All MAST catalog holdings are available via a ConeSearch endpoint. The Third Reference Catalog of Bright Galaxies (RC3) by G. and A. de Vaucouleurs, H.G. Corwin, R.J. Buta, G. Paturel, and P. Fouque. is included as held in a MAST local copy.All available missions are listed at http://archive.stsci.edu/vo/mast_services.html.

This database table contains the Third Catalog of Emission-Line Stars of the Orion Population (Herbig and Bell (1988)) which lists 735 pre-main sequence stars, members of the Orion Population, that have been observed with slit spectrographs or at equivalent resolution. It is intended to replace the Second Catalog of Herbig and Rao (1972). It gives accurate coordinates (many determined especially for this Catalog); light ranges for known variables; UBVRI data near maximum light; references to ultraviolet, X-ray, and radio observations, and to light curves; value of v sin i and the radial velocity when known; spectral type; equivalent width of the H-alpha emission line; references to spectral reproductions or scans and spectroscopic studies and to identification charts; and a classification (as a T Tau star, FU Ori object, etc.). This is a service provided by NASA HEASARC .

The authors have built a catalog of 219 Fanaroff and Riley class I edge-darkened radio galaxies (FR Is), called FRICAT, that is selected from a published sample and obtained by combining observations from the NVSS, FIRST, and SDSS surveys. They included in the catalog the sources with an edge-darkened radio morphology, redshift <= 0.15, and extending (at the sensitivity of the FIRST images) to a radius r larger than 30 kpc from the center of the host. The authors also selected an additional sample (sFRICAT) of 14 smaller (10 < r < 30 kpc) FR Is, limiting to z < 0.05. The hosts of the FRICAT sources are all luminous (-21 >~ M_r >~ 24), red early-type galaxies with black hole masses in the range 10⁸ <~ M_BH <~ 3 x 10⁹ solar masses); the spectroscopic classification based on the optical emission line ratios indicates that they are all low excitation galaxies. Sources in the FRICAT are then indistinguishable from the FR Is belonging to the Third Cambridge Catalogue of Radio Sources (3C) on the basis of their optical properties. Conversely, while the 3C-FR Is show a strong positive trend between radio and [O III] emission line luminosity, these two quantities are unrelated in the FRICAT sources; at a given line luminosity, they show radio luminosities spanning about two orders of magnitude and extending to much lower ratios between radio and line power than 3C-FR Is. The authors' main conclusion is that the 3C-FR Is represent just the tip of the iceberg of a much larger and diverse population of FR Is. This HEASARC table contains both the 219 radio galaxies in the main FRICAT sample listed in Table B.1 of the reference paper and the 14 radio galaxies in the additional sFRICAT sample listed in Table B.2 of the reference paper. To enable users to distinguish from which sample an entry has been taken, the HEASARC created a parameter galaxy_sample which is set to 'M' for galaxies from the main sample, and to 'S' for galaxies from the supplementary sFRICAT sample. Throughout the paper, the authors adopted a cosmology with H₀ = 67.8 km s^-1 Mpc^-1, Omega_M = 0.308, and Omega_Lambda = 0.692 (Planck Collaboration XIII 2016). This table was created by the HEASARC in February 2017 based on electronic versions of Tables B.1 and B.2 that were obtained from the Astronomy & Astrophysics website. This is a service provided by NASA HEASARC .

The Lynds' Catalog of Bright Nebulae lists the coordinates of the center of the cloud, the dimensions of the nebulae as measured on the photograph on which it appeared at its brightest, the area of nebulosity in square degrees, color as compared between the blue and red Palomar plates, a brightness index on a scale from 1 to 6, an identification number that indicates the complexity of the nebulosity, and a cross reference to NGC (Cat. ), Index Catalogue (IC), Sharpless (1959) Catalogue of HII Regions (Cat. ), Cederblad (1956) Catalogue of Diffuse Galactic Nebulae, and Dorschner and Gurtler (1963). This database originates from the NASA/ADC CD-ROM "Selected Astronomical Catalogs Vol. 1", dated 09-July-1992. The CDS made several corrections to this and added the LBN sequence number. The current HEASARC version of this table was revised in February 2001 and is based on the CDS version. This is a service provided by NASA HEASARC .

