This table comprises the Sternberg Astronomical Institute (SAI) Catalog of Supernovae. This version contains data on 2991 extragalactic supernovae (SNe) which were discovered from 1885 until December 12, 2004 and on their host galaxies. Data for host galaxies were compiled from the following catalogues: (1) RC3 (de Vaucouleurs et al. 1991, Cat. ); (2) UGC (Nilson 1973. Cat. ); (3) PGC (Paturel et al. 1989, Cat. ); (4) MCG (Vorontsov-Velyaminov et al. 1962-1968, Cat. , ); (5) ESO (Lauberts 1982, Cat. ); (6) CfA (Huchra et al. 1994, see Cat ), and (7) from van den Bergh (1994, Cat. ). The main source of morphological types, major diameters and axial ratios was the RC3; the data from other sources were reduced to the system of RC3. Photographic magnitudes of galaxies were adopted from the UGC and the PGC together with individual data from the literature. The sources of recession velocities or cz values were the RC3, the CfA, the PGC and IAU Circulars. Position angles were taken from the RC3, UGC and the ESO catalogues, and inclination angles were mainly derived from data in RC3 according to Holmberg (1958MeLu2.136....1H). Some data for SNe and host galaxies were adopted from the GCVS (Samus et al. 1995, Cat. ). This table was created by the HEASARC in June 2005 based on CDS table II/256/sn.dat. Notice that the number of entries (2991) is more than the number of 2780 mentioned in the published reference: this is apparently due to the fact that the CDS table contains supernovae as recent as December 12, 2004, while the latter is complete only until January 6, 2004. This is a service provided by NASA HEASARC .

The Spitzer Survey of Stellar Structure in Galaxies (S4G) is a volume-, magnitude-, and size-limited survey of over 2300 nearby galaxies at 3.6 and 4.5 microns. This is an extremely deep survey reaching an unprecedented 1 sigma surface brightness limit of μ3.6(AB) = 27 mag arcsec-2. This translates to a stellar surface density of << 1 Msun pc-2.The S4G Catalog provides photometry and model parameters derived from the IRAC images, as well as a link to the summary and data access page for each galaxy and a variety of quantities taken from previously published work.

The Swift Active galactic nucleus (AGN) and Cluster Survey (SACS) uses 125 deg² of Swift X-ray Telescope (XRT) serendipitous fields with variable depths surrounding gamma-ray bursts to provide a medium depth (4 x 10^-15 erg cm^-2 s^-1) and medium area survey filling the gap between deep, narrow Chandra/XMM-Newton surveys and wide, shallow ROSAT surveys. In the reference paper, a catalog of 22,563 point sources and 442 extended sources, and the number counts of the AGN and galaxy cluster populations are presented. SACS provides excellent constraints on the AGN number counts at the bright end with negligible uncertainties due to cosmic variance, and these constraints are consistent with previous measurements. The authors use Wide-field Infrared Survey Explorer (WISE) mid-infrared(MIR) colors to classify the sources. For AGNs, they can roughly separate the point sources into MIR-red and MIR-blue AGNs, finding roughly equal numbers of each type in the soft X-ray band (0.5-2.0 keV), but fewer MIR-blue sources in the hard X-ray band (2-8 keV). The cluster number counts, with 5% uncertainties from cosmic variance, are also consistent with previous surveys but span a much larger continuous flux range. Deep optical or IR followup observations of this cluster sample will significantly increase the number of higher redshift (z > 0.5) X-ray-selected clusters. This HEASARC table contains the list of 442 Swift XRT extended sources which were detected in the soft X-ray band image (0.5-2 keV) and contained in Table 4 of the reference paper. The authors defined the extended source catalog as those sources with S/N >= 4 and a minimum net photon count of 20 that are more than 3 sigma from the mean size of point sources for both their off-axis angle and S/N. The authors consider these extended sources to be candidate clusters of galaxies. This table was created by the HEASARC in July 2015 based on an electronic version of Table 4 of the reference paper, the list of Swift XRT extended sources detected in the soft X-ray (0.5-2 keV) band, which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .

The Swift Active galactic nucleus (AGN) and Cluster Survey (SACS) uses 125 deg² of Swift X-Ray Telescope (XRT) serendipitous fields with variable depths surrounding gamma-ray bursts to provide a medium depth (4 x 10^-15 erg cm^-2 s^-1) and medium area survey filling the gap between deep, narrow Chandra/XMM-Newton surveys and wide, shallow ROSAT surveys. In the reference paper, a catalog of 22,563 point sources and 442 extended sources, and the number counts of the AGN and galaxy cluster populations are presented. SACS provides excellent constraints on the AGN number counts at the bright end with negligible uncertainties due to cosmic variance, and these constraints are consistent with previous measurements. The authors use Wide-field Infrared Survey Explorer (WISE) mid-infrared(MIR) colors to classify the sources. For AGNs, they can roughly separate the point sources into MIR-red and MIR-blue AGNs, finding roughly equal numbers of each type in the soft X-ray band (0.5-2.0 keV), but fewer MIR-blue sources in the hard X-ray band (2-8 keV). The cluster number counts, with 5% uncertainties from cosmic variance, are also consistent with previous surveys but span a much larger continuous flux range. Deep optical or IR followup observations of this cluster sample will significantly increase the number of higher redshift (z > 0.5) X-ray-selected clusters. This HEASARC table contains the list of 22,563 Swift XRT point sources which were detected in the total X-ray band image (0.2-10 keV) using wavdetect with a false positive threshold of 10^-6 (contained in Table 1 of the reference paper). The authors consider these sources to be AGN candidates. This table was created by the HEASARC in June 2015 based on an electronic version of Table 1 of the reference paper, the list of Swift XRT point sources detected in the total X-ray (0.2-10 keV) band, which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .

