A. Caccianiga 1 - P. Severgnini1 - V. Braito1,2 - R. Della Ceca1 - T. Maccacaro1 - A. Wolter1 - X. Barcons3 - F. J. Carrera3 - I. Lehmann4 - M. J. Page5 - R. Saxton6 - N. A. Webb7
1 - INAF - Osservatorio Astronomico di Brera, via Brera 28, 20121 Milano, Italy
2 - Dipartimento di Astronomia, Università di Padova, Vicolo dell'Osservatorio 2, 35122 Padova, Italy
3 - Instituto de Fisica de Cantabria (CSIC-UC), Avenida de los Castros, 39005 Santander, Spain
4 - Astrophysikalisches Institut Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany
5 - Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, UK
6 - X-ray Astronomy Group, Department of Physics and Astronomy, Leicester University, Leicester LE1 7RH, UK
7 - Centre d'Étude Spatiale des Rayonnements, 9 avenue du Colonel Roche, 31028 Toulouse Cedex 04, France
Received 1 August 2003 / Accepted 2 December 2003
This paper presents the analysis of a statistically complete sample of 28 serendipitous X-ray sources selected in 82 pointed XMM-Newton fields down to a count-rate of 0.002 counts s-1(4.5-7.5 keV energy band). This is the first sample selected in this energy range to have complete spectroscopic identifications and redshift determinations for all the objects. Apart from one Galactic source (an interacting binary), all the objects are AGNs. Their optical and X-ray properties (derived from the spectral analysis of the XMM-EPIC data) are compared together. The good correlation between the optical spectral type and the X-ray absorption properties supports the AGN unified model. Only one object that does not fit the relation between optical and X-ray absorption is found, namely a Seyfert 1.9 with no evidence of obscuration in the X-ray band ( cm-2). In total, 7 sources out of 27 are heavily obscured in the X-ray ( cm-2), corresponding to a surface density of 0.7 deg-2 at the flux limit the sample ( erg s-1 cm-2 in the 4.5-7.5 keV energy band). Among these obscured objects, two sources show a large (intrinsic) luminosity ( erg s-1) and are thus classified as type 2 QSO. Finally, we have compared the fraction of X-ray absorbed AGNs (26%) with that predicted by the current XRB synthesis models at the flux limit of the survey. We find that the models significantly (90% confidence level) over predict the fraction of absorbed AGNs thus confirming also in this hard energy band (4.5-7.5 keV) similar results recently obtained in the 2-10 keV band.
Key words: galaxies: active - X-rays: galaxies - X-rays: diffuse background
Over 80% of the cosmic X-ray background (XRB) has been recently resolved in the 2-10 keV energy range by deep Chandra and XMM-Newton observations (Mushotzky et al. 2000; Hasinger et al. 2001; Brandt et al. 2001; Rosati et al. 2002; Moretti et al. 2003). Its spectrum can be successfully reproduced by a combination of obscured and unobscured AGNs (Setti & Woltjer 1989; Madau et al. 1994; Comastri et al. 1995, 2001; Gilli et al. 2001; Ueda et al. 2003). The obscured AGNs, in particular, play a key role in the XRB synthesis models since they are expected to make up a significant fraction of the population in hard X-ray energies (see Fabian 2003 and references therein). On the contrary, only a small fraction of absorbed AGNs is found in soft X-ray surveys even at the faintest fluxes (e.g. 15% in the ROSAT Ultra Deep Survey, Lehmann et al. 2001).
Many important issues related to this population are still to be understood, like the number of type 2 QSO, the relationship between optical absorption and X-ray obscuration (e.g. Maccacaro et al. 1982; Panessa & Bassani 2002; Risaliti et al. 1999; Maiolino et al. 2001), the evolutionary properties of type 2 AGNs (Gilli et al. 2001; Franceschini et al. 2002) and the nature of the "Optically dull X-ray loud galaxies'', firstly discovered from the analysis of Einstein and ROSAT data (e.g. Elvis et al. 1981; Maccacaro et al. 1987; Griffiths et al. 1995; Tananbaum et al. 1997) and more recently found in large number by Chandra and XMM-Newton surveys (Fiore et al. 2000; Barger et al. 2002; Comastri et al. 2002; Severgnini et al. 2003).
Many of these issues can be studied by using hard X-ray surveys with complete spectroscopic information, both in the optical and in the X-rays, to allow a direct comparison between the two bands (e.g. Akiyama et al. 2003; Ueda et al. 2003). In particular, AGN samples selected in the hardest energy band currently reachable with imaging instruments, i.e. the 5-10 keV or 5-8 keV energy band, provide the best starting point for this kind of analysis since they are less affected by obscuration.
However, the sources found in medium-deep surveys are usually so faint in the optical that the completion of the identification process is hard, if not impossible, to achieve. For instance, about 25% of the sources discovered in the Chandra Deep Fields have optical counterparts fainter than R=25 (Giacconi et al. 2002) making the direct redshift estimate very difficult even with the largest optical telescopes currently available. Furthermore, an accurate X-ray spectral analysis is usually not feasible for the faintest sources detected in deep surveys. Bright X-ray surveys, for which a complete spectroscopic identification in the optical is a feasible task and for which the X-ray spectra can be easily collected, thus complement medium and deep surveys.
