A&A 375, 739-751 (2001)
DOI: 10.1051/0004-6361:20010675
D. Donato1 - G. Ghisellini1 - G. Tagliaferri1 - G. Fossati2
1 - Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate,
Italy
2 - Center for Astrophysics and Space Sciences, University of California
at San Diego, 9500 Gilman Drive, La Jolla, CA 92093-0424, USA
Received 16 February 2001 / Accepted 3 May 2001
Abstract
We have considered all blazars observed in the X-ray band and
for which the slope of the X-ray spectrum is available.
We have collected 421 spectra of 268 blazars, including
12 archival unpublished ASCA spectra of 7 blazars whose analysis
is presented here.
The X-ray spectra of blazars show trends as a function
of their power, confirming that the blazar overall energy
distribution can be parameterized on the basis of one parameter
only, i.e. the bolometric luminosity.
This is confirmed by the relatively new hard (2-10 keV)
X-ray data.
Our results confirm the idea that in low power objects the
X-ray emission mechanism is the synchrotron process,
dominating both the soft and the hard X-ray emissions.
Low energy peaked BL Lac objects are intermediate, often showing
harder spectra in the hard X-ray band, suggesting that the synchrotron
process dominates in the soft band, with the inverse Compton process
dominating at high energies.
The most powerful objects have X-ray spectra that are flat both in the
soft and in the hard band, consistent with a dominating inverse Compton
component.
Key words: BL Lacertae objects: general - X-rays: galaxies
Thanks to -ray observations of EGRET, on board CGRO, we now
know the overall spectral energy distribution (SED) of blazars.
They are characterized, in
-
plots, by two
broad peaks.
It is believed that the first, located in the IR-soft X-ray band,
is due to synchrotron emission, while the second is due to the
inverse Compton process by the same electrons producing the
synchrotron part of the spectrum (Maraschi 1992;
Sikora et al. 1994; but see Mannheim 1993
for a different interpretation).
The 0.1-10 keV emission of blazars is therefore located in the
minimum between the two peaks, where both processes (synchrotron
and inverse Compton) can contribute.
Observations in this band are therefore useful to characterize
the relative importance of both processes.
This can constrain models, allowing a better determination
of the location of both peaks.
Usually, a steep power law energy distribution in the X-ray band
(with a spectral energy index
,
with
)
is due to the tail of the synchrotron spectrum,
while
flags the dominance of the inverse Compton spectrum.
There are exceptions to this rule, such as HBL (High energy peaked BL Lacs)
in a flaring state, which show a synchrotron spectrum peaking above 10 keV.
One dramatic example of this behavior is Mkn 501, whose synchrotron
peak energy, usually located below/at
keV, shifted to 100 keV or
more during its flare in April 1997 (Pian et al. 1998).
In these cases the X-ray spectrum, usually steep during
quiescence, becomes much flatter during flares.
Fossati et al. (1998) (F98 hereafter) have shown that blazars form a sequence,
with their SED changing in a continuous way as their bolometric
power changes:
low luminosity objects (HBL) have the synchrotron peak in the UV-soft X-ray
band, and the inverse Compton peak between the GeV and the TeV band.
The two components have approximately the same power.
As the bolometric luminosity increases, both peaks shift to lower
frequencies, and the Compton peak becomes increasingly dominant.
This trend offers the opportunity to unify in a single scheme the many
flavors of existing blazars, and calls for a physical explanation
(see e.g. Ghisellini et al. 1998).
To check the reliability of this trend we have collected data for all blazars having available spectral information in the X-ray band. For the soft band [0.1-2 keV], most of the results come from ROSAT, while for the 2-10 keV band the results are gathered from the EXOSAT, ASCA and BeppoSAX satellites.
Besides the data already published, we searched for unpublished data in the ASCA public archive, finding 12 observations of 7 sources. Results of the analysis of these data are presented here. We then add these sources to our sample.
The entire sample forms the largest database in the X-ray range: 421 spectra of 268 blazars. The X-ray data have been complemented by additional information regarding the redshift (when available), the radio flux at 5 GHz and the optical flux (in the V band).
The paper is organized as follows; Sect. 2 is devoted to the analysis of the 12 ASCA spectra, while in Sect. 3 we present the entire set of data. In Sect. 4 we compare the results in the soft and the hard X-ray bands and check for correlations with other spectral parameters, such as the broad band spectral indices connecting the radio with the optical fluxes, the optical with the X-ray fluxes, and the radio with the X-ray fluxes. In Sect. 5 we discuss our findings in the framework of the scenario proposed by Fossati et al. (1998), suggesting an improvement connected to a possible physical difference between low and high power sources.
We searched the ASCA public archive at HEASARC, finding 12 observations of 7 blazars that have not been analyzed and published before: 0405-123 and PKS 0420-014 (classified as Flat Spectrum Radio Quasars, FSRQs); B2 1308+326 and 1807+698 (classified as Low Peaked BL Lac objects, LBLs); 1ES 1028+511, 1553+511 and 1ES 2344+514 (classified as High Peaked BL Lac objects, HBLs).
1ES 1028+511 and 1ES 2344+514 have 3 separate observations each, while
B2 1308+326 was observed twice.
The search for unpublished observations is updated to November 1999.
During the preparation of this work the "Tartarus" data base
became available,
presenting results of an automatic spectral and temporal analysis for the
AGNs observed by ASCA.
We extracted the spectra of all sources from the files produced by the Revision-2 data release and included data transmitted in all 3 modes (High, Medium and Low) to increase the signal/noise ratio. The event files are obtained from all four instruments on board ASCA: the Solid-State Imaging Spectrometers (SIS0 and SIS1) and the Gas Imaging Spectrometers (GIS2 and GIS3). For the SIS we used the event files converted into BRIGHT mode. For a description of the ASCA observatory see e.g. Tanaka et al. (1994).
To screen the SIS and GIS data we follow the criteria given
in the ABC ASCA reduction guide, rejecting the data taken
during the passage of the South Atlantic Anomaly, or with
geomagnetic cutoff rigidity lower than 8 GeV/c, or with angles
between the targets and the day/night terminator smaller than 20
or for Elevation angles smaller than 5
.
The source spectra were extracted from circular regions centered
on the sources, with radii of 6 arcmin for the GIS
and 4 arcmin for the SIS0, while for the SIS1 the source is
normally nearer to the detector border and we had to use
a smaller radius of
arcmin.
For the GIS we extracted the background in circular
regions with the same dimensions used for the sources but centered on a
symmetric point with respect to the optical axis, where the contribution
of the source to the counts was negligible.
For the SIS, instead, the background was extracted from
blank field files because the sources occupied a large area of the detector.
On these blank fields we chose circular regions with the same radii
and positions used for the sources.
For the GIS spectra we used the 1994 May response matrices, while for the SIS spectra we generated the matrices with the SISRMG program of the FTOOLS V3.6 package. The ARF files for both SIS and GIS were derived with the ASCAARF V2.62 program. The GIS and SIS data were fitted in the channel ranges 69-1020 and 15-510, corresponding to the energy ranges 0.7-10 and 0.4-10 keV, respectively. The spectra were rebinned in order to have at least 25 counts in each new bin.
The ASCA spectra were fitted using XSPEC V10 with four models:
single or broken power law with free or fixed
(Galactic) absorption.
The cross section for photoelectric absorption is calculated following
Morrison & McCammon (1983), while the Galactic column density in the
direction of the sources was estimated from the 21 cm radio maps of neutral
hydrogen (Brinkmann & Siebert 1994; Danly et al. 1992; Dickey & Lockman
1990; Elvis et al. 1989; Lamer et al. 1996; Lockman & Savage
1995; Murphy et al. 1996).
The data were fitted simultaneously from all the instruments with the same
model. However, the normalizations were left as independent parameters
for each data set to account for the cross-calibration uncertainties
between the four detectors, estimated to be of the order of 6%.
The differences found between the various normalizations
were always consistent with these uncertainties.
Source | Obs. datea | ![]() |
![]() |
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F[2-10]b |
![]() |
1021 cm-2 | ![]() |
|||||
0405-123 | 09/08/1998 | 0.72 +0.51-0.63 | 1.76 +0.09-0.10 | 1.0/160 | 5.2 | 0.9 |
0420-014 | 31/08/1997 | 0.90 +1.04-0.81 | 1.86 +0.19-0.18 | 0.8/73 | 1.4 | 0.3 |
1028+511 | 28/04/1995 | 1.01 +0.23-0.21 | 2.53 +0.06-0.05 | 1.0/287 | 6.2 | 3.4 |
29/04/1995 | 1.33 +0.18-0.17 | 2.59 +0.05-0.05 | 0.9/310 | 7.4 | 4.5 | |
08/05/1995 | 1.12 +0.12-0.12 | 2.49 +0.04-0.04 | 0.9/201 | 7.8 | 4.1 | |
1308+326 | 10/06/1996 | 1.97 +2.96-1.97 | 1.99 +0.47-0.36 | 1.5/29 | 0.5 | 0.1 |
11/06/1996 | 0.97 +1.01-0.97 | 1.74 +0.32-0.23 | 1.4/78 | 0.6 | 0.1 | |
1553+113 | 16/08/1995 | 1.30 +0.62-0.61 | 2.47 +0.19-0.18 | 1.3/294 | 29.4 | 14.9 |
1807+698 | 05/11/1996 | 0.50 +0.28-0.27 | 1.75 +0.07-0.06 | 1.0/122 | 3.1 | 0.5 |
2344+514 | 10/01/1997 | 2.71 +0.17-0.17 | 2.13 +0.03-0.03 | 1.1/216 | 17.2 | 5.3 |
23/01/1997 | 2.91 +0.34-0.33 | 2.39 +0.08-0.06 | 0.9/72 | 10.4 | 5.2 | |
10/12/1997 | 2.93 +0.37-0.35 | 2.31 +0.07-0.07 | 1.2/202 | 10.4 | 4.2 |
The results of the 12 spectral fits of the 7 blazars
observed by ASCA are reported in Table 1.
The uncertainties for the spectral parameters are at the 90%
confidence errors for two parameters of interest (
).
The unabsorbed integrated 2-10 keV and monochromatic 1 keV fluxes
are obtained using only the SIS0 data.
As the observations presented in this paper were all taken after 1994,
they are most likely affected by the so-called "excess
"
problem. This is due to a degradation of the SIS efficiency below 1 keV which can give incorrect results for the column density and/or
other parameters. As suggested in the ASCA Web site, to avoid the
calibration uncertainties we considered
only the SIS data above 1 keV in the SIS+GIS combined fit.
Of the four models considered,
according to the F-test, the one that better represents the data
in all twelve cases is the single power law with free
.
In some cases (detailed below) we obtain a value for the absorbing
column greater (by a factor 3-10) than the Galactic value.
Note that the results obtained by the automatic analysis presented
in the "Tartarus" database are in excellent agreement with ours
(not surprisingly, since the same model is adopted).
What is somewhat surprising is that the broken power law model (either with
free or fixed
)
did not significantly improve the fits.
This may be indicative of true extra-absorption or a spectral behavior
more complex than those here examined (one possibility being a gradual but
continuous steepening of the spectrum).
In the following we will compare the spectral properties of blazars in the soft and hard X-ray bands considering only the single power law model. To this end, the results of this model allow a more uniform comparison.
The results of spectral fit for the 7 sources are discussed below, grouped in the three subclasses (FSRQ, LBL and HBL).
For 0405-123, the best fit gives a flat photon spectral index
,
indicating the dominance of the
inverse Compton component.
The derived
value is consistent with the Galactic value,
cm-2 (Danly et al. 1992).
Similar results are obtained for PKS0420-014, with a photon
spectral index
.