This table contains a catalog of galaxy clusters selected via their Sunyaev-Zel'dovich (SZ) effect signature from 2500 deg² of South Pole Telescope (SPT) data. This work represents the complete sample of clusters detected at high significance in the 2500 deg² SPT-SZ survey, which was completed in 2011. A total of 677 (409) cluster candidates are identified above a signal-to-noise threshold xi of 4.5 (5.0). Ground- and space-based optical and near-infrared (NIR) imaging confirms overdensities of similarly colored galaxies in the direction of 516 (or 76%) of the xi > 4.5 candidates and 387 (or 95%) of the xi > 5 candidates; the measured purity is consistent with expectations from simulations. Of these confirmed clusters, 415 were first identified in SPT data, including 251 new discoveries reported in this work. The authors estimate photometric redshifts for all candidates with identified optical and/or NIR counterparts; they additionally report redshifts derived from spectroscopic observations for 141 of these systems. The mass threshold of the catalog is roughly independent of redshift above z ~ 0.25 leading to a sample of massive clusters that extends to high redshift. The median mass of the sample is M_500c(rho_crit) ~ 3.5x10¹⁴ M_sun h₇₀^-1, the median redshift is z_med = 0.55, and the highest-redshift systems are at z > 1.4. The combination of large redshift extent, clean selection, and high typical mass makes this cluster sample of particular interest for cosmological analyses and studies of cluster formation and evolution. The South Pole Telescope (SPT) is a 10m diameter telescope located at the National Science Foundation Amundsen-Scott South Pole station in Antarctica. From 2008 to 2011 the telescope was used to conduct the SPT-SZ survey, a survey of ~ 2500 deg² of the southern sky at 95, 150, and 220 GHz. The survey covers a contiguous region from 20h to 7h in Right Ascension and -65 to -40 degrees in Declination (see, e.g., Figure 1 in Story et al. 2013, ApJ, 779, 86) and was mapped to depths of approximately 40, 18, and 70 microK-arcmin at 95, 150, and 220 GHz, respectively. The authors use optical and in some cases NIR imaging (Blanco Telescope, Magellan/Baade, Magellan/Clay, Swope, MPG/ESO, New Technology Telescope, Spitzer, WISE) to confirm candidates as clusters and to obtain redshifts for confirmed systems (see section 4 of the reference paper for more details). They have also used a variety of facilities to obtain spectroscopic observations of the SPT clusters (including VLT/FORS2 & Gemini/GMOS-S). This HEASARC table contains the total of 677 cluster candidates which were identified above a signal-to-noise threshold of xi = 4.5 in the 2500 deg² SPT-SZ survey. This table was created by the HEASARC in March 2015 based on an electronic version of Table 4 from the reference paper which was obtained from the CDS as their catalog J/ApJS/216/27 file table4.dat. This is a service provided by NASA HEASARC .

Recent broad-band 34- and 44-GHz radio continuum observations of the Galactic center have revealed 41 massive stars identified with near-IR (NIR) counterparts, as well as 44 proplyd candidates within 30 arcseconds of Sgr A*. Radio observations obtained in 2011 and 2014 have been used to derive proper motions of eight young stars near Sgr A*. The accuracy of proper motion estimates based on NIR observations by Lu et al. (2009, ApJ, 690, 1463) and Paumard et al. (2006, ApJ, 643, 1011) have been investigated by using their proper motions to predict the 2014 epoch positions of NIR stars and comparing the predicted positions with those of radio counterparts in the 2014 radio observations. Predicted positions from Lu et al. show an rms scatter of 6 milliarcseconds (mas) relative to the radio positions, while those from Paumard et al. show rms residuals of 20 mas. In the reference paper, the authors also determine the mass-loss rates of 11 radio stars, finding rates that are on average ~2 times smaller than those determined from model atmosphere calculations and NIR data. Clumpiness of ionized winds would reduce the mass loss rate of WR and O stars by additional factors of 3 and 10, respectively. One important implication of this is a reduction in the expected mass accretion rate onto Sgr A* from stellar winds by nearly an order of magnitude to a value of a few x 10^-7 solar masses per year. The authors carried out A-array observations of the Galactic center region (VLA program 14A-232) in the Ka (9 mm, 34.5 GHz) band on 2014 March 9 in which they detected 318 compact radio sources within 30" of Sgr A*. The authors searched for NIR counterparts to these compact radio sources using high-angular resolution AOs-assisted imaging observations acquired with the VLT/NACO. A K_s-band (central wavelength 2.18 micron) image was obtained in a rectangular dither pattern on 2012 September 12. L'-band (3.8 micron) observations were obtained during various observing runs between 2012 June and September. The authors found that 45 of the compact radio sources had stellar counterparts in the K_s and L' bands. This table contains the details of the 318 compact radio sources detected at 34.5 GHz and their NIR counterparts. This table was created by the HEASARC in November 2016 based on CDS table J/ApJ/809/10, file table6.dat. This is a service provided by NASA HEASARC .