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Properties of LBGs with [OIII] detection at z > 3: The importance of including nebular emission data in SED fitting

Published online by Cambridge University Press:  10 June 2020

Fang-Ting Yuan ,
Denis Burgarella ,
David Corre ,
Veronique Buat ,
Médéric Boquien  and
Shiyin Shen
Fang-Ting Yuan
Affiliation:
Shanghai Astronomical Observatory, CAS, Nandan Road 80, 200030, Shanghai, China email: [email protected]
Denis Burgarella
Affiliation:
Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d’astrophysique de Marseille) UMR 7326, 13388, Marseille, France
David Corre
Affiliation:
Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d’astrophysique de Marseille) UMR 7326, 13388, Marseille, France
Veronique Buat
Affiliation:
Aix Marseille Université, CNRS, CNES, LAM (Laboratoire d’astrophysique de Marseille) UMR 7326, 13388, Marseille, France
Médéric Boquien
Affiliation:
Centro de Astronomía (CITEVA), Universidad de Antofagasta, Avenida Angamos 601, Antofagasta, Chile
Shiyin Shen
Affiliation:
Shanghai Astronomical Observatory, CAS, Nandan Road 80, 200030, Shanghai, China email: [email protected]
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Abstract

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At high redshift, the contribution of strong emission lines to the broadband photometry can cause large uncertainties when estimating galaxy physical properties. To examine this effect, we investigate a sample of 54 LBGs at 3 < zspec < 3.8 with detected [OIII] line emissions. We use CIGALE to fit simultaneously the rest-frame UV-to-NIR SEDs of these galaxies and their emission line data. By comparing the results with and without emission line data, we show that spectroscopic data are necessary to constrain the nebular model. We examine the K-band excess, which is usually used to estimate the emissions of [OIII]+Hβ lines when there is no spectral data, and find that the difference between the estimation and observation can reach up to > 1 dex for some galaxies, showing the importance of obtaining spectroscopic measurements of these lines. We also estimate the equivalent width of the Hβ absorption and find it negligible compared to the Hβ emission.

Keywords

galaxies: high-redshiftgalaxies: formationgalaxies: emission lines
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 15 , Symposium S341: Challenges in Panchromatic Modelling with Next Generation Facilities , November 2019 , pp. 201 - 205
Copyright
© International Astronomical Union 2020

References

Boquien, M., Burgarella, D., Roehlly, Y., Buat, V., Ciesla, L., Corre, D., Inoue, A. K., Salas, H., et al. 2018, arXiv:1811.03094Google Scholar
Bruzual, G. & Charlot, S. 2003, MNRAS, 344, 100010.1046/j.1365-8711.2003.06897.xCrossRefGoogle Scholar
Buat, V., Boquien, M., Małek, K., Corre, D., Salas, H., Roehlly, Y., Shirley, R., Efstathiou, A., et al. 2018, A&A, 619, A135Google Scholar
Burgarella, D., Buat, V., Iglesias-Páramo, J., et al. 2005, MNRAS, 360, 141310.1111/j.1365-2966.2005.09131.xCrossRefGoogle Scholar
Calzetti, D. 1997, AJ, 113, 16210.1086/118242CrossRefGoogle Scholar
Calzetti, D., Armus, L., Bohlin, R. C., Kinney, A. L., Koornneef, J., Storchi-Bergmann, T., et al. 2000, ApJ, 533, 68210.1086/308692CrossRefGoogle Scholar
de Barros, S., Schaerer, D., Stark, D. P., et al. 2014, A&A, 563, A81Google Scholar
Holden, B. P., Oesch, P. A., González, V. G., Illingworth, G. D., Labbé, I., Bouwens, R., Franx, M., van Dokkum, P., et al. 2016, ApJ, 820, 7310.3847/0004-637X/820/1/73CrossRefGoogle Scholar
Inoue, A. K. 2011, MNRAS, 415, 292010.1111/j.1365-2966.2011.18906.xCrossRefGoogle Scholar
Magdis, G. E., Elbaz, D., Hwang, H. S., Daddi, E., Rigopoulou, D., Altieri, B., Andreani, P., Aussel, H., et al. 2010, ApJ, 720, L18510.1088/2041-8205/720/2/L185CrossRefGoogle Scholar
Noll, S., Burgarella, D., Giovannoli, E., Buat, V., Marcillac, D., Muñoz-Mateos, J. C., et al. 2009, A&A, 507, 1793Google Scholar
Puglisi, A., Rodighiero, G., Franceschini, A., Talia, M., Cimatti, A., Baronchelli, I., Daddi, E., Renzini, A., et al. 2016, A&A, 586, A83Google Scholar
Salpeter, E. E. 1955, ApJ, 121, 16110.1086/145971CrossRefGoogle Scholar
Sawicki, M. 2012, PASP, 124, 120810.1086/668636CrossRefGoogle Scholar
Schenker, M. A., Ellis, R. S., Konidaris, N. P., Stark, D. P., et al. 2013, ApJ, 777, 6710.1088/0004-637X/777/1/67CrossRefGoogle Scholar
Stark, D. P., Schenker, M. A., Ellis, R., Robertson, B., McLure, R., Dunlop, J., et al. 2013, ApJ, 763, 12910.1088/0004-637X/763/2/129CrossRefGoogle Scholar
Troncoso, P., Maiolino, R., Sommariva, V., Cresci, G., Mannucci, F., Marconi, A., Meneghetti, M., Grazian, A., et al. 2014, A&A, 563, A58Google Scholar
Yuan, F.-T., Argudo-Fernández, M., Shen, S., Hao, L., Jiang, C., Yin, J., Boquien, M., Lin, L., et al. 2018, A&A, 613, A13Google ScholarPubMed