Also in this case the
value is consistent with the Galactic one
(
cm-2, Elvis et al. 1989).
For B21308+326 there are two observations on two consecutive days.
The spectra are quite noisy and also the reduced
are not
very good. In both cases the best fits are obtained with
a spectral index
-2.0.
Due to the large error bars (see Table 1),
the derived absorption column density
can be consistent with the Galactic one (
cm-2, Lockman & Savage 1995).
For 1807+698 we obtained
and a value of
consistent with the Galactic one (
cm-2, Murphy et al. 1996).
1ES1028+511 has been observed three times over a time span of two weeks.
The source did not significantly vary in flux nor in shape
(
).
In all cases the best fits are obtained for a value of
a factor 10 larger than the Galactic one (
cm-2; Lamer et al. 1996).
For 1553+113 the best fit is obtained with a value of
times larger than the Galactic one (
cm-2; Brinkmann & Siebert 1994).
The source 1ES2344+514 has been observed three times, twice in Jan. 1997
and one in Dec. 1997.
Both the fluxes and the spectral indices show some variability.
The best fit value for the
is about 1.5 times the Galactic value
(
cm-2Dickey & Lockman 1990).
Our purpose is to have the most complete ensemble of spectral information (fluxes and spectral indices) in the X-ray band, from 0.1 to 10 keV, of all known blazars. We therefore considered all blazars detected in the X-ray band, for which also a measure of the X-ray spectral index is available. We collected the data obtained by five X-ray satellites: Einstein, EXOSAT, ROSAT, ASCA and BeppoSAX (see Table 2).
The first step was to recognize if a source belongs to the blazar class, and to which subclass (i.e. if a source is a FSRQ or an HBL or an LBL). We used several published lists of blazars and other publications describing single recognized sources. We considered the Slew Survey Sample (Elvis et al. 1992; Perlman et al. 1996), the 2 Jy sample of Wall & Peacock (1985), and the 1 Jy BL Lac sample (Stickel et al. 1991). In addition, we used the lists taken from the works of Bade et al. (1994); Bade et al. (1998); Brinkmann et al. (1994); Brinkmann et al. (1997); Cappi et al. (1997); Comastri et al. (1997); Ghisellini et al. (1993); Lamer et al. (1996); Laurent-Muehleisen et al. (1999); Sambruna et al. (1997); Wolter et al. (1998) and Worrall et al. (1990). We also checked the NASA Extragalactic Database (NED) for other objects classified as BL Lacs/blazars, or that could be classified as such.
The total number of considered blazars is 268. Of these, 227 have been observed by ROSAT and 88 have spectral information in the 2-10 keV band [of these latter sources, 77 have both soft (ROSAT) and hard X-ray data]. The details about the breakdown of source among HBL/LBL/FSRQ, and of the data among different X-ray telescopes is reported in Table 2. The data obtained with Einstein have large errors associated and for almost all sources better ROSAT data were available. For these reasons, the Einstein data are not used to derive any of the results (or figures) of this paper.
Some sources have been observed many times either by the same and/or by
different satellites.
For these sources, we chose the observation with the best
in the analysis
.
For the most "famous" sources, like 3C 273, Mkn 421, Mkn 501, PKS 2155-304,
we do not include the results of all the observations made by all satellites,
but we have only listed few representative data (those with the best
)
for each of these sources (typically, one spectral datum for
each observing satellite).
Of course, the resulting catalogue is not a complete sample.
Nevertheless, it is the largest database of its kind, and we think it is
representative of the entire blazar class.
The large number of sources in each sub-category of blazars guarantees
a meaningful comparison between their
X-ray properties, and their relation with the fluxes in other bands.
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HBL | LBL | FSRQ | |
ASCA | 52 | 14 | 9 | 24 |
EXOSAT | 33 | 16 | 7 | 10 |
BeppoSAX | 47 | 29 | 9 | 8 |
ROSAT | 227 | 129 | 54 | 44 |
EINSTEIN | 62 | 7 | 23 | 32 |
TOTAL | 421 | 136 | 63 | 69 |
Data are presented in Table 5 with the following format. For each source, Table 5 gives the IAU name, the redshift, the fluxes in the radio band (5 GHz), optical (V band) and X-ray (1keV) and the X-ray photon spectral index. In the last columns of Table 5 we also indicate to which subclass the blazar belongs to (1 for HBL, 2 for LBL and 3 for FSRQs) and the observing satellite (RO=ROSAT; AS=ASCA; EI=Einstein; EX=EXOSAT; SA=BeppoSAX).
For the radio fluxes we calculated the averaged value when there was more than one observation; the optical fluxes reported in the NED database are calculated using the indicated magnitude dereddened with the galactic extinction AB as reported by the NED database. When in the literature we found only the 0.1-2.4 keV and/or the 2-10 keV integrated fluxes, we derived the monochromatic ones at 1 keV using the corresponding X-ray spectral index. All fluxes presented in Table 5 are not K-corrected.
To compute the luminosities, we used H0= 50 km s-1 Mpc-1 and
q0=0.5, and for the K-correction we assumed a radio spectral index
for all sources; an optical spectral index
for HBL and
for the rest of the sources;
for the X-ray data we used the listed X-ray spectral index.
Also the broad band spectral indices have been K-corrected.
The K-correction for sources with unknown redshift was computed using the
average redshift appropriate for each sub-class (i.e.
,
and
).
Theoretical models that explain the nature of the observed behaviors of blazars predict a continuity between the various subclasses. To check if this is true for the objects belonging to our catalogue, we computed the distributions of redshifts, X-ray and broad band spectral indices and luminosities.
Moreover, another goal of this work is to compare the blazar
characteristics observed in the soft and in the hard X-ray band.
We divided our sources into two groups, one with the data obtained
with ROSAT (0.1-2.4 keV) and another one with the data obtained with
EXOSAT, ASCA, and BeppoSAX (2-10 keV).
As anticipated (see Table 2) the first group of sources
contains 227 objects, while the second one contains 88 sources (38 HBL, 19 LBL and 31 FSRQ).
In addition, since the two sources 2344+514 and 1652+398 are very variable
and we have data both for a quiescent and a flaring state, in the latter
group we put the data of two observations (one for the high and one for the
low state) for each of them.
HBL | LBL | FSRQ | |
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Log
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Figure 1:
Distribution of the energy spectral index
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Figure 2:
Distribution of the energy spectral index
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The distribution of spectral indices, redshifts and luminosities are shown by the histograms in Figs. 1-9. In the figure captions we give the probability, according to the Kolmogorov-Smirnov (KS) test, that two distributions are drawn from the same parent population, comparing HBLs and LBLs, HBLs and FSRQs, LBLs and FSRQs.
The mean values of the plotted quantities are listed in Table 3.
The distributions of the energy spectral indices (Figs. 1 and 2) show that for FSRQ we have an average value less than unity in both energy ranges. This suggests that for this subclass of blazars we are observing only the inverse Compton component in the entire X-ray band, from 0.1 to 10 keV. For HBL, instead, the average energy spectral index is greater than unity, indicating that we are observing the synchrotron component after its peak. On average, LBL show a flattening going from the soft to the hard X-ray bands.
These results suggest that both the soft and the hard X-ray bands are
dominated by the inverse Compton process in FSRQs and by the synchrotron
process in HBL, while in LBL we have the synchrotron flux dominating
in the soft band and the flatter Compton component emerging at higher X-ray
energies.
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Figure 3:
Redshift distribution for the three subclasses.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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Figure 4:
Distribution of the radio luminosity for the three subclasses.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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Figure 5:
Distribution of the optical luminosity for the three subclasses.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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Figure 6:
Distribution of the X-ray luminosity for the three subclasses.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
P=0.6 for HBL-LBL;
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Figure 7:
Distribution of the broad band radio-optical
spectral index for the three subclasses.
Fluxes have been K-corrected as explained in the text.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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Figure 8:
Distribution of the broad band optical-X-ray
spectral index for the three subclasses.
Fluxes have been K-corrected as explained in the text.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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Figure 9:
Distribution of the broad band radio-X-ray
spectral index for the three subclasses.
Fluxes have been K-corrected as explained in the text.
Thick solid lines refer to the entire sample, while
thin solid lines refer to sources with only ROSAT data.
KS test results (for the entire sample):
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While the redshifts of FSRQs are quite uniformly distributed up to a value
of 3, BL Lacs have redshifts lower than 1 (and HBL have lower
redshifts than LBL, see Fig. 3).
There is no significant difference between the redshift distributions of
sources observed in the hard and in the soft X-ray bands.
Of the sources in our sample, about 25% have no measured redshift
(38 HBL and 17 LBL).
This incompletness, even if not severe, could bias the shown redshift
distribution of HBLs towards the lower part (since larger
redshifts are more difficult to measure).
From the radio, optical and 1 keV monochromatic fluxes we have calculated
the "'' luminosities in the corresponding bands.
The distributions of radio and optical luminosities (Figs. 4
and 5) show a continue variation in the three subclasses of
blazar: HBLs are the least powerful sources, and FSRQs are the most
luminous objects.
this is more pronounced in the radio than in the optical band.
The X-ray luminosities of HBLs and LBLs are very similar
(Fig. 6), while FSRQs are more luminous by a factor of 10.
Also the broad band spectral index
changes smoothly
between the subclasses of blazar (Fig. 7).
On average, it becomes steeper going from HBL to FSRQs. The optical to
X-ray broad band index distribution (Fig. 8) is broader
for HBL, with an average value smaller than for LBL and FSRQs.
The spectral index
(Fig. 9) is on average
the same for FSRQs and LBLs, and obviously flatter (by definition) for HBLs.
In Fig. 10 we show the sequence of average SEDs as published by F98, but including the [2-10 keV] averages spectral indices and fluxes. The latter have been constructed considering only the same samples considered by F98.
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Figure 10: The average SED of the blazars studied by Fossati et al. (1998), including the average values of the hard X-ray spectra. The thin solid lines are the spectra constructed following the parameterization proposed in this paper. |
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It can be seen that in general the 2-10 keV fluxes and spectral indices connect smoothly on the softer ROSAT data even if they are, on average, flatter than the latter. This is due to the emergence, in the hard X-ray band, of the inverse Compton component which is progressively more dominant as the luminosity increases.
For the average SED corresponding to the second lowest luminosity bin, there is a mismatch between the soft and hard X-ray data. By comparing the data of each source in common, we found that all 5 sources were brighter when observed by ASCA or BeppoSAX than at the time of the ROSAT observations. We therefore believe that the mismatch is due to the variable nature of the objects and the small number of sources in this luminosity bin.
The average spectral indices of the objects in common with F98 are listed
in Table 4, which also lists the average luminosities
at 4.47 keV (the logarithmic mid point between 2 and 10 keV).
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@4.47 keV | 2-10 keV | ||
<42 | 44.2 | 12 |
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42-43 | 44.5 | 5 |
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43-44 | 44.9 | 6 |
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44-45 | 45.8 | 6 |
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>45 | 47.0 | 11 |
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The continuous lines in Fig. 10 correspond to a simple parametric model derived by the one introduced by Fossati et al. (1998). We introduce minor modifications, adopted both to better represent our data at small luminosities and to follow a more physical scenario, in which the low power HBLs can be described by a pure synchrotron-self Compton model (see e.g. Ghisellini et al. 1998). We remind the reader here of the key assumptions of the F98 parametric model:
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(1) |
We modified the Fossati et al. (1998) description in the following way:
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(2) |
In order to see if the proposed parameterization of the average SED of blazars (constructed on the basis of a subsample of the sources in our catalogue) can account for the general properties of all the blazars in our catalogue, we have investigated the correlations between the X-ray spectral index (both hard and soft) with the radio and X-ray luminosities and with the broad band spectral indices. We have then considered the correlations between broad band indices. The results are shown in Figs. 12-18 (solid line), where we have superposed the relations predicted by the new parameterization.
