Astronomy and Astrophysics, volume 595A, 118-118 (2016/11-1)
NIBLES: an H I census of stellar mass selected SDSS galaxies. I. The Nancay H I survey.
VAN DRIEL W., BUTCHER Z., SCHNEIDER S., LEHNERT M.D., MINCHIN R., BLYTH S.-L., CHEMIN L., HALLET N., JOSEPH T., KOTZE P., KRAAN-KORTEWEG R.C., OLOFSSON A.O.H. and RAMATSOKU M.
Abstract (from CDS):
To investigate galaxy properties as a function of their total stellar mass, we obtained 21 cm HI line observations at the 100-m class Nancay Radio Telescope of 2839 galaxies from the Sloan Digital Sky Survey (SDSS) in the Local Volume (900<cz<12000km/s), dubbed the NancayInterstellar Baryons Legacy Extragalactic Survey (NIBLES) sample. They were selected evenly over their entire range of absolute SDSS z-band magnitudes (Mz~-13.5 to -24mag), which were used as a proxy for their stellar masses.In this paper, 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 originally 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 of the 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 -23mag. Down to -21mag the overall detection rate is rather constant at the ∼75% level but it starts to decline steadily towards the 30% level at -23mag. 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(MHI/M*)=-0.59log(M*)+5.05, which lies significantly below the relationship found in the MHI/M*-M* plane when only using HI detections.
© ESO, 2016
galaxies: general - galaxies: distances and redshifts - galaxies: ISM - galaxies: photometry - radio lines: galaxies
VizieR on-line data:
<Available at CDS (J/A+A/595/A118): tablea12.dat tablea3.dat>
ASK 170306, ASK 178783, ASK 284467, ASK 35835, ASK 36025, ASK 401526, ASK 73575 and ASK 78238, PGC 4009364, PGC 4017004, PGC 4086014, PGC 4094769, PGC 4102270 not identified.
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