A&A 413, 843-859 (2004)
DOI: 10.1051/0004-6361:20031532
K. Kawara 1 - H. Matsuhara 2 - H. Okuda 2,3 - Y. Taniguchi 4 - Y. Sato 1 - Y. Sofue 1 - K. Wakamatsu 5 - S. Oyabu 1 - D. B. Sanders 6 - L. L. Cowie 6
1 - Institute of Astronomy, The University of Tokyo, 2-21-1 Osawa,
Mitaka, Tokyo, 181-0015, Japan
2 -
Institute of Space and Astronautical Science (ISAS), 3-1-1 Yoshinodai,
Sagamihara, Kanagawa, 229-8510, Japan
3 -
Gunma Astronomical Observatory, Gunma 377-0702, Japan
4 -
Astronomical Institute, Tohoku University, Aoba,
Sendai 980-77, Japan
5 -
Department of Physics, Gifu University, Gifu 501-11, Japan
6 -
Institute for Astronomy, University of Hawaii,
2680 Woodlawn Drive, Honolulu, HI 96822, USA
Received 28 May 2003 / Accepted 25 September 2003
Abstract
We present the catalogs and source counts for the C_90 (reference
wavelength of 90 m) and C_160 (170
m) bands, which were
extracted from our analysis of an ISO deep far-infrared survey conducted
as part of the Japan/UH ISO cosmology project. The total survey area is
0.9 deg2 in two fields within the Lockman Hole. The analysis
consists of source extraction using the IRAF DAOPHOT package and simulations
carried out by adding artificial sources to the maps to estimate the detection
rate, the flux bias, the positional accuracy, and the noise. The flux
calibration was performed using the Sb galaxy UGC06009 -
the photometric error was estimated to be
50% at C_90 and
65% at C_160. The total noise
estimated from the simulation is dominated by
the confusion noise due to the high source density. The confusion noise is
20 mJy at C_90 and
35 mJy at C_160, which is much
larger than the instrumental noise which is at the level of a few mJy or less.
The catalogs were constructed by selecting 223 C_90 sources and 72 C_160
sources with a Signal to Noise Ratio (SNR) of three or greater. The
distribution of the observed associations between C_90 and C_160 sources
indicates that the
positional errors are
20
and
35
at C_90 and C_160, respectively. The corrections for
the detection rate and the flux bias are significant for sources fainter than 200 mJy at C_90 and 250 mJy at C_160. Most of the sources detected both
at C_90 and C_160 have a F(C_160)/F(C_90) color redder than the Sb galaxy UGC 06009. Such a red color could result from reddening due to the flux
bias or a K-correction brightening due to the effect of redshift. Red sources
brighter than 200 mJy at C_160 may be very luminous galaxies like Arp 220
at moderate redshift. The source counts are derived by applying the
corrections for the detection rate and flux bias. The resultant counts are
quite consistent with the constraints derived from the fluctuation analysis
performed in Paper II. The C_160 counts are also consistent
with the results from the FIRBACK project. Our C_90 survey, which is 2-3 times deeper than those previously published, reveals an upturn in the
count slope at around 200 mJy. While recent models give a reasonable
fit to the C_160 counts, none of them are successful in accounting for the
upturn in the C_90 counts. If the upturn is caused by ultraluminous IR galaxies, their redshifts would need to be at
,
implying a major
event in galaxy evolution at moderate redshift.
Key words: galaxies: evolution - galaxies: starburst - cosmology: observations - infrared: galaxies
The IRAS all-sky survey opened up a new window on galaxy
evolution, and showed that a significant fraction of the bolometric luminosity
of all galaxies is emitted at far-infrared wavelengths through reprocessing by
dust of UV/optical light from both stars and active galactic nuclei (AGN).
The far-infrared spectra of
galaxies peak in the wavelength range 25-200 m. Cirrus-dominated normal
galaxies have an emission peak at 100-200
m, while infrared-luminous
starburst galaxies peak near 60
m, and Seyfert galaxies often show a peak
near 25
m (Sanders & Mirabel 1996 and references therein).
The infrared luminosity as observed by IRAS is
30% of the
total energy output of galaxies in the local Universe
(Soifer & Neugebauer 1991). The detection of the CIB (Cosmic
Infrared Background) with the COBE satellite at far-infrared and submillimeter
wavelengths (e.g. Puget et al. 1996) indicates that the integrated
luminosity from thermal dust emission is comparable to or greater than that of
the integrated UV/optical light of galaxies in the Hubble Deep Field (HDF)
(Guiderdoni et al. 1997), implying a potentially larger
contribution from dust-enshrouded star formation than that inferred from the
rest-frame optical/UV at high redshift.
As discussed by Steidel et al. (1999 and references therein),
at high redshift where optical observations are sampling the rest-frame
optical/UV, the SFR density derived from optical observations (e.g. Madau et al. 1996) may be substantially underestimated as a result of
absorption by dust.
The next step is to resolve the CIB into individual sources.
