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J/A+A/466/31        The HELLAS2XMM survey. VIII              (Cocchia+, 2007)

The HELLAS2XMM survey: VIII. Optical identifications of the extended sample. Cocchia F., Fiore F., Vignali C., Mignoli M., Brusa M., Comastri A., Feruglio C., Bald A., Carangelo N., Ciliegi P., D'Elia V., La Franca F., Maiolino R., Matt G., Molendi S., Perola G.C., Puccetti S. <Astron. Astrophys. 466, 31 (2007)> =2007A&A...466...31C
ADC_Keywords: X-ray sources ; Cross identifications Keywords: X-ray: background - surveys - galaxies: active - galaxies: evolution Abstract: We present the results of the photometric and spectroscopic identification of 110 hard X-ray selected sources from 5 additional XMM-Newton fields, nearly doubling the original HELLAS2XMM sample. Their 2-10keV fluxes cover the range 6x10-15-4x10-13erg/cm2/s and the total area surveyed is 0.5 square degree at the bright flux limit. We spectroscopically identified 59 new sources, bringing the spectroscopic completeness of the full HELLAS2XMM sample to almost 70% over a total area of 1.4 square degree. We found optical counterparts for 214 out of the 232 X-ray sources of the full sample down to R∼25. We measured the flux and luminosity of the [OIII]5007 emission line for 59 of these sources. Description: We have obtained relatively deep (exposure time 3-15m per image, limiting magnitude R=24-25) optical images for the majority of the sources in the 5 XMM-Newton fields, using EFOSC2 at the ESO 3.6m telescope, FORS1 at VLT, and DOLORES at the TNG. Optical spectra of 59 out of the 110 sources with optical counterparts brighter than R=24 were obtained using EFOSC2 at the ESO 3.6m telescope, DOLORES at the TNG and FORS1 at the VLT/UT1 during 6 observing runs performed between August 2001 and March 2004. A total of 12 nights at the 3.6m and TNG telescopes and 40 hours of VLT time were devoted to this program. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 118 125 The HELLAS2XMM second-source sample table3.dat 62 59 The HELLAS2XMM [OIII] sample table4.dat 34 141 IAU names for the HELLAS2XMM source sample
See also: J/A+A/409/79 : The HELLAS2XMM survey. IV. (Fiore+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 A5 --- --- [H2XMM] 7- 22 A16 --- H2XMM Source identification (JHHMMSS.s+DDMMSS) 24 A1 --- f_H2XMM [agl] Note on H2XMM (1) 26- 27 I2 h RAh X-ray right ascension (J2000) 29- 30 I2 min RAm X-ray right ascension (J2000) 32- 35 F4.1 s RAs X-ray right ascension (J2000) 37 A1 --- DE- X-ray declination sign (J2000) 38- 39 I2 deg DEd X-ray declination (J2000) 41- 42 I2 arcmin DEm X-ray declination (J2000) 44- 45 I2 arcsec DEs X-ray declination (J2000) 47- 48 I2 h RAo.h ? Optical (R band) right ascension (J2000) 50- 51 I2 min RAo.m ? Optical (R band) right ascension (J2000) 53- 56 F4.1 s RAo.s ? Optical (R band) right ascension (J2000) 58 A1 --- DEo.- ? Optical (R band) declination sign (J2000) 59- 60 I2 deg DEo.d ? Optical (R band) declination (J2000) 62- 63 I2 arcmin DEo.m ? Optical (R band) declination (J2000) 65- 66 I2 arcsec DEo.s ? Optical (R band) declination (J2000) 68- 71 F4.1 arcmin Off-axis ? Off-axis angle 73- 75 F3.1 arcsec Diff ? Separation between X-ray and optical positions 77- 82 F6.4 --- Prob ? Probability of coincidence 84- 88 F5.2 10-17W/m2 FX ? 2-10keV flux (10-14erg/cm2/s) 91- 95 F5.2 mag Rmag ? R magnitude 98-101 A4 --- Class Classification of the optical spectrum (2) 103 A1 --- n_Class [bcdef] Note on Class (1) 105-110 F6.4 --- z ? Redshift 112 A1 --- n_z [gh] Note on redshift (1) 114-118 F5.2 [10-7W] logLX ? 2-10keV luminosity
Note (1): Individual notes as follows: a = Two possible counterparts within 6" b = Broad absorption line QSO c = Two nearby objects, a type 1 AGN and an emission-line galaxy d = Tentative classification: low S/N spectrum e = Extended, emission from a group or cluster of galaxies f = Two nearby objects, a type 1 AGN and a type 2 AGN g = Aperture photometry at the position of a bright K source and photometric z (Mignoli et al., 2004A&A...418..827M) h = Near-infrared spectroscopy (Maiolino et al., 2006A&A...445..457M) l = R limiting magnitude of the optical images Note (2): Classification as follows: AGN1 = AGN type 1 AGN2 = AGN type 2 ELG = Emission Line Galaxy ETG = Early Type Galaxy * = Star
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 5 A5 --- --- [H2XMM] 7- 22 A16 --- H2XMM Source identification (JHHMMSS.s+DDMMSS) 24- 29 F6.4 --- z Redshift 31- 34 A4 --- Class Classification of the optical spectrum 36 A1 --- n_Class ? [c] Note on Class (1) 38- 42 F5.2 [10-7W] logLX 2-10keV luminosity 46- 51 F6.2 [10-3W/m2] logF[OIII] Flux at [OIII](5007) 53 A1 --- n_logF[OIII] ? [abu] Note on LogF[OIII] (1) 56- 60 F5.2 [10-7W] logL[OIII] Luminosity at [OIII](5007) 62 A1 --- n_logL[OIII] ? [abu] Note on LogL[OIII] (1)
Note (1): Individual notes as follows: a = [OIII] lines within strong telluric absorption feature at 6900Å b = [OIII] lines within strong telluric absorption feature at 7600Å c = Extended, emission from a group or cluster of galaxies u = 3 sigma upper limit
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 5 A5 --- --- [H2XMM] 7- 22 A16 --- H2XMM Source identification (JHHMMSS.s+DDMMSS) 25- 32 I08 --- IAU IAU source identification 34 A1 --- n_IAU [a] a = Sources belonging to the HELLAS2XMM 1dF sample, Cat. J/A+A/409/79
Acknowledgements: Filomena Cocchia, filomena.cocchia(at)brera.inaf.it References: Baldi et al., Paper I 2002ApJ...564..190B Comastri et al., Paper II 2002ApJ...571..771C Brusa et al., Paper III 2003A&A...409...65B Fiore et al., Paper IV 2003A&A...409...79F, Cat. J/A+A/409/79 Mignoli et al., Paper V 2004A&A...418..827M Perola et al., Paper VI 2004A&A...421..491P La Franca et al.,Paper VII 2005ApJ...635..864L Maiolino et al., Paper IX 2006A&A...445..457M
(End) Patricia Vannier [CDS] 25-Jan-2007
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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