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Collinder 69 Cluster XMM-Newton X-Ray Point Source Catalog
This table contains some of the results from the first paper of a series devoted to the Lambda Orionis star-forming region, Orion's Head, from the X-ray perspective. The final aim of this research is to provide a comprehensive view of this complex region, which includes several distinct associations and dark clouds. The authors aim to uncover the population of the central, young star cluster Collinder 69, and in particular to find those diskless Class III pre-main sequence objects which have not been identified by previous surveys based on near- and mid-infrared searches, and to establish the X-ray luminosity function for the association. The authors have combined two exposures taken with the XMM-Newton satellite with an exhaustive data set of optical, near- and mid-infrared photometry to assess the membership of the X-ray sources based on different color-color and color-magnitude diagrams, as well as other properties, such as effective temperatures, masses and bolometric luminosities derived from spectral energy distribution fitting and comparison with theoretical isochrones. The presence of circumstellar disks is discussed using mid-infrared photometry from the Spitzer Space Telescope. This table contains the XMM-Newton X-ray point source catalog for all sources detected in the EPIC observations of the Collinder 69, East and West Fields (C69E and C69W), respectively, with maximum likelihood (ML) values > 15.0. A companion HEASARC Browse table COLL69OID contains optical and infrared data as well as membership information on counterparts to these X-ray sources. This table was created by the HEASARC in July 2011 based on the electronic versions of Tables 3 and 4 from the reference paper which were obtained from the CDS (their catalog J/A+A/526/A21 files table3.dat and table4.dat). This is a service provided by NASA HEASARC .
SCUBA Legacy Fundamental and Extended Map Object Catalogs
This table contains the SCUBA Legacy Catalogs, two comprehensive sets of source catalogs using data at 850 and 450um of the various astronomical objects obtained with the Submillimetre Common User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). The Fundamental Map Data Set contains data only where superior atmospheric opacity calibration data were available. The Extended Map Data Set contains data regardless of the quality of the opacity calibration. Each data set contains 1.2 degrees x 1.2 degrees maps at locations where data existed in the JCMT archive, imaged using the matrix inversion method. The Fundamental Data Set is composed of 1423 maps at 850um and 1357 maps at 450um. The Extended Data Set is composed of 1547 maps at 850um. Neither data set includes high sensitivity, single-chop SCUBA maps of "cosmological fields" nor solar system objects. Each data set was used to determine a respective object catalog, consisting of objects identified within the respective 850um maps using an automated identification algorithm. The Fundamental and Extended Map Object Catalogs contain 5061 and 6118 objects, respectively. Objects are named based on their respective J2000.0 position of peak 850um intensity. The catalogs provide for each object the respective maximum 850um intensity, estimates of total 850um flux and size, and tentative identifications from the SIMBAD Database. Where possible, the catalogs also provide for each object its maximum 450um intensity and total 450um flux and flux ratios. Since the goal of this project was to make maps and then catalog objects therein, all raw jiggle and scan data from SCUBA available in the JCMT archive were downloaded from the CADC in 2006 May. (Photometry and polarimetry data were ignored.) A full description of the instrumental characteristics of SCUBA was made by Holland et al. (1999MNRAS.303..659H). All maps are available at <a href="http://www3.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/community/scubalegacy/">http://www3.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/community/scubalegacy/</a> This table was created by the HEASARC in December 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/175/277">CDS catalog J/ApJS/175/277</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
Swift-INTEGRAL X-Ray (SIX) Survey Catalog
The supermassive black holes at the center of active galactic nuclei (AGNs) are surrounded by obscuring matter that can block nuclear radiation. Depending on the amount of blocked radiation, the flux from the AGN can be too faint to be detected by currently operating hard X-ray (above 15 keV) missions. At these energies, only ~1% of the intensity of the cosmic X-ray background (CXB) can be resolved into point-like sources that are AGNs. In this work, the authors address the question of undetected sources contributing to the CXB with a very sensitive and new hard X-ray survey: the Swift-INTEGRAL X-ray (SIX) survey, which is obtained with the new approach of combining the Swift/BAT and INTEGRAL/IBIS X-ray observations. The authors merge the observations of both missions, which enhances the exposure time and reduces systematic uncertainties. As a result, they obtain a new survey over a wide sky area of 6200 deg<sup>2</sup> covering the region of the North Ecliptic Pole (NEP) and extending to the contiguous Coma region that is more sensitive than the surveys of Swift/BAT or INTEGRAL/IBIS alone. Their sample comprises 113 sources having S/N ratios of above 4.8 sigma: 86 AGNs (Seyfert-like and blazars), 5 galaxies, 2 clusters of galaxies, 3 Galactic sources, 3 previously detected unidentified X-ray sources, and 14 unidentified sources. The scientific outcome from the study of the sample has been properly addressed to study the evolution of AGNs at a redshift below 0.4. The authors do not find any evolution using the 1/V<sub>max</sub> method. Their sample of faint sources is a suitable target for the new generation of hard X-ray telescopes with focusing techniques. This table was created by the HEASARC in August 2012 based on an electronic version of Table 2 from the reference paper which was obtained from the ApJS web site. This is a service provided by NASA HEASARC .
