Issue |
A&A
Volume 505, Number 1, October I 2009
|
|
---|---|---|
Page(s) | 97 - 104 | |
Section | Extragalactic astronomy | |
DOI | https://doi.org/10.1051/0004-6361/200811161 | |
Published online | 22 June 2009 |
Discovery of a redshift 6.13 quasar in the UKIRT infrared deep sky survey
D. J. Mortlock1 - M. Patel1 - S. J. Warren1 - B. P. Venemans2 - R. G. McMahon2 - P. C. Hewett2 - C. Simpson3 - R. G. Sharp4 - B. Burningham5 - S. Dye6 - S. Ellis7 - E. A. Gonzales-Solares2 - N. Huélamo8
1 -
Astrophysics Group, Imperial College London, Blackett Laboratory,
Prince Consort Road, London, SW7 2AZ, UK
2 -
Institute of Astronomy, University of Cambridge,
Madingley Road, Cambridge, CB3 0HA, UK
3 -
Astrophysics Research Institute, Liverpool John Moores
University, Twelve Quays House, Egerton Wharf, Birkenhead, CH41 1LD, UK
4 -
Anglo Australian Observatory, PO Box 296, Epping, NSW 1710, Australia
5 -
Centre for Astrophysics Research, Science and Technology
Research Institute, University of Hertfordshire, Hatfield, AL10 9AB, UK
6 -
School of Physics & Astronomy, Queens Building, Cardiff University,
The Parade, Cardiff CF24 3AA, UK
7 -
Institute of Astronomy, School of Physics,
The University of Sydney, NSW 2006, Australia
8 -
Laboratorio de Astrofísica Espacial y Física Fundamental,
European Space Astronomy Center, PO Box 78,
28691 Villanueva de la Cañada, Madrid, Spain
Received 15 October 2008 / Accepted 17 April 2009
Abstract
Optical and near-infrared (NIR) spectra are presented for
ULAS J131911.29+095051.4 (hereafter ULAS J1319+0950), a new redshift
quasar discovered in the Third Data Release (DR3) of the
UKIRT Infrared Deep Sky Survey (UKIDSS).
The source has
,
corresponding to
,
which is comparable to the absolute magnitudes of the
quasars discovered in the Sloan Digital Sky Survey (SDSS).
ULAS J1319+0950 was, in
fact, registered by SDSS as a faint source with
,
just below the signal-to-noise ratio limit of the
SDSS high-redshift quasar survey. The faint z-band magnitude is a
consequence of the weak Ly
/N V emission line, which has a
rest-frame equivalent width of
and
provides only a small boost to the z-band flux. Nevertheless,
there is no evidence of a significant new population of high-redshift
quasars with weak emission lines from this UKIDSS-based search.
The Ly
optical depth to ULAS J1319+0950 is consistent with that measured
towards similarly distant SDSS quasars, implying that results from
optical- and NIR-selected quasars may be combined in studies of
cosmological reionization.
Also presented is a new NIR-spectrum of the previously discovered UKIDSS
quasar ULAS J020332.38+001229.2, which reveals the object to be a broad
absorption line quasar. The new spectrum shows that the emission
line initially identified as Ly
is actually N V, leading to a
revised redshift of z=5.72, rather than z=5.86 as
previously estimated.
Key words: galaxies: quasars: individual: ULAS J020332.38+001229.2, ULAS J131911.29+095051.4 - infrared: general - cosmology: observations
1 Introduction
Since their discovery by Schmidt (1963) and
Hazard et al. (1963), quasars have continued to be the most
revealing probes of the high-redshift Universe (e.g.,
Schneider 1999). Even though galaxies have been detected
out to greater distances (e.g., IOK-1, with a redshift of z = 6.96,
Iye et al. 2006) and gamma ray bursts may briefly be more
luminous (e.g., Haislip et al. 2006), the highest-redshift
quasars (e.g., SDSS 1148+5251 at z = 6.42, Fan et al. 2003;
CFHQS J2329-0301 at z = 6.43, Willott et al. 2007) are
more useful because they remain bright enough to be investigated in detail.
It has been possible to obtain high signal-to-noise ratio
(S/N) spectra
for all the known
quasars, robustly confirming the nature
of these sources, revealing their intrinsic properties (e.g.,
Venemans et al. 2007; Walter et al. 2004) and, through
absorption, probing the intervening matter out to the quasars' redshifts.
The resultant measurements of the
quasar population
are also of interest, as they provide critical
limits on the early structure formation scenarios
(e.g., Kurk et al. 2007).
Probably the most dramatic discovery from these studies
is the marked increase
in the optical depth to neutral hydrogen at redshifts of
(Becker et al. 2001; Fan et al. 2002,2006a). The increase
in optical depth appears to represent the end of cosmological
reionization (e.g., Barkana & Loeb 2001), a conclusion
supported by the Wilkinson Microwave Anisotropy Probe
(WMAP; Bennett et al. 2003) measurements of the cosmic
microwave background (e.g., Dunkley et al. 2009). While a
consistent picture of reionization has emerged, the direct
measurements of this process are limited to the small number of
quasars known, and it is clear that the discovery of quasars
with
is vital to further progress in this field.
