TRACING THE REIONIZATION EPOCH WITH ALMA: [C ii] EMISSION IN z ∼ 7 GALAXIES

Pentericci, L.; Carniani, Stefano; Castellano, M.; Fontana, A.; Maiolino, R.; Guaita, L.; Vanzella, E.; Grazian, A.; Santini, P.; Yan, Hao; Cristiani, S.; Conselice, Christopher J.; Giavalisco, Mauro; Hathi, N. P.; Koekemoer, Anton M.

doi:10.3847/2041-8205/829/1/l11

Cited by 179 publications

(239 citation statements)

References 35 publications

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“…In addition, Dunlop et al (2017) noted that the HST and ALMA astrometry of the HUDF presented both a systematic shift of 0 25 and a random offset of up to 0 5. Similarly, Pentericci et al (2016) note 0 1-0 6 random offsets measured from serendipitous detections in the field. Unfortunately, we do not detect any other sources in our small field of view to perform relative astrometric calibration.…”

Section: Resultsmentioning

confidence: 94%

“…At z∼7, however, Stark et al (2015) measured an offset of Δv≈60 km s −1 between Lyα and CIV for a lensed lowluminosity galaxy A1703-zd6 at z=7.045 (though CIV might not trace systemic velocity). Pentericci et al (2016) reported velocity shifts of ∼100 km s −1 between [C II] and Lyα for their three most significant detections. For a higher-luminosity galaxy, Stark et al (2017) reported an offset between CIII] and Lyα of ∼340 km s −1 .…”

Section: Resultsmentioning

confidence: 96%

“…[C II] is also a very useful tracer of the kinematics of distant galaxies. However, even with ALMA, detections at z∼7 remain sparse (see Maiolino et al 2015;Knudsen et al 2017;Pentericci et al 2016 (Ouchi et al 2013;Ota et al 2014;Schaerer et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

Bradač

Garcia‐Appadoo

Huang

et al. 2017

ApJL

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107

129

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We present the results of ALMA spectroscopic follow-up of a z=6.766 Lyα emitting galaxy behind the cluster RX J1347.1−1145. We report the detection of [C II] 158 μm line fully consistent with the Lyα redshift and with the peak of the optical emission. Given the magnification of μ=5.0±0.3, the intrinsic (corrected for lensing) luminosity of the, roughly ∼5 times fainter than other detections of z∼7 galaxies. The result indicates that low L [C II] in z∼7 galaxies compared to the local counterparts might be caused by their low metallicities and/or feedback. ) between the Lyα and [C II] line is unusual, and may be indicative of ionizing photons escaping.

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Section: Resultsmentioning

confidence: 94%

Section: Resultsmentioning

confidence: 96%

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ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

Bradač

Garcia‐Appadoo

Huang

et al. 2017

ApJL

Self Cite

107

129

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“…Some recent observations suggest that five z ∼ 7 galaxies show very small velocity offsets about 20-150km s −1 between Lyα and [CII] emission lines (Pentericci et al 2016;Bradac et al 2017). Those small V(red-peak) values may indicate that the Lyα escape fractions are high and the optical depths of ISM and CGM are small.…”

Section: Predicting Lyα Escape Fractionmentioning

confidence: 99%

Lyα Profile, Dust, and Prediction of Lyα Escape Fraction in Green Pea Galaxies

Yang

Malhotra

Grönke

et al. 2017

ApJ

204

241

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We studied Lyman-α (Lyα) escape in a statistical sample of 43 Green Peas with HST/COS Lyα spectra. Green Peas are nearby star-forming galaxies with strong [OIII]λ5007 emission lines. Our sample is four times larger than the previous sample and covers a much more complete range of Green Pea properties. We found that about 2/3 of Green Peas are strong Lyα line emitters with rest-frame Lyα equivalent width > 20Å. The Lyα profiles of Green Peas are diverse. The Lyα escape fraction, defined as the ratio of observed Lyα flux to intrinsic Lyα flux, shows anti-correlations with a few Lyα kinematic features -both the blue peak and red peak velocities, the peak separations, and FWHM of the red portion of the Lyα profile. Using properties measured from SDSS optical spectra, we found many correlations -Lyα escape fraction generally increases at lower dust reddening, lower metallicity, lower stellar mass, and higher [OIII]/[OII] ratio. We fit their Lyα profiles with the HI shell radiative transfer model and found Lyα escape fraction anti-correlates with the best-fit N HI . Finally, we fit an empirical linear relation to predict f Lyα esc from the dust extinction and Lyα red peak velocity. The standard deviation of this relation is about 0.3 dex. This relation can be used to isolate the effect of IGM scatterings from Lyα escape and to probe the IGM optical depth along the line of sight of each z > 7 Lyα emission line galaxy in the JWST era.

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“…A similar shift is also observed at higher redshift. For instance, Pentericci et al (2016) observed shifts of 100-200 km s −1 between the Lyα and [C II] emission line in four galaxies at redshifts between 6.6 and 7.2. Likewise, the Lyα emission of the z∼6 star-forming galaxy A383-5.2 appears to be shifted by 120 km s −1 with respect to the systemic redshift probed via the C III] λ1909 metal line (Stark et al 2015).…”

Section: Tentative Detection Of An Extended Emissionmentioning

confidence: 99%

Mapping the Lyα Emission around a z ∼ 6.6 QSO with MUSE: Extended Emission and a Companion at a Close Separation

Farina

Venemans

Decarli

et al. 2017

ApJ

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We utilize the Multi Unit Spectroscopic Explorer (MUSE) on the Very Large Telescope to search for extended Lyα emission around the z∼6.6 QSO J0305−3150. After carefully subtracting the point spread function, we reach a nominal 5σ surface-brightness limit of SB 5σ =1.9×10−18 ergs −1 cm −2 arcsec −2 over a 1arcsec 2 aperture, collapsing fivewavelength slices centered at the expected location of the redshifted Lyα emission (i.e., at 9256 Å). Current data suggest the presence (5σ accounting for systematics) of a Lyα nebula that extends for 9 kpc around the QSO. This emission is displaced and redshifted by 155 km s −1 with respect to the location of the QSO host galaxy traced by the [C II] 158 μm emission line. The total luminosity is L Lya ( )=(3.0 ± 0.4)× 10 42 ergs −1 . Our analysis suggests that this emission is unlikely to rise from optically thick clouds illuminated by the ionizing radiation of the QSO. It is more plausible that the Lyα emission is due to the fluorescence of the highly ionized optically thin gas. This scenario implies a high hydrogen volume density of n 6 H~c m −3 . In addition, we detect a Lyα emitter (LAE) in the immediate vicinity of the QSO, i.e., with a projected separation of ∼12.5 kpc and a line-of-sight velocity difference of 560 km s . The probability of finding such a close LAE is one order of magnitude above the expectations based on the QSO-galaxy cross-correlation function. This discovery is in agreement with a scenario where dissipative interactions favor the rapid build-up of supermassive black holes at early cosmic times.

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TRACING THE REIONIZATION EPOCH WITH ALMA: [C ii] EMISSION IN z ∼ 7 GALAXIES

Cited by 179 publications

References 35 publications

ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

ALMA [C ii] 158 μm Detection of a Redshift 7 Lensed Galaxy behind RX J1347.1−1145*

Lyα Profile, Dust, and Prediction of Lyα Escape Fraction in Green Pea Galaxies

Mapping the Lyα Emission around a z ∼ 6.6 QSO with MUSE: Extended Emission and a Companion at a Close Separation

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