/ftp/cats/aliases/G/./GFG2013



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J/A+A/551/A93 Nebular emission from z= 2-3 star-forming galaxies (Guaita+, 2013)
The following files can be converted to FITS (extension .fit or fit.gz)
	table3.dat table4.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/551/A93
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drwxr-xr-x 38 cats archive 4096 Jan 18 2018 [Up] drwxr-xr-x 4 cats archive 311 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 479 Dec 19 2022 .message -r--r--r-- 1 cats archive 7093 Nov 2 2013 ReadMe -rw-r--r-- 1 cats archive 253 Apr 10 2015 +footg5.gif -rw-r--r-- 1 cats archive 2215 Apr 10 2015 +footg8.gif -r--r--r-- 1 cats archive 1115 Aug 23 2013 table3.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 11244 Aug 23 2013 table4.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/A+A/551/A93 Nebular emission from z= 2-3 star-forming galaxies (Guaita+, 2013) ================================================================================ Magellan/MMIRS near-infrared multi-object spectroscopy of nebular emission from star-forming galaxies at 2 < z < 3. Guaita L., Francke H., Gawiser E., Bauer F.E., Hayes M., Oestlin G., Padilla N. <Astron. Astrophys., 551, A93 (2013)> =2013A&A...551A..93G ================================================================================ ADC_Keywords: Galaxies, spectra ; Spectroscopy ; Equivalent widths Keywords: techniques: spectroscopic - galaxies: high-redshift - galaxies: star formation Abstract: To investigate the ingredients, which allow star-forming galaxies to present Lyalpha line in emission, we studied the kinematics and gas phase metallicity of the interstellar medium. We used multi-object near-infrared spectroscopy with Magellan/MMIRS to study nebular emission from z= 2-3 star-forming galaxies discovered in three MUSYC fields. Description: MMIRS is a near-IR imager and multi-object spectrograph with a 4'x6.9' field-of-view, operating on the Magellan Clay telescope since the end of 2010. Mask design followed the MMT mask preparation procedure. The objects studied in this paper come from two two-night observing runs in 1-2 Nov. 2010 and 19-20 May 2011.