|obsid||position (J2000)||t||obsid||position (J2000)||t|
|0125310101||00 00 30.4 -25 06 43.4||19163.6||1||13||0067340101||18 55 37.1 -46 30 57.6||10653.3||0||11|
|0101040101||00 06 19.7 +20 12 22.8||34046.5||8||13||0081341001||19 31 21.7 -72 39 13.3||15288.1||1||13|
|0127110201||00 10 31.2 +10 58 40.7||7558.3||2||13||0081340501||20 13 30.0 -41 47 25.7||19196.8||0||13|
|0111000101||00 18 33.0 +16 26 08.0||31363.7||3||13||0111180201||20 40 10.0 -00 52 14.7||16495.8||8||13|
|0001930101||00 26 06.8 +10 41 12.5||18033.7||1||13||0111510101||20 41 50.9 -32 26 19.8||15046.1||8||13|
|0050140201||00 26 35.9 +17 09 37.8||50383.0||3||13||0130720201||20 44 09.0 -10 43 11.2||5312.0||8||13|
|0065770101||00 32 47.0 +39 34 33.3||7360.3||1||13||0111420101||20 45 09.4 -31 20 36.6||43323.5||8||13|
|0125320701||00 50 03.0 -52 07 36.7||16525.7||1||13||0112600501||20 46 20.0 -02 48 48.4||10550.3||8||13|
|0110890401||00 57 20.0 -22 23 04.1||29743.3||8||13||0083210101||20 54 18.8 -15 55 38.2||10435.5||2||13|
|0112650401||01 04 24.0 -06 24 10.6||23697.1||0||13||0112190601||20 56 21.6 -04 37 59.4||16639.4||2||13|
|0103861601||01 05 16.4 -58 26 10.4||7127.5||8||13||0081340401||20 58 27.1 -42 38 56.9||15002.3||1||13|
|0101040201||01 23 46.0 -58 48 25.8||28995.6||8||13||0041150101||21 04 11.1 -11 21 40.0||38736.2||1||13|
|0109860101||01 25 33.4 +01 45 38.2||38535.6||4||13||0038540301||21 04 40.2 -12 20 05.6||14698.6||2||13|
|0112600601||01 27 32.1 +19 10 32.3||3994.4||8||13||0088020201||21 27 38.1 -44 48 38.5||16094.7||1||13|
|0084230301||01 31 53.7 -13 36 56.4||20447.4||8||13||0103060101||21 29 12.2 -15 38 34.7||22042.9||3||13|
|0032140401||01 40 12.1 -67 48 40.3||7611.1||0||13||0109463501||21 37 56.5 -43 42 19.8||7577.7||2||13|
|0093641001||01 43 01.7 +13 38 24.4||9329.0||4||13||0061940201||21 38 07.9 -42 36 06.6||4868.2||1||13|
|0101640201||01 59 50.2 +00 23 46.8||7543.7||8||13||0008830101||21 40 15.5 -23 39 32.1||13986.7||2||13|
|0084140101||02 08 38.2 +35 23 00.2||38003.5||2||13||0103060401||21 51 55.9 -30 27 43.5||24072.9||3||13|
|0112371701||02 17 12.4 -04 39 04.2||20002.1||0||11||0124930201||21 58 52.9 -30 13 28.8||36246.3||8||13|
|0112371001||02 18 00.3 -04 59 47.8||50802.9||0||11||0130920101||22 03 09.3 +18 52 27.9||16491.3||1||13|
|0112371501||02 18 48.3 -04 39 02.9||6684.6||0||11||0012440301||22 05 10.1 -01 55 11.2||30937.5||2||13|
|0112370301||02 19 36.3 -04 59 47.7||50386.7||0||11||0106660101||22 15 31.9 -17 44 02.6||56911.8||1||13|
|0098810101||02 36 12.3 -52 19 55.6||23451.5||2||13||0009650201||22 17 55.4 -08 20 58.0||21027.5||8||13|
|0075940301||02 36 57.9 +24 38 53.7||47428.9||8||13||0049340201||22 20 45.1 -24 40 58.1||26842.3||6||13|
|0067190101||02 38 19.4 -52 11 34.1||25628.7||3||10||0018741701||22 34 32.9 -37 43 48.1||7080.3||4||13|
|0111200101||02 42 41.1 -00 00 53.7||35486.8||8||13||0111790101||22 35 45.9 -26 03 00.4||41304.4||4||13|
|0111490401||02 48 43.8 +31 06 59.2||31030.1||8||13||0103860201||22 36 55.9 -22 13 10.1||8489.9||8||13|
|0056020301||02 56 32.8 +00 06 01.7||17251.4||2||13||0006810101||22 42 39.5 +29 43 35.6||7009.4||8||13|
|0041170101||03 02 38.5 +00 07 31.9||47278.1||0||13||0109070401||22 48 41.5 -51 09 57.9||14722.6||8||13|
|0042340501||03 07 03.8 -28 40 24.1||13285.7||4||13||0112240101||22 49 48.3 -64 23 11.2||30608.4||8||13|
|0122520201||03 11 59.3 -76 51 53.0||28296.4||2||13||0081340901||22 51 49.4 -17 52 17.0||22398.6||1||13|
|0110970101||03 13 09.6 -55 03 48.4||10240.0||0||13||0112910301||22 53 58.8 -17 33 55.8||5301.3||8||13|
|0105660101||03 17 56.0 -44 14 15.1||23151.9||6||13||0112170301||23 03 15.8 +08 52 25.9||23349.6||4||13|
|0108060501||03 32 29.1 -27 48 27.1||46835.8||0||13||0109130701||23 04 43.6 -08 41 14.5||10615.6||8||13|
|0099010101||03 35 27.6 -25 44 54.5||18777.9||8||13||0033541001||23 04 45.0 +03 11 35.6||12461.5||2||13|
|0055140101||03 39 35.0 -35 25 58.1||47637.0||1||11||0123900101||23 13 58.9 -42 43 28.3||37401.3||6||13|
|0111970301||04 09 07.2 -71 17 43.9||18741.3||8||13||0109463601||23 15 18.7 -59 10 31.7||5403.6||8||13|
|0112600401||04 25 44.2 -57 13 34.4||7627.3||8||13||0112880301||23 31 49.9 +19 56 28.5||14318.0||3||13|
|0103861701||04 35 17.1 -78 01 54.3||8010.9||8||13||0093550401||23 33 40.0 -15 17 12.2||22258.0||1||13|
|0112880401||04 59 35.4 +01 47 16.0||18915.3||2||13||0100241001||23 49 40.6 +36 25 30.6||8739.0||3||13|
|Column 1: observation ID; Col. 2: sky position of the center of the field; Col. 3: MOS2 exposure time (after having removed the time intervals characterized by a high background); Col. 4: inner radius (see text for details); Col. 5: outer radius (see text for details).|
With this goal in mind, the XMM-Newton Survey Science Centre (SSC) is building up a large (1000 sources) sample of bright (flux limit 10-13 erg cm-2 s-1) serendipitous XMM-Newton sources at high Galactic latitude ( ), following well defined criteria so as to allow both a detailed study of sources of high individual interest as well as statistical population studies (see Della Ceca et al. 2002; Della Ceca 2002).
The scope of this paper is to present a first complete and representative sub-sample of 28 objects, selected in the 4.5-7.5 keV energy range. Even if small, this sample has the important advantage that a classification based on dedicated optical spectroscopy is available for all the sources. In contrast, recent samples selected in a similar very hard energy band (5-10 keV) using BeppoSAX (Fiore et al. 1999; La Franca et al. 2002) ASCA (Nandra et al. 2003), XMM-Newton (Baldi et al. 2002; Fiore et al. 2003; Mainieri et al. 2002) or Chandra data (e.g. Rosati et al. 2002) are usually characterized by a partial identification level.
In Sect. 2 the sample is presented while in Sect. 3 and in Sect. 4 the optical and the X-ray spectra respectively are discussed. In Sect. 5 the X-ray and optical properties are compared together while in Sect. 6 the relative fraction of absorbed versus un-absorbed AGNs is compared to the predictions based on the X-ray background synthesis models. Finally, in Sect. 7 an estimate of the density of type 2 QSO at the flux limit of the survey is given while in Sect. 8 we briefly discuss the problem of the X-ray Bright Optically Normal Galaxies. Summary and conclusions are presented in Sect. 9. Throughout this paper H0=65 km s-1 Mpc-1, and are assumed.
The XMM-Newton Bright Serendipitous Source (XMM-Newton BSS) sample is an ongoing project aimed at the selection of a statistically complete sample of X-ray sources serendipitously discovered in pointed XMM-Newton observations (see Della Ceca et al. 2002; Della Ceca 2002 for details). The XMM-Newton BSS consists of 2 complementary samples based on the XMM-Newton EPIC-MOS2 data and selected in the 0.5-4.5 keV and in the 4.5-7.5 keV energy range respectively. The reasons for using the MOS2 detector for the definition of the sample have been described in details by Della Ceca et al. (2002). The XMM-Newton BSS will be released to the public community (Della Ceca et al. in prep.) and, when combined with medium and deep X-ray surveys, will allow us to investigate on a wide range of luminosities and redshifts the properties of the sources responsible for the XRB at energies below 10 keV.
