This table contains some of the results from a Chandra/ACIS-I observations of the massive ~ 13-14 Myr-old cluster, h Persei, part of the famous Double Cluster (h and Chi Persei) in Perseus. Combining the list of 330 Chandra-detected sources with new optical/IR photometry and optical spectroscopy reveals ~ 165 X-ray bright stars with V <~ 23. Roughly 142 have optical magnitudes and colors consistent with cluster membership. The observed distribution of X-ray luminosity L_x peaks at L_x ~ 10^30.3 erg s^-1 and likely traces the bright edge of a far larger population of ~ 0.4-2 M_sun X-ray active stars. From a short list of X-ray active stars with IRAC 8-micron excess from warm, terrestrial zone dust, the authors derive a maximum X-ray flux incident on forming terrestrial planets. Although there is no correlation between X-ray activity and IRAC excess, the fractional X-ray luminosity correlates with optical colors and spectral type. By comparing the distribution of L_x/L_star versus spectral type and (V-I) in h Per with results for other 1-100 Myr-old clusters, the authors show that stars slightly more massive than the Sun (>~ 1.5 M_sun) fall out of X-ray saturation by ~ 10-15 Myr. Changes in stellar structure for >~ 1.5 M_sun stars likely play an important role in this decline of X-ray emission. Chandra observations of h Persei were taken with a 41.1 ks exposure on 2004 December 2, (Obs. ID 5407; Sequence Number 200341) with the ACIS detector (chips 0, 1, 2, 3, 6, and 7). The data were obtained in dithered, timed mode, with a frametime of 3.2 s. On-board event rejection and event telemetry was in the VFAINT mode. The field was centered on RA(2000) = 2h19m00s, Dec(2000) = 57d07'12", close to the center of h Persei from Bragg & Kenyon (2005, AJ, 130, 134) (RA(2000) = 2h18m56.4s, Dec(2000) = 57d08'25") and observed at a roll angle of 229 degrees. The data were not registered to an astrometric reference frame (e.g., Two Micron All Sky Survey, 2MASS). The ACIS-I field covers a 17' x 17' area. This table was created by the HEASARC in March 2009 based on the electronic versions of Tables 1 and 2 from the paper which were obtained from the Astronomical Journal web site. This is a service provided by NASA HEASARC .

This table contains some of the results from a Chandra ACIS observation of the stellar populations in and around the M17 H II region. The field reveals 886 sources (listed in the present table) with observed X-ray luminosities (uncorrected for absorption) between ~ 29.3 erg s^-1 < log L_X < 32.8 erg s^-1, 771 of which have stellar counterparts in infrared images. Spectral analysis results for the 598 brightest X-ray sources which have photometric significance of 2.0 or greater) are also given herein. For 546 of the X-ray sources, the fits used the "wabs(apec)" thermal plasma model in XSPEC assuming scaled 0.3 times solar photospheric abundances, while for the other 52 X-ray sources for which either the thermal model poorly described the data or required nonphysical parameters and the X-ray source was not identified with a known stellar counterpart, the fits used the "wabs(powerlaw)" model in XSPEC. In addition to the comprehensive tabulation of X-ray source properties, several other results were presented in the reference paper: 1. The X-ray luminosity function is calibrated to that of the Orion Nebula Cluster population to infer a total population of roughly 8000-10,000 stars in M17, one-third lying in the central NGC 6618 cluster. 2. About 40% of the ACIS sources are heavily obscured with A_V > 10 mag. Some are concentrated around well-studied star-forming regions -- IRS 5/UC1, the Kleinmann-Wright Object, and M17-North -- but most are distributed across the field. As previously shown, star formation appears to be widely distributed in the molecular clouds. X-ray emission is detected from 64 of the hundreds of Class I protostar candidates that can be identified by near- and mid-infrared colors. These constitute the most likely protostar candidates known in M17. 3. The spatial distribution of X-ray stars is complex: in addition to the central NGC 6618 cluster and well-known embedded groups, we find a new embedded cluster (designated M17-X), a 2 pc long arc of young stars along the southwest edge of the M17 H II region, and 0.1 pc substructure within various populations. These structures may indicate that the populations are dynamically young. 4. All (14/14) of the known O stars but only about half (19/34) of the known B0-B3 stars in the M17 field are detected. These stars exhibit the long-reported correlation between X-ray and bolometric luminosities of L_X ~ 10^-7 L_bol. While many O and early-B stars show the soft X-ray emission expected from microshocks in their winds or moderately hard emission that could be caused by magnetically channeled wind shocks, six of these stars exhibit very hard thermal plasma components (kT > 4 keV) that may be due to colliding wind binaries. More than 100 candidate new OB stars are found, including 28 X-ray detected intermediate- and high-mass protostar candidates with infrared excesses. 5. Only a small fraction (perhaps 10%) of X-ray selected high- and intermediate-mass stars exhibit K-band-emitting protoplanetary disks, providing further evidence that inner disks evolve very rapidly around more massive stars. This table was created by the HEASARC in December 2007 based on electronic versions of Tables 1, 2, 3, 4 and 5 of the reference paper which were obtained from the electronic ApJ web site. This is a service provided by NASA HEASARC .