The majority of the known
quasars have been identified by
looking for point-sources with very red optical colours in wide-field
surveys such as the Sloan Digital Sky Survey (SDSS;
York et al. 2000) and the Canada France High-z Quasar Survey
(CFHQS; Willott et al. 2007), and more discoveries will be
made in such projects. Optical searches are, however, unlikely to
probe beyond the current redshift limits. Almost all
quasar emission at rest-frame wavelengths shorter than the Ly
transition at
is absorbed by intervening hydrogen,
and such quasars are effectively dark at observed wavelengths
below
.
Conversely, most optical
charge-coupled device (CCD) detectors have a poor response beyond
wavelengths of
(i.e., redward of
the z or Z bands), so quasars with a redshift of
are destined to remain invisible to CCD-based surveys. Given the
rarity of
quasars
(e.g., a surface density of
to
;
Jiang et al. 2007), progress can only be made using wide-field
surveys at longer wavelengths.
In the long term, radio surveys with, e.g., the Low Frequency Array
(LOFAR) and the Square Kilometre Array
(SKA
) will provide a powerful
complementary approach (e.g., Wyithe et al. 2009), but the
first steps beyond the current limits will come in the near-infrared
(NIR), with surveys following the same basic principles as the SDSS
and CFHQS searches.
The largest completed NIR survey, the Two Micron All Sky Survey
(2MASS; Skrutskie et al. 2006), with a magnitude limit of
,
does not have sufficient depth to find any
plausible high-redshift quasars. The Visible and Infrared Survey
Telescope for Astronomy (VISTA; Emerson et al. 2004) should
cover
to
during the next decade, but progress in the search for high-redshift
quasars will come first from the partially complete UKIRT Infrared
Deep Sky Survey (UKIDSS; Lawrence et al. 2007).
One new high-redshift quasar, ULAS J020332.38+ 001229.2,
hereafter ULAS J0203+0012, with
an estimated redshift of z = 5.86(Venemans et al. 2007), has already been discovered in UKIDSS;
the second such discovery, ULAS J131911.29+095051.4, hereafter ULAS J1319+0950, is
presented here. Section 2 gives an introduction to the UKIDSS LAS
project and Sect. 3 describes the selection techniques that
led to ULAS J1319+0950 being identified as a candidate high-redshift
quasar. Optical and NIR spectra of ULAS J1319+0950 are presented and
compared to those of
SDSS quasars in Sect. 4.
In addition, a new NIR spectrum of ULAS J0203+0012 is presented in
Sect. 5, together with a revised redshift estimate for this
source. The conclusions and future prospects for
high-redshift quasar searches with UKIDSS are discussed in
Sect. 6.
All photometry is given in the native system of the telescope in
question, and explicitly subscripted.
Thus SDSS i and z photometry is on the AB
system, whereas UKIDSS Y and J photometry is Vega-based. The AB
corrections for the UKIDSS bands are
and
(Hewett et al. 2006). Calculations of absolute (AB) magnitudes
are performed assuming a fiducial flat cosmological model with
normalised matter density
,
normalised vacuum density
,
and Hubble constant
.
2 The UKIRT Infrared Deep Sky Survey
UKIDSS (Lawrence et al. 2007) is a suite of five surveys
undertaken with the Wide Field Camera (WFCAM;
Casali et al. 2007) on the 3.8 m United Kingdom Infrared
Telescope (UKIRT) at Mauna Kea, Hawaii. The WFCAM detectors are four
sparse-packed
Rockwell Hawaii-II arrays, each of
which has a field of view of
.
Observations are
generally undertaken in sets of four contiguous pointings which,
together, cover
.
Full details of the survey
operations can be found in Dye et al. (2006). The individual
images are analysed by the data reduction pipeline described by
Irwin et al. (2009) and the catalogues of detected objects are
merged across bands into a queryable relational database at the WFCAM
Science Archive
(WSA;
Hambly et al. 2008).
The UKIDSS Large Area Survey (LAS) will cover 4000
within
the SDSS footprint with a series of 40 s
exposures
in the Y, J, H and K bands. The
resulting magnitude limits are typically
,
,
and
for
point-sources detected with S/N
5,
and the average seeing is
(Warren et al. 2007).
The area, depth and wavelength coverage of
the LAS were chosen with the detection of
quasars in mind,
and the Y filter, positioned between the
and J bands in
a region of minimal atmospheric absorption (
), is particularly useful in this
regard (Hewett et al. 2006). Quasars in the redshift interval
would be identifiable as being unusually red in
i-Y and z-Y, while being significantly bluer in Y
J than the
more numerous L and T dwarfs.
All UKIDSS images and catalogues are made available to European
Southern Observatory (ESO) countries and then, 18 months later, the
world, in a series of incremental data releases. The results
presented here are based on the Third Data Release (DR3;
Warren et al. 2009) for which there is
of
LAS coverage in the Y and J bands.
