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Keywords:

  • errata, addenda;
  • astronomical data bases: miscellaneous;
  • galaxies: active;
  • galaxies: statistics;
  • cosmology: observations

The paper ‘One Centimetre Receiver Array-prototype observations of the CRATES sources at 30 GHz’ was published in Mon. Not. R. Astron. Soc. 410, 2690–2697 (2011).

In the paper, an error was made in the application of the gain–elevation corrections for data taken between 2009 August and 2010 June. As this error affected both calibrator and source measurements, it has resulted in an offset of up to 1.75σ in the mean flux densities for some sources (or up to 25 per cent of the mean source flux density for the faintest sources). It has also resulted in an increased scatter between the measurements, which has led to a small overestimate of the uncertainty on the mean flux densities. The average change of all of the source flux densities is a decrease of 1.2 per cent. This is sufficiently small that our scientific conclusions are unaltered.

The updated spectral index distributions are shown in Fig. 1, and the mean and spread for α301.4, α304.8 and α308.4 are unchanged from the values given in the paper. The other source statistics change slightly, as follows:

image

Figure 1. Updated spectral index distributions for the sources in the CRATES sample observed with OCRA-p; the difference from fig. 5 in the original paper is negligible.

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  • (i) 
    76 per cent of the sources have steepened at α308.4 compared with α4.81.4;
  • (ii) 
    33 sources (5.5 per cent) appear to be gigahertz-peaked sources that peak between 4.8 and 8.4 GHz (defined by α4.81.4 > 0.5 and α308.4 < −0.5);
  • (iii) 
    63 sources (10 per cent) are flat or rising (α4.81.4 > 0 and α308.4 > 0);
  • (iv) 
    61 sources (10 per cent) are inverted (α4.81.4 < 0 and α308.4 > 0).

The application of the Spearman-rank correlation test of the Fermi-radio correlation using the revised mean flux densities gives ρ= 0.69 compared with the previous value of ρ= 0.71.

An updated version of Table 1[comparing the One Centimetre Receiver Array (OCRA) measurements with those by the Wilkinson Microwave Anisotropy Probe (WMAP)] is included here. An updated version of the flux densities in table 3 of Peel et al. (2011) is available in the Supporting Information to that paper, which has been corrected, as well as online at http://www.jodrellbank.manchester.ac.uk/research/ocra/crates/.

Table 1.  Comparison of 42 CRATES sources measured with OCRA-p that are also in the WMAP 7-yr point source catalogue (Gold et al. 2010). The flux densities are given in Jy. Two sources – J1343+6602 and J1344+6606 – are combined in WMAP (denoted with ‘P’).
NameOCRA 30 GHzWMAP K 23 GHz Flux density/JyWMAP Ka 33 GHzNotes
J1048+71431.14±0.091.21±0.611.11±0.73 
J1101+72250.93±0.080.92±0.160.91±0.18a
J1302+57480.43±0.040.81±0.170.67±0.18a
J1343+66020.32±0.030.70±0.170.34±0.13Pa
J1344+66060.36±0.04as aboveas above 
J1419+54230.62±0.120.86±0.180.89±0.25a
J1436+63361.04±0.080.68±0.230.50±0.28a
J1549+50380.57±0.050.85±0.140.64±0.11 
J1604+57140.48±0.080.81±0.120.77±0.17a
J1625+41340.45±0.040.96±0.060.78±0.14 
J1635+38082.47±0.283.72±0.864.06±1.08 
J1637+47171.27±0.121.10±0.261.12±0.26 
J1638+57201.66±0.151.67±0.431.68±0.48 
J1642+39485.72±0.486.60±0.905.95±0.94 
J1642+68564.78±0.411.82±0.681.85±0.85 
J1648+41040.46±0.040.67±0.080.82±0.20a
J1653+39450.90±0.101.25±0.121.16±0.16a
J1657+57050.51±0.040.41±0.10 
J1658+47370.68±0.061.16±0.101.16±0.10 
J1700+68300.39±0.050.32±0.070.51±0.08 
J1701+39540.52±0.040.58±0.090.77±0.20 
J1716+68360.60±0.050.58±0.110.51±0.16 
J1727+45301.25±0.110.89±0.440.94±0.52 
J1734+38571.05±0.091.20±0.111.26±0.24 
J1735+36160.51±0.040.71±0.090.70±0.16 
J1739+47370.67±0.050.86±0.120.77±0.20 
J1740+52111.16±0.101.22±0.261.18±0.20 
J1748+70050.47±0.040.50±0.150.63±0.16 
J1753+44090.42±0.040.63±0.210.61±0.13a
J1800+38480.89±0.080.91±0.110.72±0.27a
J1801+44041.18±0.101.36±0.261.52±0.27 
J1806+69491.52±0.131.42±0.141.36±0.22 
J1812+56030.27±0.030.21±0.110.30±0.22 
J1824+56511.60±0.141.47±0.261.24±0.18 
J1835+32410.37±0.030.81±0.090.81±0.15 
J1842+68090.95±0.091.29±0.271.40±0.30a
J1849+67053.68±0.301.63±0.661.81±0.78a
J1927+61170.58±0.050.95±0.260.94±0.22 
J1927+73582.91±0.253.57±0.273.33±0.36 
J2007+66070.63±0.060.78±0.090.57±0.08 
J2009+72290.60±0.050.64±0.120.78±0.16 
J2015+65540.36±0.030.75±0.140.79±0.15a

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