The sub-millimeter
common-user bolometer array (SCUBA) on the 15 m James Clerk Maxwell
Telescope (JCMT) is now able to resolve a substantial fraction of the CIB
at 0.85 mm into luminous IR galaxies most of which appear to lie at high redshift, z > 1 (Smail et al. 1997; Hughes et al. 1998; Barger et al. 1998;
Scott et al. 2002; Sato et al. 2002). In the mid-
and far-infrared, various surveys have been conducted with the European
Space Agency (ESA) Infrared Space Telescope (ISO: Kessler 1996),
which was in operation between 1995 and 1998. Most of the deep ISO
mid-infrared surveys were
performed in the 6.7 m (LW2) and/or 15
m (LW3) bands.
6.7
m surveys are useful for looking at stellar systems at high redshift
(Serjeant et al. 1997; Taniguchi et al. 1997;
Flores et al. 1999a; Altieri et al. 1999; Sato et al.
2003; Oliver et al. 2002). The cross-identification of 6.7
m sources with SCUBA sources suggests that star
formation with a SFR of
can build up
massive stellar systems of 5
by redshift
z = 1-2 (Sato et al. 2002). 15
m surveys carried out by different groups to
different depths, probed emission both from warm dust and the unidentified
infrared bands at 6-13
m in star forming galaxies
(Serjeant et al. 1997; Flores et al. 1999b;
Aussel et al. 1999; Altieri et al. 1999;
Elbaz et al. 1999; Oliver et al. 2002). The 15
m counts show an excess at 400
Jy by a factor of
10
(Elbaz et al. 1999),
requiring strong cosmic evolution of the mid-infrared emission of galaxies.
The excess could be largely attributable to bright and massive galaxies at z < 1.5 (Elbaz et al. 1999).
The CIB has a major peak at wavelengths 100-200 m that is presumably
due primarily to emission from cool dust (e.g., Hauser & Dwek
2001). If the rest-frame SEDs of starburst galaxies peaking at 60-100
m are responsible, this might imply a high SFR at
,
corresponding to a major event in galactic evolution.
The far-infrared
imaging instrument ISOPHOT (Lemke et al. 1996) onboard ISO was
used to carry out deep far-infrared surveys in a 0.9 deg2 area
in the LH using the 90
m and 170
m bands
(Kawara et al. 1998; Matsuhara et al. 2000), in 4 deg2 in the Marano fields and northern ELAIS fields using the 170
m band as part of the FIRBACK project (Puget et al. 1999;
Dole et al. 2001), in 12 deg2 of the ELIAS fields using the 90
m band (Oliver et al. 2000; Efstathiou et al.
2000), in 0.4 deg2 in the SA57 field using the 60
m and 90
m bands (Linden-Vørnle et al. 2000), and
in 1.6 deg2 in eight fields at wavelengths between 90
m and 180
m (Juvela et al. 2000). The far-infrared source counts
derived by the various groups are in agreement with strongly
evolving models of the starburst galaxy population. While the resolved
sources brighter than 180 mJy at 170
m account for less than 10% of
the CIB (Dole et al. 2001), the constraints from the fluctuation
analysis by Matsuhara et al. (2000) indicate that
sources brighter than 35 mJy at 90
m and 60 mJy at 170 mJy contribute
5-40% of the CIB.
This is our third paper reporting results from our ISO deep
far-infrared survey that was conducted at 90 m and 170
m
in the LH. The survey was made as part of the Japan/UH
ISO cosmology program using ISAS guaranteed time. Paper I
(Kawara et al. 1998), reported that the source
counts at 90
m and 170
m are much greater than expected from a no-evolution model. The high counts at 170
m have been confirmed by
Puget et al. (1999). Paper II (Matsuhara et al. 2000),
used fluctuation analysis to place constraints on the source counts down
to a level of 35 mJy at 90
m and 60 mJy at 170
m. These
constraints suggest a steep slope in the source counts versus flux, implying
strong galaxy
evolution, most likely at moderate redshift (e.g., Takeuchi et al.
2001). In the current paper, we describe our source extraction
method, perform simulations to estimate the reliability and completeness of
our survey, construct the catalogs of far-infrared sources, derive the source
counts at 90
m and 170
m, and discuss the implications of our
results.
We have carried out a far-infrared survey in the LH using ISOPHOT, which was an imaging photopolarimeter onboard ISO. The LH is a region of the sky with the smallest HI column density (Lockman et al. 1986), and thus the far-infrared confusion noise caused by infrared cirrus is expected to be a minimum in this region (Gautier et al. 1992).
The survey was performed in two fields, LHEX and LHNW, between revolutions 194
and 215 (May 28 and June 19, 1996). Each field extends approximately
.
The center of the LHEX field is
at
(J2000), and LHNW is at
(J2000).
LHEX contains the field in which the ROSAT Deep Survey
was carried out (Hasinger et al. 1998).
Our ISOPHOT observations were made using the PHT22 raster mapping mode
in the C_90 band (reference wavelength 90
m) and the C_160 band (reference wavelength 170
m) (see
).
Each
field consists of four rasters. The
area covered by each raster is approximately
.
Four rasters making one field were executed and completed in a single revolution, except for LHNW at C_160, so that the position angles of all of the rasters are almost the same on the sky.
For C_90, each raster has 18
18 raster points with raster steps of 69
corresponding to a 1.5 pixel
overlap in both directions in the spacecraft (Y, Z) coordinate system.
