Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://www.2dfquasar.org/Papers/2001MNRAS.322L..29C.pdf Äàòà èçìåíåíèÿ: Thu Mar 4 03:27:45 2004 Äàòà èíäåêñèðîâàíèÿ: Mon Oct 1 19:35:52 2012 Êîäèðîâêà: Ïîèñêîâûå ñëîâà: clouds

Mon. Not. R. Astron. Soc. 322, L29 ± L36 (2001)

The 2dF QSO Redshift Survey ± V. The 10k catalogue
S. M. Croom,1w R. J. Smith,2 B. J. Boyle,1 T. Shanks,3 N. S. Loaring,4 L. Miller4 and I. J. Lewis1
1 2 3 4

Anglo-Australian Observatory, PO Box 296, Epping, NSW 1710, Australia Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD Department of Physics, University of Durham, South Road, Durham DH1 3LE Department of Physics, Oxford University, 1 Keble Road, Oxford OX1 3RH

Accepted 2001 March 7. Received 2001 March 6; in original form 2001 February 16

We present a catalogue comprising over 10 000 QSOs covering an effective area of 289.6 deg2, based on spectroscopic observations with the 2-degree Field (2dF) instrument at the Anglo-Australian Telescope. This catalogue forms the first release of the 2dF QSO Redshift Survey. QSO candidates with 18:25 , bJ , 20:85 were obtained from a single homogeneous colour-selected catalogue based on APM measurements of UK Schmidt photographic material. The final catalogue will contain approximately 25 000 QSOs and will be released to the public at the end of 2002, one year after the observational phase is concluded. Key words: catalogues ± surveys ± white dwarfs ± galaxies: active ± quasars: general ± galaxies: Seyfert.

ABSTR A CT

1

I NTR O DUC TION

The aim of the 2dF QSO Redshift Survey (2QZ) is to measure redshifts for ,25 000 optically selected QSOs with bJ , 20:85 and z , 3: The spectra have been obtained with the 2-degree Field (2dF) instrument (Lewis, Glazebrook & Taylor 1998) on the Anglo-Australian Telescope (AAT). The final catalogue will represent a factor of ,50 increase in the number of QSOs identified in a single homogeneous survey to this magnitude limit (cf. the Durham/AAT Survey: Boyle et al. 1990). The primary science goal of this survey is to obtain an accurate measure of the large-scale structure in the Universe out to high redshifts, z , 3; and largescales, ,1000 h21 Mpc, via thestudy of QSO clustering. As of 2001 January, the survey is over 60 per cent complete. To expedite community access to the 2QZ, we are releasing the catalogue in two stages. This paper describes the first release containing 20 590 objects, including 11 005 QSOs, for which we have obtained 2dF spectra. The release represents the `most complete' subset of the entire survey observed prior to 2000 December ± containing all fields for which we have achieved a spectroscopic completeness of 85 per cent or greater. This catalogue has been used to derive results on the QSO correlation function (Croom et al. 2001, Paper II), the power spectrum (Hoyle et al. 2001, Paper IV) and the composite spectrum (Smith et al., in preparation, Paper VI). Results on the QSO luminosity function from the 2QZ (Boyle et al. 2000, Paper I) were based on an earlier version of the catalogue comprising ,5000 QSOs. When complete the catalogue will contain approximately 48 000 objects,
w

including 25 000 QSOs. The final catalogue will be released at the end of 2002, one year after the observational phase of the survey is concluded, currently planned for the end of 2001. This paper describes the first release catalogue, hereinafter the 2QZ 10k catalogue, of the 2QZ. Sections 2 and 3 describe the spectroscopic observations and catalogue format. Section 4 then discusses estimates of the catalogue quality, and presents a new estimate of the QSO luminosity function.

