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CHANTYPGPR - Chandra Typical Galactic Plane Region Point Source Catalog |
HEASARC Archive |
Following up the Chandra observation, the authors performed a near-infrared (NIR) survey with SofI at ESO/NTT. Almost all the soft X-ray sources have been identified in the NIR, and their spectral types are consistent with main-sequence stars, suggesting that most of them are nearby X-ray-active stars. On the other hand, only 22% of the hard sources had near-IR counterparts, which are presumably Galactic. From X-ray and near-IR spectral study, they are most likely to be quiescent cataclysmic variables.
Chandra deep X-ray observation of a typical galactic plane region and near-infrared identification. Ebisawa K., Tsujimoto M., Paizis A., Hamaguchi K., Bamba A., Cutri R., Kaneda H., Maeda Y., Sato G., Senda A., Ueno M., Yamauchi S., Beckmann V., Courvoisier T.J.-L., Dubath P., Nishihara E. <Astrophys. J., 635, 214-242 (2005)> =2005ApJ...635..214E
Sequence_Number
A running sequential identification number in order of
increasing J2000 Right Ascension. This can be used to construct an alternative
name for an X-ray source in this catalog, using the prefix '[ETP2005] {X} '
followed by the sequence number of the source.
Name
The recommended designation for the X-ray source, using the
prefix 'CXOGPE J' (for Chandra X-ray Observatory, Galactic Plane, Ebisawa')
and the truncated J2000 coordinates of the source.
Source_Flag
This parameter is a flag for the X-ray source, where 'T' means
that the source shows significant time variation, whereas 'E' means that the
source is extended.
AO
The Chandra Announcement of Opportunity Cycle in which the source was
detected: 1 for the AO-1 observation which was carried out in 2000 February
25 (obsid 900021) and 2 for the AO-2 observation carried out in 2001 May 20
(obsid 900125).
RA
The Right Ascension of the X-ray source in the selected equinox. This
was given in J2000 coordinates to a precision of 0.01 seconds of time in the
originating table.
Dec
The Declination of the X-ray source in the selected equinox. This
was given in J2000 coordinates to a precision of 0.1 arcseconds in the
originating table.
LII
The Galactic Longitude of the X-ray source.
BII
The Galactic Latitude of the X-ray source.
Error_Radius
The positional error of the X-ray source, in arcseconds.
This is the statistical error calculated by wavdetect, and does not include
any systematic errors.
FB_Count_Rate_SNR
The significance of the X-ray source in the total
0.5 - 8.0 keV band, in multiples of sigma.
SB_Count_Rate_SNR
The significance of the X-ray source in the soft
0.5 - 3.0 keV band, in multiples of sigma.
HB_Count_Rate_SNR
The significance of the X-ray source in the hard
3.0 - 8.0 keV band, in multiples of sigma.
FB_Count_Rate
The normalized count rate of the X-ray source in the
total band (0.5 - 8.0 keV), in counts per second. This is the count rate
expected if the source had been located at the ACIS-I aim point (the
on-axis direction) and observed for a 100 ksec exposure.
SB_Count_Rate
The normalized count rate S of the X-ray source in the
soft band (0.5 - 3.0 keV), in counts per second. This is the count rate
expected if the source had been located at the ACIS-I aim point (the
on-axis direction) and observed for a 100 ksec exposure.
HB_Count_Rate
The normalized count rate H of the X-ray source in the
hard band (3.0 - 8.0 keV), in counts per second. This is the count rate
expected if the source had been located at the ACIS-I aim point (the
on-axis direction) and observed for a 100 ksec exposure.
Hardness_Ratio
The spectral hardness ratio, (H-S)/(H+S), of the X-ray
source.
Hardness_Ratio_Error
The uncertainty in the spectral hardness ratio.
SB_Flux
The flux of the X-ray source in the `standard' soft band (0.5 - 2
keV), in erg/s/cm^2. Notice that the definition of the bands for the fluxes
and count rates are slightly different. The technique with which the
fluxes were calculated and the adopted spectral model parameters are
discussed in Section 3.2 of the published paper.
HB_Flux
The flux of the X-ray source in the `standard' hard band (2 - 10
keV), in erg/s/cm^2. Notice that the definition of the bands for the fluxes
and count rates are slightly different. The technique with which the
fluxes were calculated and the adopted spectral model parameters are
discussed in Section 3.2 of the published paper.
Near_IR_Name
The near-IR counterpart to the X-ray source which is
within 1" from the Chandra position, either from follow-up observations
made with the SofI infrared camera on the New Technology Telescope (NTT)
at the European Southern Observatory (ESO), or, for Chandra sources outside
of the SofI fields, the 2MASS Survey. A near-IR name of the form 'SNNNNNN'
indicates a SofI ID while one of the form 'JHHMMSSss+DDMMSSs' means a 2MASS
ID. A value of 'No' means that the source is in the SOFI field of view,
but that there are no SOFI counterparts, while a value of 'OoF' means that
the source is out of the SOFI field, and has no 2MASS counterparts.
Notice that, given the SofI source number density of ~0.03 sources per
square arcsecond and the 1" arcsecond matching radius used, there is a 10%
chance that any Chandra source will have an accidental SofI counterpart.
Offset
The positional offset between the X-ray source and the near-IR
counterpart, in arcseconds.
Jmag
The J-band magnitude of the near-IR counterpart to the X-ray source.
2MASS magnitudes are used for stars brighter than 10th magnitude, since
SofI starts to saturate for sources < 10 magnitudes (see Fig. 5 in the
published paper). A value of 99.99 indicates that the source was not detected
in this band.
Hmag
The H-band magnitude of the near-IR counterpart to the X-ray source.
2MASS magnitudes are used for stars brighter than 10th magnitude, since
SofI starts to saturate for sources < 10 magnitudes (see Fig. 5 in the
published paper). A value of 99.99 indicates that the source was not detected
in this band.
Ks_Mag
The K_s-band magnitude of the near-IR counterpart to the X-ray
source. 2MASS magnitudes are used for stars brighter than 10th magnitude,
since SofI starts to saturate for sources < 10 magnitudes (see Fig. 5 in the
published paper). A value of 99.99 indicates that the source was not detected
in this band.