The integration time per raster point was 16 s. Within the maximum redundancy region, each part of sky
was thus observed by four different pixels resulting in a total integration
time per sky position of 64 s (4
16 s). For C_160, each raster has
27
14 raster points with raster steps of 46
corresponding to
a 1.5 pixel overlap in the Y axis and raster steps of 92
corresponding
to a one pixel overlap in the Z axis. The integration time per raster point
was 20 s.
Within the maximum redundancy region, each part of the sky was observed eight
times by four different pixels and thus the total
integration time per sky position was 160 s (8
20 s).
Our image processing consists of two stages. At the first stage,
the PHT Interactive Analysis (PIA) version 7.3
(Gabriel et al. 1997) was used, starting
with the edited raw data (ERD) created via the off-line processing
version 7.0. The AOT/Batch processing mode of PIA was employed using the
defaultparameters to reduce the ERD to the Astronomical Analysis Processing (AAP) level. This standard reduction includes discarding some of the readouts
at the beginning of the integration ramps, linearization and deglitching of
the ramps on the ERD level, signal deglitching and drift recognition
at the Signal-per-Ramp Data (SRD) level, reset interval normalization, signal
deglitching, dark current subtraction, and vignetting correction on the Signal-per-Chopper Plateau (SCP) data level. At the end of this stage, maps
were produced at the Astronomical Analysis Processing (AAP) level
in mapping mode using median brightness values. These are
called AAP maps in this paper. Each AAP map corresponds to the respective
raster.
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Figure 1:
The left column shows C_90 (90 ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() ![]() |
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The AAP maps, in particular for the C_90 band, are greatly affected by a slow
drift in the responsivity. No sources can be recognized because of the
overwhelming lattice pattern. At the second stage, we have developed the
so-called median filtering
technique
to remove the slow responsivity drift.
As shown in Figs. 1 and 2 in Paper I, median filtering dramatically
reduces the responsivity drift and many sources become recognizable in the map.
It should be noted that the AAP C_160 map is almost identical to that from
the median filtered signal map, implying that the detectors used for the C_160 band were stable and suffered little from responsivity drift.
Figure 1 shows the mosaiced maps of LHEX and LHNW, which are made
from the median filtered signal. The resultant maps of the four sub-fields
are first rebinned onto a 2.3
/pixel grid for C_90 and a 4.6
/pixel grid for C_160, and then combined into the 44
44
maps. Finally, the IRAF gauss routine was applied with
for smoothing the maps.
The IRAF DAOPHOT package (Davis 1994) was used to extract
sources from the maps for
the following reasons; (1) as shown in Fig. 1, the maps are very crowded,
often blending the light of two or more sources, and (2) FWHM measurements of
brightness profiles of bright sources indicate that all of their FWHMs are not
extended more than two detector pixels and thus they should be detected as
point sources.
DAOPHOT has indeed been developed to perform stellar photometry in crowded
fields (Stetson 1987) such as in the cores of globular clusters.
In DAOPHOT, the positions and relative magnitudes of
point sources are determined by using a numerical fitting
technique to match the given Point Spread Function (PSF) to the observed
light distribution. Where the light of two or more sources is blended, it fits
a model in which two or more of the expected PSFs are superimposed by
shifting each model PSF in position and scaling in intensity until a
satisfactory fit of the overall model to the image data is achieved.
IRAS F10507+5723, the brightest source in our survey, was used to define
the PSFs because the light distribution for IRAS F10507+5723 is typical
of what is expected when a point source is observed in our survey.
The following sequence from (1) to (6) was performed for extracting sources: (1) DAOFIND was used to find sources on the original map and produce a list of x and y positions of the sources; (2) PHOT was used on the original map to obtain aperture photometry and sky values for the sources in the list; (3) ALLSTAR was used to do simultaneous PSF-fitting for all the sources found on the original map, reject poorly fitted sources, and produce a list of sources and a subtracted map from which the listed sources are subtracted; (4) DAOFIND, PHOT, and ALLSTAR were used on the subtracted maps to identify sources that had been previously hidden by brighter sources, with the procedure repeated until all the significant sources were extracted from the subtracted maps; (5) PFMERGE was used to merge the original and all the other lists obtained from the subtracted maps and produce the new merged list; (6) ALLSTAR was used on the original image to do simultaneous PSF-fitting for all the sources in the merged list and produce the final list of sources.
DAOPHOT fits the PSF to the data within the specified fit-radius of 62
for C_90 and 124
for C_160, and computes the fitted
flux and flux error. The flux error is derived from a combination of the
residuals from the fitting and the uncertainty of the local sky values.
The SNR for source detection is a division of the flux by the flux
error, both of which DAOPHOT returns. However, such SNRs should
not be regarded as true, because the flux error is calculated by using
values in sub-pixels which are not themselves independent. We thus scaled the
flux error in such a way that the average of the flux errors given by DAOPHOT
agrees with that of the differences between the given and measured fluxes of
artificial objects in simulations that will be discussed later.
Figure 1 plots sources extracted by DAOPHOT on (top) the LHEX C_90 and C_160 maps and (bottom) the LHNW C_90 and C_160 maps.
The detected sources have
,
which is our
detection threshold in this paper.