In Figs. 11 and 12 we show the hard and soft
X-ray indices as a function of the radio and X-ray luminosity for all
sources, and compare these data with the model expectations.
Note that the latter have been constructed to describe the average
properties of blazars, whatever the scatter around it.
Bearing this in mind, we can consider the description of the model
quite satisfactorily.
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Figure 11: Soft and hard X-ray spectral index vs. the radio luminosity. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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Figure 12: Soft and hard X-ray spectral index vs. the X-ray luminosity. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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Figure 13: Soft and hard X-ray spectral index vs. the broad band radio to X-ray index. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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Figure 14: Soft and hard X-ray spectral index vs. the broad band radio to optical index. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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Figure 15: Soft and hard X-ray spectral index vs. the broad band optical to X-ray index. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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Figure 16: Radio to optical vs. optical to X-ray broad band indices. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
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In Fig. 13 we show the hard and soft X-ray indices as a
function of the broad band index
.
The model well describes the small
part (corresponding to HBLs),
but fails to describe the X-ray flattest sources with the steeper
value of
.
This is due to two reasons:
i) the slope of the power law of the
Compton component is assumed to be
,
so that flatter
indices are not possible;
ii) the ratio between the radio and the 1 keV Compton luminosity
is fixed for all sources.
This results in a saturated value of
,
occurring when the Compton component dominates at 1 keV
(i.e. for powerful sources).
In Figs. 14 and 15 we show
as
a function of
and
:
the average properties are
well described by the model.
In Fig. 16, we show the "classic''
-
diagram for the two subsamples of sources.
Note that the model well describes all the data but those sources
with the largest values of
,
corresponding to "transition''
sources between the LBLs and FSRQ.
Ba94: | Bade et al. (1994) | Gh99: | Ghisellini et al. (1999) | Pa95: | Padovani et al. (1995) |
Ba98: | Bade et al. (1998) | BSGh: | Ghisellini in BeppoSAX Archive | Pa99: | Padovani et al. (1999) |
Br85: | Bregman et al. (1985) | Gi98: | Giommi et al. (1998) | Pe96: | Perlman et al. (1996) |
Br94: | Brinkmann et al. (1994) | Gi99: | Giommi et al. (1999) | Sa94: | Sambruna et al. (1994) |
Br97: | Brinkmann et al. (1997) | Go95: | Ghosh et al. (1995) | Sa97a: | Sambruna et al. (1997) |
Ca97: | Cappi et al. (1997) | Gr96: | Greiner et al. (1996) | Sa97b: | Sambruna et al. (1997) |
Co95: | Comastri et al. (1995) | Kh81: | Khuer et al. (1981) | Sa99: | Sambruna et al. (1999) |
Co97: | Comastri et al. (1997) | Ku98: | Kubo et al. (1998) | Sb96: | Siebert et al. (1996) |
Cs00: | Costamante et al. (2000) | IT90: | Impey et al. (1990) | Sb99: | Siebert et al. (1999) |
El99: | Elvis et al. (1999) | IT91: | Impey et al. (1991) | Sn97: | Sing et al. (1997) |
Fa97: | Fabian et al. (1997) | La96: | Lamer et al. (1996) | Ta00: | Tagliaferri et al. (2000) |
Fa98: | Fabian et al. (1998) | Le97: | Leighly et al. (1997) | Tv99: | Tavecchio et al. (2000) |
Fo98: | Fossati et al. (1998) | LM99: | Laurent-Muehleisen et al. (1999) | VV93: | Veron-Cetty et al. (1993) |
Fo98b: | Fossati et al. (1998) | Ma98b: | Maraschi et al. (1998) | Xu99: | Xue et al. (1999) |
Ge96: | George et al. (1996) | BSMc: | Maccacaro in BeppoSAX Archive | Ya98: | Yaqoob et al. (1998) |
Gh93: | Ghisellini et al. (1993) | Na96: | Nass et al. (1996) | Wa99: | Watson et al. (1999) |
Gh98: | Ghisellini (1998) | NED: | NASA-IPAC Extragalactic Database | Wo98: | Wolter et al. (1998) |
Gh98b: | Ghisellini et al. (1998) | Or98: | Orr et al. (1998) | Wo90: | Worrall et al. (1990) |
![]() |
Figure 17: Optical to X-ray vs. radio to X-ray broad band indices. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
Open with DEXTER |
![]() |
Figure 18: Radio to optical vs. radio to X-ray broad band indices. Circles: HBL, Squares: LBL, Triangles: FSRQs. |
Open with DEXTER |
Figures 17, and 18: note that HBL are well
separated from the other classes of blazars.
Note also that the model, by construction,
has an asymptotic limit for
,
whose value therefore
saturates at
.
The large database of X-ray spectra of blazars we have collected has allowed to test the blazar sequence scheme aiming to unify the different behaviors of blazars on the basis of a single parameter, i.e. the bolometric observed luminosity. We have found that the proposed parameterization can account for the average properties of the blazars in our sample, even if the scatter around the predicted average quantities is sometimes large.
We confirm, on a statistical basis, that more powerful blazars emit the X-rays by the inverse Compton process, while in less powerful objects the dominant mechanism is synchrotron, and the transition is smooth, with LBL possibly showing both contributions.
The Fossati et al. (1998) parameterization scheme to reproduce the blazar SED is able to fit also our new hard X-ray data and the correlations between broad band indices of the sources in our sample. However, we propose to slightly change this parameterization especially for the low power objects (i.e. the HBLs), in line with the idea that HBLs are characterized by a pure synchrotron self-Compton spectrum, without extra contributions produced by non locally produced seed photons.
In this paper, and in Fossati et al. (1998), the power law relation between
the synchrotron peak frequency and the radio luminosity changes
slope at some critical radio power, of the order of 3-
erg s-1.
This agrees with the absence of broad emission lines in these objects.
It has still to be proven, however, if the non visibility of emission
lines in low power objects is due to a genuine lack of emitting clouds,
or is due to a weak ionizing continuum.
If the latter hypothesis is true, then we expect that the broad line
region indeed exists, but at smaller radii than in more powerful objects.
In this case, the lack of the external Compton component is not due
to the lack of external photons, but possibly to the fact that
the dissipation region in these sources is beyond the broad line region:
in this case the corresponding energy density of line photons
is seen, in the comoving frame of the blob, depressed by the square of
the bulk Lorentz factor.
Acknowledgements
We thank the anonimous referee for useful suggestions and Luigi Costamante for discussions. This research made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, Caltech, under contract with the National Aeronautics and Space Administration. We acknowledge finantial support from the MURST.
