[C <scp>ii</scp>] emission in <i>z</i> ∼ 6 strongly lensed, star-forming galaxies

Knudsen, K. K.; Richard, Johan; Kneib, Jean-Paul; Jauzac, Mathilde; Clément, Benjamin; Drouart, Guillaume; Egami, Eiichi; Lindroos, Lukas

doi:10.1093/mnrasl/slw114

Cited by 140 publications

(184 citation statements)

References 46 publications

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“…Other [CII] emitting galaxies (∼ 14) have been indeed discovered at high-z in the last few years (e.g. Maiolino et al 2015;Willott et al 2015;Pentericci et al 2016;Knudsen et al 2016;Aravena et al 2016;Bradač et al 2017; see also Tab. 3 in Olsen et al 2017 for an updated list of [CII] observations in z 5 star forming galaxies).…”

Section: Discussionmentioning

confidence: 93%

ALMA suggests outflows in z ∼ 5.5 galaxies

Gallerani

Pallottini

Feruglio

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the first attempt to detect outflows from galaxies approaching the Epoch of Reionization (EoR) using a sample of 9 star-forming (SFR = 31 ± 20 M yr −1 ) z ∼ 5.5 galaxies for which the [CII]158µm line has been previously obtained with ALMA. We first fit each line with a Gaussian function and compute the residuals by subtracting the best fitting model from the data. We combine the residuals of all sample galaxies and find that the total signal is characterised by a flux excess of ∼ 0.5 mJy extended over ∼ 1000 km s −1 . Although we cannot exclude that part of this signal is due to emission from faint satellite galaxies, we show that the most probable explanation for the detected flux excess is the presence of broad wings in the [CII] lines, signatures of starburst-driven outflows. We infer an average outflow rate oḟ M = 54±23 M yr −1 , providing a loading factor η =Ṁ/SFR = 1.7±1.3 in agreement with observed local starbursts. Our interpretation is consistent with outcomes from zoomed hydro-simulations of Dahlia, a z ∼ 6 galaxy (SFR ∼ 100 M yr −1 ) whose feedback-regulated star formation results into an outflow rateṀ ∼ 30 M yr −1 . The quality of the ALMA data is not sufficient for a detailed analysis of the [CII] line profile in individual galaxies. Nevertheless, our results suggest that starburst-driven outflows are in place in the EoR and provide useful indications for future ALMA campaigns. Deeper observations of the [CII] line in this sample are required to better characterise feedback at high-z and to understand the role of outflows in shaping early galaxy formation.

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Section: Discussionmentioning

confidence: 93%

ALMA suggests outflows in z ∼ 5.5 galaxies

Gallerani

Pallottini

Feruglio

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Due to gravitational lensing, we are able to measure [C II] luminosity in RX J1347:1216 that is intrinsically ∼5 times fainter than other such measurements at z∼7 to date (and similar luminosity to a z∼6 object in Knudsen et al 2016). We extract the spectrum using native spectral resolution with a channel width of 9.6 , corrected for lensing and the errors reflect both uncertainties in the flux estimates as well as magnification (Table 1).…”

Section: Resultsmentioning

confidence: 99%

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

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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“…Coppin et al (2015) stack large samples of UV-selected galaxies atz 35 -using lowresolution data from Herschel and SCUBA2 and find consistent high dust content in the typical galaxy (left panel of Figure 7). On the other hand the first small samples of high-resolution individual dust continuum detections and constraints on UVselected  z 4 galaxies (e.g., Capak et al 2015;Schaerer et al 2015;Knudsen et al 2016) indicate a typical dust content significantly below the Meurer et al (1999) relation (right panel of Figure 7). Indeed, recent stacking analyses of ALMA observations of low-mass galaxies in the Hubble Ultra Deep Field (Aravena et al 2016;Bouwens et al 2016a;Dunlop et al 2016) show surprisingly faint infrared luminosities.…”

Section: Dust Lawmentioning

confidence: 99%

INFERRED Hα FLUX AS A STAR FORMATION RATE INDICATOR AT z ∼ 4–5: IMPLICATIONS FOR DUST PROPERTIES, BURSTINESS, AND THE z = 4–8 STAR FORMATION RATE FUNCTIONS

Smit

Bouwens

Labbé

et al. 2016

ApJ

102

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Inferred H flux as a star formation rate indicator at z 4-5: α ∼ implications for dust properties, burstiness, and the z = 4-8 star formation rate functions Copyright and reuse:Sussex Research Online is a digital repository of the research output of the University.Copyright and all moral rights to the version of the paper presented here belong to the individual author(s) and/or other copyright owners. To the extent reasonable and practicable, the material made available in SRO has been checked for eligibility before being made available.Copies of full text items generally can be reproduced, displayed or performed and given to third parties in any format or medium for personal research or study, educational, or not-for-profit purposes without prior permission or charge, provided that the authors, title and full bibliographic details are credited, a hyperlink and/or URL is given for the original metadata page and the content is not changed in any way. ABSTRACTWe derive Hα fluxes for a large spectroscopic and photometric-redshift-selected sample of sources over GOODSNorth and South in the redshift range z=3.8-5.0 with deep Hubble Space Telescope (HST), Spitzer/IRAC, and ground-based observations. The Hα flux is inferred based on the offset between the IRAC 3.6 μm flux and that predicted from the best-fit spectral energy distribution (SED). We demonstrate that the Hα flux correlates well with dust-corrected UV star formation rate (SFR) and therefore can serve as an independent SFR indicator. However, we also find a systematic offset in the a b + SFR SFR HU V ratios for z∼4-5 galaxies relative to local relations (assuming the same dust corrections for nebular regions and stellar light). We show that we can resolve the modest tension in the inferred SFRs by assuming bluer intrinsic UV slopes (increasing the dust correction), a rising star formation history, or assuming a low-metallicity stellar population with a hard ionizing spectrum (increasing the a L SFR H ratio). Using Hα as an SFR indicator, we find a normalization of the star formation main sequence in good agreement with recent SED-based determinations and also derive the SFR functions atz 48 -. In addition, we assess for the first time the burstiness of star formation inz 4 galaxies on <100 Myr timescales by comparing UV and Hα-based sSFRs; their one-to-one relationship argues against significantly bursty star formation histories.

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[C ii] emission in z ∼ 6 strongly lensed, star-forming galaxies

Cited by 140 publications

References 46 publications

ALMA suggests outflows in z ∼ 5.5 galaxies

ALMA suggests outflows in z ∼ 5.5 galaxies

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

INFERRED Hα FLUX AS A STAR FORMATION RATE INDICATOR AT z ∼ 4–5: IMPLICATIONS FOR DUST PROPERTIES, BURSTINESS, AND THE z = 4–8 STAR FORMATION RATE FUNCTIONS

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