Flux scaling is done by using the same standard source as described
in Paper I. This standard source is IRAS F10507+5723, which has ISO band fluxes, F(C_90) = 1218 mJy and F(C_160) = 1133 mJy. IRAS F10507+5723
is the only cataloged IRAS source in our survey fields,
and it is the brightest source in our survey fields. It is identified with a Sb galaxy
UGC 06009 (Thuan & Sauvage 1992). The IRAS fluxes are
F(60
m) = 533
59 mJy and F(100
m) = 1218
292 mJy
(IRAS FSC 1990). Its flux ratio, F(100
m)/F(60
m) = 2.29, can be
fit with a combination of IR cirrus and starburst spectra
(Pearson & Rowan-Robinson 1996), if 76% of the 100
m flux comes from
the cirrus component. This predicts F(C_160)/F(100
m) = 0.93, which
implies F(C_160) = 1133 mJy. F(C_90) is simply assumed to be identical to F(100
m) because the central wavelength at the C_90 band is 95
m
which is close enough to the IRAS's 100
m band. A large error may be
associated with the F(C_160) flux density. For example, combining recent
model spectra by Dale et al. (2001) with the same IRAS flux ratio
implies F(C_160)/F(100
m) = 1.15, leading to a F(C_160) value greater
than the former by
25%, which is comparable to the IRAS flux
error.
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Figure 2:
Comparison with the C_90 flux by Linden-Vørnle et al.
The mean ratio of ours to those in Linden-Vørnle et al. are 1.03
and the mean deviation from the line for ratio = 1 (dashed line) is
25% of the flux.
The dotted lines denote flux deviations of ![]() |
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The following arguments suggest that our flux calibration is associated with
a larger source of error than those discussed so far.
Our IRAF flux calibration results in 14.4 MJy sr-1 at C_90 and 5.17 MJy sr-1 at C_160 for the sky background. These are 3.5 times and 1.9 times greater than the COBE values (Paper I).
Note that the intensity of interplanetary dust emission varies little with
solar elongation at such high ecliptic latitude (
).
The discrepancy can be mostly attributed to the flux loss in the PSF
wings and to transients in the detector signals.
The fluxes for IRAS F10507+5723 were determined from the light
within the apertures used by the aperture photometry routine PHOT. The radii
of the apertures are 69
for C_90 and 138
for C_160.
The fractions of the PSFs, taken from the calibration files PC1FOOTP.FITS and PC2FOOTP.FITS, passing through the apertures are 0.92 for both C_90 and C_160. Note that the PSFs given in the calibration files agree with the
theoretical model PSFs that take into account the ISO primary mirror,
secondary mirror, and tripod (Okumura 2000).
The transient effects in the ISOPHOT data have been analyzed and discussed
by Acosta-Pulido et al. (1999). When the illumination changes, a generally
observed effect in the transients is an instantaneous signal jump followed by
a slow rise of the signal until stabilization is reached.
The instantaneous signal jumps are 0.30 of the stabilized value
at C_90 with the C100 detectors and
0.85 at C_160 with the C200 detectors. For the C200 detectors, the time constant for the slow rise is
40 s (see Fig. 5 in Lagache & Dole 2001).
In our 20 s integration, the signal reaches a level of 0.91.
Hence, the correction for the transient effect
is 0.88 (i.e., average of 0.85 and 0.91) at C_160 for point sources.
Note that such a correction should not be applied
to the sky background because its spatial distribution is extremely smooth and
flat. For the C100 detectors, the time constant is longer than that for the C200 detectors, and
it takes several hundreds of seconds to reach stabilization of the signal
(see Fig. 7 in Acosta-Pulido et al. 1999).
In our 16 s integratio, the signal reaches a level of
0.60. Thus,
the correction for the transients is roughly
0.45 at C_90.
After applying the corrections to the point source for the effects of the PSFs and the transients, the IRAS flux scaling gives sky background
values that are 1.45 and 1.55 times greater than the COBE values.
Thus, our calibration may overestimate the fluxes by 45% at C_90 and 55% at C_160. Taking all of the errors into account, the total errors
associated with our flux calibrations are estimated to be 50% at C_90 and 65% at C_160; i.e., in the case of C_160, a 25% error for the IRAS 100 m flux,
25% for the model prediction, and 55% for the deviation from the COBE flux.
Table 1: Identification with sources in Linden-Vørnle et al.
Linden-Vørnle et al. (2000) have reduced our C_90 data in the LHEX and LHNW fields by using the PIA with median filtering similar to our image processing. They then used SExtractor to detect and measure sources. Their flux calibration is based on the calibration files supplied with PIA v7.31(e). IRAS F10507+5723 then has a C_90 flux of 747 mJy, which is 1.63 times smaller than the IRAS value. To be consistent with our flux scaling, their C_90 fluxes are multiplied by 1.63 in the following discussion.
They detected 8 sources that are brighter than 269 mJy. In Fig. 1,
these sources are marked by a "+" symbol. As can be seen from the maps, these
are the brightest sources in our observations. Table 1 identifies their
sources with our sources having a .
Two of their eight sources are
resolved into two sources, while two are not detected because the SNRs are
less than 3. One of the two resolved sources, called E4_3 by
Linden-Vørnle et al. (2000), is also resolved into two sources
in high spatial resolution VLA observations (De Ruiter et al.
1997), suggesting that DAOPHOT is a useful tool for extracting
far-infrared sources in crowded fields. It is also possible that the two
undetected sources are extended or that they are multiple sources, where
DAOPHOT has failed to fit PSFs with sufficient SNRs.