2

S PE CTR O SC OPIC OBSER VA T IO NS

2.1 The candidate catalogue QSO candidates with 18:25 , bJ , 20:85 were selected for observation with 2dF from measurements of ubJr UK Schmidt photographic material. Full details are given in Smith et al. (2001, Paper III). The 2QZ area comprises 30 UKST fields, arranged in two 758 á 58 declination strips centred on d 2308 and d 08: The d 2308 strip extends from a 21h 40 to a 3h 15 in the South Galactic Cap and the equatorial strip from a 9h 50 to a 14h 50 in the North Galactic Cap (B1950). When complete, the total survey area will be 740 deg2, allowing for regions of sky excised around bright stars. The 2QZ area forms an exact subset of the 2dF Galaxy Redshift Survey (2dFGRS: see Colless 1998) area. 2dF observations of the 2QZ were therefore combined with those of the 2dFGRS. A tiling algorithm devised by the 2dFGRS team was used to determine the positions of individual 2dF field centres in order to obtain near-complete spectroscopic coverage (95 per cent for galaxies, 99 per cent for QSO candidates) for the 2QZ and

E-mail: scroom@aaoepp.aao.gov.au

q 2001 RAS


L30

S. M. Croom et al.
turned out to be QSOs or galaxies. The ubJr colour-selection process used to generate the input catalogue has non-negligible contamination (originally estimated to be ,45 per cent, see Paper III) from Galactic stars (subdwarfs and white dwarfs) and compact emission-line galaxies. autoz fits a variety of templates to each observed spectrum. These templates include QSOs, both `normal' and broad-absorption-line (BAL) QSOs, emission-line galaxies and a library of stellar spectra including main-sequence types from O to M and DA, DB and DZ white dwarfs. The autoz program uses the fact that data are collected on a large number of different objects (QSOs, galaxies and stars) at once (,200 per spectrograph) to estimate the wavelength-dependent sensitivity and noise. These terms are then taken into account when carrying out a x 2 fit to the templates to derive the best-fitting model. In general autoz produces reliable identifications for a wide variety of the objects. However, we have carried out manual checks of all spectra in the survey to identify the small fraction of objects with peculiar or low signal-to-noise ratio (S/N) spectra which autoz had difficulty in identifying correctly. Each member of the 2QZ team independently examined 5000±6000 spectra by eye and corrected any autoz identifications that were clearly in error. As a further double-check, two members of the survey (BJB and SMC) re-examined all spectra to ensure a degree of homogeneity in this re-classification procedure. The sources are classified into six categories: QSO: spectrum with one or more broad (.1000 km s21) emission lines; NELG (narrow-emission-line galaxy): galaxy spectrum with one or more narrow (,1000 km s21) emission lines; gal: galaxy spectrum with no emission lines; star: Galactic star spectrum; cont: high-S/N spectrum S=N . 10 with no identifiable emission or absorption features; ??: unclassifiable spectrum because of low S/N. The quality of the identification and redshift estimation is divided into three levels of confidence: quality 1: high-quality identification or redshift; quality 2: low-quality identification or redshift; quality 3: no classification or redshift assignment. A quality flag is assigned independently to both the identification and redshift of an object. Approximately 6 per cent of objects were found to have low-quality identifications (quality 2); these objects appear in the final catalogue with a `?' against their identification (apart from objects identified as cont, which all have quality 2 identifications). For each 2dF pointing we calculate a spectroscopic completeness, being the ratio of objects observed in the field with quality 1 or quality 2 identifications to the total number of spectroscopically observed objects. Stars are likely to dominate the unidentified population, at least for low levels of incompleteness. This is because their weak spectral features make them very difficult to identify from low-S/N spectra. In contrast, QSOs with broad emission lines should be amongst the easiest class of objects to identify from low-S/N spectra. To establish the spectroscopic incompleteness level at which we also begin to lose significant numbers of QSOs, we compared the normalized QSO number ± magnitude relation obtained from fields with greater than 95 per cent completeness with those from fields with completenesses in the range 90±95; 85±90; 80±85 and 75±80 per cent. Using a Kolmogorov ± Smirnov test, we found that the N(m) showed a
q 2001 RAS, MNRAS 322, L29 ± L36

