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J/PASJ/53/445    ASCA Deep survey in Lockman Hole Field  (Ishisaki+, 2001)

ASCA Deep survey in the Lockman Hole Field Ishisaki Y., Ueda Y., Yamashita A., Ohashi T., Lehmann I., Hasinger G. <Publ. Astron. Soc. Jap., 53, 445 (2001)> =2001PASJ...53..445I
ADC_Keywords: X-ray sources ; Active gal. nuclei Mission_Name: ASCA Keywords: galaxies: active - surveys - X-rays: galaxies - X-rays: general Abstract: We present the results of deep observations of the Lockman Hole field with the ASCA SIS, covering 926arcmin2 in the 1-7keV energy range, with a sensitivity 3-5 times deeper than the previous ASCA larger area surveys. Utilizing the results of the ROSAT Ultra Deep survey, we have detected 32, 25, and 15 sources in the 1-7, 1-2, and 2-7keV bands, and only 4, 4, and 1 sources remain unidentified, respectively. The average hardness of the sources detected in the 1-7keV band with fluxes of between 10-14 and 10-13erg/cm2/s corresponds to a photon index of 1.65±0.10. Type-2 AGNs show significantly harder spectra than type-1s, which can be explained by absorption column densities of NH∼1022-23cm^-2 at the source redshifts. Fifteen sources are detected in the hard-band (2-7keV), consisting of six type-1 AGNs, six type-2 AGNs, one star, one cluster of galaxies, and one unidentified source. Type-2 AGNs make up a major part of hard X-ray populations in the 2-7keV band at a flux level of 3x10-14erg/cm2/s (2-7 keV). The redshift distributions of type-1 and type-2 AGNs suggest a lack of high luminosity (optically-defined) type-2 AGNs with intrinsic NH<1023cm^-2, n the redshift range z∼1-2 and/or with intrinsic luminosities larger than 3x1044erg/s (2-10keV at source frame). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 109 50 ASCA properties of the X-ray sources in the Lockman Hole Field
See also: J/A+A/371/833 : ROSAT Ultra Deep Survey (Lehmann+, 2001) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 2 I2 --- [IUY2001] Sequential number 3- 4 A2 --- n_[IUY2001] [* ] **: variable source 6- 12 F7.3 deg RAdeg Right ascension (J2000) 14- 20 F7.3 deg DEdeg Declination (J2000) 22- 26 F5.3 --- z ? Redshift 27- 28 A2 --- n_z [+ ] ++: Photometric redshift from Lehmann et al., 2001, Cat. J/A+A/371/833) 30- 33 A4 --- Class Classification (1) 35- 45 A11 --- OthClass Classification from other works (2) 48 A1 --- l_F1-7keV Limit flag on F1-7keV 49- 53 F5.3 10-16W/m2 F1-7keV X-flux at 1-7keV, in 10^-13^erg/s/cm^2^ (3) 55- 58 F4.2 10-16W/m2 e_F1-7keV ? rms uncertainty on F1-7keV 60 A1 --- l_F1-2keV Limit flag on F1-2keV 61- 65 F5.3 10-16W/m2 F1-2keV X-flux at 1-2keV, in 10^-13^erg/s/cm^2^ (3) 67- 71 F5.3 10-16W/m2 e_F1-2keV ? rms uncertainty on F1-2keV 73 A1 --- l_F2-7keV Limit flag on F2-7keV 74- 78 F5.3 10-16W/m2 F2-7keV X-flux at 2-7keV, in 10^-13^erg/s/cm^2^ (3) 80- 83 F4.2 10-16W/m2 e_F2-7keV ? rms uncertainty on F2-7keV 85- 88 F4.1 --- SF1-7keV Detection significance for 1-7keV band (4) 89 A1 --- --- [/] 90- 93 F4.1 --- SF1-2keV Detection significance for 1-2keV band (4) 94 A1 --- --- [/] 95- 98 F4.1 --- SF2-7keV Detection significance for 2-7keV band (4) 100-104 F5.2 --- HR Hardness ratio (5) 106-109 F4.2 --- e_HR rms uncertainty on HR
Note (1): Classification: AGN1: AGNs with ID class a-c in Schmidt et al. (1998A&A...329..495S) and Lehmann et al. (2000A&A...354...35L) AGN2: AGNs with ID class d and e in Schmidt et al. (1998A&A...329..495S) and Lehmann et al. (2000A&A...354...35L) CLUS: Cluster GAL: Galaxy GRP: STAR: Star UnID: Unidentified Note (2): PSPC-NNN : Classification given in table 4 of Hasinger et al. (1998A&A...329..482H) HRI-NNN : Classification given in table 3 of Lehmann et al. (2001, Cat. J/A+A/371/833) ASCA-NNN : ASCA classification Note (3): X-ray flux is calculated from a counting rate in the corresponding energy band,assuming a power-law spectrum with Γ=1.7 with no intrinsic absorption. Errors or upper limits are 1σ. Note (4): Detection significances for 1-7/1-2/2-7keV bands, defined as (best fit count rate)/(its 1σ statistical error). Note (5): Hardness ratio, calculated as (H-S)/(H+S) where H and S represent the SIS vignetting-corrected count rate in the 2-7keV and 1-2keV bands, respectively. Errors are 1σ.
History: From electronic version of the journal
(End) James Marcout, Patricia Bauer [CDS] 28-Sep-2001
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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