Browse
this table...

NAPEXMMCXO - North America (NGC 7000) & Pelican (IC 5070) Nebulae X-ray Source Catalog

HEASARC
Archive

Overview

This table contains some of the results from the first extensive X-ray study of the North-America and Pelican star-forming region (NGC 7000/IC 5070), with the aim of finding and characterizing the young population of this cloud. X-ray data from Chandra (four pointings) and XMM-Newton (seven pointings) were reduced and source detection algorithm applied to each image. The authors complement the X-ray data with optical and near-IR data from the IPHAS, UKIDSS, and 2MASS catalogs, and with other published optical and Spitzer IR data. More than 700 X-ray sources are detected, the majority of which have an optical or NIR counterpart. This allowed the authors to identify young stars in different stages of formation. Less than 30% of the X-ray sources are identified with a previously known young star. the authors argue that most X-ray sources with an optical or NIR counterpart, except perhaps for a few tens at near-zero reddening, are likely candidate members of the star-forming region, on the basis of both their optical and NIR magnitudes and colors, and of their X-ray properties such as spectral hardness or flux variations. They are characterized by a wide range of extinction, and sometimes near-IR excesses, both of which prevent derivation of accurate stellar parameters. The optical color-magnitude diagram suggests ages between 1-10 Myr. The X-ray members have a very complex spatial distribution with some degree of subclustering, qualitatively similar to that of previously known members. The detailed distribution of X-ray sources relative to the objects with IR excesses identified with Spitzer is sometimes suggestive of sequential star formation, especially near the 'Gulf of Mexico' region, probably triggered by the O5 star which illuminates the whole region. The authors confirm that around the O5 star no enhancement in the young star density is found, in agreement with previous results. Thanks to the precision and depth of the IPHAS and UKIDSS data used, the authors also determine the local optical-IR reddening law, and compute an updated reddening map of the entire region.

This table contains the catalog of X-ray sources, with their optical and near-IR identifications, in the NGC 7000/IC 5070 (North America/Pelican) star formation complex. The final X-ray source list comprises 721 objects, of which there are 378 ACIS detections (of which 34 have an XMM-Newton counterpart), and 343 XMM-Newton-only detection. The chosen detection threshold, corresponding to approximately one spurious detection per field, ensures that no more than approximately ten of the 721 detections are spurious. The 11 XMM-Newton and Chandra fields analyzed in this study are listed in Tables 1 and 2, respectively, of the reference paper.


Catalog Bibcode

2017A&A...602A.115D

References

X-ray survey of the North-America and Pelican star-forming complex
(NGC7000/IC5070).
    Damiani F., Pillitteri I., Prisinzano L.
    <Astron. Astrophys. 602, A115 (2017)>
    =2017A&A...602A.115D        (SIMBAD/NED BibCode)

Provenance

This table was created by the HEASARC in July 2017 based on CDS Catalog J/A+A/602/A115 file table3.dat, the list of detected X-ray sources in the North America (NGC 7000) & Pelican Nebulae (IC 5070), and file table4.dat, the list of optical and near-IR photometric information for the counterparts of these X-ray sources. It does not contain table5.dat, the list of X-ray undetected stars that have IR or H-alpha excesses.

Parameters

Source_Number
A unique sequential identification number for each X-ray source in the catalog, sorted in order of increasing J2000.0 Right Ascension.

CXO_Name
The name of the Chandra source using the 'CXOU' prefix (for Chandra X-ray Observatory Unregistered source) and the J2000.0 coordinates of the source in the standard "JHHMMSS.s+DDMMSS" format.

XMM_Name
The name of the XMM-Newton source using the 'XMMU' prefix (for XMM-Newton Unregistered source) and the J2000.0 coordinates of the source in the standard "JHHMMSS.s+DDMMSS" format.

Name
The preferred X-ray source designation. This HEASARC-created parameter defaults to the Chandra name (cxo_name) if the source was detected by Chandra; otherwise, it is set to the XMM-Newton name (xmm_name).

RA
The Right Ascension of the X-ray source in the selected equinox. This was given in J2000 decimal degree coordinates to a precision of 10-5 degrees in the original table.

