SIMBAD references

We present a study of the far-infrared (IR) properties of a stellar mass selected sample of 1.5 < z < 3 galaxies with log(M_*/M_☉) > 9.5 drawn from the Great Observatories Origins Deep Survey (GOODS) Near Infrared Camera and Multi-Object Spectrometer (NICMOS) Survey (GNS), the deepest H-band Hubble Space Telescope survey of its type prior to the installation of Wide Field Camera 3 (WFC3). We use far-IR and submm data from the Photoconductor Array Camera and Spectrometer (PACS) and Spectral and Photometric Imaging Receiver (SPIRE) instruments on-board Herschel, taken from the PACS Evolutionary Probe (PEP) and Herschel Multi-Tiered Extragalactic Survey (HerMES) key projects, respectively. We find a total of 22 GNS galaxies, with median log(M_*/M_☉) = 10.8 and z = 2.0, associated with 250µm sources detected with signal-to-noise ratio (SNR) > 3. We derive mean total IR luminosity logL_IR(L_☉) = 12.36±0.05 and corresponding star formation rate (SFR)_ IR + UV_= (280 ±40)M_☉yr^–1 for these objects, and find them to have mean dust temperature T_dust ≈ 35K. We find that the SFR derived from the far-IR photometry combined with ultraviolet (UV)-based estimates of unobscured SFR for these galaxies is on average more than a factor of 2 higher than the SFR derived from extinction-corrected UV emission alone, although we note that the IR-based estimate is subject to substantial Malmquist bias. To mitigate the effect of this bias and extend our study to fainter fluxes, we perform a stacking analysis to measure the mean SFR in bins of stellar mass. We obtain detections at the 2–4σ level at SPIRE wavelengths for samples with log(M_*/M_☉) > 10. In contrast to the Herschel detected GNS galaxies, we find that estimates of SFR_ IR + UV_for the stacked samples are comparable to those derived from extinction-corrected UV emission, although the uncertainties are large. We find evidence for an increasing fraction of dust obscured star formation with stellar mass, finding \mi SFR\mi IR\mo/\mi SFR\mi UVprop.to\mi M\mo *\mn 0.7\mo ±\mn 0.2, which is likely a consequence of the mass–metallicity relation. Constraining the variation of fundamental constants at z ∼ 1.3 using 21-cm absorbers