Swift/UVOT Serendipitous Source Catalog, v1.1: Observations IDs
The first version of the Swift UVOT Serendipitous Source Catalog (UVOTSSC) provides positions and magnitudes, as well as errors and upper limits of confirmed sources, for observations taken from the start of operations in 2005 until October 1st of 2010. The first version of the UVOTSSC has been produced by processing the image data obtained from the Swift Ultraviolet and Optical Telescope (UVOT). The data processing was performed at the Mullard Space Science Laboratory (MSSL, University College London, U.K.) using Swift FTOOLS from NASA's High Energy Astrophysics Software package (HEASoft-6.11), with some customizing of the UVOT packages in order to get more complete source detection and to properly apply quality flags to those sources that were detected within the UVOT image artifacts. The total number of observations with 17'x17' images used for version 1 of the catalog is 23,059, giving 6,200,016 sources in total, of which 2,027,265 have multiple entries in the source table because they have been detected in more than one observation. Some sources were only observed in one filter. The total number of entries in the source table is 13,860,568. The S/N ratio for all sources exceeds 5 in at least one UVOT filter, the rest of the filters having a S/N greater than 3. One Swift ObsID can consist of one or more images, which for this catalog have been summed, yielding the quoted total exposure times. The original UVOT images can be found in the on-line archives at MAST, and in the Swift archives at <a href="http://swift.ac.uk/">http://swift.ac.uk/</a> and at the HEASARC (<a href="http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html">http://heasarc.gsfc.nasa.gov/W3Browse/all/swiftmastr.html</a>), using the ObsID as the search key. For higher temporal resolution, the original images need to be used because the catalog data herein are summed over all of the individual images within an ObsID. The upper limits per filter for the summed images are constructed for each ObsID because the sensitivity hardly varies over the detector. Usually the images within one ObsID share the same pointing, however, whereas the quoted upper limits always apply for sources near the pointing direction given, if the images had small offsets in pointing they may not apply to sources near the edge of the summed image, which is typically about 8 arcminutes from the quoted pointing direction. U, B, V, UVW2, UVM2 and UVW1 refer to the filter bandpasses defined in the UVOT Filterwheel section of the MSSL documentation at <a href="http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html">http://www.mssl.ucl.ac.uk/www_astro/uvot/uvot_instrument/filterwheel/filterwheel.html</a>. This HEASARC table contains version 1.1 of the Swift UVOT table of observations in which the sources in the source table were detected and contains the details of 23,059 Swift UVOT observations. The HEASARC has changed the names of many of the parameters from those given in the original table. In such cases, we have listed the original names in parentheses at the end of the parameter descriptions given below. There is a related table which lists the 13,860,568 source detections that is available at the HEASARC as the SWUVOTSSC table. This table was created by the HEASARC in May 2017 based upon the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/II/339">CDS Catalog II/339</a> file summary.dat. This is a service provided by NASA HEASARC .