Figure 2 compares the Linden-Vørnle et al. fluxes with ours. After multiplying by 1.63, the mean ratio of our fluxes to their fluxes is 1.03 and the mean deviation from the line of ratio = 1 is 25% of the flux, thus being in agreement within 25%. As can be recognized from Table 1 and Fig. 2, their flux errors are approximately two or three times smaller than ours. As will be discussed in Sect. 4.2, our flux error is estimated from the simulations, and thus it includes the confusion noise due to the high source density which is a dominant noise source in our survey observation. On the other hand, Linden-Vørnle et al. (2000) did not perform simulations, thus their flux error does not include such confusion noise. This could explain why their flux errors are two to three times smaller than ours.
To estimate the errors and bias in detection, photometry, and astrometry, we have carried out simulations using artificial objects. In crowded fields where the detection limits are controlled by the confusion noise, strong Eddington/Malmquist noise is expected. Near the detection limit, more sources are scattered to brighter fluxes (e.g., Oliver 2002). In fact, in crowed fields there is a good chance of having more than one source within a photometric aperture resulting in the two sources being detected as a single brighter source. This results in overestimating the flux (flux bias) and thus the number of bright sources.
It would be ideal to add the signals of artificial sources to the ERD data in such a way that all of the routines used in the data reduction can be checked by the simulations. However, such simulations are very time-consuming and require complete knowledge of such systematic effects as transient behavior of the detectors and incident stray light. However, because of our incomplete understanding of such effects, we decided to perform the simulation by adding artificial objects to the original maps shown in Fig. 1.
Detections and measurements were made on simulation maps, to which artificial
objects were added by using the same set of DAOPHOT parameters as used
to detect sources in the original maps. The simulations were repeated by
changing the positions and fluxes of artificial objects until a
statistically sufficient number of objects had been detected.
The fluxes given in the
simulations range from 50-200 mJy for C_90 and from 70-280 mJy
for C_160 in steps of 0.15 dex (
). The results from
the simulations are summarized in Figs. 3 and 4.
The top panels in Fig. 3 indicate the expected flux bias; the ratio of the
measured flux over the given flux increases as the given flux decreases. The
bottom panels show a rapid slowdown of the growth in source counts toward the
faint end of the flux range. In other words, the detection rates rapidly
decrease as the flux decreases.
Table 2: Corrections for source confusion estimated from simulation.
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Figure 3: Summary of the simulations for detection of C_90 (left panels) and C_160 (right panels) sources. The top panels plot the flux given to artificial objects against the flux measured by DAOPHOT. The dotted lines denote the ideal case where the given flux is identical to the measured flux. Due to Eddington/Malmquist bias, the ratio of the measured flux to the given flux increases as the given flux decreases. The bottom panels shows the detection rates as a function of the measured flux. The crosses represent the values of the corrections applied to the source counts (see Table 2). |
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Figure 4:
Accuracy of the catalog data estimated from the simulations for C_90 (left panels) and C_160 (right panels) sources. The top panels show
the ratio
of the flux measured by DAOPHOT to the flux given to artificial sources. The
error bars associated with the flux ratio represent a standard deviation as
defined by
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The derived correction factors to the source counts are given
in Table 2. The values of the correction factors listed in the table are
marked by crosses in Fig. 3. It can reasonably be assumed that sources
brighter than 400 mJy are free from the effects of Eddington/Malmquist bias.
As one can see from this table and Fig. 3, the corrections for source confusion are important for determining source counts. For example,
30% of the 100-141 mJy C_90 sources are detected as 1.78
brighter sources, while 64% of the 200-283 mJy C_160 sources are
detected as 1.31
brighter sources.
The PIA provides a determination of the signal uncertainty at the individual
raster positions. This PIA noise can be used to estimate the instrument noise
(Kiss et al. 2001). With PIA Ver8.1, we have produced
uncertainty maps. The median filtering technique reduces the PIA noise
significantly, namely 2
and 5
smaller than those without this
technique at C_90 and C_160, respectively. The typical 1
noise
levels are 1.3 mJy per
pixel at C_90 and 0.6 mJy per
pixel at C_160, after the IRAS-based
flux calibration is applied. These values correspond to 3.1 mJy within
a PSF-fitting radius of 62
at C_90 and 1.4 mJy within a 124
radius at C_160. As will be discussed later, the instrumental
noise is much smaller than that estimated from the simulations.
The confusion noise due to IR cirrus should not be a dominant noise source given the low level of the total HI column density for our two LH fields. Analyzing the brightness fluctuation at C_90 and C_160 in our fields, Matsuhara et al. (2000) in Paper II found that the spatial power spectrum was flat at low spatial frequencies (f < 0.1 arcmin-1) and was slowly decreasing toward higher frequencies. These spectra are quite different from the power-law spectra expected from IR cirrus, and are well explained by randomly distributed sources (i.e., galaxies). In addition, a point-to-point comparison between C_90 and C_160 brightness shows that the slope of the linear fit is quite different from that expected from IR cirrus (Paper II; Juvela et al. 2000).
Following the technique described by Dole et al. (2001),
the total noise including the confusion noise due to the high number density
of sources, can be estimated from the results of the simulations.
In this technique, the difference between the measured and given
fluxes of the artificial objects is regarded as the noise. The middle panels
in Fig. 4 show 1
dispersions of the differences in flux as a function of the measured flux. The dispersions increase with the fluxes.