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
0014+813 | 3.366 | 0.551 | Ca97 | 0.910 | Ca97 | 0.350 | Ca97 | 1.890 | 1.700 | Ca97 | 3 | Ca97 | RO |
0.430 | Ca97 | 1.720 | 0.070 | Ca97 | AS | ||||||||
0016+731 | 1.781 | 1.750 | NED | 0.060 | NED | 0.050 | Sa97b | 1.430 | 1.100 | Sa97b | 3 | Gh93 | RO |
0038-020 | 1.178 | 0.581 | NED | 0.030 | NED | 0.100 | Wo90 | 1.400 | 1.100 | Wo90 | 3 | Wo90 | EI |
0045+214 | ... | 0.043 | NED | 0.310 | NED | 0.450 | Br97 | 2.160 | 0.250 | Br97 | 1 | Br97 | RO |
0048-097 | 0.200 | 2.743 | Fo98 | 1.750 | Fo98 | 0.420 | Pa98 | 1.730 | 0.380 | Pa98 | 2 | Gh93 | SA |
0.770 | Pa99 | 2.570 | 0.070 | Pa99 | RO | ||||||||
0109+182 | ... | 0.077 | NED | 1.440 | NED | 1.180 | LM99 | 1.940 | -- | LM99 | 1 | LM99 | RO |
0110+418 | 0.096 | 0.036 | NED | 0.390 | NED | 0.300 | Br97 | 2.110 | 0.700 | Br97 | 1 | Br97 | RO |
0112-017 | 1.365 | 1.200 | Kh81 | 0.230 | NED | 0.150 | Wo90 | 1.570 | 1.000 | Wo90 | 3 | Wo90 | EI |
0112+227 | ... | 0.257 | NED | 2.220 | NED | 0.160 | LM99 | 2.960 | -- | LM99 | 2 | LM99 | RO |
0113+2504 | ... | 0.031 | NED | 0.120 | NED | 0.710 | Br97 | 1.840 | 0.370 | Br97 | 1 | Br97 | RO |
0118-272 | 0.557 | 1.284 | Fo98 | 1.560 | Fo98 | 0.280 | Fo98 | 2.740 | 0.740 | Fo98 | 2 | NED | RO |
0120+340 | 0.272 | 0.034 | NED | 3.600 | NED | 2.420 | Cs00 | 1.960 | 0.020 | Cs00 | 1 | Br94 | SA |
6.260 | Br94 | 1.900 | 0.130 | Br94 | RO | ||||||||
0122+0903 | 0.339 | 0.001 | Pa95 | 0.050 | Pa95 | 0.030 | Pe96 | 1.620 | 0.500 | Pe96 | 1 | Pe96 | RO |
0133+388 | ... | 0.053 | NED | 4.590 | NED | 2.390 | LM99 | 2.160 | -- | LM99 | 1 | LM99 | RO |
0133+476 | 0.859 | 2.920 | Fo98 | 0.470 | Fo98 | 0.300 | Fo98 | 1.920 | 0.390 | Fo98 | 3 | Gh93 | RO |
0145+138 | 0.125 | 0.005 | Fo98 | 0.260 | Fo98 | 0.220 | BSMc | 2.320 | 0.160 | BSMc | 1 | BSMc | SA |
0152+017 | 0.080 | 0.058 | NED | 0.900 | NED | 0.470 | Br97 | 2.480 | 0.170 | Br97 | 1 | Br97 | RO |
0156+1032 | ... | 0.044 | NED | 0.950 | NED | 0.630 | Br97 | 1.730 | 0.630 | Br97 | 1 | Br97 | RO |
0158+003 | 0.299 | 0.011 | Fo98 | 0.230 | Fo98 | 1.210 | Fo98 | 2.460 | 0.270 | Fo98 | 1 | NED | RO |
1.030 | Wo98 | 2.270 | 0.180 | Wo98 | SA | ||||||||
0159+0835 | ... | 0.071 | NED | 0.120 | NED | 0.270 | Br97 | 2.360 | 0.480 | Br97 | 1 | Br97 | RO |
0202+149 | 0.405 | 2.400 | Co97 | 0.020 | Co97 | 0.060 | Co97 | 0.680 | 0.550 | Co97 | 3 | NED | RO |
0205+3509 | 0.318 | 0.004 | Pa95 | 0.180 | Pa95 | 0.150 | Pe96 | 2.710 | 0.220 | Pe96 | 1 | Pe96 | RO |
0.550 | Wa99 | 2.220 | 0.040 | Wa99 | AS | ||||||||
0208-512 | 1.003 | 3.311 | Fo98 | 0.590 | Fo98 | 0.610 | Fo98 | 2.040 | 0.040 | Fo98 | 3 | IT90 | RO |
1.200 | Ku98 | 1.660 | 0.090 | Ku98 | AS | ||||||||
0212+735 | 2.370 | 2.198 | Fo98 | 0.450 | Fo98 | 0.260 | Fo98 | 0.660 | 0.590 | Fo98 | 3 | Gh93 | RO |
0214+517 | 0.049 | 0.271 | NED | 1.550 | NED | 1.600 | LM99 | 2.040 | -- | LM99 | 1 | LM99 | RO |
0219+428 | 0.444 | 1.040 | Fo98 | 4.550 | Fo98 | 0.720 | Sa94 | 2.390 | 0.270 | Sa94 | 2 | Gh93 | EX |
1.560 | Fo98 | 2.600 | 0.170 | Fo98 | RO | ||||||||
3.460 | Wo90 | 2.620 | 0.850 | Wo90 | EI | ||||||||
0224+014 | ... | 0.009 | Br97 | 0.120 | NED | 3.360 | Br97 | 1.900 | 0.110 | Br97 | 1 | Br97 | RO |
0235+164 | 0.940 | 3.336 | Fo98 | 2.580 | Fo98 | 0.150 | Go95 | 1.750 | 0.730 | Go95 | 2 | Gh93 | EX |
0.270 | Ku98 | 1.820 | 0.130 | Ku98 | AS | ||||||||
1.150 | Fo98 | 2.590 | 0.860 | Fo98 | RO | ||||||||
1.510 | Wo90 | 3.250 | 2.100 | Wo90 | EI | ||||||||
0237-233 | 2.223 | 3.520 | Kh81 | 0.810 | NED | 0.310 | Wo90 | 1.620 | 1.250 | Wo90 | 3 | Wo90 | EI |
0.390 | Re97 | 1.680 | 0.060 | Re97 | AS | ||||||||
0250+172 | ... | 0.035 | NED | 2.060 | NED | 0.730 | LM99 | 2.020 | -- | LM99 | 1 | LM99 | RO |
0257+3429 | 0.245 | 0.010 | Pa95 | 0.140 | Pa95 | 0.020 | Pe96 | 2.670 | 0.320 | Pe96 | 1 | Pe96 | RO |
0301-243 | ... | 0.397 | NED | 0.980 | NED | 0.270 | La96 | 2.680 | 0.310 | La96 | 2 | La96 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
0316+090 | ... | 0.045 | NED | 1.160 | NED | 0.020 | LM99 | 4.280 | -- | LM99 | 2 | LM99 | RO |
0317+1834 | 0.190 | 0.017 | Pa95 | 0.210 | Pa95 | 0.170 | Pe96 | 2.320 | 0.240 | Pe96 | 1 | Wo98 | RO |
3.060 | Sa94 | 1.800 | 0.200 | Sa94 | EX | ||||||||
2.050 | Wo98 | 2.080 | 0.100 | Wo98 | SA | ||||||||
0323+022 | 0.147 | 0.042 | Fo98 | 0.900 | Fo98 | 6.810 | Wo90 | 2.160 | 0.230 | Wo90 | 1 | Wo90 | EI |
4.000 | Sa94 | 2.730 | 0.100 | Sa94 | EX | ||||||||
1.460 | BSMc | 2.410 | 0.120 | BSMc | SA | ||||||||
0.730 | Ku98 | 2.740 | 0.160 | Ku98 | AS | ||||||||
3.210 | Fo98 | 2.270 | 0.090 | Fo98 | RO | ||||||||
0331-365 | 0.308 | 0.009 | VV93 | 0.240 | NED | 0.340 | La96 | 2.200 | 0.490 | La96 | 1 | La96 | RO |
0332-403 | 1.445 | 2.600 | Ca97 | 0.140 | Ca97 | 0.140 | Ca97 | 1.600 | 0.120 | Ca97 | 3 | Ca97 | AS |
0333+321 | 1.258 | 2.500 | Ca97 | 0.520 | Gh93 | 1.600 | Ca97 | 1.530 | 0.920 | Ca97 | 3 | Gh93 | RO |
1.340 | Ku98 | 1.600 | 0.050 | Ku98 | AS | ||||||||
2.320 | Wo90 | 3.730 | 2.100 | Wo90 | EI | ||||||||
0.440 | Go95 | 1.360 | 0.260 | Go95 | EX | ||||||||
0347-121 | 0.188 | 0.009 | Fo98 | 0.190 | Fo98 | 2.050 | Wo98 | 2.170 | 0.100 | Wo98 | 1 | Wo98 | SA |
2.560 | Fo98 | 2.120 | 0.090 | Fo98 | RO | ||||||||
0350-3712 | 0.165 | 0.017 | VV93 | 0.590 | NED | 0.350 | La96 | 2.170 | 0.260 | La96 | 1 | La96 | RO |
0403-132 | 0.571 | 2.889 | Fo98 | 0.540 | Fo98 | 0.400 | Fo98 | 1.780 | 0.220 | Fo98 | 3 | IT90 | RO |
0.490 | Wo90 | 4.300 | 4.300 | Wo90 | EI | ||||||||
0405-123 | 0.574 | 1.960 | Fo98 | 5.170 | Fo98 | 0.090 | TW | 1.760 | 0.090 | TW | 3 | Sa97b | AS |
1.160 | Fo98 | 2.150 | 0.170 | Fo98 | RO | ||||||||
0406+121 | 1.020 | 0.746 | Na96 | 0.120 | NED | 0.050 | La96 | 1.790 | 0.450 | La96 | 2 | La96 | RO |
0414+009 | 0.287 | 0.070 | Fo98 | 0.850 | Fo98 | 5.220 | Wo98 | 2.540 | 0.100 | Wo98 | 1 | Wo98 | SA |
5.460 | Sa94 | 2.150 | 0.070 | Sa94 | EX | ||||||||
4.690 | Wo98 | 2.630 | 0.080 | Wo98 | RO | ||||||||
4.620 | Ku98 | 2.620 | 0.040 | Ku98 | AS | ||||||||
0419+1943 | 0.512 | 0.008 | Pa95 | 0.030 | Pa95 | 0.300 | Pe96 | 1.720 | 0.270 | Pe96 | 1 | Pe96 | RO |
0420-014 | 0.915 | 3.720 | Co97 | 0.340 | Co97 | 0.370 | Wo90 | 0.850 | 2.100 | Wo90 | 3 | Co97 | EI |
0.280 | TW | 1.860 | 0.180 | TW | AS | ||||||||
0426-380 | 1.030 | 1.416 | Fo98 | 0.230 | Fo98 | 0.090 | Fo98 | 3.200 | 1.250 | Fo98 | 2 | NED | RO |
0430+052 | 0.033 | 7.526 | NED | 3.910 | Gh93 | 3.240 | Go95 | 1.760 | 0.070 | Go95 | 3 | Gh93 | EX |
0438-436 | 2.852 | 6.189 | Fo98 | 0.410 | Fo98 | 0.190 | Ca97 | 1.420 | 0.060 | Ca97 | 3 | Ca97 | AS |
0.150 | Fo98 | 1.720 | 0.390 | Fo98 | RO | ||||||||
0454+844 | 0.112 | 1.430 | Fo98 | 1.050 | Fo98 | 0.030 | Fo98 | 1.870 | 0.590 | Fo98 | 2 | Gh93 | RO |
0502+675 | ... | 0.032 | Fo98 | 0.790 | Fo98 | 8.510 | Wo98 | 2.340 | 0.060 | Wo98 | 1 | Wo98 | SA |
7.740 | Br94 | 1.910 | 0.290 | Br94 | RO | ||||||||
0505+042 | ... | 0.121 | NED | 0.960 | NED | 0.730 | LM99 | 2.350 | -- | LM99 | 1 | LM99 | RO |
0507-040 | 0.304 | 0.027 | Fo98 | 0.110 | Fo98 | 3.000 | Sa94 | 1.770 | 0.260 | Sa94 | 1 | NED | EX |
