ALMA Reveals Strong Emission in a Galaxy Embedded in a Giant Lyα Blob at z = 3.1

Abstract

Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe report the result from observations conducted with the Atacama Large Millimeter/submillimeter Array (ALMA) to detect [C II] 158 μm fine structure line emission from galaxies embedded in one of the most spectacular Lyα blobs (LABs) at z = 3.1, SSA22-LAB1. Of three dusty star-forming galaxies previously discovered by ALMA 860 μm dust continuum survey toward SSA22-LAB1, we detected the [C II] line from one, LAB1-ALMA3 at z = 3.0993±0.0004. No line emission was detected, associated with the other ALMA continuum sources or from three rest-frame UV/optical selected z spec ;3.1 galaxies within the field of view. For LAB1-ALMA3, we find relatively bright [C II] emission compared to the infrared luminosity (L emission could be causally related to the location within the giant LAB, although the relationship between extended Lyα emission and interstellar medium conditions of associated galaxies is yet to be understand.

A high dust emissivity index β for a CO-faint galaxy in a filamentary Lyα nebula at z = 3.1

“…Lyα blobs (LABs) are extended Lyα emitting nebulae, primarily found in galaxy over-dense regions at z ∼ 1 − 3 (e.g., Steidel et al 2000;Matsuda et al 2004;Matsuda et al 2009;Matsuda et al 2011;Dey et al 2005;Prescott et al 2008;Barger, Cowie, & Wold 2012;Valentino et al 2016;Caminha et al 2016;Cai et al 2017). It has been found that some 100 kpc-scale LABs are bright in submillimeter/millimeter wavelengths, suggesting a possible connection between LABs and dusty star-forming galaxies (DSFGs, e.g., Chapman et al 2001;Chapman et al 2004;Geach et al 2005;Geach et al 2014;Tamura et al 2013;Yang et al 2014;Hine et al 2016;Alexander et al 2016;Ao et al 2017;Umehata et al 2017a;Umehata et al 2017b;Umehata et al 2018). However, we don't know if the DSFGs in LABs differ from typical DSFGs population.…”

Deep Submillimeter and Radio Observations in the SSA22 Field. I. Powering Sources and the Lyα Escape Fraction of Lyα Blobs

“…SSA22 is such a suitable field because it has 35 LABs detected at z≈3.1 (Matsuda et al 2004), providing an ideal laboratory to study the LABs in a large sample. One of them, SSA22-LAB01 is the best studied source (e.g., Matsuda et al 2007;Yang et al 2012;Geach et al 2014Geach et al , 2016Umehata et al 2017a). At (sub) millimeter wavelength, most LABs of SSA22 have been studied with the Submillimetre Common-User Bolometer Array (SCUBA, Geach et al 2005) and SCUBA-2 (Hine et al 2016) on the James Clerk Maxwell Telescope (JCMT), and with the AzTEC 1.1mm camera (Tamura et al 2009(Tamura et al , 2013Umehata et al 2014) on the Atacama Submillimeter Telescope Experiment (ASTE).…”

Low Star Formation Efficiency in Typical Galaxies at z = 5–6

“…[Cii]/[Nii] line luminosity ratios observed in high redshift galaxies to-date as a function of their FIR luminosityDe Breuck et al 2014;Béthermin et al 2016;Rawle et al 2014;Combes et al 2012;Riechers et al 2013Riechers et al , 2014Capak et al 2015;Wagg et al 2010;Umehata et al 2017;Lu et al 2018;Pavesi et al 2018b).For comparison we also show a sample of local ULIRGs from Farrah et al (2013) (using the [Nii] 122 µm line) and LIRGs with [Nii] (using the [Nii] 205 µm line) from Zhao et al (2016) and [Cii] from Díaz-Santos et al (2013). The range of ratios in dwarfs (Cormier et al 2015) (using the [Nii] 122 µm line) is shown as a cyan band.…”