2017A&A...608A..51M


C.D.S. - SIMBAD4 rel 1.7 - 2021.02.25CET18:26:04

2017A&A...608A..51M - Astronomy and Astrophysics, volume 608A, 51-51 (2017/12-1)

The WISSH quasars project. III. X-ray properties of hyper-luminous quasars.

MARTOCCHIA S., PICONCELLI E., ZAPPACOSTA L., DURAS F., VIETRI G., VIGNALI C., BIANCHI S., BISCHETTI M., BONGIORNO A., BRUSA M., LANZUISI G., MARCONI A., MATHUR S., MINIUTTI G., NICASTRO F., BRUNI G. and FIORE F.

Abstract (from CDS):

We performed a survey of the X-ray properties of 41 objects from the WISE/SDSS selected hyper-luminous (WISSH) quasars sample, which includes 86 broad-line quasars with bolometric luminosity LBol≥2 x 1047erg/s shining at z∼2-4. We used both proprietary and archival Chandra and XMM-Newton observations. Twenty-one quasars have sufficient quality data to perform a spectroscopic analysis, while for the remaining sources, X-ray properties are derived through hardness-ratio analysis (apart for six sources that result to be undetected). The bulk (∼70%) of the detected WISSH quasars exhibit NH<5x1022cm–2, in agreement with their optical Type 1 AGN classification. All but three quasars show unabsorbed 2-10 keV luminosities L2–10≥1045erg/s. Thanks to their extreme radiative output across the mid-IR-to-X-ray range, WISSH quasars therefore offer the opportunity to significantly extend and validate the existing relations involving L2–10. Specifically, we studied the X-ray luminosity as a function of (i) X-ray-to-optical (X/O) flux ratio; (ii) mid-IR luminosity (LMIR); (iii) LBol, and (iv) αOX versus 2500Å luminosity. We find that the WISSH quasars show (i) unreported very low X/O (<0.1) compared to typical AGN values; (ii) L2–10/LMIR ratios that are significantly smaller than those derived for AGN with lower luminosity; (iii) a large X-ray bolometric correction, kBol,X~=100-1000; and (iv) steep -2≥αOX≥-1.7. These results lead to a scenario in which the X-ray emission of hyper-luminous quasars is relatively weaker compared to lower luminosity AGN. Models predict that such an X-ray weakness can be relevant for the acceleration of powerful high-ionization, emission-line-driven winds, which are commonly detected in the UV spectra of WISSH quasars and can, in turn, perturb the X-ray corona and weaken its emission. Accordingly, hyper-luminous quasars represent the ideal laboratory to study the link between the AGN energy output and wind acceleration. Additionally, WISSH quasars exhibit very large SMBH masses (log [MBH/M]≥9.5). This enables a more robust modeling of the Γ-MBH relation by increasing the statistics at high masses. We derive a flatter Γ dependence than previously found over the broad range 5≤log(MBH/M)≤11. Finally, we estimate that only 300 ks observations of X-IFU on board Athena will offer a detailed view of the properties of absorption features associated with powerful X-ray SMBH winds for a representative sample of WISSH quasars.

Abstract Copyright: © ESO, 2017

Journal keyword(s): galaxies: active - galaxies: nuclei - quasars: emission lines - quasars: general - quasars: supermassive black holes - techniques: imaging spectroscopy - techniques: imaging spectroscopy