2dFGRS targets in the survey area with the minimum number of individual 2dF pointings. The 2QZ colour selection is designed to be largely complete (.90 per cent) for QSOs with 0:3 , z , 2:2: At higher redshifts, 2:2 , z , 3:0; the photometric completeness of the survey gradually drops, with the highest redshift QSOs in the 2QZ being found at z . 3: Paper I provides an estimate of the completeness contours based on ubJr selection as a function of bJ and z. The stellar morphological criterion also causes incompleteness at low redshifts. This is more difficult to estimate but it is likely to cause some form of incompleteness up to z , 0:5: The photometric errors in the magnitudes will be discussed extensively in Paper III. They are approximately constant over the magnitude range of the survey sbJ sr 0:1; su 0:15: Independent CCD sequences have been used to calibrate each UKST field (Boyle, Shanks & Croom 1995; Croom et al. 1999). 2.2 2dF observations

Observations of the 2QZ began in 1997 October. This initial release is based on 304 individual 2dF fields observed over the period 1997 October to 2000 November. The two 2dF spectrographs each contain one 1024 á 1024 Tektronix CCD with 24-mm pixels and are each fed by 200 optical fibres. 2QZ objects were observed with 2dF using the low-resolution 300B gratings, é é providing a dispersion of 178.8 A mm21 (4.3 A pixel21) and a é resolution of .8.6 A (.2 pixel FWHM) over the range 3700±7900 A: Each optical fibre has a diameter on the sky of 2.16 arcsec at the centre of a field, falling to 2 arcsec at the edge of the field. The fibre spectra are projected to ,1.5 pixel (FWHM) on the detector and are each separated by ,5 pixel. Each field received an approximately 55-min integration 3 á 1100 s; combined with a flat-field, used to determine the positions of the fibre spectra on each CCD frame, and a CuArHe arc for wavelength calibration. The fields were observed in a wide variety of seeing conditions 1±2:5 arcsec FWHM) and transparency (details of conditions are included in the data release). Where possible, integration times were adjusted to match conditions. However, the instrumental requirement to observe 2dF fields at the hour angle for which they had been configured limited the opportunity to extend integration times significantly. As a result the quality of data can vary significantly from field to field. We have attempted to minimize the effects of this variation in the 10k release by only including objects from fields where at least 85 per cent of the objects observed yielded a spectroscopic identification. Data from 2dF were reduced using the pipeline reduction system 2dfdr (Bailey et al. 2001). CCD frames from each spectrograph were reduced separately. Following bias removal, fibre extraction and wavelength calibration, the transmissions of each fibre were normalized using the relative strengths of the night sky lines in each fibre spectrum. Sky subtraction was then done by subtracting a median sky spectrum determined from up to 20 skydedicated fibres in each frame (the minimum number of sky fibres used was six per spectrograph). 3 3.1 T HE CA T A LO GUE Spectroscopic identification

Reduced spectra of QSO candidates were then passed through a non-interactive program, autoz (Miller et al., in preparation), to classify individual objects and measure a redshift for those that


The 2QZ 10k catalogue

L31

Figure 1. The coverage map for the 2QZ 10k catalogue (taken from Paper II). The grey-scale indicates the observational completeness as a function of position on the sky. The tiling pattern of 2dF pointings used to cover the survey area can be seen clearly from this figure.

Table 1. Composition of the 2QZ catalogue. Identification QSO NELG star gal cont ?? Total Number 11 005 2104 5842 44 108 1487 20 590 Quality 1 10 689 2059 5081 37 ± ± 17 866 Quality 2 316 45 761 7 108 ± 1237 Percentage 53.4 10.2 28.4 0.2 0.5 7.2