This table contains some of the results from the first X-ray study of Collinder 261 (Cr 261), which at an age of 7 Gyr is one of the oldest open clusters known in the Galaxy. This observation with the Chandra X-Ray Observatory was aimed at uncovering the close interacting binaries in Cr 261, and reached a limiting X-ray luminosity of L_X ~ 4 x 10²⁹ erg s^-1 (0.3-7 keV) for stars in the cluster. The authors detected 107 sources within the cluster half-mass radius r_h, and they estimate that among the sources with L_X >~ 10³⁰ erg s^-1, about 26 are associated with the cluster. They identify a mix of active binaries and candidate active binaries, candidate cataclysmic variables, and stars that have "straggled" from the main locus of CR 261 in the color-magnitude diagram. Based on a deep optical source catalog of the field, the authors estimate that Cr 261 has an approximate mass of 6500 M_sun, roughly the same as the old open cluster NGC 6791. The X-ray emissivity of Cr 261 is similar to that of other old open clusters, supporting the trend that they are more luminous in X-rays per unit mass than old populations of higher (globular clusters) and lower (the local neighborhood) stellar density. This implies that the dynamical destruction of binaries in the densest environments is not solely responsible for the observed differences in X-ray emissivity. Cr 261 was observed with the Advanced CCD Imaging Spectrometer (ACIS) on board Chandra starting 2009 November 9 14:50 UTC, for a total exposure time of 53.8 ks (ObsID 11308). The observation was made in Very Faint, Timed exposure mode, with a single frame exposure time of 3.2 s. Kharchenko et al. (2013, A&A, 558, A53) estimate that the radius of Cr 261 is ~ 14.1 arcminutes. This is considerably larger than a single ACIS chip (8 4 x 8 4 arcminute²) and therefore the authors placed the center of the cluster (J2000.0 RA = 12^h 38^m 06.0^s, Dec = -68^o 22' 01" according to Kharchenko et al. 2013) close to the I3 aimpoint so that a larger contiguous part of the cluster could be imaged (see Figure 1 in the reference paper). The CCDs used were I0, I1, I2, and I3 from the ACIS-I array, and S2 and S3 from the ACIS-S array. The authors limited the X-ray analysis to the data from chips I0, I1, I2, and I3. The S2 and S3 chips lie far from the I3 aimpoint, giving rise to large positional errors on any sources detected on them. Such large errors make it hard to identify optical counterparts, and thus to classify the sources. The authors retrieved optical images of Cr 261 in the B and V bands from the ESO public archive. These data were taken as part of the ESO Imaging Survey (EIS; program ID 164.O-0561). The observations of Cr 261 were made using the Wide Field Imager (WFI), mounted on the 2.2 m MPG/ESO telescope at La Silla, Chile. After correcting the X-ray source positions for the (almost negligible) boresight correction (0.06 =/- 0.07 arcseconds in RA and 0.09 +/- 0.08 arcseconds in Dec), the authors matched their X-ray source list with the entire optical source list, using 95% match radii. For 89 unique X-ray sources, they found 124 optical matches; of the latter, 104 are present in both the V and B images, while for 20 there is only a V or B detection. The authors also inspected the area around each X-ray source in the WFI images by eye, and discovered that five more X-ray sources have candidate optical counterparts that are saturated and therefore missing from their optical catalog. Finally, they added to the list of candidate counterparts six optical sources that lay just outside the 95% match radius, but inside the 3-sigma radius. In total, 98 of the 151 unique X-ray sources were thus matched to one or more optical sources. This HEASARC table contains the list of the 135 optical counterparts to 98 of the 151 X-ray sources from Table 2 of the reference paper.