J0045-7319 is a B star/pulsar binary in the Small Magellanic Cloud (SMC) with an orbital period of 51 days. The system is highly eccentric, with a closest approach of only 6 B-star radii, and it offers an unusual probe into massive stars in the SMC. Although similar systems exhibit strong dispersion measure (DM) variation during periastron arising from the stellar wind, observations in 1996 on the Parkes 70 cm receiver found no evidence of a wind from the B star. We propose a new set of observations on the Ultra-Wide Low-frequency receiver (UWL) designed to measure the wind. A null result will decrease the known upper limit on the B-star wind's contribution to DM by a factor of 9.

J0045-7319 is a B star/pulsar binary in the Small Magellanic Cloud (SMC) with an orbital period of 51 days. The system is highly eccentric, with a closest approach of only 6 B-star radii, and it offers an unusual probe into massive stars in the SMC. Although similar systems exhibit strong dispersion measure (DM) variation during periastron arising from the stellar wind, observations in 1996 on the Parkes 70 cm receiver found no evidence of a wind from the B star. We propose a new set of observations on the Ultra-Wide Low-frequency receiver (UWL) designed to measure the wind. A null result will decrease the known upper limit on the B-star wind's contribution to DM by a factor of 9.

J0045-7319 is a B star/pulsar binary in the Small Magellanic Cloud (SMC) with an orbital period of 51 days. The system is highly eccentric, with a closest approach of only 6 B-star radii, and it offers an unusual probe into massive stars in the SMC. Although similar systems exhibit strong dispersion measure (DM) variation during periastron arising from the stellar wind, observations in 1996 on the Parkes 70 cm receiver found no evidence of a wind from the B star. We propose a new set of observations on the Ultra-Wide Low-frequency receiver (UWL) designed to measure the wind. A null result will decrease the known upper limit on the B-star wind's contribution to DM by a factor of 9.

This table contains the catalog of high Galactic-latitude (|b| > 10^o) X-ray sources detected in the first 37 months of data accumulation of the Monitor of All-sky X-ray Image/Gas Slit Camera (MAXI/GSC). To achieve the best sensitivity, the authors developed a background model of the GSC that well reproduced the data based on the detailed on-board calibration. Source detection was performed through image fits with a Poisson likelihood algorithm. The catalog contains 500 objects detected with significances >= 7 in the 4-10 keV band. The limiting sensitivity is ~7.5 x 10^-12 erg cm^-2 s^-1 ( ~0.6 mCrab) in the 4-10 KeV band for 50% of the survey area, which is the highest ever achieved in an all-sky survey mission covering this energy band. In their paper, the authors summarize the statistical properties of the catalog and results from cross-matching with the Swift/BAT 70-month catalog (BAT70), the meta-catalog of X-ray detected clusters of galaxies (MCXC), and the MAXI/GSC 7-month catalog (GSC7). This catalog lists the source name (2MAXI), the position and its error, the detection significances and fluxes in the 4-10 keV and 3-4 keV bands, the hardness ratio, and the basic information on the likely counterpart (the latter available for 296 of the sources). This table was created by the HEASARC in September 2013 based on the electronic version of Table 1 from the reference paper which was obtained from The ApJS web site. This is a service provided by NASA HEASARC .