Cep B/OB3 Star-Forming Region Chandra Point Source Optical/IR IDs Catalog
The Cepheus B (Cep B) molecular cloud and a portion of the nearby Cep OB3b OB association, one of the most active regions of star formation within 1 kpc, have been observed with the Infrared Array Camera (IRAC) detector on board the Spitzer Space Telescope. The goals were to study protoplanetary disk evolution and processes of sequential triggered star formation in the region. Out of ~400 pre-main-sequence (PMS) stars selected with an earlier Chandra X-ray Observatory observation, ~95% are identified with mid-infrared sources and most of these are classified as diskless or disk-bearing stars. The discovery of the additional >200 IR-excess low-mass members gives a combined Chandra+Spitzer PMS sample that is almost complete down to 0.5 * M<sub>sun</sub> outside of the cloud, and somewhat above 1 * M<sub>sun</sub> in the cloud. The X-ray observations of the Cep B/Cep OB3b region and their data analysis are described in detail by Getman et al. (2006, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/163/306">CDS Cat. J/ApJS/163/306</a>, HEASARC CEPBOB3CXO table). The 30 ks exposure was obtained on 2003 March 11.51-11.88 with the Advanced CCD Imaging Spectrometer (ACIS) detector on board the Chandra X-ray Observatory as part of the ACIS Instrument Team's Guaranteed Time Observations (ObsId No. 3502, P.I.: G. Garmire). The mid-IR observation of Cep B and Cep OB3b was obtained on 2007 February 18 with the IRAC detector on the Spitzer Space Telescope in the 3.6, 4.5, 5.8, and 8.0 micron channels. This was a General Observer project (program identification No. 30361; P.I.: J. Wang). This table contains the optical and infrared counterpart information on the 431 X-ray sources detected by Chandra. It does not contain the 224 IR-excess objects which were not detected as X-ray sources (listed in Table 3 of the reference paper) that are thought to be additional low-mass members of this complex. This table was created by the HEASARC in August 2011 primarily based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/699/1454">CDS catalog J/ApJ/699/1454</a> files table.dat and table 2.dat which list the optical and infrared counterpart information on the 431 X-ray sources detected by Chandra. The names and positions of these X-ray sources were taken from the Getman et al. (2006, ApJS, 163, 306) Catalog, which is available as the HEASARC Browse table CEPBOB3CXO. This is a service provided by NASA HEASARC .
VLA Goulds Belt Survey Taurus-Auriga Complex Source Catalog
This table contains results from a multi-epoch radio study of the Taurus-Auriga complex made with the Karl G. Jansky Very Large Array (JVLA) at frequencies of 4.5 GHz and 7.5 GHz. A total of 610 sources were detected, 59 of which are related to young stellar objects (YSOs) and 18 to field stars. The properties of 56% of the young stars are compatible with non-thermal radio emission. The authors also show that the radio emission of more evolved YSOs tends to be more non-thermal in origin and, in general, that their radio properties are compatible with those found in other star-forming regions. By comparing their results with previously reported X-ray observations, the authors noticed that YSOs in Taurus-Auriga follow a Guedel-Benz relation with a scaling factor, kappa, of 0.03, as they previously suggested for other regions of star formation. In general, YSOs in Taurus-Auriga and in all the previous studied regions seem to follow this relation with a dispersion of ~1 dex. Finally, the authors propose that most of the remaining sources are related with extragalactic objects but provide a list of 46 unidentified radio sources whose radio properties are compatible with a YSO nature (identified in this implementation of their catalog by values for the parameter radio_yso_flag of 'Y'). The observations were obtained with the JVLA of the National Radio Astronomy Observatory (NRAO) in its B and BnA configuration. Two frequency sub-bands, each 1 GHz wide, and centered at 4.5 and 7.5 GHz, respectively, were recorded simultaneously. The observations were obtained in three different time periods (February 25/26/28 to March 6, April 12/17/20/25, and April 30 to May 1/5/14/22, all in 2011) typically separated from one another by a month: see Table 1 of the reference paper for more details. For their study, the authors observed 127 different target fields distributed across the cloud complex (Figure 1 of the reference paper). The fields were chosen to cover previously known YSOs. In 33 of those fields, the authors could observe more than one YSO target, while in the remaining 94 fields, only one YSO was targeted. In most cases, the infrared evolutionary class (i.e., Classes I, II, or III) or T Tauri evolutionary status (classical or weak line) of the targeted sources was known from the literature. The final images covered circular areas of 8.8 and 14.3 arcminutes in diameter, for