As a pilot study we have selected a representative sub-sample (the HBS28 sample) in the 4.5-7.5 keV energy range. In particular we have used the XMM-Newton MOS2 fields available to the XMM-Newton SSC until December 2002 and selected according to the criteria described in Della Ceca et al. (2002) and Della Ceca (2002) i.e.:
For the source detection and characterization we have followed the same pipeline processing used for the First XMM-Newton Serendipitous Source Catalogue, which is described in details in http://xmmssc-www.star.le.ac.uk/. The sources are then selected with the following constraints:
The total area covered by the HBS28 sample is 9.756 deg2. The list of 28 sources selected in the sample is presented in Table 2.
|name||Observation ID||Gal.||CR||EPIC cameras||Notes|
|XBS J002618.5+105019||0001930101||5.07||2.3||MOS2, MOS1, pn|
|XBS J013240.1-133307||0084230301||1.64||3.2||MOS2, MOS1, pn|
|XBS J013944.0-674909||0032140401||2.49||2.0||MOS2, MOS1, pn|
|XBS J014100.6-675328||0032140401||2.49||70.9||MOS2, MOS1||a|
|XBS J015957.5+003309||0101640201||2.59||3.8||MOS2, MOS1, pn|
|XBS J021640.7-044404||0112371701||2.42||2.1||MOS2, MOS1, pn|
|XBS J021808.3-045845||0112371001*||2.52||2.7||MOS2, MOS1, pn|
|XBS J021817.4-045113||0112371001*||2.52||3.3||MOS2, MOS1, pn|
|XBS J021822.2-050615||0112371001*||2.52||4.5||MOS2, MOS1, pn|
|XBS J023713.5-522734||0098810101||3.28||3.2||MOS2, MOS1, pn|
|XBS J030206.8-000121||0041170101||7.16||3.1||MOS2, MOS1, pn|
|XBS J030614.1-284019||0042340501||1.36||4.6||MOS2, MOS1||e|
|XBS J031015.5-765131||0122520201||8.21||4.4||MOS2, MOS1, pn|
|XBS J031146.1-550702||0110970101||2.55||5.9||MOS2, MOS1, pn|
|XBS J031859.2-441627||0105660101||2.60||2.2||MOS2, pn||c|
|XBS J033845.7-352253||0055140101||1.31||2.4||MOS2, MOS1, pn|
|XBS J040658.8-712457||0111970301||7.57||3.4||MOS2, MOS1, pn||b|
|XBS J040758.9-712833||0111970301||7.57||5.0||MOS2, pn||c|
|XBS J041108.1-711341||0111970301||7.57||2.2||MOS2, MOS1||a, b|
|XBS J185613.7-462239||0067340101||5.29||8.2||MOS2, MOS1, pn|
|XBS J193248.8-723355||0081341001||5.95||4.5||MOS2, MOS1, pn|
|XBS J204043.4-004548||0111180201||6.72||3.2||MOS2, MOS1, pn|
|XBS J205635.7-044717||0112190601||4.96||2.1||MOS2, MOS1||e|
|XBS J205829.9-423634||0081340401||3.89||3.9||MOS2, MOS1, pn|
|XBS J213002.3-153414||0103060101||4.99||2.3||MOS2, MOS1||d|
|XBS J213824.0-423019||0061940201||2.68||2.5||MOS2, MOS1||e|
|XBS J214041.4-234720||0008830101||3.55||3.3||MOS2, MOS1, pn|
|XBS J220601.5-015346||0012440301||6.13||2.3||MOS2, MOS1||d|
Column 1: source name;
Col. 2: identification number of the corresponding XMM observation;
Col. 3: Galactic column density;
Col. 4: source count-rate in the 4.5-7.5 keV energy band;
Col. 5: EPIC cameras used for the spectral analysis (see notes);
Col. 6: notes.
a = source on a gap in the pn.
b = MOS1 and MOS2 not summed.
c = source on a gap in MOS1.
d = source outside the pn field of view.
e = problems with the pn data.
* for the spectral analysis we have summed these data with the 0112370101 sequence.
The optical counterpart for each source in the sample has been searched in the Digitized Sky Survey (DSS) and a magnitude has been collected from the APM (Automatic Plate Measuring machine) catalogue. Thanks to the good positional accuracy (3 -4 ) and the brightness of the XMM sources, there is no ambiguity in the detection of the optical counterpart. When another source is present just outside the X-ray error circle we have spectroscopically observed also this second object. In all these cases (4 in total) the object within the error circle has turned out to be a more reliable counterpart (an AGN) than the object outside the circle (always a star) thus confirming the good accuracy of the X-ray position. All the optical counterparts are within 4 from the X-ray position.
For 26 sources out of 28, an APM counterpart with a red magnitude brighter than 20.1 was found. For the remaining 2 sources, an optical counterpart is visible in the acquisition image taken at the ESO 3.6 m telescope during the spectroscopic run (see below for the details) and a magnitude (R) is computed. Hence, for the totality of the sample an optical counterpart has been found. The magnitude distribution of the 28 sources is presented in Fig. 1.
It is worth noting that, given the small X-ray-to-optical positional offset
and the brightness of the optical counterparts, the expected number of
spurious optical identifications is completely negligible in the HBS28 sample.
considering the stars, that represent the most probable chance coincidence,
the expected number of spurious matches in the HBS28 sample
is below unity. Indeed, as explained below, no "normal'' stars
are found in the HBS28 sample. The only Galactic object found is
an accreting binary star whose X-ray emission properties are
|Figure 1: Red magnitude distribution of the 28 sources in the HBS28 sample. For most of the object (26) the magnitude is the APM red magnitude, while for the 2 faintest sources the R magnitude is considered.|
|Figure 2: Redshift distribution of the 27 extragalactic sources in the HBS28 sample. The shaded area represents the type 2 objects asdefined in the text.|
A search through the literature has produced 5 spectroscopic identifications (3 QSOs, 1 Narrow Line Radio Galaxy and 1 accreting binary star). Three more identifications have been taken from the AXIS project (Barcons et al. 2002a,b); one of these 3 objects has been re-observed at the SUBARU telescope (Severgnini et al. 2003). The remaining sources have been observed and spectroscopically identified during dedicated observing runs. Most of the sources were observed at the ESO 3.6 m in May and October 2002 using the EFOSC2 coupled with CCD40 and grism n.13 (October) or grism n.6 (May). The slit width ranges from 1.2 up to 1.5 , depending on the seeing conditions, and was usually oriented according to the parallactic angle to avoid differential flux losses, except when it was oriented so as to include two objects. Four additional objects were observed at the TNG telescope in November 2001 and September 2002, using DOLORES and grism LR-B. For the data reduction we have used the standard IRAF longslit package. The spectra have been wavelength calibrated using an helium-argon reference spectrum. A relative flux calibration has been obtained by observing the standard stars G191-B2B, BD 25+4655 (TNG) and LTT 7987 (ESO). The weather conditions (not always photometric) and the observing set-up usually do not guarantee a correct absolute flux calibration. For this reason, the spectra reported here are given in arbitrary units.
All the 28 sources selected in the HBS28 sample are emission line objects, including one accreting binary star (BL Hyi) which is the only Galactic source in the sample. We will not discuss this object any further as the main scientific target of the HBS28 is the extragalactic population. In Appendix A.1 we briefly outline the main properties of this source.