Figure 2. The distribution of spectroscopic magnitude minus catalogue magnitude across a 2dF field for sources in the 10k catalogue. Contours are at Dmag 0:2 intervals, the thick solid contour being at Dmag 0 and the dashed line contours being at Dmag , 0:

significant difference (at the 99 per cent confidence level) for fields with lower than 85 per cent completeness. We therefore chose to include only those fields with spectroscopic completenesses of 85 per cent or greater in this initial release. This corresponds to 233 2dF fields. The coverage provided by these fields is indicated in Fig. 1 (taken from Paper II). Note that many areas of sky have not yet received their full complement of 2dF pointings in the adaptive tiling strategy. As a result, the current survey exhibits a spatially dependent observational incompleteness. Hence, although these fields have 85 per cent or greater identification rate, there remains a still larger fraction of incompleteness owing to sources that have yet to be observed. The 2QZ coverage map shown in Fig. 1 (released in digital form as a survey product) can be used to account for this. This coverage map is produced by calculating the ratio of spectroscopically observed objects to input catalogue objects in each region defined by the intersection of 2dF pointings. This distribution is then pixelized using 1 á 1 arcmin2 pixels to produce a final observational completeness map.
q 2001 RAS, MNRAS 322, L29 ± L36

We have also checked whether there is any variation in the catalogue over the area of one 2dF field. In Fig. 2 we plot the mean difference (Dmag) between the catalogue bJ magnitude and a bJ-band magnitude estimated from the spectroscopic data averaged over all the 2dF fields in the 10k catalogue (note that the averaging is carried out in flux, not magnitude). This is only a relative difference as the zero-points of the spectroscopic magnitudes are derived from the mean differences in each 2dF field. A positive Dmag indicates a spectroscopic magnitude that is fainter than the catalogue magnitude. We see that there is a deficit of flux at the edge of the field (particularly on the left side). This is probably due to residual errors that have not been completely accounted for by the 2dF astrometric model. This should not significantly affect the spatial distribution of QSOs in our sample, for two reasons. First, the tiling algorithm used to place the fields produces significant overlap so that any effect in a 2dF field area will be blurred out. Secondly, if we measure the identification rate as a function of field position, the only significant variation is at : radii .08 7. On scales smaller than this the mean completeness is .95 per cent. At the extreme edges of the field, radii .08 9, the : mean completeness only drops to .87 per cent. This variation in completeness, internal to 2dF fields, is of the same order as the variations in completeness between 2dF fields. 3.2 10k catalogue description Based on the criteria defined above, the initial release of the 2QZ catalogue contains entries for 20 590 objects, including 11 005 QSOs. The composition of the 10k catalogue as a function of spectroscopic class is given in Table 1. As defined by the fraction of objects with quality 1 or 2 classifications, the mean overall spectroscopic completeness of the catalogue is 93 per cent. The effective area of the survey (after correction for the observational


L32

S. M. Croom et al.

Figure 3. The number ± magnitude and number ± redshift distributions for the sources in the 10k catalogue. (a) The number ± magnitude distribution for QSOs (filled circles), stars (crosses), NELGs (filled squares) and unidentified objects (open triangles). (b) The number ± redshift distribution for QSOs (solid line) and NELGs (dotted line). No corrections for spectroscopic or photometric incompleteness are made in either figure. Table 2. Format for the 2QZ catalogue. The format entries are based on the standard fortran format descriptors. Field Name RA Dec RA Dec bJ u 2 bJ bJ 2 r Nobs Observation # 1 z1 q1 ID1 date1 fld1 S/N1 Observation # 2 z2 q2 ID2 date2 fld2 S/N2 zprev radio X-ray dust Format a20 i2 i2 f5.2 a1i2 i2 f4.1 f8.6 f9.6 f5.2 f5.2 f6.2 i1 f5.3 i2 a11 a8 i4 f6.2 f5.3 i2 a11 a8 i4 f6.2 f5.3 f6.1 f7.4 f5.3 Description IAU format object name RA J2000 (hh mm ss.ss) Dec. J2000 (^dd mm ss.s) RA J2000 (radians) Dec. J2000 (radians) bJ magnitude u 2 bJ colour bJ 2 r colour [including r upper limits as: bJ 2 r Number of observations

lim

2 10:0

Redshift Identification quality á10 1 redshift quality Identification Observation date 2dF field number á10 1 spectrograph number Signal-to-noise ratio in 4000±5000 A band Redshift Identification quality á10 1 redshift quality Identification Observation date 2dF field number á10 1 spectrograph number Signal-to-noise ratio in 4000±5000 A band á á Previously known redshift (Veron-Cetty & Veron 2000) 1.4-GHz radio flux, mJy (NVSS) X-ray flux, á10213 erg s21 cm22 (RASS) EB 2 V (Schlegel et al. 1998)

incompleteness) is 289.6 deg2. The function of bJ magnitudeis shown in source counts at all but the brightest a smooth redshift distribution over 0:1 , z , 3:0; with a maximum at 1:5 (Fig. 3b).

