultra Deep Field

Cited by 35 publications

References 36 publications

HUBBLE SPACE TELESCOPEIMAGING OF Lyα EMISSION ATz≈ 4.4

HUBBLE SPACE TELESCOPEIMAGING OF Lyα EMISSION ATz≈ 4.4

SIZING UP Lyα AND LYMAN BREAK GALAXIES

THE ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: CONTINUUM NUMBER COUNTS, RESOLVED 1.2 mm EXTRAGALACTIC BACKGROUND, AND PROPERTIES OF THE FAINTEST DUSTY STAR-FORMING GALAXIES

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