A redshift has been secured for all the 27 extragalactic objects in the sample. The redshift distribution is shown in Fig. 2.
To classify the emission line objects we have adopted the criteria presented for instance in Véron-Cetty & Véron (2001) which are based on the line widths and the [OIII]5007 Å/H flux ratio. In particular, we have divided the extragalactic sources into two groups, i.e. type 1 and type 2 objects:
|Figure 4: The spectra of the 2 NLSy1 candidates discovered in the sample: XBS J023713.5-522734 ( top) and XBS J205829.9-423634 ( bottom). The two small boxes inside the two figures show the expanded region around the Fe II4600 Å hump.|
|Figure 5: Top panel: the spectrum of the NEL AGN (a Seyfert 2) XBS J040758.9-712833. Bottom panel: The spectrum of the object XBS J193248.8-723355 optically classified as a Emission Line Galaxy (ELG, i.e. a starburst or a LINER, see text for details). As explained in the text, the X-ray analysis indicates the presence of an AGN in this object.|
In conclusion, the percentage of type 1 and type 2 objects is 70% and 30% respectively of the extragalactic sources. The redshift distributions for type 1 and type 2 objects taken separately are only marginally different (K-S probability of 6% of being drawn from the same parent population).
|Figure 6: The spectra of the two Sy1.9 discovered in the sample: XBS J040658.8-712457 ( top) and XBS J031146.1-550702 ( bottom).|
|name||X-ray position||optical position||id||type||z||mag||id ref|
|XBS J002618.5+105019||00 26 18.50 +10 50 19.3||00 26 18.70 +10 50 19.5||BEL AGN||1||0.473||17.5||TNG11/01|
|XBS J013240.1-133307||01 32 40.11 -13 33 07.8||01 32 40.27 -13 33 07.2||NEL AGN||2||0.562||20.0||ESO10/02|
|XBS J013944.0-674909||01 39 44.02 -67 49 09.4||01 39 43.77 -67 49 08.4||BEL AGN||1||0.104||16.7||ESO10/02|
|XBS J014100.6-675328||01 41 00.66 -67 53 28.9||01 41 00.23 -67 53 27.6||E.L.star||-||-||16.4||(a)|
|XBS J015957.5+003309||01 59 57.52 +00 33 09.7||01 59 57.60 +00 33 10.5||BEL AGN||1||0.310||18.3||TNG11/01|
|XBS J021640.7-044404||02 16 40.74 -04 44 04.9||02 16 40.66 -04 44 04.7||BEL AGN||1||0.873||16.5||TNG11/01|
|XBS J021808.3-045845||02 18 08.34 -04 58 45.7||02 18 08.20 -04 58 45.7||BEL AGN||1||0.712||17.7||AXIS|
|XBS J021817.4-045113||02 18 17.40 -04 51 13.3||02 18 17.43 -04 51 13.0||BEL AGN||1||1.070||19.5||AXIS|
|XBS J021822.2-050615||02 18 22.28 -05 06 15.7||02 18 22.15 -05 06 14.5||NEL AGN||2||0.044||14.8||(b)|
|XBS J023713.5-522734||02 37 13.54 -52 27 34.4||02 37 13.66 -52 27 34.7||NLSy1||1||0.193||17.1||ESO10/02|
|XBS J030206.8-000121||03 02 06.86 -00 01 21.2||03 02 06.76 -00 01 21.7||BEL AGN||1||0.641||18.8||(c)|
|XBS J030614.1-284019||03 06 14.19 -28 40 19.9||03 06 14.21 -28 40 19.3||BEL AGN||1||0.278||18.5||ESO10/02|
|XBS J031015.5-765131||03 10 15.56 -76 51 31.5||03 10 15.88 -76 51 33.8||BEL AGN||1||1.187||17.6||(d)|
|XBS J031146.1-550702||03 11 46.12 -55 07 02.5||03 11 46.18 -55 06 59.9||Sy1.9||2||0.162||17.3||ESO10/02|
|XBS J031859.2-441627||03 18 59.29 -44 16 27.6||03 18 59.41 -44 16 26.7||BEL AGN||1||0.140||15.9||(b), ESO10/02|
|XBS J033845.7-352253||03 38 45.77 -35 22 53.4||03 38 46.02 -35 22 52.7||NEL AGN||2||0.113||17.0||(e)|
|XBS J040658.8-712457||04 06 58.87 -71 24 57.7||04 06 58.88 -71 24 59.8||Sy1.9||2||0.181||18.7||ESO10/02|
|XBS J040758.9-712833||04 07 58.97 -71 28 33.5||04 07 58.58 -71 28 32.2||NEL AGN||2||0.134||17.0||ESO10/02|
|XBS J041108.1-711341||04 11 08.10 -71 13 41.1||04 11 08.78 -71 13 42.8||BEL AGN||1||0.923?||20.3*||ESO10/02|
|XBS J185613.7-462239||18 56 13.75 -46 22 39.2||18 56 13.78 -46 22 37.1||BEL AGN||1||0.768||19.0||ESO05/02|
|XBS J193248.8-723355||19 32 48.80 -72 33 55.2||19 32 48.77 -72 33 53.3||ELG||2||0.287||18.8||ESO05/02|
|XBS J204043.4-004548||20 40 43.46 -00 45 48.2||20 40 43.46 -00 45 51.9||NEL AGN||2||0.615||21.2*||ESO10/02|
|XBS J205635.7-044717||20 56 35.75 -04 47 17.9||20 56 35.67 -04 47 17.2||BEL AGN||1||0.217||17.3||TNG09/02|
|XBS J205829.9-423634||20 58 29.97 -42 36 35.0||20 58 29.89 -42 36 34.2||NLSy1||1||0.232||18.3||ESO10/02|
|XBS J213002.3-153414||21 30 02.32 -15 34 14.1||21 30 02.30 -15 34 13.2||BEL AGN||1||0.562||17.3||ESO10/02|
|XBS J213824.0-423019||21 38 24.03 -42 30 19.2||21 38 24.03 -42 30 17.5||BEL AGN||1||0.257||16.6||(f)|
|XBS J214041.4-234720||21 40 41.45 -23 47 20.1||21 40 41.53 -23 47 19.3||BEL AGN||1||0.490||18.4||ESO10/02|
|XBS J220601.5-015346||22 06 01.50 -01 53 46.9||22 06 01.45 -01 53 46.1||BEL AGN||1||0.211||20.1||ESO10/02|
Column 1: name;
Col. 2: X-ray position;
Col. 3: optical position;
Col. 4: spectroscopic classification (BEL AGN = Broad Emission Line AGN; NEL AGN = Narrow Emission Line AGN; NLSy1 = Narrow Line Seyfert 1; Sy1.9 = Seyfert 1.9; ELG = Emission Line Galaxy);
Col. 5: optical spectral type;
Col. 6: redshift;
Col. 7: APM red magnitude; the asterisk indicates that the magnitude (R) has been derived from our own observations;
Col. 8: reference for the identification i.e. the observing run, if the source has been identified by us, or a reference, if the source has been identified from the literature. The notes are:
(a) V* BL Hyi. See Appendix A.1;
(b) identification from Severgnini et al. (2003);
(c) identification from La Franca et al. (1992);
(d) identification from Fiore et al. (2000);
(e) identification from Carter & Malin (1983);
(f) identification from Hewett et al. (1995);
AXIS: identification from the AXIS project (Barcons et al. 2002a,b).
|class||Spectral type||Number||% extragalactic|
|Broad Emission Line AGN||17||63%|
|Narrow Emission Line AGN||5||19%|
On the basis of the MOS2 data, used for the sample definition, we have
firstly studied the hardness ratios of the sources in the sample.