distribution of sources as a Fig. 3(a). QSOs dominate the magnitudes. The QSOs show the full range of the survey, the 2QZ median redshift z ,

The released catalogue is available as an ASCII file from http://www.2dfquasar.org. It is also available from CDS (http://cdsarc.u-strasbg.fr/) and the electronic version of MNRAS on Synergy. The catalogueformat is given in Table2. The first part of a catalogue entry contains details from the input catalogue, such as position and magnitude. We note in particular that sources
q 2001 RAS, MNRAS 322, L29 ± L36


The 2QZ 10k catalogue
which had only upper limits (i.e. non-detections) on the r plates are also included in the catalogue and have a listed bJ 2 r colour. In this case the colour term is bJ 2 r lim 2 10; the 210 being used to differentiate upper limits from normal colours (objects with real r-band detections have colours in the range 21:4 , bJ 2 r , 3:4; while upper limits have bJ 2 r , 29:8: The input catalogue information is followed by details of observations and identifications. In a number of cases (,1200 objects, ,5 per cent of the catalogue) we have two observations for a source. These are useful to assess the quality of the final catalogue (see below). The identification and redshift that we adopt are those with the lowest quality value (where the quality value is identification quality á10 1 redshift quality), and, if there are equal quality values, the highest S/N. In all cases the final adopted identification (ID) is listed as observation #1, with the lower quality observation being listed as observation #2. Finally we also include cross-matches to other selected data bases. Where a 2QZ source matches the position (to within 6 arcsec) of a previously known QSO or active á á galactic nucleus (AGN) in the catalogue of Veron-Cetty & Veron (2000), we include the previously known redshift. We also include radio fluxes at 1.4 GHz from the National Radio Astronomy Observatory (NRAO) Very Large Array (VLA) Sky Survey (NVSS: Condon et al. 1998) and X-ray fluxes from the ROSAT All Sky Survey (RASS: Voges et al. 1999, 2000), converting from RASS counts per second to flux (in erg s21 cm22) by multiplying by 5:6 á 10212 : Lastly we include an estimate of the Galactic reddening EB 2 V to each source taken from the work of Schlegel, Finkbeiner & Davis (1998). We do not distinguish between different NELG classifications (e.g. LINER, Seyferts) in the catalogue. Also, the spectral coverage provided by 2dF limits our ability to detect broad Mg ii l 2798 emission until z . 0:35: In some QSOs with 0:35 , z , 0:5; broad Mg ii is clearly detected with no corresponding broad Hb seen. Thus at lower redshifts, 0:15 , z , 0:35; some objects classified as NELGs on the basis of a narrow Hb line may exhibit broad Mg ii below the blue limit of the 2dF spectral window. For QSOs with z . 1:6; autoz fits both `normal' and BAL QSO templates. Objects identified as BALs are indicated by `QSO(BAL)' in the identification column. However, owing to the varied nature of BAL QSOs, this will not be a comprehensive list of BALs. A more detailed search for BALs has not yet been applied. Within the objects that we classify as stars, in the main we only give classifications for white dwarfs (WDs). We do not attempt spectral classification of main-sequence stars. The ,1000 WDs are mostly DAs with strong broad hydrogen Balmer absorption lines. At low S/N these can be confused with A stars. Only detailed fitting of the temperature and gravity of these stars can easily resolve this issue, and this is beyond the scope of the present paper. As well as DAs we also find a number of DB and DO WDs which are dominated by neutral and singly ionized helium respectively. A small number of DZs are also found, with broad calcium H and K absorption. The only other stellar types that we classify are six emission-line stars with strong hydrogen Balmer emission which we classify as cataclysmic variable (CV), and WD1M dwarf binary systems which are denoted as DA/M. We note that our code has been designed primarily simply to identify an object as a star (and therefore not a QSO), and that a more detailed analysis would no doubt provide more accurate classifications. The above classifications are denoted within the catalogue in parentheses after the main stellar identification [e.g. star(DB), star(CV)].
q 2001 RAS, MNRAS 322, L29 ± L36

