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|Title:||Emission-line-selected galaxies at z = 0.6-2 in GOODS South: Stellar masses, SFRs, and large-scale structure||Authors:||Kochiashvili, I.
Fynbo, J. P. U.
Cuby, J. -G.
|Issue Date:||2015||Journal:||ASTRONOMY & ASTROPHYSICS||Number:||580||First Page:||A42||Abstract:||We have obtained deep NIR narrow and broad (J and Y) band imaging data of the GOODS-South field. The narrow band filter is centered at 1060 nm corresponding to redshifts z = 0.62,1.15,1.85 for the strong emission lines Hα, [Oiii]/Hβ and [Oii], respectively. From those data we extract a well defined sample (M(AB) = 24.8 in the narrow band) of objects with large emission line equivalent widths in the narrow band. Via SED fits to published broad band data we identify which of the three lines we have detected and assign redshifts accordingly. This results in a well defined, strong emission line selected sample of galaxies down to lower masses than can easily be obtained with only continuum flux limited selection techniques. We compare the (SED fitting-derived) main sequence of star-formation (MS) of our sample to previous works and find that it has a steeper slope than that of samples of more massive galaxies. We conclude that the MS steepens at lower (below M<SUB>⋆</SUB> = 10<SUP>9.4</SUP>M<SUB>☉</SUB>) galaxy masses. We also show that the SFR at any redshift is higher in our sample. We attribute this to the targeted selection of galaxies with large emission line equivalent widths, and conclude that our sample forms the upper boundary of the MS. We briefly investigate and outline how samples with accurate redshifts down to those low stellar masses open a new window to study the formation of large scale structure in the early universe. In particular we report on the detection of a young galaxy cluster at z = 1.85 which features a central massive galaxy which is the candidate of an early stage cD galaxy, and we identify a likely filament mapped out by [Oiii] and Hβ emitting galaxies at z = 1.15. <P />Tables 1 and 2, and Appendix A are available in electronic form at <A href="http://www.aanda.org/10.1051/0004-6361/201425535/olm">http://www.aanda.org</A>||Acknowledgments:||We thank Thomas Krühler and Jens Hjorth for useful suggestions. Special thanks to Olivier Ilbert for immense help with the LePhare code. We thank the referee for comments that helped improve the paper. The Dark Cosmology Centre is funded by the DNRF. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/20072013)/ERC Grant agreement no. EGGS-278202. B.C. acknowledges support from the ERC starting grant CALENDS. This research has made use of the SIMBAD database, operated at the CDS, Strasbourg, France.||URI:||http://hdl.handle.net/20.500.12386/23486||URL:||https://www.aanda.org/articles/aa/abs/2015/08/aa25535-14/aa25535-14.html||ISSN:||0004-6361||DOI:||10.1051/0004-6361/201425535||Bibcode ADS:||2015A&A...580A..42K||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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