The 2dF Galaxy Redshift Survey: spectra and redshifts
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Citations
First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters
Simulations of the formation, evolution and clustering of galaxies and quasars
Detection of the baryon acoustic peak in the large-scale correlation function of SDSS luminous red galaxies
The physical properties of star-forming galaxies in the low-redshift universe
Cosmological constant—the weight of the vacuum
References
Maps of Dust Infrared Emission for Use in Estimation of Reddening and Cosmic Microwave Background Radiation Foregrounds
Maps of Dust IR Emission for Use in Estimation of Reddening and CMBR Foregrounds
A survey of galaxy redshifts. I. Data reduction techniques.
The 2dF galaxy redshift survey: near-infrared galaxy luminosity functions
A measurement of the cosmological mass density from clustering in the 2dF Galaxy Redshift Survey
Related Papers (5)
The Sloan Digital Sky Survey: Technical summary
First year Wilkinson Microwave Anisotropy Probe (WMAP) observations: Determination of cosmological parameters
The Seventh Data Release of the Sloan Digital Sky Survey
Frequently Asked Questions (10)
Q2. What is the effect of the close packing of the fibres on the detector?
The close packing of the fibres on the detector means that their spatial profiles overlap, producing cross-talk between neighbouring spectra.
Q3. What is the spectra that is not a fluxcalibrated?
The spectra, which are not fluxcalibrated, are finally multiplied by a simple quadratic approximation to the mean flux calibration correction in order to give appropriate weighting across the whole spectral range.
Q4. How many unallocated fibres can be assigned?
If no unallocated fibres can be assigned the authors repeat this process recursively until one of the following conditions have been satisfied: either (i) a previously unallocated fibre is allocated (implying that u has been allocated and that all previously allocated targets remain allocated), or (ii) the search exceeds a depth of 10 iterations.
Q5. What is the average rms residual for the spectral range?
The final fits usually include 21–22 lines over the 4400-Å spectral range, and have typical rms residuals of 0.3 Å (0.07 pixels).
Q6. What is the smallest and homogeneous set of radio-source spectra?
Using 20 per cent of the full 2dFGRS area, Sadler et al. find 757 optical counterparts for NVSS sources – the largest and most homogeneous set of radio-source spectra to date.
Q7. Why is the slit block not precisely reproducible?
This is necessary because the positioning of the slit block is not precisely reproducible, so that the locations of the fibres on the CCD can change by a few pixels, and occasionally the first or last fibre may fall off the edge of the detector.
Q8. How many unallocated fibres are allocated to blank sky positions?
After this correction to the configuration, a number of unallocated fibres (at least 10 for each spectrograph) are allocated to blank sky positions.
Q9. How does the algorithm compensate for the higher surface density of targets in the region of overlap?
This results in a higher surface density of targets in the region of overlap, for which the authors compensate by reducing the separation in declination of the tiling strips in the QSO survey regions to 75 per cent of the original value (i.e., to 18: 125).
Q10. What is the rms precision of single measurements?
Table 1 gives the rms precision of single measurements as a function of redshift quality class or measurement method (ABS¼ cross-correlation of absorption features; EMI¼ automatic fit to emission lines; MAN¼manual fit to features).