This is useful as reference for other
(deeper) samples for which the available number of counts per source
is not enough to perform a detailed spectral analysis.
The hardness ratios have been computed using the data in the 0.5-2.0 keV,
2.0-4.5 keV and 4.5-7.5 keV
energy intervals adopting the following standard definitions:
Qualitatively, the correlation between the hardness-ratio and the optical spectral type is expected in the context of the unified models. A more quantitative assessment of this correlation is done in the following Section on the basis of a detailed spectral analysis.
|Figure 7: The hardness-ratio HR3 versus HR2. Filled circles represent the type 2 objects while the open circles are the type 1 objects.|
Thanks to the relatively bright flux limit which characterizes the sample, most of the sources have enough counts to perform a reliable X-ray spectral analysis. Except for 2 sources, the total counts in the MOS2 range from 100 to 3900. The availability of the MOS1 and, in most cases, of the pn increases the counts by a factor 2 (if only the MOS1 is available) or 4 (if both MOS1 and pn are available) the actual number of counts available for the spectral analysis. For 7 sources the pn was either not available or the object was outside the field of view or under a bad column. In another case the source falls under a gap in the MOS1 camera. In Table 2 the EPIC detectors used for the X-ray analysis of each source are summarized. Before the extraction of the spectra, we have removed the time intervals characterized by a high background.
All the spectra have been extracted using a circular region with a radius of 20 -30 , depending on the source off axis distance. The background is extracted in a nearby source-free circular region of a radius a factor 2 larger than the one used to extract the source counts. When the same blocking filters are used in the two MOS cameras the data are combined after the extraction.
The MOS and pn data have been re-binned in order to have at least 15-25 counts per channel depending on the brightness of the source. XSPEC 11.2 was then used to fit simultaneously the MOS and pn data, leaving the relative normalization free to vary. During the fitting procedure only the data in the 0.3-10 keV and 0.4-10 keV energy ranges are considered for the MOS and the pn respectively. Errors are given at the 90% confidence level for one interesting parameter ( ).
Initially, we attempted to fit a simple absorbed power-law model to all the 27 spectra taking into account both the Galactic hydrogen column density along the line of sight (from Dickey & Lockman 1990) and a possible intrinsic absorption at the source redshift.
For 20 sources the resulting fit is good enough (i.e. no systematic trends are observed in the residuals) and kept as the best-fit model while for the remaining 7 sources a simple absorbed power-law model does not give an acceptable fit.
|XBS J002618.5+105019||BEL AGN||PL||< 0.011||...||1.15 / 97||2.8||44.44|
|XBS J013240.1-133307||NEL AGN||PL||1.9 (frozen)||...||1.11 / 19||1.7||44.41|
|XBS J013944.0-674909||BEL AGN||PL||< 0.018||...||0.91 / 34||1.2||42.56|
|XBS J015957.5+003309||BEL AGN||PL||< 0.010||...||1.19 / 99||2.9||44.03|
|XBS J021640.7-044404||BEL AGN||PL||< 0.020||...||1.17 / 67||1.1||44.74|
|XBS J021808.3-045845||BEL AGN||PL + BB||< 0.007||1.07 / 527||2.3||44.79|
|XBS J021817.4-045113||BEL AGN||PL||<0.04||...||1.07 / 346||2.7||45.22|
|-050615a||NEL AGN||Leaky||...||1.41 / 63||3.0||42.76|
|XBS J023713.5-522734||NLSy1||PL + BB||< 0.18||0.86 / 80||2.7||43.52|
|XBS J030206.8-000121||BEL AGN||PL||< 0.015||...||1.14 / 125||2.2||44.63|
|-284019b||BEL AGN||PL||< 0.048||...||1.15 / 16||2.9||43.87|
|XBS J031015.5-765131||BEL AGN||PL||< 0.022||...||0.90 / 189||3.4||45.47|
|XBS J031146.1-550702||Sy1.9||PL||< 0.013||...||0.93 / 44||2.8||43.37|
|XBS J031859.2-441627||BEL AGN||PL||...||0.73 / 18||1.7||42.99|
|XBS J033845.7-352253||NEL AGN||Leaky + RS||1.9 (frozen)||0.83 / 29||1.7||43.21|
|XBS J040658.8-712457||Sy1.9||PL||1.9 (frozen)||...||1.25 / 4||1.6||43.56|
|XBS J040758.9-712833||NEL AGN||Leaky||1.9 (frozen)||...||1.13 / 5||2.5||43.44|
|XBS J041108.1-711341||BEL AGN||PL||< 0.61||...||0.99 / 6||0.8||44.59|
|XBS J185613.7-462239||BEL AGN||PL||< 0.058||...||1.15 / 26||1.4||44.69|
|XBS J193248.8-723355||ELG||PL||1.9 (frozen)||...||1.06 / 35||1.9||43.76|
|XBS J204043.4-004548||NEL AGN||PL||1.9 (frozen)||...||1.35 / 16||1.7||44.50|
|XBS J205635.7-044717||BEL AGN||PL + BB||< 0.56||1.18 / 21||1.7||43.42|
|XBS J205829.9-423634||NLSy1||PL||...||0.76 / 120||3.2||43.76|
|XBS J213002.3-153414||BEL AGN||PL||...||0.82 / 26||1.8||44.45|
|-423019c||BEL AGN||PL||< 0.057||...||0.86 / 26||1.6||43.60|
|XBS J214041.4-234720||BEL AGN||PL||< 0.012||...||1.06 / 93||1.7||44.28|
|XBS J220601.5-015346||BEL AGN||PL + BB||<0.670||0.72 / 15||1.7||43.36|
Column 1: source name;
Col. 2: optical identification;
Col. 3: best-fit model (PL = absorbed power-law; Leaky = leaky absorbed power-law;
PL + BB = absorbed power-law plus
Col. 4: best-fit photon index of the power-law component;
Col. 5: best-fit intrinsic hydrogen column density [cm-2];
Col. 6: temperature of the thermal component (if present) [keV];
Col. 7: reduced Chi-squared and degrees of freedom of the best-fit;
Col. 8: observed 2-10 keV flux (corrected for the Galactic absorption) [erg s-1 cm-1];
Col. 9: logarithm of the intrinsic luminosity in the 2-10 keV energy range [erg s-1];
a results from the X-ray analysis taken from Severgnini et al. (2003);
b in this object the presence of an emission line at 1.9 keV (source rest frame, consistent with the Si XIII at 1.86 keV) is required;
c in this object the presence of an emission line at 6.4 keV (source rest frame, consistent with the Fe I K) is required.
