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J/ApJS/165/173      Chandra sources in Galaxy central 150pc     (Muno+, 2006)

A Chandra catalog of X-ray sources in the central 150 pc of the Galaxy. Muno M.P., Bauer F.E., Bandyopadhyay R.M., Wang Q.D. <Astrophys. J. Suppl. Ser., 165, 173-187 (2006)> =2006ApJS..165..173M
ADC_Keywords: X-ray sources Keywords: catalogs - Galaxy: center - X-rays: general Abstract: We present the catalog of X-ray sources detected in a shallow Chandra survey of the inner 2°x0.8° of the Galaxy and in two deeper observations of the Radio Arches and Sgr B2. The catalog contains 1352 objects that are highly absorbed (NH≳4x1022cm-2) and are therefore likely to lie near the Galactic center (D∼8kpc), and 549 less absorbed sources that lie within 6kpc of Earth. Description: The central 300pcx125pc of the Galaxy has been observed on several occasions with the imaging array of the Chandra Advanced CCD Imaging Spectrometer (ACISI). The entire region was surveyed with overlapping 12ks observations (Wang et al., 2002Natur.415..148W), and one additional short observation was obtained centered on the LMXB 1E 1740.72942. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 136 1899 *Catalog of Point Sources within 2 by 0.8 degrees of the Galactic Center
Note on table2.dat: We omitted two bright, previously known LMXBs from the table (1E 1740.72942 and 2E 1743.12842), because they were badly saturated in our survey images, and their positions and properties are reported elsewhere (e.g., Marti et al. 2000A&A...363..184M; Porquet et al. 2000A&A...363..184M).
See also: B/chandra : The Chandra Archive Log (CXC, 1999-) J/ApJ/589/225 : Chandra X-ray sources toward Galactic Center (Feigelson+ 2003) J/ApJ/613/1179 : X-ray sources in Galactic Center (Muno+, 2004) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 15 A15 --- CXOGC The IAU Designation (HHMMSS.s+DDMMSS, J2000) 17- 25 F9.5 deg RAdeg Right Ascension in decimal degrees (J2000) 27- 35 F9.5 deg DEdeg Declination in decimal degrees (J2000) 37- 39 F3.1 arcsec ePos Positional uncertainty 41- 44 I4 --- ObsID Observation identifier 46- 49 F4.1 arcmin Offset Angular offset from aimpoint 51- 55 F5.1 ks ExpTime Total live time 57- 62 F6.1 ct Cnet Net (0.5-8.0 keV) counts 64- 69 F6.1 ct e_Cnet Lower uncertainty on Cnet 71- 76 F6.1 ct E_Cnet Upper uncertainty on Cnet 78- 81 F4.2 --- Prob Chance of detecting source 83- 88 F6.2 --- HR0 ?=-9.00 Soft color [2.0-3.3]/[0.5-2.0] (1) 90- 95 F6.2 --- e_HR0 ?=-9.00 Lower uncertainty on HR0 (2) 97-102 F6.2 --- E_HR0 ?=-9.00 Upper uncertainty on HR0 (3) 104-109 F6.2 --- HR2 ?=-9.00 Hard color [4.7-8.0]/[3.3-4.7] (1) 111-116 F6.2 --- e_HR2 ?=-9.00 Lower uncertainty on HR2 (2) 118-123 F6.2 --- E_HR2 ?=-9.00 Upper uncertainty on HR2 (3) 125-132 E8.1 cm-2/s Flux Photon flux (0.5-8.0kev) 134-136 A3 --- Flags [cfls -] Notes about the source (4)
Note (1): Colors are defined according to (H-L)/(H+L), where H and L are the net counts in high and low energy bands, respectively. * For the soft color, H is 2.0-3.3keV, and L is 0.5-2.0keV. * For the hard color, H is 4.7-8.0keV, and L is 3.3-4.7keV. Values are set to -9.00 if both the 90% confidence interval of both bands contain zero counts. Note (2): Values are set to -9.00 if the harder band is consistent with zero. Note (3): Values are set to -9.00 if the softer band is consistent with zero. Note (4): Sources are flagged as follows: s = if there is short-term variability within an observation l = if there was long-term variability when comparing the flux in multiple observations c = if the source was confused with its neighbors in some observations so that the photometry was computed from a region enclosing <90% of the flux in the PSF f = if the source was only detected below 2keV
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 14-Dec-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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