Dec
The Declination of the X-ray source in the selected equinox. This was given in J2000 decimal degree coordinates to a precision of 10-5 degrees in the original table.

LII
The Galactic Longitude of the X-ray source.

BII
The Galactic Latitude of the X-ray source.

Error_Radius
The positional uncertainty of the X-ray source, in arcseconds.

Count_Rate
The count rate of the X-ray source in the 0.4-7.9 keV energy range, in ct/s (converted by the HEASARC from the ct/ks units used in the original table). The HEASARC believes that, for sources detected by both X-ray observatories, the value quoted is the Chandra count rate.

Count_Rate_Error
The uncertainty in the count rate of the X-ray source in the 0.4-7.9 keV energy range, in ct/s (converted by the HEASARC from the ct/ks units used in the original table).

ACIS_Hardness_Ratio_1
The hardness ratio HR1 for the detected Chandra ACIS source. The HEASARC believes that HR1 = (M-S)/(M+S), where M is the counts in the 1.2-2.4 keV energy band and S is the counts in the 0.4-1.2 keV energy band.

ACIS_Hardness_Ratio_2
The hardness ratio HR2 for the detected Chandra ACIS source. The HEASARC believes that HR2 = (H-M)/(H+M), where M is the counts in the 1.2-2.4 keV energy band and H is the counts in the 2.4-7.9 keV energy band.

XMM_Hardness_Ratio_1
The hardness ratio HR1 for the detected XMM-Newton EPIC source. The HEASARC believes that HR1 = (M-S)/(M+S), where M is the counts in the 1.2-2.4 keV energy band and S is the counts in the 0.4-1.2 keV energy band.

XMM_Hardness_Ratio_2
The hardness ratio HR2 for the detected XMM-Newton EPIC source. The HEASARC believes that HR2 = (H-M)/(H+M), where M is the counts in the 1.2-2.4 keV energy band and H is the counts in the 2.4-7.9 keV energy band.

Log_Lx
The logarithm of the X-ray luminosity for the source, in erg s-1, presumably in the 0.4-7.9 keV energy range and assuming a distance of 560 pc to the star-formation complex.

Imag
The magnitude in the i band of the optical counterpart to the X-ray source, taken from IPHAS (Drew et al. 2005, MNRAS, 362, 753).

RI_Color
The color index r-i of the optical counterpart to the X-ray source, taken from IPHAS (Drew et al. 2005, MNRAS, 362, 753).

R_Halpha_Color
The color index r-Halpha of the optical counterpart to the X-ray source, taken from IPHAS (Drew et al. 2005, MNRAS, 362, 753).

Jmag
The magnitude in the J band of the infrared counterpart to the X-ray source, taken from UKIDSS (Lawrence et al. 2007, MNRAS, 379, 1599), else from 2MASS.

Hmag
The magnitude in the H band of the infrared counterpart to the X-ray source, taken from UKIDSS (Lawrence et al. 2007, MNRAS, 379, 1599), else from 2MASS.

Kmag
The magnitude in the K band of the infrared counterpart to the X-ray source, taken from UKIDSS (Lawrence et al. 2007, MNRAS, 379, 1599), else from 2MASS.

IR_Excess_Flag
This Boolean flag parameter is set to 'Y' to indicate that the star has a greater than 4-sigma NIR excess in the (J-H) vs. (H-K) plane compared to a fiducial sequence, as discussed in Section 5.3 and Figure 10 of the reference paper.

Halpha_Emission_Flag
This Boolean flag parameter is set to 'Y' to indicate that the star has a greater than 4-sigma excess in the (r-Halpha) vs. (r-i) plane (indicating the presence of Halpha emission) compared to a fiducial sequence, as discussed in Section 5.2 and Figure 9 of the reference paper.

RGS2011_Source_Number
The source number of the star in the catalog of Rebull et al. (2011, ApJS, 193, 25).


Contact Person

Questions regarding the NAPEXMMCXO database table can be addressed to the HEASARC User Hotline.
Page Author: Browse Software Development Team
Last Modified: Tuesday, 11-Jul-2017 13:09:54 EDT