3 Candidate selection
High-redshift quasar candidates are selected in a two-step process, using survey data initially (Sect. 3.1), followed by additional photometric observations of the most promising objects (Sect. 3.2).
3.1 Initial shortlist
Redshift 6 quasars are expected to appear as stationary
point-sources with extremely red optical-NIR colours. The first
stage of the candidate selection process is to extract a fairly
complete (if highly contaminated) sample of all such sources from the
UKIDSS and SDSS databases.
The initial selection from the UKIDSS LAS was of all point-sources
with
that were also detected in the J band and
have measured
(to
exclude L and T dwarfs). The resulting sample was then cross-matched
to the SDSS Fifth Data Release (DR5;
Adelman-McCarthy et al. 2007) and all sources either undetected
by SDSS or with
(but
undetected in u, g and r) were selected. Any
sources with inter-band (or inter-survey) positional mis-matches of
greater than 0
7 were rejected to avoid nearby Galactic
stars with appreciable proper motions, as well as most
asteroids
.
A number of heuristic algorithms were applied to reject sources for which the UKIDSS or SDSS database photometry is likely to be unreliable. Contaminating sources eliminated at this stage include those arising from WFCAM cross-talk (Dye et al. 2006), objects in the haloes of bright stars, and close pairs separated by a few arcsec for which deblending is required in SDSS.
For the sources that were undetected in SDSS i and z,
aperture fluxes, corrected for aperture loss, were measured from the
SDSS images. Acquisition of the aperture fluxes represents the final
step in a fully automatic procedure that, in the analysis of UKIDSS
DR3, yielded
pre-candidates with i-, z-,
Y- and J-band photometry.
The next stage of the selection process is to use
Bayesian model comparison to determine the
probability,
given the photometric data,
that each source is a high-redshift quasar,
.
This calculation is described in detail in Mortlock et al. (2009).
The key to this approach is having an accurate model of the stellar
population, specifically the intrinsic magnitude and colour distributions
of the cool M dwarfs
which scatter into the quasar selection box described above.
Convolving this distribution in i,
z, Y and J with the observational noise gives the likelihood
that any candidate is an M dwarf.
This can be compared directly with the likelihood that the candidate is
a quasar, which is calculated
using an extrapolation of the high-redshift quasar luminosity function
of Fan et al. (2004) and simulated colours from Hewett et al. (2006).
The result is a fully self-consistent value
of
that, in principle, combines the available information on the
candidate with the constraints on the quasar and star populations
in an optimal way.
Of course there are practical limitations, the most important of
which result from incomplete sampling of the tails of the noise
distributions and the limited knowledge of the
stellar population fainter than the UKIDSS and
SDSS survey limits. The latter is important as the probability calculation
necessarily includes the possibility of faint sources scattered into
the sample, but is difficult to assess empirically using the survey data.
Despite these ambiguities
(which are explored further in Mortlock et al. 2009),
the probabilities which result from the adopted noise and population models
clearly provide a good objective ranking scheme for quasar candidates.
![]() |
Figure 1:
Finding chart for ULAS J131911.29+095051.4 showing the UKIDSS LAS
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Most of the candidates are clustered close to the stellar locus and
their low quasar probabilities (i.e.,
)
merely
confirm the obvious. The motivation for the method is to
assess the ambiguous sources lying between the quasar
and star loci in colour space, or close to the Y-band limit
with quasar-like colours but large errors. The sometimes
counter-intuitive results are explored in some detail in
Mortlock et al. (2009), but the critical point is that the
candidates can be ranked by
and thus prioritised
objectively for further investigation.
It is only at this stage that any visual inspection was undertaken,
with the UKIDSS and SDSS images of the few hundred best candidates
checked for artefacts such as hot pixels, bad columns,
obviously wrong photometry,
and
undetected, blended or moving sources.
(Although the UKIDSS and SDSS data reduction pipelines flag the
vast majority of such instances, the selection of unusual sources
on the basis of observed inter-survey colours inevitably
produces samples with an over-representation of the very rare cases
for which at least one of the surveys has produced anomalous measurements.)
Following visual inspection,
only a small sample of 100 plausible quasar candidates
with
remained
, one of which was ULAS J1319+0950, shown in Fig. 1.
Follow-up observations were needed to
either reject these candidates as stars or,
hopefully, confirm some as high-redshift quasars.
Table 1: Original survey and follow-up photometric observations of ULAS J1319+0950.
3.2 Follow-up photometry
Rather than immediately taking spectra of all the candidates (cf.
Glikman et al. 2008), it is more efficient first to refine the
photometry, obtaining short exposures in the i, z, Y and
J bands on a variety of telescopes. The quasar probability defined
in Sect. 3.1 is recalculated whenever new data are obtained, and
a source is dropped from the candidate list if
falls
below the selection threshold at any point.
As almost all the candidates initially
have minimal S/N in the i band SDSS images, follow-up
observations in this band are the most efficient way to quickly reject
such sources, revealing most to be cool stars scattered to have
quasar-like colour by photometric noise. Observations in i are
thus prioritised, although initial follow-up observations are
sometimes made in z, Y or J, depending on weather,
telescope scheduling, and other external factors. Candidates are not
considered for spectroscopy until follow-up photometry
has been obtained in at least the
,
Y and J bands.