It is reasonable to approximate the dispersions by a quadratic sum of
,
where
is constant and
is
proportional to the flux (i.e.,
= a
flux). The dotted lines
in the figures represent
= 20 mJy with a = 0.16 for C_90 and
= 35 mJy with a = 0.2 for C_160. The
values,
corresponding to the noise at zero flux, are much greater than the instrumental
noise and the noise due to IR cirrus fluctuations. Thus, we conclude
that our observations are limited by the confusion noise due to the high
density of galaxies.
Our confusion noises are
20 mJy at C_90 and
35 mJy at C_160. These values are consistent with the value of 45 mJy derived from the C_160 source
counts by Dole et al. (2001) and those from the fluctuation analysis
of C_90 and C_160 brightness by Kiss et al. (2001).
The standard rule of thumb is that confusion becomes important at 1/30 of a source per beam (Hogg 2001).
One sigma confusion noise can be represented as
by integrating sources fainter than
falling within one beam
(e.g., Helou & Beichman 1990; Lagache & Puget
2000) . Assuming the cumulative number counts down to
to be a power law function of the flux density, namely,
,
we have
.
Our cumulative source counts have forms of
at C_90 and
at C_160. Hence, at the 3
limit, namely
,
the number of sources for
is
= 1/27. In our source counts, the number
of sources brighter than the 3
noise levels are
1.5
106 and 3.5
105 per steradian at C_90 and C_160,
respectively. Because the beam solid angles are
for C_90 and
for C_160,
the numbers of sources per beam are 1/13 at C_90 and 1/14 at C_160.
Our analysis has thus pushed the confusion limited flux levels beyond the
classical limit by a factor of two in terms of sources per beam. This may be
largely attributed to use of DAOPHOT for source extraction. As already pointed
out, DAOPHOT has been developed to do stellar photometry in crowded fields
like the cores of globular clusters. In hoping that DAOPHOT would push the
confusion limit to a fainter flux level, we decided to use it for source
extraction.
Table 3: Cumulative numbers of sources.
To construct the ISO far-infrared catalogs that will be used in the
subsequent analysis, we have selected sources with SNR > 3,
excluding areas near the edges of the maps. The redundancy of the observations
along the edges of the maps is less than for the inner regions, implying
poorer sensitivity near the edges.
The widths of these edges correspond to the size of the detector, namely
46
at C_90 and 92
at C_160.
As given in Table 3, the total survey areas
are 0.904 deg2 at C_90 and 0.885 deg2 at C_160. C_90 and C_160
observations were not performed in the same revolution so that each has a different roll angle, resulting in some small areas where observations were
only performed at a single band. The common areas in which both C_90 and C_160 observations were made are 0.426 deg2 for LHEX and 0.431 deg2
for LHNW.
The total common area is thus 0.857 deg2, which is 95% of the total area
observed at C_90 and 97% at C_160.
The catalogs are given in Tables 4-7. As summarized in Table 3, the numbers
of sources listed in the catalogs are 223 at C_90 and 72 at C_160; thus
there are
295 entries in total. The first column of the catalogs gives the names of sources. C_90 and C_160 sources in LHEX are prefixed 1EX and 2EX,
respectively, and those in LHNW are prefixed 1NW and 2NW, respectively.
The three digits following
the prefix are running numbers given by DAOPHOT. Therefore, 2NW007 means
the 7th source in LHNW detected in the C_160 band. Columns 2
and 3 give the right ascension and declination (J2000). The errors
in position estimated from the simulations are given in the bottom panels of Fig. 4. They
are estimated to be 20
at C_90 and 35
at C_160.
As will be discussed in the next subsection, these errors are consistent
with those estimated from Fig. 5.
Column 4 shows the flux density in mJy along with the error. Column 5 gives
the SNR estimated from DAOPHOT photometry.
The flux errors for sources fainter than 400 mJy are estimated from the simulations as shown in the middle panels of Fig. 4. For brighter sources, the flux errors are simply the flux divided by
the SNR.
No correction for flux bias was applied to the flux density values
given in the catalogs. Notes are given in Col. 6. The area observed
at C_90 differs slightly from that at C_160 due to
field rotation; therefore some sources were only observed at either C_90 or C_160. Such sources are marked "*'' in the last column.
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Figure 5:
The distributions of associations between C_160
and C_90 sources as a function of distance, where distance is an angular
separation from a C_160 source to the nearest C_90 source.
The top panel shows the observed 65 associations with a distance of 300
![]() ![]() ![]() ![]() ![]() ![]() |
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Table 4:
C_90 (90 m) sources in LHEX.
Table 5:
C_90 (90 m) sources in LHNW.
Table 6:
C_160 (170 m) sources in LHEX.
To merge the separate catalogs, C_160 sources were cross-associated with
C_90 sources. To do this, C_160 sources were coupled to the nearest C_90
source and their angular separations were computed. This was done for
70 C_160 sources that were all "detected" at C_90.
The results are given in the top panel of Fig. 5. The
distribution of the observed associations consist of real physical
associations and fault background associations that are produced by chance.
To estimate the number of background associations, we generated C_90 and C_160 sources at
positions which are distributed at random. The number of sources and
the field areas are the same as those where the observations were performed.