0521-365 | 0.055 | 9.700 | Co97 | 2.380 | Co97 | 1.230 | Wo90 | 2.140 | 1.650 | Wo90 | 3 | Gh93 | EI |
2.120 | Co97 | 1.890 | 0.050 | Co97 | RO | ||||||||
1.780 | Sa94 | 1.850 | 0.330 | Sa94 | EX | ||||||||
0528+134 | 2.060 | 3.980 | Fo98 | 0.210 | Fo98 | 1.590 | Fo98 | 1.540 | 0.290 | Fo98 | 3 | Gh93 | RO |
1.480 | Ku98 | 1.580 | 0.050 | Ku98 | AS | ||||||||
0.310 | Gh98b | 1.480 | 0.040 | Gh98b | SA | ||||||||
0.220 | Br85 | 2.600 | -- | Br85 | EI | ||||||||
0537-441 | 0.896 | 4.755 | Fo98 | 1.570 | Fo98 | 0.400 | Sa94 | 1.300 | 0.600 | Sa94 | 2 | Gh93 | EX |
0.780 | Fo98 | 2.040 | 0.330 | Fo98 | RO | ||||||||
0.170 | Wo90 | 1.270 | 1.700 | Wo90 | EI | ||||||||
0537-286 | 3.104 | 0.990 | Ca97 | 0.040 | Ca97 | 0.180 | Ca97 | 1.360 | 0.060 | Ca97 | 3 | Ca97 | AS |
0.170 | Ca97 | 1.500 | 0.450 | Ca97 | RO | ||||||||
0548-322 | 0.069 | 0.170 | Fo98 | 1.370 | Fo98 | 8.220 | Ku98 | 1.960 | 0.020 | Ku98 | 1 | NED | AS |
9.590 | Fo98 | 1.950 | 0.050 | Fo98 | RO | ||||||||
6.460 | Gh99 | 2.040 | 0.070 | Gh99 | SA | ||||||||
7.710 | Sa94 | 1.980 | 0.060 | Sa94 | EX | ||||||||
9.960 | Wo90 | 1.690 | 0.120 | Wo90 | EI | ||||||||
0556-3838 | 0.034 | 0.068 | Pa95 | 0.530 | Pa95 | 2.200 | Ge96 | 2.520 | 0.100 | Ge96 | 1 | Ge96 | RO |
1.730 | Ge96 | 2.510 | 0.100 | Ge96 | AS | ||||||||
0607+7108 | 0.267 | 0.018 | Pa95 | 0.050 | Pa95 | 0.030 | Pe96 | 2.210 | 0.320 | Pe96 | 1 | Pe96 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
0615+820 | 0.710 | 1.000 | Kh81 | 0.470 | NED | 0.040 | Sa97b | 1.680 | 0.590 | Sa97b | 3 | Gh93 | RO |
0637-752 | 0.651 | 5.849 | Fo98 | 2.380 | Fo98 | 1.060 | Wo90 | 1.580 | 0.800 | Wo90 | 3 | Sa97b | EI |
3.760 | Fo98 | 1.450 | 0.480 | Fo98 | RO | ||||||||
0.490 | Ya98 | 1.640 | 0.070 | Ya98 | AS | ||||||||
0642+449 | 3.400 | 1.204 | NED | 0.150 | NED | 0.120 | Wo90 | 1.410 | 1.300 | Wo90 | 3 | Wo90 | EI |
0647+250 | ... | 0.077 | NED | 3.710 | NED | 6.010 | Br94 | 2.470 | 0.320 | Br94 | 1 | Br94 | RO |
0651+428 | 0.126 | 0.188 | NED | 0.770 | NED | 0.360 | LM99 | 3.590 | -- | LM99 | 1 | LM99 | RO |
0656+426 | 0.059 | 0.480 | NED | 0.890 | NED | 0.130 | LM99 | 3.180 | -- | LM99 | 2 | LM99 | RO |
0706+5913 | 0.125 | 0.080 | NED | 0.180 | NED | 1.830 | Br94 | 2.150 | 0.220 | Br94 | 1 | Br94 | RO |
0716+714 | 0.300 | 1.150 | Fo98 | 2.200 | Fo98 | 0.990 | Fo98 | 2.770 | 0.090 | Fo98 | 2 | Gh93 | RO |
0.370 | Ku98 | 2.070 | 0.120 | Ku98 | AS | ||||||||
0.500 | Wo90 | 5.750 | 4.400 | Wo90 | EI | ||||||||
0735+178 | 0.424 | 2.490 | Fo98 | 1.660 | Fo98 | 0.220 | Fo98 | 2.340 | 0.510 | Fo98 | 2 | Gh93 | RO |
0.290 | Wo90 | 1.710 | 0.400 | Wo90 | EI | ||||||||
0.140 | Ku98 | 1.760 | 0.200 | Ku98 | AS | ||||||||
0736+017 | 0.191 | 1.999 | Fo98 | 1.330 | Fo98 | 0.370 | Wo90 | 4.200 | 3.500 | Wo90 | 3 | IT90 | EI |
0.640 | Sa99 | 1.760 | 0.040 | Sa99 | AS | ||||||||
1.490 | Fo98 | 2.820 | 0.600 | Fo98 | RO | ||||||||
0737+746 | 0.315 | 0.024 | Fo98 | 0.650 | Fo98 | 0.880 | Wo98 | 2.530 | 0.250 | Wo98 | 1 | Wo98 | SA |
1.110 | Fo98 | 1.910 | -- | Fo98 | RO | ||||||||
0754+100 | 0.660 | 1.480 | Pa95 | 3.640 | Pa95 | 0.720 | Sa94 | 2.110 | 0.650 | Sa94 | 2 | Sa94 | EX |
0804+499 | 1.433 | 2.050 | Co97 | 0.390 | Co97 | 0.170 | Co97 | 1.560 | 0.360 | Co97 | 3 | Gh93 | RO |
0806+3504 | 0.082 | 0.180 | NED | 0.660 | NED | 0.740 | Ba98 | 2.870 | -- | Ba98 | 1 | Ba98 | RO |
0806+524 | 0.138 | 0.177 | NED | 3.150 | NED | 4.910 | Br94 | 2.930 | 0.160 | Br94 | 1 | Br94 | RO |
0806+595 | ... | 0.042 | NED | 1.410 | NED | 0.710 | LM99 | 1.500 | -- | LM99 | 1 | LM99 | RO |
0808+019 | ... | 0.670 | Pa95 | 0.480 | Pa95 | 0.380 | Wo90 | 1.920 | 1.400 | Wo90 | 2 | Wo90 | EI |
0812+026 | ... | 0.071 | NED | 6.250 | NED | 1.850 | Br97 | 2.160 | 0.110 | Br97 | 1 | Br97 | RO |
0814+425 | 0.258 | 3.500 | Fo98 | 0.150 | Fo98 | 0.050 | Fo98 | 1.160 | 0.780 | Fo98 | 2 | IT91 | RO |
0820+225 | 0.951 | 1.977 | Fo98 | 0.060 | Fo98 | 0.050 | Fo98 | 2.050 | 0.470 | Fo98 | 2 | NED | RO |
0828+493 | 0.548 | 1.158 | Fo98 | 0.130 | Fo98 | 0.040 | Fo98 | 1.680 | 0.630 | Fo98 | 2 | NED | RO |
0829+046 | 0.180 | 2.105 | Pa95 | 1.450 | Pa95 | 0.400 | Wo90 | 3.260 | 3.400 | Wo90 | 2 | Gh93 | EI |
0833+3300 | 0.671 | 0.004 | Ba98 | 0.020 | NED | 0.370 | Ba98 | 1.570 | -- | Ba98 | 1 | Ba98 | RO |
0836+710 | 2.170 | 2.590 | Fo98 | 1.060 | Fo98 | 1.270 | Ca97 | 1.320 | 0.030 | Ca97 | 3 | Gh93 | AS |
2.260 | Tv99 | 1.310 | 0.030 | Tv99 | SA | ||||||||
1.600 | Fo98 | 1.420 | 0.040 | Fo98 | RO | ||||||||
0847+115 | 0.198 | 0.022 | Br97 | 0.900 | NED | 1.980 | Br97 | 2.500 | 0.090 | Br97 | 1 | Br97 | RO |
0850+443 | ... | 0.075 | NED | 0.090 | NED | 0.190 | Br97 | 2.800 | 0.300 | Br97 | 1 | Br97 | RO |
0851+202 | 0.306 | 2.173 | Fo98 | 2.640 | Fo98 | 0.930 | Fo98 | 2.500 | 0.170 | Fo98 | 2 | Gh93 | RO |
2.240 | Sa94 | 2.370 | 0.100 | Sa94 | EX | ||||||||
0.370 | Pa99 | 1.710 | 0.240 | Pa99 | SA | ||||||||
0.730 | Ku98 | 1.620 | 0.050 | Ku98 | AS | ||||||||
0855+143 | 1.408 | 0.890 | Br85 | 0.030 | NED | 0.320 | Br85 | 2.000 | -- | Br85 | 3 | NED | EI |
0906+430 | 0.670 | 1.300 | Fo98 | 0.160 | Fo98 | 0.110 | Fo98 | 1.570 | 0.100 | Fo98 | 3 | Gh93 | RO |
0906+311 | 0.274 | 0.087 | NED | 2.050 | NED | 0.650 | Ba98 | 2.210 | -- | Ba98 | 1 | Ba98 | RO |
0912+297 | ... | 0.228 | Na96 | 1.000 | Pa95 | 1.060 | Pa99 | 2.250 | 0.140 | Pa99 | 1 | NED | SA |
0.510 | Wo90 | 1.760 | 0.700 | Wo90 | EI | ||||||||
0.580 | La96 | 2.310 | 0.240 | La96 | RO | ||||||||
0913+5251 | 0.190 | 0.067 | NED | 0.060 | NED | 0.590 | Ba98 | 2.180 | -- | Ba98 | 1 | Ba98 | RO |
0917+449 | 2.180 | 1.030 | Co97 | 0.070 | Co97 | 0.470 | Co97 | 1.390 | 0.100 | Co97 | 3 | NED | RO |
0922+7459 | 0.638 | 0.003 | Pa95 | 0.050 | Pa95 | 0.150 | Pe96 | 1.780 | 0.140 | Pe96 | 1 | Pe96 | RO |
0923+392 | 0.699 | 8.101 | Fo98 | 0.430 | Fo98 | 0.620 | Fo98 | 2.260 | 0.130 | Fo98 | 3 | Gh93 | RO |
0.370 | Wo90 | 1.360 | 0.190 | Wo90 | EI | ||||||||
0.880 | Sa99 | 1.880 | 0.050 | Sa99 | AS | ||||||||
0925+5026 | ... | 0.558 | NED | 1.520 | NED | 0.120 | Br97 | 2.300 | 0.390 | Br97 | 2 | Br97 | RO |
0927+500 | 0.188 | 0.015 | Na96 | 0.500 | NED | 4.000 | Ba98 | 1.880 | -- | Ba98 | 1 | Ba98 | RO |
0945+408 | 1.252 | 1.450 | NED | 0.380 | NED | 0.110 | Sa97b | 1.960 | 0.230 | Sa97b | 3 | IT91 | RO |
0950+445 | 0.207 | 0.003 | Fo98 | 0.120 | Fo98 | 0.290 | Fo98 | 2.760 | 0.250 | Fo98 | 1 | NED | RO |
0952+656 | ... | 0.027 | LM99 | 0.800 | NED | 0.150 | LM99 | 2.230 | -- | LM99 | 1 | LM99 | RO |
0954+556 | 0.909 | 2.169 | Fo98 | 0.430 | Fo98 | 0.100 | Fo98 | 2.170 | 0.140 | Fo98 | 3 | IT91 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
0954+658 | 0.367 | 1.589 | Fo98 | 1.720 | Fo98 | 0.160 | Fo98 | 1.960 | 1.310 | Fo98 | 2 | Gh93 | RO |
1008+4705 | 0.343 | 0.004 | Na96 | 0.090 | NED | 1.510 | Ba94 | 2.340 | 0.270 | Ba94 | 1 | Ba94 | RO |
1009+427 | 0.364 | 0.056 | NED | 0.960 | NED | 1.110 | Br97 | 1.840 | 0.090 | Br97 | 1 | Br97 | RO |
1011+496 | 0.200 | 0.286 | Fo98 | 1.620 | Fo98 | 2.150 | Fo98 | 2.490 | 0.080 | Fo98 | 1 | NED | RO |
1019+5139 | 0.141 | 0.002 | Pa95 | 0.210 | Pa95 | 0.790 | Pe96 | 1.520 | -- | Pe96 | 1 | Pe96 | RO |
1028+511 | 0.361 | 0.044 | Fo98 | 0.800 | Fo98 | 3.350 | TW | 2.530 | 0.050 | TW | 1 | NED | AS |