Follow-up observations of ULAS J1319+0950 were obtained in i, z, Y and J, as summarised in Table 1.
ULAS J1319+0950 was
first re-observed in the i band at the Liverpool Telescope (LT)
on the nights beginning 2008 January 8 and 12 for a total of
.
The candidate's quasar probability remained high, and
so
exposures in each of the Y and J bands were
obtained using the UKIRT Fast-Track Imager (UFTI) on the night
beginning 2008 January 16. The candidate still appeared promising so
the UFTI observations were repeated the following night.
The improved i-, Y- and J-band measurements were
sufficiently precise that ULAS J1319+0950 had
(i.e., it was essentially implausible for a cool star to have scattered
to the candidate's observed colours given the precision of the new
photometric data), whereas all the other initial candidates were
rejected on the basis of their follow-up photometry.
A spectrum of ULAS J1319+0950 was thus
obtained on the night beginning 2008 January 22,
with the result that it was immediately confirmed
as a high-redshift quasar (Sect. 4).
That the entire selection, follow-up and
confirmation process for ULAS J1319+0950 was completed less than seven
weeks after the UKIDSS DR3 release (on 2007 December 6) is a powerful
illustration of the advantages of queue-scheduling for the three
telescopes involved, especially considering the RA of the target and
the time of year.
ULAS J1319+0950 had already been detected as a faint source in SDSS,
although with
its S/N was too low for it to be selected into the high-redshift quasar sample
defined by Fan et al. (2003). Post-confirmation, improved z-band
photometry of ULAS J1319+0950 was obtained using the ESO Multi-Mode
Instrument (EMMI) on the New Technology Telescope (NTT) on the night
of 2008 January 29. The observations were made with the long-pass
filter, the bandpass of which, in combination with the red
cut-off of the CCD response, is quite similar to the SDSS z bandpass (Venemans et al. 2007). To calibrate the NTT-image, SDSS
i- and z-band photometry of bright, unsaturated stars in
the frame was converted to the natural system of the image using
(Venemans et al. 2007), and the result quoted in Table 1 is
in this natural system.
4 ULAS J1319+0950
After the series of follow-up photometric observations described in Sect. 3.2 showed ULAS J1319+0950 to be a promising high-redshift quasar candidate, an optical spectrum was obtained to confirm the identification (Sect. 4.1). A more accurate redshift was estimated from a NIR spectrum covering the Mg II emission line (Sect. 4.2), after which both spectra were used to compare ULAS J1319+0950's emission and absorption properties with those of similarly distant quasars discovered in SDSS (Sect. 4.3).
4.1 Spectroscopic observations
An optical spectrum of ULAS J1319+0950 was obtained using the Gemini
Multi-Object Spectrograph (GMOS) on the
Gemini South Telescope on the night beginning 2008 January 22. Two
spatially-offset spectra, each of duration 900 s, were obtained
using a 1 arcsec slit and the R400 grating, covering
the wavelength range of 0.5-1.0 m over the three CCDs.
The standard bias subtraction and flat-fielding steps were followed.
Then, because of the strong sky lines in the red part of the spectrum,
the ``double subtraction'' method was used for the first-order sky
subtraction (i.e., frame B was subtracted from frame A, and then the
negative spectrum subtracted from the positive spectrum, after the two
spectra were aligned). This procedure removes most systematic errors,
but at the price of increasing the noise in the final frame by a
factor of
1.4 compared to the theoretical limit.
Second-order sky subtraction was achieved by fitting a smooth function
to each column. At this point cosmic rays were removed using the
Laplacian Cosmic Ray Removal Algorithm (LCRRA;
van Dokkum 2001). Wavelength-calibration was carried out
using observations of a Cu Ar lamp. Relative spectrophotometry, and
correction for telluric absorption, was achieved using observations of
a standard star, and the spectrum was then scaled to match the NTT
z-band photometry given in Table 1. The final GMOS
spectrum is shown in Fig. 2.
![]() |
Figure 2:
The Gemini GMOS spectrum of ULAS J1319+0950 (black curve) and the
noise spectrum (red curve), both binned by a factor of four.
The gaps at wavelengths of
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The spectrum is recognisable as that of a
quasar from the
presence of a broad emission line, identified as Ly
,
at the same
wavelength as a strong continuum break, attributed to Ly
forest absorption.
The Ly
emission peaks at a wavelength of
,
which leads to a preliminary redshift estimate of
z = 6.12. However the Ly
line is strongly absorbed to the blue and
such high-ionization lines can exhibit velocity shifts relative to the
quasar systemic redshift (e.g., Tytler & Fan 1992),
limiting the utility of the optical redshift measurement.
