J/A+A/566/A115 XMM sources in NGC1512/1510 (Ducci+, 2014) ================================================================================ XMM-Newton observation of the interacting galaxies NGC 1512 and NGC 1510. Ducci L., Kavanagh P.J., Sasaki M., Koribalski B.S. =2014A&A...566A.115D ================================================================================ ADC_Keywords: Galaxies, nearby ; X-ray sources ; Cross identifications Keywords: galaxies: individual: NGC1512 - X-rays: galaxies - galaxies: individual: NGC1510 Abstract: The galaxy NGC1512 is interacting with the smaller galaxy NGC1510 and shows a peculiar morphology, characterised by two extended arms immersed in an HI disc whose size is about four times larger than the optical diameter of NGC1512. For the first time we performed a deep X-ray observation of the galaxies NGC1512 and NGC1510 with XMM-Newton to gain information on the population of X-ray sources and diffuse emission in a system of interacting galaxies. We identified and classified the sources detected in the XMM-Newton field of view by means of spectral analysis, hardness-ratios calculated with a Bayesian method, X-ray variability, and cross-correlations with catalogues in optical, infrared, and radio wavelengths. We also made use of archival Swift (X-ray) and Australia Telescope Compact Array (radio) data to better constrain the nature of the sources detected with XMM-Newton. We detected 106 sources in the energy range of 0.2-12keV, out of which 15 are located within the D_25_ regions of NGC1512 and NGC1510 and at least six sources coincide with the extended arms. We identified and classified six background objects and six foreground stars. We discussed the nature of a source within the D_25_ ellipse of NGC1512, whose properties indicate a quasi-stellar object or an intermediate ultra-luminous X-ray source. Taking into account the contribution of low-mass X-ray binaries and active galactic nuclei, the number of high-mass X-ray binaries detected within the D_25_ region of NGC1512 is consistent with the star formation rate obtained in previous works based on radio, infrared optical, and UV wavelengths. We detected diffuse X-ray emission from the interior region of NGC1512 with a plasma temperature of kT=0.68(0.31-0.87)keV and a 0.3-10keV X-ray luminosity of 1.3E+38erg/s, after correcting for unresolved discrete sources. Description: We analyzed XMM-Newton data of NGC1512/1510. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file tableb1.dat 126 106 NGC1512/1510 sources detected by XMM-Newton tableb2.dat 106 106 *NGC1512/1510 sources detected by XMM-Newton cross-correlated with optical, infrared, and radio counterparts -------------------------------------------------------------------------------- Note on tableb2.dat: For each source the identification proposed by the respective authors and our classification are given. -------------------------------------------------------------------------------- See also: B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2012) Byte-by-byte Description of file: tableb1.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq Sequential number 5- 6 I2 h RAh Right ascension (J2000) 8- 9 I2 min RAm Right ascension (J2000) 11- 15 F5.2 s RAs Right ascension (J2000) 17 A1 --- DE- Declination sign (J2000) 18- 19 I2 deg DEd Declination (J2000) 21- 22 I2 arcmin DEm Declination (J2000) 24- 27 F4.1 arcsec DEs Declination (J2000) 29- 32 F4.2 arcsec ePos Positional error 34- 39 F6.4 ct/s CR ? count rate in (0.2-12keV) 41- 46 F6.4 ct/s e_CR ? rms uncertainty on CR 48- 54 F7.2 --- L ? Likelihood 56- 60 F5.2 --- HR1 Hardness ratio 0.2/0.5/1, (R2-R1)/(R2+R1) (1) 62 A1 --- --- [+] 63- 66 F4.2 --- E_HR1 Upper uncertainty on HR1 68 A1 --- --- [-] 69- 72 F4.2 --- e_HR1 Lower uncertainty on HR1 74- 78 F5.2 --- HR2 Hardness ratio 0.5/1/2, (R3-R2)/(R3+R2) (1) 80 A1 --- --- [+] 81- 84 F4.2 --- E_HR2 Upper uncertainty on HR2 86 A1 --- --- [-] 87- 90 F4.2 --- e_HR2 Lower uncertainty on HR2 92- 96 F5.2 --- HR3 Hardness ratio 1/2/4.5, (R4-R3)/(R4+R3) (1) 98 A1 --- --- [+] 99-102 F4.2 --- E_HR3 Upper uncertainty on HR3 104 A1 --- --- [-] 105-108 F4.2 --- e_HR3 Lower uncertainty on HR3 110-114 F5.2 --- HR4 Hardness ratio 2/4.5/12, (R5-R4)/(R5+R4) (1) 116 A1 --- --- [+] 117-120 F4.2 --- E_HR4 Upper uncertainty on HR4 122 A1 --- --- [-] 123-126 F4.2 --- e_HR4 Lower uncertainty on HR4 -------------------------------------------------------------------------------- Note (1): HRi = (Ri+1 - Ri)/(Ri+1 + Ri), where the bands are: R1 = 0.2-0.5keV R2 = 0.5-1keV R3 = 1-2keV R4 = 2-4.5keV R5 = 4.5-12keV -------------------------------------------------------------------------------- Byte-by-byte Description of file: tableb2.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 3 I3 --- Seq Sequential number 5- 16 A12 --- USNO-B1 USNO-B1 (I/284) identification 18- 33 A16 --- 2MASS 2MASS (II/246) identification 35- 56 A22 --- Opt Optical identification 59- 87 A29 --- Radio Radio identification 90-109 A20 --- Class Classification -------------------------------------------------------------------------------- Acknowledgements: Lorenzo Ducci, ducci(at)astro.uni-tuebingen.de History: * 23-Jun-2014: Original version * 15-Jul-2014: units of X-ray counts fixed (originally dt/ks, actually ct/s) ================================================================================ (End) Patricia Vannier [CDS] 23-Jun-2014