4.070 | TW | 2.490 | 0.040 | TW | AS | ||||||||
4.480 | TW | 2.590 | 0.050 | TW | AS | ||||||||
4.940 | BSMc | 2.410 | 0.040 | BSMc | SA | ||||||||
2.550 | Fo98 | 2.440 | 0.050 | Fo98 | RO | ||||||||
1034-293 | 0.312 | 1.510 | Kh81 | 1.110 | NED | 0.240 | Sa97b | 1.410 | 0.360 | Sa97b | 3 | Gh93 | RO |
1034-293 | 0.312 | 1.510 | NED | 0.930 | Gh93 | 0.160 | Wo90 | 0.660 | 1.800 | Wo90 | 2 | Gh93 | EI |
1037+571 | ... | 0.088 | NED | 0.770 | NED | 0.380 | Sb99 | 2.420 | 0.250 | Sb99 | 1 | Br97 | SA |
0.210 | Br97 | 2.500 | 0.190 | Br97 | RO | ||||||||
1039+811 | 1.260 | 1.140 | Kh81 | 0.980 | NED | 0.180 | Sa97b | 1.830 | 0.130 | Sa97b | 3 | Gh93 | RO |
1040+123 | 1.029 | 1.560 | Kh81 | 0.470 | Gh93 | 0.100 | Wo90 | 1.450 | 0.900 | Wo90 | 3 | Gh93 | EI |
1047+546 | ... | 0.004 | Br97 | 0.040 | NED | 0.070 | Br97 | 1.630 | 0.370 | Br97 | 1 | Br97 | RO |
1053+494 | 0.140 | 0.019 | LM99 | 0.430 | NED | 0.090 | LM99 | 2.620 | -- | LM99 | 1 | LM99 | RO |
1055+018 | 0.888 | 3.470 | Fo98 | 0.400 | Fo98 | 0.210 | Fo98 | 1.930 | 0.440 | Fo98 | 3 | NED | RO |
1055+567 | 0.144 | 0.260 | NED | 1.810 | NED | 0.470 | Br97 | 2.310 | 0.130 | Br97 | 1 | Br97 | RO |
2.190 | Sb99 | 2.760 | 0.080 | Sb99 | AS | ||||||||
1.080 | Sb99 | 2.780 | 0.250 | Sb99 | SA | ||||||||
1101+384 | 0.031 | 0.722 | Fo98 | 16.970 | Fo98 | 58.370 | Fo98b | 2.820 | 0.030 | Fo98b | 1 | Gh93 | SA |
23.850 | Ku98 | 2.970 | 0.020 | Ku98 | AS | ||||||||
36.100 | Fo98 | 3.100 | 0.080 | Fo98 | RO | ||||||||
1101-232 | 0.186 | 0.066 | Fo98 | 0.640 | Fo98 | 10.230 | Wo98 | 2.030 | 0.050 | Wo98 | 1 | Wo98 | SA |
11.200 | Wo98 | 2.430 | 0.080 | Wo98 | RO | ||||||||
19.630 | Wo90 | 2.310 | 0.180 | Wo90 | EI | ||||||||
17.740 | Sa94 | 2.500 | 0.170 | Sa94 | EX | ||||||||
1112+3452 | 0.212 | 0.004 | Ba98 | 0.060 | NED | 0.810 | Ba98 | 2.290 | -- | Ba98 | 1 | Ba98 | RO |
1114+2030 | ... | 0.074 | NED | 3.210 | NED | 7.310 | Br97 | 1.900 | 0.050 | Br97 | 1 | Br97 | RO |
1118+424 | 0.124 | 0.035 | Fo98 | 0.560 | Fo98 | 1.830 | BSMc | 2.620 | 0.070 | BSMc | 1 | BSMc | SA |
0.670 | LM99 | 2.300 | -- | LM99 | RO | ||||||||
1133+6753 | 0.135 | 0.048 | NED | 0.450 | NED | 3.230 | Br94 | 2.390 | 0.240 | Br94 | 1 | Br94 | RO |
1133+704 | 0.046 | 0.274 | Fo98 | 4.140 | Fo98 | 4.870 | Sa94 | 2.340 | 0.060 | Sa94 | 1 | NED | EX |
9.200 | Wo90 | 1.970 | 0.170 | Wo90 | EI | ||||||||
2.620 | Fo98 | 2.510 | 0.100 | Fo98 | RO | ||||||||
2.610 | Wo98 | 2.470 | 0.090 | Wo98 | SA | ||||||||
1144-379 | 1.048 | 2.779 | Fo98 | 0.800 | Fo98 | 0.140 | Pa98 | 1.700 | 0.030 | Pa98 | 2 | IT90 | SA |
0.410 | Pa99 | 2.540 | 0.190 | Pa99 | RO | ||||||||
1146-037 | 0.341 | 0.354 | NED | 0.630 | NED | 0.580 | Wo90 | 1.390 | 0.710 | Wo90 | 3 | Wo90 | EI |
1147+245 | 0.200 | 1.385 | Fo98 | 1.200 | Fo98 | 0.300 | Go95 | 1.960 | 0.620 | Go95 | 2 | Gh93 | EX |
0.040 | Fo98 | 2.180 | 0.790 | Fo98 | RO | ||||||||
1148+592 | ... | 0.134 | NED | 0.480 | NED | 0.270 | Br97 | 1.620 | 0.230 | Br97 | 1 | Br97 | RO |
1150+497 | 0.334 | 0.699 | NED | 0.560 | NED | 0.550 | Sa97b | 2.140 | 0.050 | Sa97b | 3 | Sa97b | RO |
0.630 | Sa99 | 1.770 | 0.050 | Sa99 | AS | ||||||||
1150+812 | 1.250 | 1.180 | Kh81 | 0.180 | NED | 0.090 | Sa97b | 1.450 | 0.310 | Sa97b | 3 | Gh93 | RO |
1156+295 | 0.729 | 1.543 | NED | 6.640 | NED | 0.440 | Sa94 | 2.300 | 0.470 | Sa94 | 3 | NED | EX |
1206+416 | ... | 0.515 | NED | 1.150 | NED | 0.100 | LM99 | 2.100 | -- | LM99 | 2 | LM99 | RO |
1207+3945 | 0.615 | 0.006 | Pa95 | 0.080 | Pa95 | 0.280 | Pe96 | 2.130 | 0.100 | Pe96 | 1 | Pe96 | RO |
1212+0748 | 0.130 | 0.094 | NED | 1.550 | NED | 0.620 | Br97 | 1.880 | 0.130 | Br97 | 1 | Br97 | RO |
1215+303 | 0.237 | 0.445 | Fo98 | 3.110 | Fo98 | 0.490 | Fo98 | 2.880 | 0.080 | Fo98 | 2 | Gh93 | RO |
0.590 | Wo90 | 2.420 | 0.900 | Wo90 | EI | ||||||||
1217+348 | ... | 0.355 | NED | 0.550 | NED | 0.100 | La96 | 1.980 | 0.710 | La96 | 2 | La96 | RO |
1217+023 | 0.240 | 0.698 | NED | 0.890 | NED | 0.780 | Wo90 | 1.700 | 0.350 | Wo90 | 3 | Wo90 | EI |
1218+304 | 0.130 | 0.056 | Fo98 | 1.390 | Fo98 | 7.510 | Sa94 | 2.460 | 0.140 | Sa94 | 1 | NED | EX |
10.050 | Fo98 | 2.220 | 0.030 | Fo98 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
1219+285 | 0.102 | 0.981 | Fo98 | 3.150 | Fo98 | 1.010 | Wo90 | 3.750 | 1.500 | Wo90 | 2 | Gh93 | EI |
0.400 | Fo98 | 2.240 | 0.160 | Fo98 | RO | ||||||||
1.790 | Ta00 | 1.510 | 0.270 | Ta00 | SA | ||||||||
1220+345 | ... | 0.355 | NED | 0.550 | NED | 0.060 | LM99 | 1.980 | -- | LM99 | 2 | LM99 | RO |
1221+2452 | 0.218 | 0.026 | Pa95 | 0.330 | Pa95 | 0.090 | Pe96 | 2.470 | 0.270 | Pe96 | 1 | Pe96 | RO |
1225+317 | 2.200 | 0.342 | NED | 1.630 | NED | 0.180 | Wo90 | 1.720 | 1.000 | Wo90 | 3 | Wo90 | EI |
1226+023 | 0.158 | 42.861 | Fo98 | 27.640 | Fo98 | 20.420 | Ku98 | 1.510 | 0.010 | Ku98 | 3 | Gh93 | AS |
12.270 | Fo98 | 1.890 | 0.050 | Fo98 | RO | ||||||||
7.600 | Go95 | 1.580 | 0.030 | Go95 | EX | ||||||||
11.150 | Wo90 | 1.340 | 0.170 | Wo90 | EI | ||||||||
1.960 | Or98 | 1.570 | 0.050 | Or98 | SA | ||||||||
1229+6430 | 0.164 | 0.042 | Pa95 | 0.630 | Pa95 | 1.210 | Pe96 | 1.990 | 0.150 | Pe96 | 1 | Pe96 | RO |
1230+2517 | 0.135 | 0.425 | NED | 2.220 | NED | 0.320 | Ba94 | 2.890 | 0.720 | Ba94 | 2 | Ba94 | RO |
1235+6315 | 0.297 | 0.007 | Pa95 | 0.130 | Pa95 | 0.060 | Pe96 | 2.910 | 0.080 | Pe96 | 1 | Pe96 | RO |
1237+3020 | 0.700 | 0.003 | Na96 | 0.010 | NED | 0.960 | Ba98 | 1.850 | -- | Ba98 | 1 | Ba98 | RO |
1239-143 | ... | 0.042 | NED | 0.290 | NED | 1.620 | Ba94 | 2.580 | 0.570 | Ba94 | 1 | Ba94 | RO |
1242+3440 | ... | 0.008 | Na96 | 0.060 | NED | 0.320 | Ba98 | 1.930 | -- | Ba98 | 1 | Ba98 | RO |
1246+586 | ... | 0.414 | NED | 9.450 | NED | 0.500 | Ba98 | 2.420 | -- | Ba98 | 2 | Ba98 | RO |
1252+119 | 0.871 | 1.140 | Kh81 | 0.800 | NED | 0.140 | Wo90 | 1.070 | 1.300 | Wo90 | 3 | Wo90 | EI |
1253-055 | 0.536 | 14.950 | Fo98 | 1.660 | Fo98 | 1.340 | Fo98 | 1.830 | 0.040 | Fo98 | 3 | Gh93 | RO |
0.850 | Ma98 | 1.650 | 0.030 | Ma98 | SA | ||||||||
1.500 | Ku98 | 1.650 | 0.060 | Ku98 | AS | ||||||||
0.630 | Wo90 | 1.550 | 0.270 | Wo90 | EI | ||||||||
1255+244 | 0.141 | 0.077 | Pa95 | 2.510 | Pa95 | 1.450 | Gr96 | 2.400 | 0.200 | Gr96 | 1 | Gr96 | RO |
1303+5056 | 0.688 | 0.001 | Ba98 | 0.030 | NED | 0.830 | Ba98 | 1.940 | -- | Ba98 | 1 | Ba98 | RO |
1308+326 | 0.997 | 1.832 | Fo98 | 1.580 | Fo98 | 0.110 | TW | 1.990 | 0.420 | TW | 2 | Gh93 | AS |
0.090 | TW | 1.740 | 0.250 | TW | AS | ||||||||
0.150 | Co95 | 1.950 | 0.100 | Co95 | RO | ||||||||
1312-423 | 0.105 | 0.019 | Pa95 | 0.830 | Pa95 | 1.520 | Wo98 | 2.210 | 0.200 | Wo98 | 1 | Wo98 | SA |
1324+5739 | 0.115 | 0.042 | NED | 0.950 | NED | 0.330 | Ba98 | 2.040 | -- | Ba98 | 1 | Ba98 | RO |
1326+2933 | 0.431 | 0.006 | Na96 | 0.050 | NED | 0.430 | Ba98 | 2.110 | -- | Ba98 | 1 | Ba98 | RO |
1332-295 | 0.513 | 0.011 | Fo98 | 0.090 | Fo98 | 0.340 | Fo98 | 2.140 | 0.210 | Fo98 | 1 | NED | RO |
1334-127 | 0.539 | 2.250 | Kh81 | 0.600 | NED | 0.450 | Sa97b | 1.630 | 0.160 | Sa97b | 3 | Gh93 | RO |
1353+5601 | 0.370 | 0.012 | Na96 | 0.110 | NED | 0.390 | Ba98 | 2.010 | -- | Ba98 | 1 | Ba98 | RO |