The Mg II line, if observable in the K band, should give a more reliable
estimate of the redshift, and so a NIR spectrum of ULAS J1319+0950 was
obtained. The source was observed using the Near-IR Instrument (NIRI)
on the Gemini North Telescope on the two nights beginning 2008
February 26 and 27. Observations were made with a 0.75 arcsec slit
and the K grism G5204, covering the wavelength range
1.9-2.5 m
with a resolving power of R = 500.
With NIRI it is standard procedure to discard
the first exposure of a sequence, leaving a total of 11 usable
300 s exposures over the two nights. The observation and data
reduction methodology of Weatherley et al. (2005) was adopted,
with six different slit positions used to reduce the noise from
sky-subtraction relative to the more standard ABBA sequence. The data
suffered from increasing slit losses as the observations proceeded,
which is believed to be due to differential flexure between the guide
probe and the instrument. The additional slit losses, relative to the
first frames on each night, reduced the final S/N of the detected
emission line by a factor of
1.5. Because of the varying
throughput, each sky-subtracted frame was first scaled to a common
count level, and then weighted by the inverse variance in the sky (as
evaluated in a region free of strong emission lines). Wavelength
calibration was performed using the list of sky emission lines from
Rousselot et al. (2000). A standard star observed at similar
airmass was used to correct for telluric absorption, and for relative
flux calibration, after which the spectrum was scaled to match the
UKIDSS K-band photometry given in Table 1. The final NIR
spectrum is plotted in Fig. 3.
![]() |
Figure 3:
The Gemini NIRI spectrum of ULAS J1319+0950 (black curve) and the
error spectrum (red curve), both binned by a factor of two. The
continuum+line fit to the Mg II emission line is also shown (blue).
The fit implies a source redshift of
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4.2 Redshift estimation
The NIR spectrum of ULAS J1319+0950 shown in Fig. 3 reveals the
broad Mg II emission line near
,
corroborating the initial redshift estimate of
.
To obtain a more accurate
measurement (and to quantify the absorption in the
Ly
forest in Sect. 4.3) a power-law fit to the
continuum was made to the combined optical and NIR spectrum by
minimizing
and iteratively clipping outliers to eliminate the
emission lines. The best-fit power-law is
,
where
(defined so that
). This is plotted in
Fig. 4. This continuum was subtracted from the data and then
a Gaussian was fit to the residual Mg II emission line; the resultant
continuum+line fit is plotted in Fig. 3. The central
wavelength of the Mg II emission is
,
implying that ULAS J1319+0950 has a redshift of
.
The Mg II emission line has a rest-frame
equivalent width of
,
substantially less
than the typical value of
for
quasars found by Kurk et al. (2007).
![]() |
Figure 4: The optical spectrum, binned by a factor of four (left black curve), and the NIR spectrum, binned by a factor of five (right black curve), of ULAS J1319+0950. The power-law continuum fit is also shown (blue). |
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4.3 Comparison with SDSS quasars
ULAS J1319+0950 is, after ULAS J0203+0012 (Venemans et al. 2007), only the
second redshift 6 quasar discovered in the NIR. Given that
surveys at these wavelengths are the first capable of probing beyond
the current limit of
,
it is important to determine
whether quasars selected in the NIR exhibit significant
differences from those selected in the optical.
This preliminary exploration focuses on
the emission line strengths,
the neutral hydrogen optical depth,
and the ionization region around the quasar.
![]() |
Figure 5:
Rest-frame spectra of ULAS J0203+0012 (blue) and ULAS J1319+0950 (green) compared to the composite spectrum of
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4.3.1 Emission line properties
Redshift 6 quasars are identifiable in photometric surveys
primarily due to their extreme colours which result from the strong
neutral hydrogen absorption blueward of the quasars' Ly
emission
lines. However Fig. 5, which compares the rest-frame spectrum
of ULAS J1319+0950 (and ULAS J0203+0012; see Sect. 5) to a composite
SDSS quasar spectrum (Fan et al. 2006b), shows that ULAS J1319+0950 has a noticeably weaker Ly
emission line than is typical for
optically-identified sources.
Measuring the
rest-frame equivalent width of ULAS J1319+0950's Ly line is somewhat
problematic as the continuum level is ambiguous and the power-law fit
shown in Fig. 4 is probably too steep to give a good local
continuum estimate. For the purposes of comparison the continuum
levels shown in Fig. 5 were adopted, yielding rest-frame
equivalent widths of
for ULAS J1319+0950 and
for the Fan et al. (2004) composite.
This quantifies
the visual impression that ULAS J1319+0950 has a weaker Ly
emission line than an average
quasar,
although there are several examples of high-redshift quasars
with even weaker lines
(e.g., Diamond-Stanic et al. 2009; Fan et al. 1999).
If ULAS J1319+0950 differed only in that its Ly
emission was marginally
stronger (or, equivalently, less absorbed to the blue), it would
almost certainly have been discovered in the SDSS high-redshift quasar
sample.
With
in the SDSS database, it was brighter
than the Fan et al. (2003) limit of
,
but it
failed the S/N cut of
.
