Skip to main content Accessibility help
×
Home
Hostname: page-component-559fc8cf4f-sbc4w Total loading time: 0.391 Render date: 2021-03-03T09:53:43.853Z Has data issue: true Feature Flags: { "shouldUseShareProductTool": true, "shouldUseHypothesis": true, "isUnsiloEnabled": true, "metricsAbstractViews": false, "figures": false, "newCiteModal": false, "newCitedByModal": true }

First [NII] 122 μm line detection in a starburst pair at z = 4.7

Published online by Cambridge University Press:  10 June 2020

Minju M. Lee
Affiliation:
Max-Planck-Institut für Extraterrestrische Physik (MPE), Giessenbachstr., D-85748 Garching, Germnay Division of Particle and Astrophysical Science, Graduate School of Science, Nagoya University, Furo-cho, Chikusa-ku, Nagoya464-8602, Japan National Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo181-0015, Japan email: minju@mpe.mpg.de
Tohru Nagao
Affiliation:
Graduate School of Science and Engineering, Ehime University, 2-5 Bunkyo-cho, Matsuyama790-8577, Japan
Carlos De Breuck
Affiliation:
European Southern Observatory, Karl Schwarzschild Straß e 2, 85748Garching, Germany
Corresponding
E-mail address:

Abstract

We report the first detection of [NII] 122 μm line toward a QSO-SMG pair, BRI 1202-0725, at z = 4.7 using ALMA. Combining with [NII] 205 μm line detection and taking the line ratio of [NII]122/[NII]205, we constrain electron densities of both galaxies. The derived electron densities are ${26_{ - 11}^{ + 12}$ and ${134_{ - 39}^{ + 50}$ cm−3 for the SMG and the QSO, respectively, which are the first measurements for galaxies at z > 4. The electron density of the SMG is comparable to the Galactic plane and the average of local spiral galaxies, while the value for the QSO is comparable to local starbursts and optical-line based measurements for star-forming galaxies at z ∼ 2–3. Considering the similar star-formation rates (SFRs) of ≍ 1000 M yr−1 for both galaxies, our results suggest a large scatter of electron densities at fixed SFR and caution against using optical lines for dusty starbursts. The details of this report are presented in Lee et al. 2019 (submitted).

Type
Contributed Papers
Copyright
© International Astronomical Union 2020

Access options

Get access to the full version of this content by using one of the access options below.

References

Beirão, P., Armus, L., Helou, G., et al. 2012, ApJ, 751, 14410.1088/0004-637X/751/2/144CrossRefGoogle Scholar
Bennett, C. L., Fixsen, D. J., Hinshaw, G., et al. 1994, ApJ, 434, 58710.1086/174761CrossRefGoogle Scholar
Daz-Santos, T., Armus, L., Charmandaris, V., et al. 2017, ApJ, 846, 3210.3847/1538-4357/aa81d7CrossRefGoogle Scholar
Goldsmith, P. F., Yldz, U. A., Langer, W. D., & Pineda, J. L. 2015, ApJ, 814, 13310.1088/0004-637X/814/2/133CrossRefGoogle Scholar
Herrera-Camus, R., Bolatto, A., Smith, J. D., et al. 2016, ApJ, 826, 17510.3847/0004-637X/826/2/175CrossRefGoogle Scholar
Iono, D., Yun, M. S., Elvis, M., et al. 2006, ApJL, 645, L9710.1086/506344CrossRefGoogle Scholar
Luridiana, V., Morisset, C., & Shaw, R. A. 2015, A&A, 573, A42Google Scholar
Omont, A., Petitjean, P., Guilloteau, S., et al. 1996, Nature, 382, 42810.1038/382428a0CrossRefGoogle Scholar
Pavesi, R., Riechers, D. A., Capak, P. L., et al. 2016, ApJ, 832, 15110.3847/0004-637X/832/2/151CrossRefGoogle Scholar
Petuchowski, S. J., Bennett, C. L., Haas, M. R., et al. 1994, ApJL, 427, L1710.1086/187354CrossRefGoogle Scholar
Sanders, R. L., Shapley, A. E., Kriek, M., et al. 2016, ApJ, 816, 2310.3847/0004-637X/816/1/23CrossRefGoogle Scholar
Yun, M. S., Carilli, C. L., Kawabe, R., et al. 2000, ApJ, 528, 17110.1086/308164CrossRefGoogle Scholar
Zhang, Z.-Y., Ivison, R. J., George, R. D., et al. 2018, MNRAS, 481, 5910.1093/mnras/sty2082CrossRefGoogle Scholar

Full text views

Full text views reflects PDF downloads, PDFs sent to Google Drive, Dropbox and Kindle and HTML full text views.

Total number of HTML views: 0
Total number of PDF views: 8 *
View data table for this chart

* Views captured on Cambridge Core between 10th June 2020 - 3rd March 2021. This data will be updated every 24 hours.

Send article to Kindle

To send this article to your Kindle, first ensure no-reply@cambridge.org is added to your Approved Personal Document E-mail List under your Personal Document Settings on the Manage Your Content and Devices page of your Amazon account. Then enter the ‘name’ part of your Kindle email address below. Find out more about sending to your Kindle. Find out more about sending to your Kindle.

Note you can select to send to either the @free.kindle.com or @kindle.com variations. ‘@free.kindle.com’ emails are free but can only be sent to your device when it is connected to wi-fi. ‘@kindle.com’ emails can be delivered even when you are not connected to wi-fi, but note that service fees apply.

Find out more about the Kindle Personal Document Service.

First [NII] 122 μm line detection in a starburst pair at z = 4.7
Available formats
×

Send article to Dropbox

To send this article to your Dropbox account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Dropbox.

First [NII] 122 μm line detection in a starburst pair at z = 4.7
Available formats
×

Send article to Google Drive

To send this article to your Google Drive account, please select one or more formats and confirm that you agree to abide by our usage policies. If this is the first time you use this feature, you will be asked to authorise Cambridge Core to connect with your <service> account. Find out more about sending content to Google Drive.

First [NII] 122 μm line detection in a starburst pair at z = 4.7
Available formats
×
×

Reply to: Submit a response


Your details


Conflicting interests

Do you have any conflicting interests? *