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ABSTRACT  We present a study of the far‐infrared (IR) properties of a stellar mass selected sample of 1.5 &lt;  z  &lt; 3 galaxies with log ( M  * /M ⊙ ) &gt; 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 250 μm sources detected with signal‐to‐noise ratio (SNR) &gt; 3. We derive mean total IR luminosity log  L  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  ≈ 35 K. 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 ⊙ ) &gt; 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, findingSFR    IR    /    SFR    UV    ∝   M  *   0.7  ±  0.2, which is likely a consequence of the mass–metallicity relation.

Herschel observations of a z ∼ 2 stellar mass selected galaxy sample drawn from the GOODS NICMOS Survey