Given that the NTT
re-observation described in Sect. 3.2 gave
,
the SDSS team were unlucky that their z-band flux was
less than the true value and that the source was observed in slightly
worse than average conditions, both of which combined to leave the
source outside their selection cuts. This
illustrates the more general limitation inherent in any selection
method which applies a hard data cut in a region of parameter space
where there are appreciable numbers of objects. A way to avoid the
problem, at least in principle, is to apply the probabilistic approach
adopted in Sect. 3.1 and described in full by
Mortlock et al. (2009), although it remains difficult to deal with
the large numbers of low S/N candidates near the survey limit.
4.3.2 Neutral hydrogen optical depth
Observations of
quasars have revealed a marked increase
in the density of neutral hydrogen above a redshift of
5.7(e.g., Fan et al. 2002), possibly indicating the end of
cosmological reionization (e.g., Fan et al. 2006a). As
hydrogen absorption also has an effect on the detectability of
quasars, it is important to assess whether the measured
optical depths of optical- and NIR-selected quasars differ
significantly.
Here, the spectrum of ULAS J1319+0950 is analysed following the method of
Fan et al. (2006a), with the effective optical depth,
,
at redshift
estimated to be
![]() |
(1) |
where

















The estimated optical depths towards ULAS J1319+0950 are consistent with
measurements of SDSS quasars by Fan et al. (2006a),
which gives some confidence that
Gunn & Peterson (1965) effect measurements of optical- and
NIR-selected
quasars may be combined.
4.4 Quasar ionization region
The ultraviolet (UV) photons from quasars are sufficiently energetic to ionize the neutral hydrogen in a volume around them, creating a Strömgren (1939) sphere. The extent of the ionization region depends in part on the UV luminosity of the quasar and the neutral fraction of the surrounding medium, potentially providing a complementary probe of reionization. Unfortunately, the measurement is difficult in practice, due to uncertainties in the quasars' UV spectral energy distributions (SEDs), unknown ionizing flux from nearby galaxies, and difficulty in establishing the extent of the H II region from heavily absorbed and otherwise noisy spectra (e.g., Fan et al. 2006a).
It has proved more useful to adopt a relative approach in which the
evolution of the size of quasars' H II regions with redshift is
estimated without reference to an absolute model of the neutral
hydrogen fraction. The relative measurement is attempted here for
ULAS J1319+0950, once again following the methodology of
Fan et al. (2006a), by defining the quasar proximity region as the
volume within which the transmitted flux fraction is 0.1. After
dividing the Gemini spectrum by the continuum+line fit (described in
Sect. 4.2) to convert to transmitted flux, the spectrum was
smoothed to a resolution of
.
This smoothed
transmission spectrum remains below 0.1 down to a wavelength of
;
converting to redshift and then
to a co-moving physical length implies that ULAS J1319+0950 has a
proximity zone of radius
.
The inferred radius is broadly consistent with measurements from
optically-detected SDSS quasars (Fan et al. 2006a), although to
make a more quantitative comparison it is necessary to standardise the
above measurement of
to a fiducial absolute magnitude
according to
.
With
this gives
for ULAS J1319+0950. This is lower than the
fiducial value of
given by Fan et al. (2006a) for
quasars,
although this difference is not significant given the
range of
values seen in the optical sample.
Table 2: Effective optical depths of the absorption systems seen in the spectrum of ULAS J1319+0950.
5 ULAS J0203+0012
ULAS J0203+0012 was the first
quasar found in UKIDSS,
Venemans et al. (2007) describing the discovery and reporting a
redshift of z=5.86. The source was subsequently recovered
by Jiang et al. (2008) in their
survey for high-redshift quasars using deep co-added data from
multiple scans of SDSS Stripe 82;
they quote a redshift of z=5.85.
An improved redshift for ULAS J0203+0012 was
sought by acquiring a NIR spectrum (Sect. 5.1). These data
revealed ULAS J0203+0012 to be a broad-absorption line (BAL) quasar,
resulting in a modified redshift estimate (Sect. 5.2), and
also showing some discrepancies compared to the existing optical
spectrum in the region 0.9-1.0
m. The origin of the
discrepancy was traced to the relatively poor quality of the published
standard star data used to flux-calibrate the optical spectrum,
which has hence been re-reduced (Sect. 5.1).
5.1 Spectroscopic observations
5.1.1 Optical spectrum
The original optical spectroscopic observations of ULAS J0203+0012 were made
in 2006 September using the
FOcal Reducer and low dispersion Spectrograph (FORS2)
on the Very Large Telescope (VLT),
and are described in detail in Venemans et al. (2007).
The re-reduction followed a similar
sequence to that described there, up to the point of flux
calibration. Instead of using the published
spectrophotometry of the white dwarf standard star GD50 from
Oke (1990), a model spectrum with effective temperature
and surface gravity
from Dobbie et al. (2005)
was used to establish the flux calibration curve. Finally, the data were
scaled to match the measured z-band photometry. The revised
spectrum, plotted in Fig. 6, shows a sharp downturn longward of
0.95
m compared to the original spectrum.