This operation was repeated 50 times so that a statistically sufficient
number of background associations were obtained. The distribution of
background associations are given in the middle panel of Fig. 5. The background
is normalized in such a way that the total number of background
associations within a distance range (i.e., angular separation)
100-300
is equal to that of observed associations in the same
distance range. The difference between the observed and the background
associations, which presumably represents real associations only (plus
statistical fluctuation), is given
in the bottom panel of Fig. 5. The dotted lines in Fig. 5 show the
distribution for the real associations with positional errors of 20
and 35
for C_90 and C_160 sources, respectively. These errors are
obtained through the simulations. Judging from a comparison between the
top panel (observed associations) and the bottom panel (presumably real
associations plus statistical fluctuation), 85% of the observed associations
with a distance of 50
or less are real.
Table 7:
C_160 (170 m) in LHNW.
The cross-association catalogs are given in Tables 8 and 9. All the
associations with a distance of 50
or less are regarded as real, and
listed in the catalogs.
Table 8:
C_160 (170 m) sources associated with C_90 (90
m)
sources in LHEX.
Table 9:
C_160 (170 m) sources associated with C_90 (90
m)
sources in LHNW.
Table 10: Source counts without the corrections.
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Figure 6:
The C_160 flux plotted versus the ratio of the C_160 flux to
the C_90 flux. The upper panel shows error bars, while the error bars are
omitted in the bottom panel.
The solid lines are predictions for the flux-color relations at various
redshifts for M 82, Arp 220, and 10 ![]() |
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32 C_160 sources are listed in the cross-association catalogs. The diagrams plotting the F(C_160) flux versus the IR color i.e., the flux ratio F(C_160)/F(C_90) are shown in Fig. 6. The upper panel shows error bars, while error bars are omitted from the bottom panel. The errors shown in the upper panel do not include the errors associated with the flux calibration. As discussed above, the flux calibration errors are estimated to be 50% at C_90 and 65% at C_160. In the diagrams the relative positions of all the data points are fixed to each other, but they can move tanslationally up to 65% in the flux axis and 80% in the color axis. The standard source UGC 06009 for the flux calibration is plotted as a filled circle. As discussed in Sect. 3.2, UGC 06009 is likely to be a cirrus dominated Sb galaxy and is expected to have a red F(C_160)/F(C_90) color. Nonetheless, most of our sources are redder than UGC 06009. There are three possible reasons making the color red. These are reddening due to flux bias, K-correction brightening (in particular at C_160 due to reshift), and the presence of very cold dust.
Table 11: Source counts after corrections for the detection rate and flux bias.
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Figure 7:
The source count versus flux-density relations plotted
for ISO far-infrared sources in the Lockman Hole.
The top panels show
differential counts for C_90 sources on the left and C_160
sources on the right. The data connected by the dashed line are
those without the corrections. The vertical error bars shown
are statistical errors only i.e., ![]() |
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![]() |
Figure 8:
The number versus flux-density relations for ISO far-infrared
sources in the Lockman Hole are compared with other observations
and various models. The top panels show the differential counts
for C_90 sources on the left and C_160 sources on the right.
The filled circles are from the present data after
corrections for the detection rate and the flux bias,
the open diamonds are from the ISO C_90 ELAIS survey, the plus signs are from the IRAS 100 ![]() ![]() ![]() |
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To examine the first two causes, the flux-color relations for starburst
galaxy M 82, ultra-luminous IR galaxy Arp 220, and 10
Arp 220 at various redshifts are overlaid in the panels by the solid and
dotted lines. These relations are calculated based on the SEDs of M 82 (Efstathiou et al. 2000 and
references therein), and the ultra-luminous IR galaxy Arp 220 (Rigopoulou et al. 1996; Klaas et al. 1997).
The solid lines include the effect of the flux bias given in the upper
panels of Fig. 3 and Table 2, while the dotted lines represent the case
without this effect.
The flux bias makes the flux brighter and the color redder, and the
effect becomes more significant as the flux decreases. The figures
imply that a significant fraction of faint sources below 200 mJy at C_160
are starburst galaxies like M 82 and their intrinsic blue colors are
reddened by the flux bias.
On the other hand, bright sources above 200 mJy with a red color could be
dominated by very luminous galaxies such as Arp 220 at moderate redshifts.
In addition, there may be a contribution from galaxies having very cold dust
(Alton et al. 1998; Haas et al. 1998).
The large errors associated with the flux calibration hampers further
insight into the flux-color diagrams. Precise measurements of the
far-infrared flux for our calibration source UGC 06009
(IRAS F10507+5723) are required from
future missions like SIRTF and ASTRO-F.
The cumulative and differential source counts are tabulated in Table 10. These are "raw'' counts derived from Table 3 without any corrections. To obtain "true'' counts, the corrections for flux bias and the detection rate should be applied to the un-corrected counts. This is done by using the correction factors tabulated in Table 2, and the resultant corrected counts are given in Table 11. The corrected counts, both in differential and cumulative forms, are compared with the un-corrected counts in Fig. 7. The differential counts are plotted in the top panels, and the cumulative counts in the bottom panels. The data connected by solid lines are corrected counts and those dashed lines are un-corrected counts. The zones enclosed by the dotted lines in the bottom panels are constraints derived from the fluctuation analysis performed on the present survey data in Paper II. It is very encouraging to know that the results from the different methods, i.e., the fluctuation analysis in Paper II and the source extraction in this work, are consistent with each other. It should be noted that the corrections become significant in the flux range below 200 mJy at C_90 and below 250 mJy at C_160, underscoring the importance of the simulations.