In most (13) of the 20 objects that are well fitted by a simple absorbed power-law model, no intrinsic absorption is found while for 7 sources the best-fit intrinsic is larger than the local Galactic column density. Among these latter sources, 4 present an hydrogen column density larger than 1022 cm-2 and the related best fit photon index is flatter ( ) than the flattest found for the unabsorbed AGNs (see below). This is probably due to the poor statistics available for spectral analysis which do not allow us to adequately constrain at the same time both the spectral index and the absorption. In order to better constrain the correct value of we have fixed for these 4 sources the to 1.9 (which corresponds to the average value found for the type 1 AGNs, see below) and derived the corresponding column density . This procedure is justified in the context of the unified scheme according to which the absorbed AGNs should have the same intrinsic power-law and a larger absorption with respect to the type 1 AGNs. Since the values of found for the type 1 AGNs have an intrinsic dispersion, we have checked the variation of when extreme values of (within the observed distribution) are assumed. We have found that the variation of is usually within the reported errors.
Finally, for the 7 sources for which the simple absorbed power-law model does not offer a good representation of the data, an improved fit is obtained with a more complex model, like a "leaky absorbed power-law'' model or by adding a thermal component. In one case (XBS J040758.9-712833) the value of in the "leaky absorbed power-law'' has been fixed to 1.9 to better constrain the absorption.
The results of the X-ray spectral analysis for the extragalactic sources are summarized in Table 5. The X-ray spectra of the extragalactic sources are reported in Appendix B.1.
The distribution of the photon indices of the type 1 objects is shown in Fig. 8. The mean value is with a standard deviation of 0.16 consistent with the mean value found in other similar samples (e.g. Mainieri et al. 2002). The distribution of the photon indices of the type 2 objects is not presented since, for most of these sources, the value of has been fixed to the value 1.9 to better constrain the absorption.
|Figure 8: The X-ray photon-index distribution of the type 1objects obtained from the spectral fitting.|
We discuss below in greater detail the results for the single classes of extragalactic objects.
Broad Emission Line AGNs. For 12 out of 17 Broad Line AGNs the simple absorbed power-law model gives an acceptable fit (reduced below 1.2) and a column density consistent with the Galactic value. In one object (XBS J031859.2-441627) an intrinsic column density (see Table 5) significantly larger than the Galactic value results from the fitting procedure. This is one of two sources mentioned at the beginning of Sect. 4 for which a departure from the HR2/optical classification segregation has been noted. The optical spectrum of this source is dominated by the host galaxy while the AGN activity is suggested only by the presence of a weak ( Å), possibly broad H emission line. In Severgnini et al. (2003) we show that the observed optical spectrum of this object can be modeled by using the computed from the X-ray data and assuming a standard Galactic value for the ratio.
In three other objects (XBS J021808.3-045845, XBS J205635.7-044717, XBS J220601.5-015346) the simple absorbed power-law model leaves significant residuals. A better fit is obtained by adding a soft component (a Black-body spectrum with a temperature of 0.1-0.2 keV).
In summary, all the objects with broad ( km s-1) emission lines in the optical spectra are unabsorbed or only weakly absorbed in the X-ray band ( cm2). In 18% of cases, a soft excess is also detected.
Narrow Line Seyfert 1. The 2 NLSy1 candidates found in the sample show only a moderate intrinsic absorption ( cm-2, XBS J205829.9-423634) or no absorption at all (XBS J023713.5-522734). In the case of XBS J023713.5-522734, a better fit is obtained by adding a soft-component modeled with a black-body spectrum with kT=0.1 keV. The spectral indices in the two sources are quite similar ( for XBS J023713.5-522734 and for XBS J205829.9-423634) and slightly lower but still consistent with those found with ASCA by Vaughan et al. (1999) for a sample of 22 NLSy1 ( with a standard deviation of 0.3 in the 2-10 keV band).
In summary, the 2 NLSy1 candidates are not significantly absorbed in the X-ray ( cm-2) and, in one case, a soft-excess is also present. With the available data there is no evidence that NLSy1 have steeper values when compared to Sy1.
Narrow Line AGNs and ELG. The X-ray spectra of all the Narrow Line AGNs and the ELG show strong evidence of intrinsic absorption ( cm-2).
In two cases, a more complex model, including a "scattered'' component ("leaky absorbed power-law'' model) is needed to obtain a better fit to the data. The scattered component is found to be 5%-10% of the flux of the primary component in agreement with what has been observed in other well studied Type 2 AGNs (e.g. Turner et al. 1997a,b).
Finally, in one case (XBS J033845.7-352253) the leaky absorbed power-law model does not give an acceptable fit leaving significant residuals at low energies. The inclusion of a thermal component with kT=0.16+0.04-0.08 keV is required to achieve a better fit (see Appendix A.3 for a more detailed discussion of this source).
In summary, the 6 objects with an optical spectrum showing only narrow emission lines ( km s-1) are significantly absorbed at X-ray energies ( cm2).
Notably, two objects (XBS J013240.1-133307 and XBS J204043.4-004548) have an unabsorbed X-ray luminosity ( erg s-1 and erg s-1 respectively) in the typical range of the type 2 QSO. The optical spectra of these two sources are shown in Fig. 9.
|Figure 9: The optical spectra of the 2 type 2 QSO discovered in the HBS28 sample: bottom panel: XBS J013240.1-133307, top panel: XBS J204043.4-004548.|
Seyfert 1.9. The 2 "intermediate'' Seyfert galaxies show very different spectra: XBS J040658.8-712457 is absorbed ( cm-2) while XBS J031146.1-550702 is well fitted by a simple un-absorbed power-law model with cm-2. The very low X-ray absorption observed in this latter source is in contrast with what is usually found in Sy1.9 for which typical values of are between 1022 and 1024 cm-2 (e.g. Risaliti et al. 1999; Maiolino et al. 2001). The source XBS J031146.1-550702 seems to be a case where the measured X-ray absorption is much lower than the one inferred by the optical spectrum, which shows no broad lines except for a broad wing in the H profile and an [OIII]5007 Å/H ratio typical of a Sy2. Other cases like this have been presented in the literature (see next section). A more detailed discussion of this object is reported in Appendix A.2.
|Figure 10: The distribution of the intrinsic derived from the spectral fit, for type 1 objects and type 2 objects. The shaded histograms show the detections while the empty histograms represent the upper limits on .|
The unified models (Antonucci 1993) predict a strict correlation between the optical and the X-ray absorption. Although the presence of this correlation is suggested by the large values of usually observed in Seyfert 2 galaxies (e.g. Awaki et al. 1991; Turner et al. 1997a; Risaliti et al. 1999; Guainazzi et al. 2001), many important exceptions are known since the first observations taken with the Einstein Observatory (e.g. Maccacaro et al. 1982). More recently, Panessa & Bassani (2002) have presented a significant number of type 2 AGNs whose X-ray spectra are indicative of a very low (or even absent) absorption ( cm-2), thus confirming earlier results from Ptak et al. (1996), Pappa et al. (2001) and Bassani et al. (1999). Similarly, Barcons et al. (2003) have recently shown the case of a Sy1.9 with no X-ray absorption and more cases like this are emerging from recent XMM-Newton observations (Lehmann et al. in prep.). Quantifying the percentage of this type of source is a difficult task. However, Panessa & Bassani (2002) estimate this percentage in the range 10%-30%. This number is larger than that found by Risaliti et al. (1999) in a sample of Seyfert 2 (4%).
