An ALMA view of the interstellar medium of the<i>z</i>= 4.77 lensed starburst SPT-S J213242-5802.9

Béthermin, M.; Breuck, C. De; Gullberg, B.; Aravena, M.; Bothwell, M. S.; Chapman, Scott; Gonzalez, Anthony H.; Greve, T. R.; Litke, Katrina C.; Ma, Jingzhe; Malkan, M.; Marrone, Dan; Murphy, E. J.; Spilker, Justin; Stark, A. A.; Strandet, M.; Vieira, J. D.; Weiß, A.; Welikala, N.

doi:10.1051/0004-6361/201527739

Cited by 33 publications

(48 citation statements)

References 42 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The latter was discussed by R14, where it was interpreted as analogous to the deficit found in local ULIRGs (e.g., Luhman et al 1998Luhman et al , 2003. On the other hand, the [Nii] line in AzTEC-3 also appears marginally fainter compared to [Cii] than observed in local (U)LIRGs (Farrah et al 2013;Kamenetzky et al 2016;Rosenberg et al 2015;Diaz-Santos et al 2013;Zhao et al 2016) and in other high redshift SMGs (Decarli et al 2014 5 ; Bethermin et al 2016), for which typical sample averages of L [CII] /L [NII] are in the range ∼ 10 − 20. In addition, the measured…”

Section: Analysis Of the Individual Sourcesmentioning

confidence: 83%

“…The [Nii] line is detected with high significance for the QSO, SMG, and LAE-2, but is not detected in LAE-1. [Cii]/[Nii] line luminosity ratios observed in high redshift galaxies to date as a function of their FIR luminosity De Breuck et al 2014;Bethermin et al 2016;Rawle et al 2014;Combes et al 2012;Riechers et al 2013;R14;C15). For comparison we also show a sample of ULIRGs from Farrah et al (2013) Zhao et al (2016) and [Cii] from Diaz-Santos et al (2013).…”

Section: Discussionmentioning

confidence: 99%

See 1 more Smart Citation

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

Pavesi

Riechers

Capak

et al. 2016

ApJ

132

View full text Add to dashboard Cite

We report interferometric measurements of [Nii] 205 µm fine-structure line emission from a representative sample of three galaxies at z = 5-6 using the Atacama Large (sub)Millimeter Array (ALMA). These galaxies were previously detected in [Cii] and far-infrared continuum emission and span almost two orders of magnitude in star formation rate (SFR). Our results show at least two different regimes of ionized inter-stellar medium properties for galaxies in the first billion years of cosmic time, separated by theirUV star-forming galaxy, likely directly or indirectly (by its effect on the radiation field) related to low dust abundance and low metallicity. The infrared-luminous modestly star-forming Lyman Break Galaxy (LBG) in our sample is characterized by an ionized-gas fraction (L [CII] /L [NII] 20) typical of local star-forming galaxies and shows evidence for spatial variations in its ionized-gas fraction across an extended gas reservoir. The extreme SFR, warm and compact dusty starburst AzTEC-3 shows an ionized fraction higher than expected given its star-formation rate surface densitydominantly traces a diffuse ionized medium rather than star-forming Hii regions in this type of galaxy. This highest redshift sample of [Nii] detections provides some of the first constraints on ionized and neutral gas modeling attempts and on the structure of the inter-stellar medium at z = 5-6 in "normal" galaxies and starbursts.

show abstract

Section: Analysis Of the Individual Sourcesmentioning

confidence: 83%

Section: Discussionmentioning

confidence: 99%

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

Pavesi

Riechers

Capak

et al. 2016

ApJ

132

View full text Add to dashboard Cite

show abstract

“…The ratio of LAB1-ALMA3 is shown, compared with those of various galaxies at z∼5 (Decarli et al 2014;Rawle et al 2014;Béthermin et al 2016;Pavesi et al 2016 and references therein) and local (U)LIRGs (Díaz-Santos et al 2013;Zhao et al 2016). ALMA3 shows one of the highest values seen to date, which indicates an enhanced [C II] emission.…”

Section: Discussion and Summarymentioning

confidence: 97%

“…ratio is also sensitive to estimate gas metallicity (e.g., Nagao et al 2012;Béthermin et al 2016;Pavesi et al 2016). Nagao et al (2012) suggest that the line ratio increases as metallicity decreases, considering both PDRs and HII regions in their model.…”

Section: Discussion and Summarymentioning

confidence: 99%

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

Umehata

Matsuda

Tamura

et al. 2017

ApJL

View full text Add to dashboard Cite

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.

show abstract

“…If the fraction can be found by other means, this dependence can also be turned around to determine the gas metallicity independently of classical optical diagnostics (e.g. Nagao et al 2011Nagao et al , 2012De Breuck et al 2014;Béthermin et al 2016;Pereira-Santaella et al 2017). An easier solution is to consider only HII-dominated FSL to determine the physical parameters.…”

Section: Introductionmentioning

confidence: 99%

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Breuck

Weiß

Béthermin

et al. 2019

A&A

View full text Add to dashboard Cite

We present a study of six far-infrared fine structure lines in the z=4.225 lensed dusty star-forming galaxy SPT 0418-47 to probe the physical conditions of its inter stellar medium (ISM). In particular, we report Atacama Pathfinder EXperiment (APEX) detections of the [OI] 145µm and [OIII] 88µm lines and Atacama Compact Array (ACA) detections of the [NII] 122 and 205µm lines. The [OI] 145µm / [CII] 158µm line ratio is ∼5× higher compared to the average of local galaxies. We interpret this as evidence that the ISM is dominated by photo-dissociation regions with high gas densities. The line ratios, and in particular those of [OIII] 88µm and [NII] 122µm imply that the ISM in SPT 0418-47 is already chemically enriched close to solar metallicity. While the strong gravitational amplification was required to detect these lines with APEX, larger samples can be observed with the Atacama Large Millimeter/submillimeter Array (ALMA), and should allow observers to determine if the dense, solar metallicity ISM is common among these highly star-forming galaxies.

show abstract

An ALMA view of the interstellar medium of thez= 4.77 lensed starburst SPT-S J213242-5802.9

Cited by 33 publications

References 42 publications

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

ALMA REVEALS WEAK [N ii] EMISSION IN “TYPICAL” GALAXIES AND INTENSE STARBURSTS AT z = 5–6

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

A dense, solar metallicity ISM in the z = 4.2 dusty star-forming galaxy SPT 0418−47

Contact Info

Product

Resources

About