![]() |
Figure 6: Re-calibrated VLT spectrum of ULAS J0203+0012 (black curve) and the noise spectrum (red curve), binned by a factor of two. The wavelengths of common emission lines redshifted by z = 5.72 are indicated. |
Open with DEXTER |
5.1.2 NIR spectrum
A NIR spectrum of ULAS J0203+0012 was obtained using the Gemini Near
Infra-Red Spectrograph (GNIRS) on the Gemini South Telescope on the
night beginning 2007 March 22. The observations were taken in
cross-dispersed mode with the short camera, the 32 lines mm-1grism, and a 0.75 arcsec slit, providing coverage from
to
at a resolving
power of R=500. Due to the limited slit length it was impractical
to adopt the observation strategy used for the NIRI observations of
ULAS J1319+0950 (Sect. 4.1) and so a standard ABBA offset pattern was
used.
The observations comprise eight frames, with a total exposure time of
.
The data were reduced mainly using the Gemini-GNIRS
package in the Image Reduction and Analysis Facility (IRAF;
Tody 1993). After correction for pattern noise and
flat-fielding, each of the diffraction orders was separated, and the
double-subtraction method (described in Sect. 4.1) was applied to
each of the four pairs of images. The resulting four frames for each
order were then averaged. S-distortion correction and wavelength
calibration were then applied using observations of an Ar lamp, and
one-dimensional spectra were extracted. The data were corrected for
telluric absorption and flux-calibrated using the spectrum of a
spectroscopic standard star. Finally, the different diffraction orders
were spliced together to produce a single continuous spectrum. Strong
telluric absorption bands occur at 1.35-1.43
m and
1.80-1.95
m, and so the data in these wavelength ranges
were discarded. The spectrum was placed on an absolute flux scale by
matching to the K-band photometry.
Comparison of the optical and NIR spectra in the region of overlap
(0.8-1.0 m) showed good detailed agreement, except for a
10 per cent normalisation offset, and so the optical spectrum
was scaled to the NIR spectrum. The declining S/N of the NIR spectrum
towards the blue, and of the optical spectrum towards the red, are
approximately equal at
,
so the two spectra were
spliced at this point. The final combined spectrum is plotted in
Fig. 7.
![]() |
Figure 7:
The combined optical and NIR spectrum, spliced at
|
Open with DEXTER |
5.2 Redshift estimation
The most striking features of the combined ULAS J0203+0012 spectrum shown
in Fig. 7 are the broad absorption lines near
0.9 m and 1.0
m.
These are attributed to Si IV and C IV, respectively.
Despite the increased wavelength coverage, the redshift
is difficult to determine accurately, as is common with BAL quasars
(e.g. Trump et al. 2006). Venemans et al. (2007) and
Jiang et al. (2008) identified the peak of the line near
with Ly
,
and the shoulder at
with N V, but matching Si IV,
C IV and C III] lines for this redshift are not evident. Instead it seems
likely that the peak at
is the N V emission
line, and that the Ly
emission line has been absorbed by a N V BAL. As shown in Fig. 7, a redshift of z=5.72provides a reasonable match to the N V peak, as well as weak features
that match Si IV, C IV, and C III]; but any redshift in the range
5.70<z<5.74 is consistent with the data.
Unfortunately the Mg II line,
which ought to give a definitive redshift, lies in the
region of atmospheric absorption near
.
In the wavelength region 0.85-1.08 m it is difficult to
determine the extent of the BAL troughs and the regions of unabsorbed
continuum emission. The best fit power-law, plotted in
Fig. 7, is a poor match. It seems likely that the sharp
step near 0.865
m marks the blue edge of the Si IV BAL,
and that the shoulder at 0.855
m, previously identified
with N V, is in fact continuum emission. The resulting estimate of the
rest frame equivalent width of the N V line is
.
Given the presence of BAL troughs, it is difficult to infer very much
about the neutral hydrogen along the line-of-sight to ULAS J0203+0012, as
the Ly
emission line is all but completely absorbed.
Similarly, it is not possible to measure the Gunn & Peterson (1965)
optical depth to ULAS J0203+0012: assuming the N V BAL has a similar
velocity width to the C IV and Si IV BALs, the absorption blueward
of Ly
is most likely dominated by the wing of the N V BAL, and not by
intervening neutral hydrogen along the line-of-sight.
The case of ULAS J0203+0012 is rather similar to that of the BAL quasar
SDSS J1044-0125 (Fan et al. 2000). The initial redshift
measurement of z=5.80 by Fan et al. (2000) was revised to
z=5.74 by Goodrich et al. (2001) on the basis of NIR
spectroscopy, after which Jiang et al. (2007) used the C III] line
to estimate z=5.78. Both ULAS J0203+0012 and SDSS J1044-0125
demonstrate the importance of NIR spectra to obtaining reliable
redshifts of
quasars (and especially BALs).