Another important exception to the optical/X-ray absorption correlation is the discovery of type 1 AGNs with large X-ray absorption (e.g. Fiore et al. 2001). Similarly, Maiolino et al. (2001) have pointed out that in a fraction of AGNs the ratio is significantly lower than that observed in our Galaxy.
The statistical completeness of the HBS28 sample together with its complete spectroscopic classification allows us to perform a statistical analysis of the relationship between X-ray and optical absorption at the flux limit of the survey ( erg s-1 cm-2 in the 4.5-7.5 keV energy range). In Fig. 10 the distribution of the intrinsic for the extragalactic objects is presented. The number of X-ray obscured AGNs ( cm-2) is 7 corresponding to a surface density of 0.7 deg-2.
In Fig. 11 the best-fit values of are plotted against the 2-10 keV intrinsic luminosity. In panel (a) of Fig. 11 only the sources optically classified as type 1 objects are plotted while in panel (b) only the type 2 objects are presented. The plot confirms what has been already inferred from the analysis of the hardness ratios, i.e. that a correlation between the optical type and the X-ray absorption is clearly present: type 1 objects always have low values of (<1022 cm-2, panel a) while the majority (88%) of type 2 objects have large values of (>1022 cm-2, panel b). This correlation holds also in the other sense: the great majority (95%) of sources with cm-2 are type 1 while all the objects with cm-2 are type 2 sources.
|Figure 11: The intrinsic versus the unabsorbed X-ray luminosity in the 2-10 keV energy range for a) type 1 objects (open circles) and for b) the type 2 objects (filled circles).|
In the HBS28 sample one source out of eight type 2 sources has cm-2 (see previous section). Hence, we can infer that the fraction of these sources is 12% with a standard deviation range of 2%-41%. Given the large uncertainity, this result is consistent with both the estimate made by Panessa & Bassani (2002) and with that of Risaliti et al. (1999).
Moreover, we have found two type 1 AGNs in which the absorption exceeds the Galactic column density, but in only one of these the intrinsic absorption is relatively large ( cm-2, XBS J031859.2-441627). As already discussed, also in this object the observed and the optical spectrum are consistent with a standard Galactic AV/ (Severgnini et al. 2003).
Interestingly, we have not found any type 1 object for which the value of is higher than 1022 cm-2 (see Fig. 10). Based on the available numbers we can estimate an upper limit of 10% on the percentage of type 1 sources with cm-2.
The relative percentage of absorbed versus un-absorbed AGNs found in the HBS28 sample can be directly compared to the theoretical predictions of the XRB synthesis models. We stress once again the great advantage of dealing with a completely identified sample for which a value for the redshift is available for all sources. This is fundamental for a correct determination of the intrinsic absorbing column density.
The 4.5-7.5 keV selection interval is useful for probing the real fraction of obscured objects even at relatively bright flux limits. The expected fraction of obscured AGNs ( cm-2) in the HBS28 predicted by the XRB synthesis model discussed in Comastri et al. (2001) is equal to 0.62-0.65, considering the range of fluxes sampled by the HBS28 (between 0.4 to erg s-1 cm-2). This fraction corresponds to 17-18 AGNs obscured in the X-rays expected in the HBS28 sample. This number is significantly (at the 99% confidence level) larger than the observed one (7), assuming the Poissonian statistics.
A similar overprediction, although less significant (90%), of the population of absorbed AGNs is also found by comparing our results with the "modified unified model'' recently presented by Ueda et al. (2003), which includes a dependence of the fraction of absorbed AGNs on the X-ray luminosity.
In the 2-10 keV energy band Piconcelli et al. (2002, 2003) have already pointed out that the observed fraction of the absorbed AGNs at a flux limit of 10-14 erg s-1 cm-2 is a factor 2 lower that predicted by the CXB synthesis models. We thus confirm this result and extend it to the hardest 4.5-7.5 keV energy band. Clearly, current XRB synthesis models have to be revised.
|Figure 12: The ratio between the (observed) flux between 2 and 10 keV and the optical flux (see text for details) versus the observed 2-10 keV flux. The loci of constant R (Cousins) magnitudes are also plotted for R=16, 18, 20 and 22. Symbols are the same as in previous figure.|
The existence of optically "passive'' galaxies for which the X-ray observations reveal an intense AGN activity has been hotly discussed in the recent literature (e.g. Fiore et al. 2000; Barger et al. 2002; Comastri et al. 2002; Severgnini et al. 2003). Even if these X-ray Bright Optically Normal Galaxies (XBONG) seem to emerge at faint X-ray fluxes (<10-13 erg cm-2 s-1), some examples have been discovered also at relatively high X-ray fluxes (e.g. Piconcelli et al. 2002; Severgnini et al. 2003).
In the HBS28 sample two sources were at a first glance classified as XBONG candidates, based on the optical information available at the time of the sample selection. The source XBS J021822.2-050615 was initially classified as an XBONG since no strong emission lines were present in the discovery spectrum. However, a more accurate re-observation of this source with the 8.2 m Subaru telescope has revealed the presence of narrow emission lines that were outshone by the host-galaxy light in the previous spectrum (Severgnini et al. 2003). This source is thus classified as Type 2 AGN.
Similarly, the source XBS J031859-441627 was initially classified as an "optically dull galaxy'' on the basis of an optical spectrum covering the spectral range between 4900 and 5800 Å. Further observations, covering a wider spectral range, have revealed the presence of a weak and possibly broad H emission line (Severgnini et al. 2003). We consider this object to be a type 1 AGN.
Interestingly, the two objects have the lowest X-ray-to-optical flux ratio (and the brightest magnitude) among the objects in the HBS28 sample (see Fig. 12). This peculiar X-ray-to-optical flux ratio found for this type of sources has been already noted, for instance, by Comastri et al. (2003).
In conclusion, two sources in the HBS28 sample are potentially similar to some XBONG that are emerging from different X-ray surveys although a closer look at their spectra, based on high resolution data and/or a better spectral coverage, reveal their real AGN nature. We stress that similar detailed observations, relatively easy to do for low-z sources (like those discovered in the HBS28 sample), are hard to carry out for higher z objects.
We have presented a statistically complete sample of 28 X-ray sources selected in the 4.5-7.5 keV energy band at a flux limit of erg s-1 cm-2. The sample is completely identified and a spectroscopic classification and redshift is available for each object. This is the first sample, selected in this energy band, to have such complete optical information. Apart from one Galactic accreting binary star, all the remaining 27 sources are AGNs. We have discussed the optical classification of these 27 objects based on the presence and the intensities of the broad/narrow emission lines. In particular, we have divided the sources into 19 type 1 objects, including Sy1, QSO and NLSy1, and 8 type 2 objects, including Sy2, Sy1.9, Narrow Line Radio Galaxies (NLRG) and ELG. We have then presented the X-ray spectral analysis based on the XMM-Newton EPIC data for the 27 AGNs. Thanks to the relatively bright flux limit of the sample, the available number of counts (from hundreds to thousands) is large enough to allow a reliable spectral analysis in nearly all cases.