the 7.5 and 4.5 GHz sub-bands, respectively, and were corrected for the effects of the position-dependent primary beam response. The noise levels reached for each individual observation was about ~40 µJy and ~30 µJy, at 4.5 GHz and7.5 GHz, respectively. The visibilities of the three, or two, observations obtained for each field were concatenated to produce a new image with a lower noise level (of about ~25 µJy at 4.5 GHz and ~18 µJy at 7.5 GHz). The angular resolution of ~1 arcsecond (see the synthesized beam sizes in Table 1 of the reference paper) allows an uncertainty in position of ~0.1 arcseconds or better. In the observed area, there are a total of 196 known YSOs.The first step was the identification of radio sources in the observed fields. The authors follow the procedure and criteria presented by Dzib et al. (2013, ApJ, 775, 63) who consider a detection as firm if the sources have a flux larger than 4 times the noise level and there is a counterpart known at another wavelength, else they require a flux which is 5 times the noise level. The identification was done using the images corresponding to the concatenation of the observed epochs, which provides the highest sensitivity. From this, a total of 609 sources were detected. Of these sources, 215 were only detected in the 4.5 GHz sub-band, while six were only detected in the 7.5 GHz sub-band. The remaining 388 sources were detected in both sub-bands. The authors searched the literature for previous radio detections, and for counterparts at X-ray, optical, near-infrared, and mid-infrared wavelengths. The search was done using SIMBAD, and accessed all the major catalogs. They considered a radio source to be associated with a counterpart at another wavelength if the separation between the two was below the combined uncertainties of the two data sets. This was about 1.0 arcsecond for the optical and infrared catalogs, but could be significantly larger for some of the radio catalogs (for instance, the NVSS has a positional uncertainty of about 5 arcseconds). They found that only 120 of the sources detected here had previously been reported at radio wavelengths, while the other 491 are new radio detections. On the other hand, the authors found a total of 270 counterparts at other wavelengths. In the literature, 18 are classified as field stars, 49 as extragalactic, 1 is classified as either a star or an extragalactic source in different surveys, 49 are classified as YSOs, 11 are classified as either YSO and extragalactic, and the remaining 143 sources are unclass
Spitzer Wide-area InfraRed Extragalactic Survey XMM-LSS MIPS 70 micron Catalog
The Spitzer Wide-area InfraRed Extragalactic survey (SWIRE), the largest Spitzer Legacy program, is a wide-area, imaging survey to trace the evolution of dusty, star-forming galaxies, evolved stellar populations, and AGN as a function of environment, from redshifts z~3 to the current epoch. SWIRE surveys 6 high-latitude fields, totaling ~50 sq. deg. in all 7 Spitzer bands: 3.6, 4.5, 5.8, and 8 microns with IRAC and 24, 70, and 160 microns with MIPS (Lonsdale et al. 2003). The SWIRE Legacy Extragalactic Source Catalogs will eventually contain in excess of 2 million IR-selected galaxies, from those dominated by the light of stellar populations detected primarily by IRAC, to starbursts, ultra-luminous infrared galaxies and AGN detected also by MIPS.
Bolocam Galactic Plane Survey Distance Catalog
The Bolocam Galactic Plane Survey (BGPS) is a 1.1 mm continuum survey of the Galactic Plane made using Bolocam on the Caltech Submillimeter Observatory. Millimeter-wavelength thermal dust emission reveals the repositories of the densest molecular gas, ranging in scale from cores to whole clouds. By pinpointing these regions, the connection of this gas to nascent and ongoing star formation may be explored. The BGPS coverage totals 170 square degrees (with 33" FWHM effective resolution). The survey is contiguous over the range -10.5 ≤ l ≤ 90.5, |b| ≤ 0.5. Towards the Cygnus X spiral arm, the coverage was flared to |b| ≤ 1.5 for 75.5 ≤ l ≤ 87.5. In addition, cross-cuts to |b| ≤ 1.5 were made at l = 3, 15, 30 and 31. The total area of this section is 133 square degrees. With the exception of the increase in latitude, no pre-selection criteria were applied to the coverage in this region. In addition to the contiguous region, four targeted regions in the outer Galaxy were observed: IC1396 (9 square degrees, 97.5 ≤ l ≤ 100.5, 2.25 ≤ l ≤ 5.25), a region towards the Perseus Arm (4 square degrees centered on l = 111, b=0 near NGC7538), W3/4/5 (18 square degrees, 132.5 ≤ l ≤ 138.5) and Gem OB1 (6 square degrees, 187.5 ≤ l ≤ 193.5). The survey has detected approximately 8,400 sources, to an rms noise level in the maps ranging from 30 to 60 mJy beam-1. The BGPS survey and catalog provide an important database for sub/millimeter observations with the Herschel Space Observatory, ALMA, SCUBA-2, APEX, and others.