L33

To allow others to carry out more detailed spectral analysis of both QSOs and other sources, spectra for all objects in the 2QZ 10k catalogue are provided as a primary data product in this release. This includes objects for which no identification could be made. Many of these are low-S/N spectra, but objects also remained unclassified for a number of other reasons. Occasionally a damaged fibre will produce fringing which shows up as a strong oscillation as a function of wavelength, rendering the underlying spectrum unusable. Also badly subtracted night sky emission (and in some cases moonlight) can sometimes seriously affect our ability to identify an object. The spectra are available in FITS format from thesamelocation as thecatalogue. Fig. 4 shows some example spectra from the 10k catalogue. Figs 4(a) and (b) are randomly selected QSO spectra. Figs 4(c) ± (f) show a range of peculiar spectra. Fig. 4(c) shows narrow emission lines implying a redshift of z 0:350 and broad emission lines suggesting a redshift of z 2:111: This appears to be a superposition of a QSO and a NELG, and as such is a potential gravitational lens. Fig. 4(d) shows the spectrum of a starburst 1 QSO; a less extreme version of the post-starburst object found in thecross-matching of the2QZ and the NVSS by Brotherton et al. (1999). Fig. 4(e) is a rare carbon (DQ) white dwarf and Fig. 4(f) is a white dwarf ± M dwarf binary system. 4 C A T ALOGUE Q U A LITY

4.1 Identification The overlap between the 2dF pointings has resulted in a number of objects in the 2QZ catalogue for which we have two independent 2dF observations. By comparing the identification/redshift estimates for different observations we can obtain an estimate of the reliability of the identification and accuracy of the redshift determination. For the 1019 objects with quality 1 or 2 identifications and more than one 2dF observations in fields included in the 10k catalogue, we find 87 with identifications that differ between the observations (excluding the five objects with identifications that changed from QSO to NELG but with the same redshift). This corresponds to a mis-identification rate of 8.5 per cent. If we restrict our attention to those objects with quality 1 identifications for both observations, this mis-identification rate drops to 3.8 per cent (34 objects with different classifications out of 889 objects). The mis-identification rate amongst class 2 identifications is higher. If we directly compare the identifications for those objects with a quality 2 identification from both observations, we find eight objects with different identifications from a total sample of 22 objects; equivalent to a mis-classification rate of 36 per cent. Comparison between quality 1 observations and quality 2 observations gives similar results. Of the 108 objects given an identification quality of 1 in one observation and a quality of 2 in the other, 45 (42 per cent) changed their identification in the subsequent higher quality observation. Thus the reliability of quality 2 identifications is approximately 60 per cent. A more quantitative measure of the quality of the spectrum (although not necessarily the reliability of the identification) is the S/N. If we restrict our comparison to objects where both spectra have S=N . 5 per pixel, we find a overall mis-classification rate of 1.7 per cent (six objects out of 359). 4.2 Redshift accuracy We can also obtain an estimate of the reliability of the redshift


L34

S. M. Croom et al.

Figure 4. A selection of spectra taken from the 2QZ 10k catalogue. (a) and (b) show two randomly selected examples of QSO spectra; (c) shows a potential gravitational lens, with QSO emission lines at z 2:111 (dashed lines) and NELG emission lines at z 0:350 (dotted lines); (d) shows a QSO starburst composite; (e) shows a DQ white dwarf with the molecular carbon (Swan) bands indicated; (f) shows a white dwarf ± M dwarf binary, showing broad hydrogen Balmer absorption in the blue and TiO absorption bands in the red.

