Imperial College London
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Dr Clements

Faculty of Natural Sciences, Department of Physics

Reader in Astrophysics
 
 
 
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Contact

 

+44 (0)20 7594 7693d.clements

 
 
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Location

 

1011Blackett LaboratorySouth Kensington Campus

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Summary

 

Publications

Citation

BibTex format

@unpublished{Greenslade:2019,
author = {Greenslade, J and Aguilar, E and Clements, DL and Dannerbauer, H and Cheng, T and Petitpas, G and Yang, C and Messias, H and Oteo, I and Farrah, D and Michalowski, MJ and Fournon, IP and Aretxaga, I and Yun, MS and Eales, S and Dunne, L and Cooray, A and Andreani, P and Hughes, DH and Velazquez, M and Sanchez-Arguelles, D and Ponthieu, N},
publisher = {arXiv},
title = {A SCUBA-2 selected herschel-SPIRE dropout and the nature of this population},
url = {http://arxiv.org/abs/1910.03512v1},
year = {2019}
}
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RIS format (EndNote, RefMan)

TY  - UNPB
AB  - Dusty star-forming galaxies (DSFGs) detected at $z > 4$ provide importantexamples of the first generations of massive galaxies. However, few exampleswith spectroscopic confirmation are currently known, with Hershel struggling todetect significant numbers of $z > 6$ DSFGs. NGP6_D1 is a bright 850 $\mu m$source (12.3 $\pm$ 2.5 mJy) with no counterparts at shorter wavelengths (aSPIRE dropout). Interferometric observations confirm it is a single source,with no evidence for any optical or NIR emission, or nearby likely foregroundlensing sources. No $>3\sigma$ detected lines are seen in both LMT RSR and IRAM30m EMIR spectra of NGP6_D1 across 32 $GHz$ of bandwidth despite reachingdetection limits of $\sim 1 mJy/500 km~s^{-1}$, so the redshift remainsunknown. Template fitting suggests that NGP6_D1 is most likely between $z =5.8$ and 8.3. SED analysis finds that NGP6_D1 is a ULIRG, with a dust mass$\sim 10^8$ - $10^9$ $M_{\odot}$ and a SFR of $\sim$ 500 $M_{\odot}~yr^{-1}$.We place upper limits on the gas mass of NGP6_D1 of $M_{H2}$ $ < (1.1~\pm~3.5)\times 10^{11}$ $M_{\odot}$, consistent with a gas-to-dust ratio of $\sim$ 100- 1000. We discuss the nature of NGP6_D1 in the context of the broader submmpopulation, and find that comparable SPIRE dropouts account for $\sim$ 20% ofall SCUBA-2 detected sources, but with a similar flux density distribution tothe general population.
AU  - Greenslade,J
AU  - Aguilar,E
AU  - Clements,DL
AU  - Dannerbauer,H
AU  - Cheng,T
AU  - Petitpas,G
AU  - Yang,C
AU  - Messias,H
AU  - Oteo,I
AU  - Farrah,D
AU  - Michalowski,MJ
AU  - Fournon,IP
AU  - Aretxaga,I
AU  - Yun,MS
AU  - Eales,S
AU  - Dunne,L
AU  - Cooray,A
AU  - Andreani,P
AU  - Hughes,DH
AU  - Velazquez,M
AU  - Sanchez-Arguelles,D
AU  - Ponthieu,N
PB  - arXiv
PY  - 2019///
TI  - A SCUBA-2 selected herschel-SPIRE dropout and the nature of this population
UR  - http://arxiv.org/abs/1910.03512v1
UR  - http://hdl.handle.net/10044/1/73831
ER  -
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