6 Conclusions and future prospects
Two new high-redshift quasars have now been discovered in the UKIDSS
LAS: ULAS J0203+0012 at z = 5.72 (previously given as z =
5.86; Venemans et al. 2007);
and ULAS J1319+0950 at z =
6.13. Two previously known high-redshift quasars,
SDSS 0836+0054 at z = 5.82 (Fan et al. 2001) and SDSS 1411+1217 at z = 5.93 (Fan et al. 2004), have also been recovered in the
UKIDSS DR3 LAS area. The two new quasars are well within the
redshift range covered by optical surveys, but they
were both too faint in SDSS to be included
in the high-redshift quasar sample defined by
Fan et al. (2003).
While the revised lower redshift of ULAS J0203+0012 puts its Ly
emission near the peak of the SDSS z band response,
the line is almost completely absorbed by a N V BAL, which results in a
reduction of the z-band flux. ULAS J1319+0950 has a very weak Ly
line, with a rest-frame equivalent width of just
.
The small Ly
equivalent width results in the
z-band S/N falling marginally below the limit of the SDSS
quasar sample defined by Fan et al. (2003). Nonetheless, the
detection of four
quasars brighter than
in the
of UKIDSS DR3 LAS is consistent with
expectations from the luminosity function of Jiang et al. (2008),
and so these new detections do not imply the existence of a previously
unidentified quasar population with weak emission features.
These results demonstrate that the UKIDSS data are of sufficient quality
to recover
quasars down to
with reasonable
completeness. Quantification of the completeness will be explored in
more detail when the sample is larger. At the time of writing the
UKIDSS Fifth Data Release (DR5; Warren et al. 2009) has
already taken place, increasing the LAS area covered in the Y and Jbands to
.
DR5 is of sufficient size that finding no quasars of
redshift z > 6.4 would be somewhat inconsistent with expectations.
Acknowledgements
Many thanks to the staffs of UKIRT, the Cambridge Astronomical Survey Unit, and the Wide Field Astronomy Unit, Edinburgh, for their work in implementing UKIDSS. Thanks to Marie Lemoine-Buserolle, Kathy Roth and Claudia Winge for help in setting up the Gemini observations. Paul Dobbie kindly provided the synthetic spectrum of GD50 used for flux-calibrating the optical spectrum of ULAS J0203+0012. Based on observations obtained at the Gemini Observatory (acquired through the Gemini Science Archive), which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the Science and Technology Facilities Council (United Kingdom), the National Research Council (Canada), CONICYT (Chile), the Australian Research Council (Australia), CNPq (Brazil) and SECYT (Argentina). The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. M.P. acknowledges support from the University of London's Perren Fund. P.C.H., R.G.M. and B.V. acknowledge support from the STFC-funded Galaxy Formation and Evolution programme at the Institute of Astronomy. The referee, Michael Strauss, made a number of valuable suggestions which have significantly improved this paper.
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Footnotes
- ...
(LOFAR
- See the LOFAR web-site at http://www.lofar.org/
- ...
(SKA
- See the SKA web-site at http://www.skatelescope.org/
- ... Archive
- The WSA is located at http://surveys.roe.ac.uk/wsa/
- ...
exposures
- 80 s exposures are sometimes taken in mediocre conditions, an example of which is the finding chart shown in Fig. 1.
- ...
asteroids
- Some asteroids, observed at a turning point between prograde and retrograde motion, can appear stationary in UKIDSS survey images taken within an hour of each other.
- ... remained
- The choice of
threshold value for
(which defines the list of candidates and determines the completeness and contamination of the quasar sample) depends on the resources available for follow-up photometry and spectroscopy.
All Tables
Table 1: Original survey and follow-up photometric observations of ULAS J1319+0950.
Table 2: Effective optical depths of the absorption systems seen in the spectrum of ULAS J1319+0950.
All Figures
![]() |
Figure 1:
Finding chart for ULAS J131911.29+095051.4 showing the UKIDSS LAS
|
Open with DEXTER | |
In the text |
![]() |
Figure 2:
The Gemini GMOS spectrum of ULAS J1319+0950 (black curve) and the
noise spectrum (red curve), both binned by a factor of four.
The gaps at wavelengths of
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
The Gemini NIRI spectrum of ULAS J1319+0950 (black curve) and the
error spectrum (red curve), both binned by a factor of two. The
continuum+line fit to the Mg II emission line is also shown (blue).
The fit implies a source redshift of
|
Open with DEXTER | |
In the text |
![]() |
Figure 4: The optical spectrum, binned by a factor of four (left black curve), and the NIR spectrum, binned by a factor of five (right black curve), of ULAS J1319+0950. The power-law continuum fit is also shown (blue). |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Rest-frame spectra of ULAS J0203+0012 (blue) and ULAS J1319+0950 (green) compared to the composite spectrum of
|
Open with DEXTER | |
In the text |
![]() |
Figure 6: Re-calibrated VLT spectrum of ULAS J0203+0012 (black curve) and the noise spectrum (red curve), binned by a factor of two. The wavelengths of common emission lines redshifted by z = 5.72 are indicated. |
Open with DEXTER | |
In the text |
![]() |
Figure 7:
The combined optical and NIR spectrum, spliced at
|
Open with DEXTER | |
In the text |
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