determination from these repeat observations. For all quality 1 and 2 QSO, NELG or galaxy identifications there are 21 cases (out of 602 objects) where the redshift estimate differs by more than 5 per cent between the different observations. The comparison between the redshifts obtained from the different observations is shown in Fig. 5. All objects with significantly different redshifts are classified as QSOs; in most cases the difference in the redshift estimate is caused by the incorrect identification of a single emission line seen in the QSO spectrum. In total there are 518 QSOs with two observations, thus the reliability rate for QSO redshifts is 97 per cent and effectively 100 per cent for NELGs and galaxies. Excluding objects with incorrect redshifts owing to the misidentification of emission lines, the rms difference between the redshift measurements is 0.005. We also compared our identifications with those objects that had been previously classified as QSOs. Based on positional á á matches with QSOs in the Veron-Cetty & Veron (2000) catalogue, we found that 331 objects in the 2QZ 10k catalogue had been previously identified as QSOs. These objects are flagged in the

released catalogue (see Table 2). Of these, 305 were confirmed as QSOs by 2QZ. However, 33 QSOs were found to have redshifts that disagreed significantly between the 2QZ and previous estimates. Visual inspection of the 2QZ spectrum revealed that, in all but one case, the 2QZ redshift was secure (i.e. two or more strong emission lines correctly identified). The remaining 29 objects were not classified as QSOs in the 2QZ; these identifications included seven stars (two white dwarfs), four star?s, three NELGs, one cont, onecont?, oneQSO? and 13 with unclassifiable spectra. Visual inspection of the quality 1 spectra confirmed the 2dF classification in all cases. In summary, the comparison between independent observations of over 1000 objects in the 2QZ release (approximately 5 per cent of the catalogue) reveals the overall reliability of the identifications is over 90 per cent. For quality 1 classifications this figure is close to 97 per cent; for quality 2 classifications the reliability is approximately 60 per cent. The redshift reliability for QSOs is 97 per cent with an rms error in the redshift measurement of sz 0:0035:
q 2001 RAS, MNRAS 322, L29 ± L36


The 2QZ 10k catalogue

L35

Figure 5. Comparison between redshifts obtained for different observations of the same object. Figure 7. Upper panel: derived number ± magnitude, N(m), relation for QSOs with M B , 223 and 0:3 , z , 2:3 in the 2QZ survey (filled dots) and the prediction from the best-fitting polynomial luminosity evolution model. The data have been corrected for photometric and spectroscopic incompleteness as in Paper I. Lower panel: observed number ± redshift relation, N(z), for the 2QZ QSOs with M B , 223 and 0:3 , z , 2:3 together with the prediction from the same model as in the upper panel. Here the model prediction has been corrected to take into account the survey incompleteness.

Figure 6. The optical QSO luminosity function derived from the 10k catalogue and the LBQS for an Einstein ± de Sitter universe. Only QSOs with M B , 223 and 0:3 , z , 2:3 are included in this analysis.

4.3

The 10k luminosity function

For completeness, we have also repeated the analysis of Paper I to derive a luminosity function (LF) of the QSOs in the 10k catalogue, including objects from the Large Bright Quasar Survey (LBQS: Hewett, Foltz & Chaffee 1995) at bright magnitudes. In total, 9633 QSOs with M B , 223 and 0:3 , z , 2:3 (8743 from the 2QZ and 890 from the LBQS) were used to obtain the binned LF for an Einstein ± de Sitter universe H 0 50 km s21 Mpc21 which is shown in Fig. 6. We also fitted to this data set a two-power-law LF and pure luminosity evolution models with polynomial evolution in L* such 2 that L*z G 10k1 z1k2 z : The best-fitting model has F* 0:2 á
q 2001 RAS, MNRAS 322, L29 ± L36

