Journal
ASTROPHYSICAL JOURNAL
Volume 881, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.3847/1538-4357/ab2f81
Keywords
dark ages, reionization, first stars; galaxies: formation; galaxies: high-redshift; galaxies: ISM; galaxies: kinematics and dynamics
Categories
Funding
- European Union [746119]
- NASA [NAS 5-26555]
- [294.A-5018]
- [097.A-0943]
- [99.A-0462]
- [14699]
- STFC [ST/P00038X/1, ST/R000514/1] Funding Source: UKRI
- Marie Curie Actions (MSCA) [746119] Funding Source: Marie Curie Actions (MSCA)
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We present new deep ALMA and Hubble Space Telescope (HST)/WFC3 observations of MASOSA and VR7, two luminous Lya emitters (LAEs) at z = 6.5, for which the UV continuum levels differ by a factor of four. No IR dust continuum emission is detected in either, indicating little amounts of obscured star formation and/or high dust temperatures. MASOSA, with a UV luminosity M-1500 = -20.9, compact size, and very high Ly alpha EW0 approximate to 145 angstrom, is undetected in [C II] to a limit of L-[C II] < 2.2. x. 10(7) L-circle dot, implying a metallicity Z less than or similar to 0.07 Z(circle dot). Intriguingly, our HST data indicate a red UV slope beta = -1.1 +/- 0.7, at odds with the low dust content. VR7, which is a bright (M-1500 = -22.4) galaxy with moderate color (beta = -1.4 +/- 0.3) and Ly alpha EW0 = 34 angstrom, is clearly detected in [C II] emission (S/N = 15). VR7's rest-frame UV morphology can be described by two components separated by approximate to 1.5 kpc and is globally more compact than the [C II] emission. The global [C II]/UV ratio indicates Z approximate to 0.2 Z(circle dot), but there are large variations in the UV/[C II] ratio on kiloparsec scales. We also identify diffuse, possibly outflowing, [C II]-emitting gas at approximate to 100 km s(-1) with respect to the peak. VR7 appears to be assembling its components at a slightly more evolved stage than other luminous LAEs, with outflows already shaping its direct environment at z similar to 7. Our results further indicate that the global [C II]-UV relation steepens at SFR < 30 M-circle dot yr(-1), naturally explaining why the [C II]/UV ratio is anticorrelated with Lya EW in many, but not all, observed LAEs.
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