1400+162 | 0.244 | 0.528 | Pa95 | 0.510 | NED | 0.140 | Wo90 | 1.550 | 1.100 | Wo90 | 2 | Gh93 | EI |
1402+042 | 0.344 | 0.020 | Fo98 | 0.630 | Fo98 | 1.200 | Sa94 | 2.320 | 0.110 | Sa94 | 1 | NED | EX |
0.680 | Fo98 | 2.850 | 0.170 | Fo98 | RO | ||||||||
1405+6554 | 0.364 | 0.015 | Ba98 | 0.070 | NED | 0.310 | Ba98 | 2.260 | -- | Ba98 | 1 | Ba98 | RO |
1407+5954 | 0.495 | 0.017 | Pa95 | 0.050 | Pa95 | 0.040 | Pe96 | 2.740 | 0.140 | Pe96 | 1 | Pe96 | RO |
1410+6100 | 0.384 | 0.033 | Ba98 | 0.040 | NED | 0.410 | Ba98 | 1.900 | -- | Ba98 | 1 | Ba98 | RO |
1413+135 | 0.247 | 1.200 | Pa95 | 0.040 | NED | 0.050 | Wo90 | 0.600 | 1.500 | Wo90 | 2 | Wo90 | EI |
1415+485 | ... | 0.035 | NED | 0.720 | NED | 0.040 | LM99 | 2.400 | -- | LM99 | 2 | LM99 | RO |
1415+259 | 0.237 | 0.054 | Pa95 | 1.450 | Pa95 | 4.280 | Sa94 | 2.370 | 0.050 | Sa94 | 1 | NED | EX |
2.870 | Br94 | 2.120 | 0.320 | Br94 | RO | ||||||||
1418+546 | 0.152 | 1.610 | Fo98 | 1.910 | Fo98 | 0.210 | Wo90 | 1.480 | 0.650 | Wo90 | 2 | Wo90 | EI |
0.300 | Fo98 | 2.140 | 0.190 | Fo98 | RO | ||||||||
1421+582 | 0.638 | 0.050 | Br94 | 0.120 | NED | 2.950 | Br94 | 1.980 | 0.070 | Br94 | 1 | Br94 | RO |
1424+240 | ... | 0.316 | NED | 1.090 | NED | 1.470 | Sb99 | 2.780 | 0.040 | Sb99 | 1 | Gh93 | AS |
1.260 | La96 | 3.180 | 0.160 | La96 | RO | ||||||||
1426+428 | 0.129 | 0.030 | NED | 1.050 | Sa97 | 13.420 | Sa94 | 2.100 | 0.070 | Sa94 | 1 | NED | EX |
6.500 | Sa97a | 2.150 | 0.040 | Sa97a | RO | ||||||||
5.940 | Ku98 | 2.170 | 0.030 | Ku98 | AS | ||||||||
4.640 | Gh99 | 1.920 | 0.040 | Gh99 | SA | ||||||||
1427+541 | 0.105 | 0.024 | LM99 | 0.470 | LM99 | 0.110 | LM99 | 1.860 | -- | LM99 | 1 | LM99 | RO |
1428+422 | 4.715 | 0.337 | Fa97 | 0.020 | Fa98 | 0.210 | Fa98 | 1.290 | 0.050 | Fa98 | 3 | Fa98 | AS |
1437+398 | ... | 0.063 | NED | 1.520 | NED | 1.190 | LM99 | 2.550 | -- | LM99 | 1 | LM99 | RO |
1437+5639 | ... | 0.011 | Na96 | 0.120 | NED | 0.300 | Ba98 | 2.220 | -- | Ba98 | 1 | Ba98 | RO |
1440+122 | 0.162 | 0.050 | NED | 0.570 | NED | 1.220 | LM99 | 2.200 | -- | LM99 | 1 | LM99 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
1442+101 | 3.530 | 1.260 | Kh81 | 0.280 | NED | 0.120 | Wo90 | 2.000 | 1.300 | Wo90 | 3 | Wo90 | EI |
1443+6349 | 0.299 | 0.012 | Pa95 | 0.050 | Pa95 | 0.190 | Pe96 | 2.100 | 0.290 | Pe96 | 1 | Pe96 | RO |
1448+361 | ... | 0.029 | LM99 | 1.140 | NED | 0.500 | LM99 | 2.600 | -- | LM99 | 1 | LM99 | RO |
1456+5048 | 0.480 | 0.274 | NED | 0.070 | NED | 2.560 | Ba98 | 2.060 | -- | Ba98 | 1 | Ba98 | RO |
1458+2249 | 0.235 | 0.030 | Pa95 | 0.690 | Pa95 | 0.110 | Pe96 | 3.310 | 0.200 | Pe96 | 1 | Pe96 | RO |
1458+4832 | 0.539 | 0.003 | Ba98 | 0.030 | NED | 0.800 | Ba98 | 1.900 | -- | Ba98 | 1 | Ba98 | RO |
1509+559 | ... | 0.042 | NED | 0.950 | NED | 0.050 | LM99 | 2.990 | -- | LM99 | 1 | LM99 | RO |
1510-089 | 0.361 | 3.080 | Fo98 | 1.090 | Fo98 | 0.750 | Sn97 | 1.310 | 0.070 | Sn97 | 3 | Gh93 | AS |
0.500 | Wo90 | 0.800 | 1.350 | Wo90 | EI | ||||||||
0.830 | Sa94 | 1.380 | 0.280 | Sa94 | EX | ||||||||
0.490 | Tv99 | 1.350 | 0.070 | Tv99 | SA | ||||||||
0.740 | Fo98 | 1.900 | 0.160 | Fo98 | RO | ||||||||
1514-241 | 0.049 | 2.000 | Pa95 | 2.900 | NED | 0.620 | Wo90 | 2.360 | 1.950 | Wo90 | 2 | Wo90 | EI |
1516+293 | 0.130 | 0.034 | LM99 | 1.320 | NED | 0.190 | LM99 | 2.320 | -- | LM99 | 1 | LM99 | RO |
1517+656 | ... | 0.038 | Fo98 | 1.530 | Fo98 | 7.420 | Wo98 | 2.290 | 0.100 | Wo98 | 1 | Wo98 | RO |
4.990 | Wo98 | 2.440 | 0.090 | Wo98 | SA | ||||||||
1519-273 | 0.200 | 3.255 | Fo98 | 0.200 | Fo98 | 0.390 | Pa99 | 2.030 | 0.430 | Pa99 | 2 | Gh93 | RO |
0.320 | Pa99 | 1.440 | 0.970 | Pa99 | SA | ||||||||
1532+302 | 0.064 | 0.055 | NED | 2.600 | NED | 0.760 | LM99 | 2.000 | -- | LM99 | 1 | LM99 | RO |
1533+342 | ... | 0.028 | NED | 0.560 | NED | 0.400 | LM99 | 2.600 | -- | LM99 | 1 | LM99 | RO |
1533+535 | 0.890 | 0.030 | Ba98 | 0.350 | NED | 2.390 | Ba98 | 1.940 | -- | Ba98 | 1 | Ba98 | RO |
1534+0148 | 0.312 | 0.034 | Pa95 | 0.120 | Pa95 | 0.420 | Pe96 | 1.890 | 0.180 | Pe96 | 1 | Pe96 | RO |
1534+372 | 0.143 | 0.030 | NED | 0.880 | NED | 0.030 | LM99 | 2.840 | -- | LM99 | 2 | LM99 | RO |
1538+149 | 0.605 | 2.648 | Fo98 | 0.440 | Fo98 | 0.090 | Fo98 | 2.050 | 0.900 | Fo98 | 2 | Gh93 | RO |
0.280 | Wo90 | 2.130 | 1.100 | Wo90 | EI | ||||||||
1541+0507 | ... | 0.056 | NED | 0.120 | NED | 0.260 | Br97 | 1.740 | 0.660 | Br97 | 1 | Br97 | RO |
1542+614 | ... | 0.131 | NED | 0.960 | NED | 0.120 | LM99 | 2.500 | -- | LM99 | 2 | LM99 | RO |
1546+027 | 0.413 | 1.450 | Kh81 | 0.230 | NED | 0.840 | Wo90 | 2.180 | 2.250 | Wo90 | 3 | Wo90 | EI |
1548+114 | 0.436 | 0.410 | VV93 | 0.500 | Gh93 | 0.320 | Wo90 | 1.350 | 1.100 | Wo90 | 3 | Gh93 | EI |
1552+2020 | 0.222 | 0.038 | Pa95 | 0.300 | Pa95 | 1.570 | Pe96 | 1.790 | 0.140 | Pe96 | 1 | Pe96 | RO |
1553+113 | 0.360 | 0.636 | Pa95 | 4.800 | Pa95 | 13.420 | BSMc | 2.850 | 0.040 | BSMc | 1 | NED | SA |
14.860 | TW | 2.470 | 0.180 | TW | AS | ||||||||
7.660 | Br94 | 2.490 | 0.250 | Br94 | RO | ||||||||
1602+308 | ... | 0.013 | Br97 | 0.230 | NED | 0.160 | Br97 | 2.560 | 0.890 | Br97 | 1 | Br97 | RO |
1611+343 | 1.404 | 2.671 | Fo98 | 0.350 | Fo98 | 0.240 | Fo98 | 1.760 | 0.060 | Fo98 | 3 | IT90 | RO |
1614+051 | 3.197 | 0.850 | Ca97 | 0.060 | Ca97 | 0.030 | Ca97 | 1.600 | -- | Ca97 | 3 | Ca97 | AS |
1626+352 | 0.500 | 0.014 | LM99 | 0.140 | LM99 | 0.160 | LM99 | 1.890 | -- | LM99 | 1 | LM99 | RO |
1631+4217 | 0.468 | 0.006 | Na96 | 0.040 | NED | 0.860 | Ba98 | 1.910 | -- | Ba98 | 1 | Ba98 | RO |
1633+382 | 1.814 | 2.929 | Fo98 | 0.230 | Fo98 | 0.420 | Fo98 | 1.530 | 0.080 | Fo98 | 3 | Gh93 | RO |
0.250 | Ku98 | 1.510 | 0.320 | Ku98 | AS | ||||||||
1641+399 | 0.594 | 7.821 | Fo98 | 0.890 | Fo98 | 0.700 | Wo90 | 1.430 | 0.350 | Wo90 | 3 | Gh93 | EI |
0.980 | Fo98 | 1.850 | 0.230 | Fo98 | RO | ||||||||
1642+458 | 0.223 | 0.111 | NED | 0.350 | NED | 0.260 | Ba98 | 2.360 | -- | Ba98 | 1 | Ba98 | RO |
1652+398 | 0.034 | 1.443 | Fo98 | 10.970 | Fo98 | 46.420 | Gh98 | 1.800 | 0.020 | Gh98 | 1 | Gh93 | SA |
23.440 | Ku98 | 2.220 | 0.020 | Ku98 | AS | ||||||||
13.400 | Wo90 | 2.090 | 0.170 | Wo90 | EI | ||||||||
8.300 | Fo98 | 2.630 | 0.050 | Fo98 | RO | ||||||||
12.900 | Sa94 | 2.500 | 0.100 | Sa94 | EX | ||||||||
1652+403 | ... | 0.011 | LM99 | 1.060 | NED | 0.030 | LM99 | 2.800 | -- | LM99 | 1 | LM99 | RO |
1704+607 | 0.280 | 0.002 | VV93 | 0.070 | NED | 0.160 | La96 | 2.360 | 0.350 | La96 | 1 | La96 | RO |
1704+716 | ... | 0.041 | NED | 0.480 | NED | 0.160 | LM99 | 3.100 | -- | LM99 | 1 | LM99 | RO |
1717+178 | ... | 0.940 | Pa95 | 0.140 | NED | 0.480 | Wo90 | 2.540 | 2.100 | Wo90 | 2 | Wo90 | EI |
1721+343 | 0.206 | 0.468 | NED | 0.980 | NED | 1.990 | Wo90 | 1.500 | 0.350 | Wo90 | 3 | Wo90 | EI |
1722+119 | 0.018 | 0.094 | Pa95 | 1.740 | Pa95 | 3.600 | Sa94 | 2.650 | 0.250 | Sa94 | 1 | NED | EX |
1727+502 | 0.055 | 0.159 | Fo98 | 1.700 | Fo98 | 3.630 | Fo98 | 2.390 | 0.080 | Fo98 | 1 | Gh93 | RO |
3.720 | Sa94 | 2.820 | 0.210 | Sa94 | EX | ||||||||
1732+389 | 0.976 | 0.845 | NED | 0.110 | NED | 0.050 | Sa97b | 1.580 | 0.380 | Sa97b | 3 | Sa97b | RO |
1741+196 | 0.084 | 0.339 | NED | 0.900 | NED | 1.610 | Sb99 | 2.100 | 0.080 | Sb99 | 1 | Br97 | SA |
