Q1549-C25: A CLEAN SOURCE OF LYMAN-CONTINUUM EMISSION AT z = 3.15<sup>∗</sup>

Shapley, Alice E.; Steidel, Charles C.; Strom, Allison L.; Bogosavljević, M.; Reddy, Naveen A.; Siana, Brian; Mostardi, R.; Rudie, Gwen C.

doi:10.3847/2041-8205/826/2/l24

Cited by 181 publications

(196 citation statements)

References 33 publications

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“…One known high-redshift LyC emitter is GP-like (Vanzella et al 2016), while at least one other is not (Shapley et al 2016). Ultimately, the reionization of the universe may require the contribution of different types of galaxies (e.g., Fontanot et al 2012).…”

Section: Discussionmentioning

confidence: 99%

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

Jaskot

Oey

Scarlata

et al. 2017

ApJL

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By clearing neutral gas away from a young starburst, superwinds may regulate the escape of Lyman continuum (LyC) photons from star-forming galaxies. However, models predict that superwinds may not launch in the most extreme, compact starbursts. We explore the role of outflows in generating low optical depths in the Green Peas (GPs), the only known star-forming population with several confirmed and candidate LyC-leaking galaxies. With Hubble Space Telescope UV spectra of 25 low-redshift GPs, including new observations of 13 of the most highly ionized GPs, we compare the kinematics of UV absorption lines with indirect H i optical depth diagnostics: Lyα escape fraction, Lyα peak separation, or low-ionization absorption line equivalent width. The data suggest that high ionization kinematics tracing superwind activity may correlate with low optical depth in some objects. However, the most extreme GPs, including many of the best candidate LyC emitters with weak low-ionization absorption and strong, narrow Lyα profiles, show the lowest velocities. These results are consistent with models for suppressed superwinds, which suggests that outflows may not be the only cause of LyC escape from galaxies.

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Section: Discussionmentioning

confidence: 99%

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

Jaskot

Oey

Scarlata

et al. 2017

ApJL

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“…Early observations resulted in confusing results, with many of the direct detections being attributed to contamination by foreground sources (Vanzella et al 2010(Vanzella et al , 2012Nestor et al 2011;Mostardi et al 2015;Siana et al 2015;Grazian et al 2016). However, recently a small sample of three galaxies with confirmed direct detections of their LyC emission has emerged (Mostardi et al 2015;Shapley et al 2016;Vanzella et al 2016). One of these is Ion2 at z 3.2 = , which was originally identified in Vanzella et al (2015, henceforth V15) using a method similar to the one we adopt in this paper.…”

Section: Introductionmentioning

confidence: 84%

The HDUV Survey: Six Lyman Continuum Emitter Candidates at z ∼ 2 Revealed by HST UV Imaging*

Naidu

Oesch

Reddy

et al. 2017

ApJ

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We present six galaxies at z 2 that show evidence of Lyman continuum (LyC) emission based on the newly acquired UV imaging of the Hubble Deep UV legacy survey (HDUV) conducted with the WFC3/UVIS camera on the Hubble Space Telescope (HST). At the redshift of these sources, the HDUV F275W images partially probe the ionizing continuum. By exploiting the HST multiwavelength data available in the HDUV/GOODS fields, models of the UV spectral energy distributions, and detailed Monte Carlo simulations of the intergalactic medium absorption, we estimate the absolute ionizing photon escape fractions of these galaxies to be very high-typically 60% > ( 13% > for all sources at 90% likelihood). Our findings are in broad agreement with previous studies that found only a small fraction of galaxies with high escape fraction. These six galaxies compose the largest sample yet of LyC leaking candidates at z 2 whose inferred LyC flux has been observed at HST resolution. While three of our six candidates show evidence of hosting an active galactic nucleus, two of these are heavily obscured and their LyC emission appears to originate from star-forming regions rather than the central nucleus. Extensive multiwavelength data in the GOODS fields, especially the near-IR grism spectra from the 3D-HST survey, enable us to study the candidates in detail and tentatively test some recently proposed indirect methods to probe LyC leakage. High-resolution spectroscopic follow-up of our candidates will help constrain such indirect methods, which are our only hope of studying f esc at z 5 9 -in the JWST era.

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“…It was analysed in detail by de and confirmed by Vanzella et al (2016). A second clear Lyman continuum emitter was recently identified at z = 3.15 by Shapley et al (2016). They used the spectroscopic technique combined with high-resolution HST imaging and inferred a value of f esc ≥ 42% at 95% confidence for this source.…”

Section: Introductionmentioning

confidence: 98%

New constraints on the average escape fraction of Lyman continuum radiation in z ~ 4 galaxies from the VIMOS Ultra Deep Survey (VUDS)

Marchi

Pentericci

Guaita

et al. 2017

A&A

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Context. Determining the average fraction of Lyman continuum (LyC) photons escaping high redshift galaxies is essential for understanding how reionization proceeded in the z>6 Universe. Aims. We want to measure the LyC signal from a sample of sources in the Chandra Deep Field South (CDFS) and COSMOS fields for which ultra-deep VIMOS spectroscopy as well as multi-wavelength Hubble Space Telescope (HST) imaging are available. Methods. We select a sample of 46 galaxies at z ∼ 4 from the VIMOS Ultra Deep Survey (VUDS) database, such that the VUDS spectra contain the LyC part of the spectra, that is, the rest-frame range 880 − 910Å. Taking advantage of the HST imaging, we apply a careful cleaning procedure and reject all the sources showing nearby clumps with different colours, that could potentially be lower-redshift interlopers. After this procedure, the sample is reduced to 33 galaxies. We measure the ratio between ionizing flux (LyC at 895Å) and non-ionizing emission (at ∼ 1500Å) for all individual sources. We also produce a normalized stacked spectrum of all sources. Results. Assuming an intrinsic average L ν (1470)/L ν (895) of 3, we estimate the individual and average relative escape fraction. We do not detect ionizing radiation from any individual source, although we identify a possible LyC emitter with very high Lyα equivalent width (EW). From the stacked spectrum and assuming a mean transmissivity for the sample, we measure a relative escape fraction f rel esc = 0.09±0.04. We also look for correlations between the limits in the LyC flux and source properties and find a tentative correlation between LyC flux and the EW of the Lyα emission line. Conclusions. Our results imply that the LyC flux emitted by V = 25 − 26 star-forming galaxies at z∼4 is at most very modest, in agreement with previous upper limits from studies based on broad and narrow band imaging.

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Q1549-C25: A CLEAN SOURCE OF LYMAN-CONTINUUM EMISSION AT z = 3.15^∗

Cited by 181 publications

References 33 publications

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

The HDUV Survey: Six Lyman Continuum Emitter Candidates at z ∼ 2 Revealed by HST UV Imaging*

New constraints on the average escape fraction of Lyman continuum radiation in z ~ 4 galaxies from the VIMOS Ultra Deep Survey (VUDS)

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Q1549-C25: A CLEAN SOURCE OF LYMAN-CONTINUUM EMISSION AT z = 3.15∗

Cited by 181 publications

References 33 publications

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

Kinematics and Optical Depth in the Green Peas: Suppressed Superwinds in Candidate LyC Emitters*

The HDUV Survey: Six Lyman Continuum Emitter Candidates at z ∼ 2 Revealed by HST UV Imaging*

New constraints on the average escape fraction of Lyman continuum radiation in z ~ 4 galaxies from the VIMOS Ultra Deep Survey (VUDS)

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Q1549-C25: A CLEAN SOURCE OF LYMAN-CONTINUUM EMISSION AT z = 3.15^∗