The optical and the X-ray properties of the sources are thus analysed together. The main results can be summarized as follows:
We thank Andrea Comastri for providing us with the predictions of the XRB synthesis model adapted to the 4.5-7.5 keV energy band. This work has received partial financial support from ASI (I/R/062/02, I/R/037/01) and from the Italian Ministry of University and Scientific and Technological Research (MURST) through grant Cofin. X.B. and F.J.C. acknowledge financial support from the Spanish Ministry of Science and Technology, under project AYA2000-1690. The TNG telescope is operated on the island of La Palma by the Centro Galileo Galilei of the INAF in the Spanish Observatorio del Roque de Los Muchachos of the Instituto de Astrofísica de Canarias. We would like to thank the staff members of the ESO and TNG Telescopes for their support during the observations. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. We finally thank the APM team for maintaining this facility.
XBS J014100.6-675328 (BL Hyi) is a known AM Herculis object (a polar), i.e. a binary system composed of a magnetic white dwarf and a low-mass star. These sources are characterized by soft and hard X-ray variable emission, modulated on the rotational period of the white dwarf. The hard X-ray properties of BL Hyi have been discussed by Wolff et al. (1999) on the basis of RXTE data and by Matt et al. (1998) by using ASCA and BeppoSAX observations.
The X-ray spectrum of XBS J014100.6-675328 is well fitted by a unabsorbed power-law model with plus a thermal component ( kT=55+3-1 eV) and an emission line at keV. The 2-10 keV flux is erg s-1 cm-2.
XBS J031146.1-550702 has been classified as Sy1.9 and its X-ray emission does not show significant absorption, as described in the text. Other examples of Sy2 objects with low X-ray absorption have been recently presented by Panessa & Bassani (2002) and Barcons et al. (2003). Panessa & Bassani (2002) have suggested that a large-scale dusty environment (e.g. dust lanes or an HII region), instead of an obscuring torus close to the nucleus, can hide the BLR without producing a significant X-ray absorption ( cm-2 or slightly lower than this value). However, the upper limit on the value estimated for XBS J031146.1-550702 is cm-2 which is almost two orders of magnitude below the value expected in the scenario proposed by Panessa & Bassani (2002). Another possibility considered by Panessa & Bassani (2002) is that the BLR is not efficiently activated due to an extremely sub-Eddington accretion rate. This scenario, however, is expected to work for low-luminosity AGNs (LLAGN, erg s-1) which represent a large fraction of the Sy2 studied by Panessa & Bassani (2002). On the contrary, the source XBS J031146.1-550702 has an X-ray luminosity of erg s-1, thus significantly higher than the luminosity expected in LLAGNs. Two objects similar to XBS J031146.1-550702 in terms of X-ray luminosity (1042-1043 erg s-1) and low value (<1020-1021 cm-2) are NGC 7679 (Della Ceca et al. 2001) and IRAS 00317-2142 (Georgantopoulos 2000). These two sources are dominated by the starburst emission in the optical and by an unabsorbed AGN in the X-ray. Selective obscuration due to a dusty ionized absorber has been invoked to explain the observed X-ray and optical properties of these sources. A more detailed analysis of XBS J031146.1-550702 is required to assess whether a similar interpretation could also be applied to this source.
Another possibility is that XBS J031146.1-550702 is a Compton-thick source ( cm-2). In this case, the observed X-ray spectrum represents only the fraction of the total emission reflected towards the observer. If this hypothesis is correct, a strong neutral iron K line is expected at 6.4 keV (source rest frame), corresponding to 5.5 keV in the observer rest frame, i.e. very close to the extreme end of the observed spectrum. In this spectral region an upper limit on the emission line is very poorly determined ( keV) and cannot be used to rule out the Compton thick nature of the source.
In principle, the thickness parameter / , where is the 2-10 keV observed flux (corrected for the Galactic absorption) and is the reddening corrected flux of the [OIII]5007 Å line, could be used to assess the Compton thickness of the source. According to Bassani et al. (1999), in fact, a Compton-thick source should present low values of the / ratios (below 1) while Compton-thin sources should have / significantly above 1. As previously stated, the optical spectra collected by us do not have an absolute flux calibration so the measurement of the / flux ratio is not simple. However, considering the good weather conditions of the night during the observation of XBS J031146.1-550702 and taking into account the flux lost due to the slit width we have obtained a rough absolute calibration for this spectrum. The result is in good agreement with the APM photometric point (red magnitude). We have thus estimated the line flux and the / flux ratio. The computed ratio is between 8 and 30, hence suggesting a Compton-thin nature for this object. Clearly, better data are required to put this estimate on a firmer ground.
The X-ray spectrum of this NLRG is not fitted by a simple absorbed power-law or a leaky absorbed power-law models. A reasonable fit is obtained by allowing the two spectral indices free to vary. The best fit gives a very steep slope ( ) at low energies plus a flatter slope ( ) at higher energies. Alternatively, a leaky absorbed ( cm-2) power-law with frozen to 1.9 plus a thermal (Raymond-Smith) model with kT=0.16+0.04-0.08 keV gives an acceptable fit. The simple absorbed power-law plus a thermal component, instead, is unable to fit both the high and the low energy parts of the spectrum.
XBS J033845.7-352253 is a known Narrow Line Radio galaxy (NLRG, Carter & Malin 1983) resolved in the NRAO VLA Sky Survey (NVSS, Condon et al. 1998) into two bright radio-lobes with a total radio flux of 2.1 Jy corresponding to a radio power of W Hz-1 at 1.4 GHz. In principle, the flat component ( ) of the 2 power-laws model could be ascribed to the non-thermal emission from the jet. However, this component is usually not observed in lobe-dominated radio-loud AGNs, like XBS J033845.7-352253, where relativistic beaming is not important while it is probably at the origin of the flat X-ray spectrum observed in core-dominated AGNs (e.g. Sambruna et al. 1999).
|Figure A.1: The optical spectrum taken with EFOSC2 in November 2002 of the XBS J041108.1-71134. The weak ( EW=10-15 Å) emission line is tentatively identified with MgII2798 Å.|
We consider the second model, which includes a thermal emission, as more appropriate. In fact, the presence of a thermal emission is a quite frequent feature in NLRGs. For instance, 50% of the NLRGs observed with ASCA (Sambruna et al. 1999) show a thermal component; the 0.1-2.4 keV unabsorbed luminosity of the thermal emission found in XBS J033845.7-352253 is erg s-1, in the range of luminosity obtained by Sambruna et al. (1999) ( ergs s-1).
Therefore, we have adopted the thermal plus leaky absorbed power-law model for XBS J033845.7-352253.
This is one of the optically faintest sources in the sample (R=20.25). The noisy spectrum collected in 2400 s with EFOSC2 shows only one weak broad emission line which we have tentatively identified as the MgII2798 Å line. With this assumption, the redshift is 0.923. The equivalent width of the line is 10-15 Å (source rest-frame) which is close to the border-line of the BL Lac objects classification (EW<5 Å, e.g. Stocke et al. 1991). The spectrum is reported in Fig. A.1. A firmer classification and z estimate requires a better signal-to-noise spectrum.
In this appendix we present the spectra of the extragalactic sources (all AGNs) present in the HBS28 sample.
|Figure B.1: The best-fit X-ray spectra of the extragalactic sources in the HBS28 sample (note that the sources XBS J021822.2-050615 and XBS J031859.2-441627 are not included since these spectra have been already presented and discussed in Severgnini et al. 2003).|