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28 May 2022
 
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NIBLES - an HI census of stellar mass selected SDSS galaxies: I. The Nanc{c}ay HI survey
W. van Driel ; Z. Butcher ; S. Schneider ; M.D. Lehnert ; R. Minchin ; S-L. Blyth ; L. Chemin ; N. Hallet ; T. Joseph ; P. Kotze ; R.C. Kraan-Korteweg ; A.O.H. Olofsson ; M. Ramatsoku ;
Date 10 Jul 2016
AbstractTo investigate galaxy properties as a function of their total stellar mass, we obtained 21cm HI line observations at the 100-m class Nanc{c}ay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900<cz<12,000 km/s), dubbed the Nanc{c}ay Interstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. They were selected evenly over their entire range of absolute SDSS z-band magnitudes (-13.5 to -24 mag), which were used as a proxy for their stellar masses. Here, a first, global presentation of the observations and basic results is given, their further analysis will be presented in other papers in this series. The galaxies were selected based on their properties, as listed in SDSS DR5. Comparing this photometry to their total HI masses, we noted that, for a few percent, the SDSS magnitudes appeared severely misunderestimated, as confirmed by our re-measurements for selected objects. Although using the later DR9 results eliminated this problem in most cases, 384 still required manual photometric source selection. Usable HI spectra were obtained for 2600 galaxies, of which 1733 (67%) were clearly detected and 174 (7%) marginally. The spectra for 241 other observed galaxies could not be used for further analysis owing to problems with either the HI or the SDSS data. We reached the target number of about 150 sources per half-magnitude bin over the Mz range -16.5 to -23 mag. Down to -21 mag the overall detection rate is rather constant at the ~75% level but it starts to decline steadily towards the 30% level at -23 mag. Making regression fits by comparing total HI and stellar masses for our sample, including our conservatively estimated HI upper limits for non-detections, we find the relationship log(M_HI/M*) = -0.59 log(M*) + 5.05, which lies significantly below the relationship found in the M_HI/M* - M* plane when only using HI detections.
Source arXiv, 1607.2787
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