10215 Mpc23 mag21 ; a 3:28; b 1:08; M B 221:45; k1 * 1:41 and k2 20:29 (see Paper I). However, even this best-fitting model is formally rejected at high significance (.99 per cent confidence) by the 2QZ data. A comparison between the 2QZ data set used in the LF anlaysis and the best-fitting model is shown in Fig. 7. This illustrates that, while the overall fit of the model to the data set is good, the cause of the disagreement is a sharp peak in the redshift distribution of 2QZ QSOs at z . 1:5 which cannot be matched by the evolution model. This is likely to be caused by systematic variations in our ability to determine a QSO redshift. z . 1:5 corresponds to the redshift where the C iv emission line moves into the observable wavelength range of 2dF. This strong emission line will increase the probability of obtaining a goodquality identification and redshift. The new measurement of the QSO LF demonstrates that studies such as these are now limited by the systematic errors, rather than Poisson errors from small numbers of objects. When the completed catalogue is released, we will provide independent measurements of these systematic effects, which can be derived from measurements of the efficiency of our automated classification code. We note that a preliminary estimate of completeness as a function of bJ and redshift (used here and in Paper I) will be available electronically as part of the data release. 5 D A T A A CCES S

The 2QZ 10k catalogue and associated data products are available from http://www.2dfquasar.org along with basic tools to access


L36

S. M. Croom et al.
Brotherton M. S. et al., 1999, ApJ, 520, L87 Colless M., 1998, in Mellier Y., Colombi S., eds, 14th IAP meeting, Wide à Field Surveys in Cosmology. Editions Frontieres, Gif-sur-Yvette, p. 77 Condon J. J., Cotton W. D., Greisen E. W., Yin Q. F., Perley R. A., Taylor G. B., Broderick J. J., 1998, AJ, 115, 1693 Croom S. M., RatcliffeA., Parker Q. A., Shanks T., BoyleB. J., Smith R. J., 1999, MNRAS, 306, 592 Croom S. M., Shanks T., Boyle B. J., Smith R. J., Miller L., Loaring N. S., Hoyle F., 2001, MNRAS, in press (Paper II) Hewett P. C., Foltz C. B., Chaffee F. H., 1995, AJ, 109, 1499 HoyleF., Outram P. J., Shanks T., Croom S. M., BoyleB. J., Loaring N. S., Miller L., Smith R. S., 2001, MNRAS, submitted (Paper IV) Lewis I. J., Glazebrook K., Taylor K., 1998, Proc. SPIE, 3355, 828 Schlegel D. J., Finkbeiner D. P., Davis M., 1998, ApJ, 500, 525 Smith R. J., Croom S. M., Boyle B. J., Shanks T., Miller L., Loaring N. S., 2001, MNRAS, submitted (Paper III) á á Veron-Cetty M. P., Veron P., 2000, Quasars and ActiveGalactic Nuclei, 9th edn. ESO Sci. Rep., 19, 1 Voges W. et al., 1999, A&A, 349, 389 Voges W. et al., 2000, IAU Circ. 7432

and interrogate the catalogue. A CD-ROM containing the same data and tools is also available, and the catalogue can also be accessed at CDS (http://cdsarc.u-strasbg.fr/) and in the electronic version of MNRAS on Synergy. Any authors using the 2QZ 10k catalogue should include the following acknowledgement: `The 2dF QSO Redshift Survey (2QZ) was compiled by the 2QZ survey team from observations made with the 2-degree Field on the Anglo-Australian Telescope.' A C K N O W L E DGMENT S The 2QZ was based on observations made with the AngloAustralian Telescope and the UK Schmidt Telescope. NSL was supported by a PPARC studentship during the course of this work. REFER E NC ES
Bailey J., Glazebrook K., Offer A., Taylor K., 2001, MNRAS, submitted Boyle B. J., Fong R., Shanks T., Peterson B. A., 1990, MNRAS, 243, 1 Boyle B. J., Shanks T., Croom S. M., 1995, MNRAS, 276, 33 Boyle B. J., Shanks T., Croom S. M., Smith R. J., Miller L., Loaring N., Heymans C., 2000, MNRAS, 317, 1014 (Paper I)

A This paper has been typeset from a TEX/L TEX file prepared by the author.

q 2001 RAS, MNRAS 322, L29 ± L36