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.
<Astron. Astrophys. 566, A115 (2014)>
=2014A&A...566A.115D 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 D25 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 D25 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 D25 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