1.280 | Br97 | 1.980 | 0.180 | Br97 | RO |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
1742+597 | ... | 0.089 | NED | 1.370 | NED | 0.030 | LM99 | 2.960 | -- | LM99 | 2 | LM99 | RO |
1746+470 | 1.484 | 0.631 | NED | 0.010 | NED | 0.020 | LM99 | 3.080 | -- | LM99 | 2 | LM99 | RO |
1747+433 | ... | 0.360 | NED | 0.640 | NED | 0.050 | LM99 | 2.320 | -- | LM99 | 2 | LM99 | RO |
1748+470 | 0.160 | 0.010 | LM99 | 0.110 | LM99 | 0.540 | LM99 | 1.940 | -- | LM99 | 1 | LM99 | RO |
1749+096 | 0.322 | 1.973 | Fo98 | 1.130 | Fo98 | 0.150 | Fo98 | 1.450 | 1.430 | Fo98 | 2 | Gh93 | RO |
0.760 | Sa97 | 1.890 | 0.080 | Sa97 | AS | ||||||||
0.370 | Wo90 | 1.150 | 1.100 | Wo90 | EI | ||||||||
1749+701 | 0.770 | 2.113 | Fo98 | 0.960 | Fo98 | 0.150 | Fo98 | 2.440 | 0.710 | Fo98 | 2 | Gh93 | RO |
1755+552 | ... | 0.007 | Br97 | 0.490 | NED | 0.940 | Br97 | 2.640 | 0.190 | Br97 | 1 | Br97 | RO |
1757+7034 | 0.407 | 0.007 | Pa95 | 0.170 | Pa95 | 0.470 | Pe96 | 2.120 | 0.130 | Pe96 | 1 | Pe96 | RO |
1803+784 | 0.684 | 3.016 | Fo98 | 0.610 | Fo98 | 0.240 | Pa99 | 1.450 | 0.130 | Pa99 | 2 | Gh93 | SA |
0.260 | Fo98 | 2.420 | 0.450 | Fo98 | RO | ||||||||
0.220 | Wo90 | 1.460 | 1.000 | Wo90 | EI | ||||||||
1807+698 | 0.051 | 1.713 | Fo98 | 5.180 | Fo98 | 0.300 | Pa99 | 1.740 | 0.240 | Pa99 | 2 | Gh93 | SA |
0.520 | TW | 1.750 | 0.060 | TW | AS | ||||||||
0.400 | Wo90 | 1.660 | 0.420 | Wo90 | EI | ||||||||
0.350 | Co95 | 2.220 | 0.110 | Co95 | RO | ||||||||
2.570 | Sa94 | 1.950 | 0.460 | Sa94 | EX | ||||||||
1808+468 | ... | 0.056 | NED | 0.450 | NED | 0.060 | LM99 | 2.700 | -- | LM99 | 2 | LM99 | RO |
1811+442 | ... | 0.030 | NED | 0.350 | NED | 0.070 | LM99 | 2.180 | -- | LM99 | 1 | LM99 | RO |
1823+568 | 0.664 | 1.905 | Fo98 | 0.180 | Fo98 | 0.270 | Pa99 | 1.960 | 0.350 | Pa99 | 2 | IT91 | SA |
0.410 | Pa99 | 1.150 | 0.190 | Pa99 | RO | ||||||||
1829+540 | ... | 0.024 | NED | 0.770 | NED | 0.060 | LM99 | 3.310 | -- | LM99 | 1 | LM99 | RO |
1838+480 | ... | 0.032 | NED | 0.900 | NED | 0.100 | LM99 | 3.100 | -- | LM99 | 1 | LM99 | RO |
1841+591 | 0.530 | 0.006 | LM99 | 0.220 | NED | 0.010 | LM99 | 3.540 | -- | LM99 | 2 | LM99 | RO |
1845+797 | 0.056 | 4.450 | Kh81 | 8.060 | NED | 3.630 | Sa94 | 1.740 | 0.200 | Sa94 | 3 | Gh93 | EX |
5.470 | Le97 | 1.820 | 0.030 | Le97 | AS | ||||||||
1848+427 | ... | 0.007 | Br97 | 0.200 | NED | 1.810 | Br94 | 2.170 | 0.220 | Br94 | 1 | Br94 | RO |
1921-293 | 0.352 | 12.696 | NED | 0.840 | NED | 0.770 | Wo90 | 1.570 | 1.300 | Wo90 | 3 | Gh93 | EI |
0.380 | Go95 | 1.670 | 0.270 | Go95 | EX | ||||||||
1.060 | Sa97b | 1.890 | 0.050 | Sa97b | RO | ||||||||
1928+738 | 0.360 | 3.339 | Fo98 | 1.110 | Fo98 | 0.520 | Go95 | 2.250 | 0.480 | Go95 | 3 | Gh93 | EX |
1.470 | Fo98 | 2.330 | 0.190 | Fo98 | RO | ||||||||
1959+650 | 0.048 | 0.251 | Fo98 | 17.490 | Fo98 | 9.200 | BSMc | 2.680 | 0.050 | BSMc | 1 | BSMc | SA |
2005-489 | 0.071 | 1.252 | Fo98 | 12.470 | Fo98 | 5.400 | Sa94 | 3.200 | 0.700 | Sa94 | 1 | Co97 | EX |
25.380 | Pa98 | 2.320 | 0.040 | Pa98 | SA | ||||||||
5.000 | Fo98 | 2.940 | 0.060 | Fo98 | RO | ||||||||
2007+777 | 0.342 | 1.364 | Fo98 | 0.770 | Fo98 | 0.360 | Wo90 | 5.110 | 4.800 | Wo90 | 2 | Gh93 | EI |
0.170 | Fo98 | 1.750 | 0.560 | Fo98 | RO | ||||||||
2032+107 | 0.601 | 0.770 | Pa95 | 1.000 | Pa95 | 1.220 | Wo90 | 2.430 | 1.400 | Wo90 | 2 | Wo90 | EI |
2039+523 | ... | 0.025 | NED | 1.420 | NED | 0.230 | Br97 | 2.800 | 0.890 | Br97 | 1 | Br97 | RO |
2126-158 | 3.268 | 1.240 | Ca97 | 0.580 | Ca97 | 0.720 | Ca97 | 1.530 | 0.300 | Ca97 | 3 | Ca97 | RO |
0.860 | Ca97 | 1.680 | 0.090 | Ca97 | AS | ||||||||
0.710 | Wo90 | 3.180 | 2.100 | Wo90 | EI | ||||||||
2131-021 | 0.557 | 2.390 | Fo98 | 0.130 | Fo98 | 0.050 | Fo98 | 2.050 | 0.460 | Fo98 | 2 | IT90 | RO |
2134+004 | 1.936 | 12.249 | Fo98 | 0.720 | Fo98 | 0.260 | Fo98 | 1.820 | 0.420 | Fo98 | 3 | Gh93 | RO |
2136-428 | ... | 0.108 | NED | 0.390 | NED | 0.120 | La96 | 3.200 | 0.410 | La96 | 2 | La96 | RO |
2143+0704 | 0.237 | 0.050 | Pa95 | 0.230 | Pa95 | 0.120 | Pe96 | 2.910 | 0.320 | Pe96 | 1 | Pe96 | RO |
2149-306 | 2.345 | 1.150 | NED | 0.710 | NED | 0.880 | Sb96 | 2.040 | 0.940 | Sb96 | 3 | Ca97 | RO |
0.760 | El99 | 1.370 | 0.030 | El99 | SA | ||||||||
1.270 | Ca97 | 1.540 | 0.050 | Ca97 | AS | ||||||||
2155-152 | 0.672 | 2.150 | NED | 0.420 | NED | 0.220 | Sa97b | 2.170 | 0.100 | Sa97b | 3 | Sa97b | RO |
2155-304 | 0.117 | 0.310 | Fo98 | 18.950 | Fo98 | 41.050 | Sa94 | 2.630 | 0.080 | Sa94 | 1 | Co97 | EX |
5.980 | Wo90 | 2.610 | 0.180 | Wo90 | EI | ||||||||
44.900 | Ku98 | 2.620 | 0.010 | Ku98 | AS | ||||||||
43.900 | Fo98 | 2.340 | 0.030 | Fo98 | RO | ||||||||
73.550 | Gi98 | 2.880 | 0.050 | Gi98 | SA |
IAU Name | z | ![]() |
Ref. | ![]() |
Ref. | ![]() |
Ref. | ![]() |
err | Ref. | Type | Ref. | Sat |
(Jy) | (mJy) | (![]() |
|||||||||||
2200+420 | 0.069 | 4.857 | Fo98 | 5.450 | Fo98 | 2.200 | Pa99 | 1.830 | 0.080 | Pa99 | 2 | Gh93 | SA |
4.320 | Wo90 | 2.340 | 1.900 | Wo90 | EI | ||||||||
2.220 | Sa97 | 1.960 | 0.040 | Sa97 | AS | ||||||||
0.880 | Fo98 | 1.920 | 0.470 | Fo98 | RO | ||||||||
2201+171 | 1.080 | 0.843 | NED | 0.120 | NED | 0.080 | Wo90 | 1.410 | 0.800 | Wo90 | 3 | Wo90 | EI |
2208-137 | 0.392 | 0.580 | NED | 0.660 | NED | 0.960 | Sa94 | 1.400 | 0.900 | Sa94 | 3 | Sa94 | EX |
2223-052 | 1.404 | 4.519 | Fo98 | 1.020 | Fo98 | 1.460 | Wo90 | 1.340 | 0.720 | Wo90 | 3 | Gh93 | EI |
0.270 | Fo98 | 2.090 | 0.230 | Fo98 | RO | ||||||||
0.220 | BSGh | 1.730 | 0.210 | BSGh | SA | ||||||||
2230+114 | 1.037 | 3.689 | Fo98 | 0.690 | Fo98 | 0.420 | Ku98 | 1.580 | 0.120 | Ku98 | 3 | Ku98 | AS |
0.730 | Tv99 | 1.510 | 0.040 | Tv99 | SA | ||||||||
2240-260 | 0.774 | 1.203 | Fo98 | 0.260 | Fo98 | 0.070 | Fo98 | 1.790 | 0.400 | Fo98 | 2 | NED | RO |
2243+203 | ... | 0.120 | NED | 2.900 | NED | 0.060 | LM99 | 2.680 | -- | LM99 | 2 | LM99 | RO |
2247+381 | 0.119 | 0.119 | NED | 6.840 | NED | 0.600 | LM99 | 2.510 | -- | LM99 | 1 | LM99 | RO |
2251+158 | 0.859 | 8.759 | Fo98 | 1.020 | Fo98 | 1.310 | Wo90 | 1.830 | 1.750 | Wo90 | 3 | IT90 | EI |
1.370 | Fo98 | 1.620 | 0.040 | Fo98 | RO | ||||||||
2254+024 | 2.090 | 0.426 | NED | 0.230 | NED | 0.150 | Wo90 | 3.870 | 3.300 | Wo90 | 3 | Wo90 | EI |
2254+074 | 0.190 | 1.216 | Fo98 | 0.600 | Fo98 | 0.080 | Wo90 | 0.950 | 2.100 | Wo90 | 2 | Gh93 | EI |
0.090 | Fo98 | 2.890 | 0.610 | Fo98 | RO | ||||||||
2316-423 | 0.055 | 0.540 | Pa95 | 5.770 | Pa95 | 0.100 | Xu99 | 2.600 | 0.300 | Xu99 | 2 | Xu99 | AS |
0.360 | Xu99 | 2.000 | 0.200 | Xu99 | RO | ||||||||
2319+161 | ... | 0.024 | LM99 | 0.720 | NED | 0.360 | LM99 | 2.200 | -- | LM99 | 1 | LM99 | RO |
2322+346 | 0.098 | 0.076 | NED | 11.890 | NED | 0.420 | LM99 | 1.800 | -- | LM99 | 1 | LM99 | RO |
2344+514 | 0.044 | 0.215 | Co97 | 2.370 | Co97 | 4.170 | TW | 2.310 | 0.070 | TW | 1 | Co97 | AS |
5.180 | TW | 2.390 | 0.080 | TW | AS | ||||||||
5.260 | TW | 2.130 | 0.030 | TW | AS | ||||||||
3.400 | Gi99 | 2.310 | 0.050 | Gi99 | SA | ||||||||
6.870 | Gi99 | 1.770 | 0.040 | Gi99 | SA | ||||||||
2356-309 | 0.165 | 0.029 | NED | 0.700 | NED | 5.780 | Cs00 | 2.100 | 0.050 | Cs00 | 1 | NED | SA |