Our corrected source counts are compared with other observations and models
in Fig. 8. The differential counts for C_90 sources are plotted on the left
of the top panels and C_160 sources on the right, and the cumulative counts
are given in the middle and bottom panels.
The filled circles are from the present work, the open diamonds from
the ISO C_90 ELAIS survey (Efstathiou et al. 2000),
the "+'' (plus) symbols from the IRAS 100 m counts reported by
Efstathiou et al. (2000), the "
'' (cross) symbols are from
Linden-Vørnle et al. (2000), and the open squares are from
the FIRBACK C_160 survey
(Dole et al. 2001). The regions enclosed by the dash-dot lines are
constraints on the cumulative counts that were derived from the fluctuation
analysis in Paper II.
As can be seen in the right panels, our C_160 counts are consistent
with the results by Dole et al. (2001). The essence of our work
is shown in the left panels. It is clear that our C_90 observations
are 2-3 times deeper than those previously published and that there is
an upturn in the count slope at 200 mJy for C_90 which has never
been
recognized with the depth of the previous surveys. To explore the nature of
the sources, the source counts are compared with various models.
The dash-dot lines in the top panels show the model by Chary & Elbaz
(2001), based on the differential number counts at 15
m,
especially the "knee'' in the count slope at 0.4 mJy (Elbaz et al.
1999). Far-infrared counts are predicted by utilizing the
correlations between far-infrared and 15
m fluxes.
In their model, the SFR density peaks
at z = 0.8 with a value 30
greater than the local value, and
gradually decreases towards higher redshift.
The solid and dashed lines in the top and middle panels represent the
evolution #3 and no-evolution models by Takeuchi et al. (2001),
respectively, where they assumed a spike in the star formation
history; the SFR density peaks at
z = 0.5-0.8 where
it is 30
greater than in the local universe, while at higher redshift
it is only 3
the local value to be consistent with the CIB.
The dotted lines illustrate the model of scenario E by Guiderdoni et al.
(1998) that yields the maximum counts of far-infrared sources
among their models. In scenario E, the SFR density is 3
the local
value at
and peaks at
with a density
of 10
the local value. The models by Rowan-Robinson (2001)
and
Franceschini et al. (2001) are overlaid in the bottom panels
by using the long-dashed and dash-dot-dot lines, respectively.
In the models by Rowan-Robinson and Franceschini et al., the SFR densities
rapidly increase with redshift, from peaks at
.
The densities are
the local value at z = 0.5, and
the local
value at z = 1.
While the models give a reasonable fit to the C_160 counts, all of them, except
for the one by Chary & Elbaz (2001), fail to account for the upturn
in the C_90 counts. Unfortunately, Chary & Elbaz (2001) only
plotted the prediction down to 200 mJy at 90 m. The model by
Takeuchi et al. (2001) is also consistent with the C_90 counts
down to 200 mJy, but it underestimates the differential counts by
a factor of three at 100 mJy.
The model by Takeuchi et al. (2001)
is characterized by a spike in the star formation history - the luminosity
density from
z = 0.5 - 0.8 is
the local value. Thus a spike with
a three times higher (
the local value) and a
narrower
redshift range, for example from
z = 0.5- 0.6, would be worth exploring.
If the upturn in the C_90 counts is caused by ultraluminous IR galaxies,
their redshifts would be at
.
It is urgent to identify the optical
counterparts of the faint C_90 sources because these sources would result
from a major event of galaxy evolution at moderate redshift.
Unfortunately, our C_90
survey is the only ISO survey that detects sources to a depth of 100 mJy at C_90. Thus, it is not clear whether the C_90 upturn can be seen in
all directions or if it is specific to the direction of our fields and we are
just looking at the high density part of the large scale structure of the
galaxy distribution. In future missions such as SIRTF and ASTRO-F, surveys in
similar bands are planned and thus should add further information on such
questions.
Our survey using a 60 cm diameter aperture telescope is heavily limited by
the confusion noise due to the high density of far-infrared emitting galaxies,
and the correction for the effect of the source confusion is significant,
hampering further insight on the nature of sources detected in our survey.
For SIRTF and ASTRO-F, with telescope diameters similar to ISO, the
super-resolution technique with a carefully designed sampling density would
minimize such confusion. Otherwise, we must wait for the Herschel 3.5 m telescope and the SPICA 3.5 m telescope being planned by ISAS.
An ISO deep far-infrared survey was conducted in the C_90 (reference
wavelength of 90 m) and C_160 (170
m) bands in two fields of
the Lockman Hole (LHEX and LHNW), covering a combined area of
0.9 deg2. This paper presents the catalogs and source counts.
Paper I discussed image processing and reported initial results, while
Paper II used a fluctuation analysis of the brightness distribution to derive
constraints on the source counts.
A summary of the results presented in this paper follows:
Acknowledgements
We would like to thank the ISOPHOT team, in particular Carlos Gabriel for many helpful discussion. T. T. Takeuchi has kindly made his models available in differential count form.