Simbad objects: 47

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Number of rows : 47

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 [VV2006] J002822.8-283041 QSO 00 28 22.7726384470 -28 30 40.270405801     20.30     ~ 6 0
2 [VV2006] J004527.7+143815 QSO 00 45 27.6883225636 +14 38 16.137315633   18.23 17.72     DZ 29 1
3 QSO B0207-0019 QSO 02 09 50.7146360498 -00 05 06.459317612   17.45 17.21     ~ 124 0
4 NAME Chandra Deep Field-South reg 03 32 28.0 -27 48 30           ~ 1856 1
5 [VV2006] J073502.3+265911 QSO 07 35 02.3056069899 +26 59 11.532940903   17.01 16.68     ~ 32 0
6 QSO J0745+4734 QSO 07 45 21.7881463456 +47 34 36.191344902   16.76 16.44     ~ 88 0
7 QSO J0747+2739 QSO 07 47 11.1475926883 +27 39 03.365274417     17.20     ~ 55 0
8 QSO J0801+5210 QSO 08 01 17.7968518079 +52 10 34.600380950   17.41 17.04     ~ 48 0
9 QSO B0900+42 QSO 09 00 33.5093000271 +42 15 47.031257024   17.63 17.18     ~ 68 0
10 2MASS J09042337+1309208 QSO 09 04 23.3740479717 +13 09 20.717771127   18.13 17.71     ~ 19 0
11 2MASS J09473420+1421168 QSO 09 47 34.1974500082 +14 21 16.934532564   17.89 17.65     ~ 23 0
12 QSO B1011+4315 QSO 10 14 47.1892442829 +43 00 30.171082487   17.39 17.05     ~ 57 0
13 [VV2000] J102714.7+354318 QSO 10 27 14.7801577582 +35 43 17.394409696   16.96 16.69     ~ 32 0
14 QSO J1057+4555 QSO 10 57 56.2613130231 +45 55 53.068171990   20.19 18.80 17.2 16.8 ~ 104 0
15 QSO B1103+6416 QSO 11 06 10.7342664415 +64 00 09.646278482   16.36 16.16     ~ 60 0
16 QSO B1107+4847 QSO 11 10 38.6373081925 +48 31 15.693241688   17.09 16.87     ~ 76 0
17 QSO J1111+1336 QSO 11 11 19.1031733986 +13 36 03.821438785   18.59 17.96     ~ 32 0
18 QSO J1159+1337 QSO 11 59 06.5237058914 +13 37 37.669759166   19.50 18.53     ~ 41 0
19 QSO B1157+3143 QSO 12 00 06.2494598212 +31 26 30.839054589   16.76 16.47     ~ 60 0
20 QSO J1201+0116 QSO 12 01 44.3651168135 +01 16 11.738588370   18.09 17.74 17.4   ~ 52 2
21 QSO B1159+123 QSO 12 01 47.9113685833 +12 06 30.254501010   18.85 18.16     ~ 90 0
22 2MASS J12102762+1741088 QSO 12 10 27.6311982162 +17 41 08.835057535   21.23 19.98     ~ 11 0
23 QSO J1215-0034 QSO 12 15 49.8118973656 -00 34 32.174769639   17.76 17.51     ~ 77 0
24 [VV2006] J123641.5+655441 QSO 12 36 41.4593292099 +65 54 42.187925135   18.21 17.72     ~ 30 0
25 LBQS 1243+0121 QSO 12 45 51.4511943707 +01 05 05.032485812   18.43 18.26     ~ 60 0
26 QSO J1249-0159 QSO 12 49 57.2387444582 -01 59 28.776474497   18.93 18.19     ~ 42 0
27 LB 19 QSO 12 50 05.726 +26 31 07.51   16.12 15.92     ~ 191 0
28 Mrk 231 Sy1 12 56 14.2340989340 +56 52 25.238555193   14.68 13.84     ~ 1815 3
29 [VV2006] J132827.1+581836 QSO 13 28 27.0685362777 +58 18 36.917791203   18.67 18.67     ~ 38 0
30 QSO B1331+170 QSO 13 33 35.7828550018 +16 49 04.012528106   16.84 16.71 16.41   ~ 419 0
31 [VV2006] J142124.0+463318 QSO 14 21 23.9851528711 +46 33 17.955335686   18.53 17.99     ~ 36 0
32 [VV2006] J142243.0+441721 QSO 14 22 43.0266144858 +44 17 21.324202449   19.96 19.08     ~ 31 0
33 QSO B1425+606 QSO 14 26 56.1848058014 +60 25 50.814100630   16.82 16.54     ~ 126 0
34 QSO J1433+0227 QSO 14 33 52.2086962626 +02 27 13.984739230   22.31 20.74     ~ 37 0
35 [VV2006] J144105.5+045454 QSO 14 41 05.5361384564 +04 54 54.961282916   17.77 17.47     ~ 25 0
36 QSO J1506+5220 QSO 15 06 54.5500668499 +52 20 04.740607965   21.72 20.14     ~ 50 0
37 QSO B1511+091 QSO 15 13 52.5260150813 +08 55 55.726621813   18.22 17.92     ~ 57 1
38 2MASS J15215647+5202387 QSO 15 21 56.4822619037 +52 02 38.598808258   16.02 15.70     ~ 46 0
39 QSO J1538+0855 QSO 15 38 30.5594703954 +08 55 17.150684209   18.77 17.98     ~ 25 0
40 ULAS J153910.16+055749.7 QSO 15 39 10.16040 +05 57 49.7160           ~ 12 0
41 2MASS J15493872+1245092 QSO 15 49 38.7150556228 +12 45 09.160054709   19.21 18.54 17.61   ~ 32 0
42 QSO B1618-0035 QSO 16 21 16.9225064465 -00 42 50.911354748   18.92 17.97     ~ 61 0
43 2MASS J16390910+2824471 QSO 16 39 09.1110374235 +28 24 47.167825199   19.61 18.48     ~ 27 0
44 HS 1700+6416 QSO 17 01 00.6195618802 +64 12 09.118927057   16.39 16.17     ~ 345 0
45 QSO B1725-142 QSO 17 28 19.7893541722 -14 15 55.855574749   14.69 14.03 13.7   ~ 248 0
46 SDSS J212329.46-005052.9 QSO 21 23 29.4639237667 -00 50 52.916067995   16.91 16.62     ~ 97 0
47 ULAS J231556.23+014350.3 QSO 23 15 56.236 +01 43 50.38           ~ 12 0

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2021.02.25-18:26:04

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