Upper Sco XMM-Newton X-Ray Point Source Catalog
The authors studied the X-ray emission from young stars by analyzing the deep (a ~53 ks exposure centered at a J2000.0 RA and Dec of 16 14 00.0, -23 00 00 and a ~43 ks exposure at 15 56 25.0, -23 37 47) XMM-Newton observations of two regions of the Upper Scorpius (USco) subgroup of the Scorpius-Centaurus (Sco-Cen) association which is estimated to have an age of 5 Myr. Portions of the USco association were observed in the optical with the CTIO Curtis Schmidt telescope and the Danish 1.54m telescope. This table contains all the X-ray sources detected in the two XMM-Newton observations, as well as their near-IR counterparts from the 2MASS and DENIS catalogs, and their optical counterparts from the CTIO and Danish 1.54 m observations. Based on the near-infrared and optical photometry, 22 Upper Scorpius photometric members have been identified among the 224 detected X-ray sources. This table was created by the HEASARC in March 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/459/199">CDS catalog J/A+A/459/199</a> files tabled1.dat and table2.dat. This is a service provided by NASA HEASARC .
DeepDrill Forced Photometry Catalog
The DeepDrill team presents a catalog of multi-band forced photometry in the CDFS and XMM-LSS fields. They used The Tractor image-modeling software to produce de-blended photometry across 13 to 15 optical/infrared bands and determine photometric redshifts. The Catalog contains ~1.5 million sources covering a total area of ~9 square degrees.
MSX6C Infrared Point Source Catalog
Version 2.3 of the Midcourse Space Experiment (MSX) Point Source Catalog (PSC), which supercedes the version (1.2) that was released in 1999, contains over 100,000 more sources than the previous version. The photometry is based on co-added image plates, as opposed to single-scan data, which results in improved sensitivity and hence reliability in the fluxes. Comparison with Tycho-2 positions indicates that the astrometric accuracy of the new catalog is more than 1'' better than that in Version 1.2. In addition to the Galactic plane, Areas Missed by the Infrared Astronomical Satellite (IRAS), and the Large Magellanic Cloud, which were included in the previous catalog, Version 2.3 includes data from the Small Magellanic Cloud, eight nearby galaxies, and several molecular clouds and star forming regions.
CGRO/BATSE Earth Occultation Catalog of Low-Energy Gamma-Ray Sources
This table contains the CGRO/BATSE Earth Occultation Catalog of Low-Energy Gamma-Ray Sources. The Burst and Transient Source Experiment (BATSE), aboard the Compton Gamma Ray Observatory (CGRO), provided a record of the low-energy gamma-ray sky (20 - 1000 keV band) between 1991 April and 2000 May (a 9.1 year period). Using the Earth Occultation Technique to extract flux information, a catalog of sources using data from the BATSE large area detectors has been prepared. The first part of the catalog consists of results from the monitoring of 58 sources, mostly Galactic. For these sources, the authors included tables of flux and spectral data, and outburst times for transients, in their published paper. The authors also performed a deep-sampling of 180 objects (including the aforementioned 58 objects) combining data from the entire 9.1 year BATSE dataset. (One extra object, GRO J1735-27, has been added in this HEASARC table in addition to the 179 objects discussed in the reference paper). Source types considered were primarily accreting binaries, but a small number of representative active galaxies, X-ray-emitting stars, and supernova remnants were also included. The deep sample results include definite detections of 83 objects and possible detections of 36 additional objects. The definite detections spanned three classes of sources: accreting black hole and neutron star binaries, active galaxies and supernova remnants. Flux data for the deep sample are presented in four energy bands: 20-40, 40-70, 70-160, and 160-430 keV. The limiting average flux level (9.1 years) for the sample varies from 3.5 to 20 mCrab (5 sigma) between 20 and 430 keV, depending on systematic error, which in turn is primarily dependent on the sky location. To strengthen the credibility of detection of weaker sources (5-25 mCrab), the authors generated Earth occultation images, searched for periodic behavior using FFT and epoch folding methods, and critically evaluated the energy-dependent emission in the four flux bands. For more information, visit the website <a href="https://heasarc.gsfc.nasa.gov/docs/cgro/batse/hilev/highlevel.html">https://heasarc.gsfc.nasa.gov/docs/cgro/batse/hilev/highlevel.html</a> or refer to the Harmon et al. 2004 paper. This table was first created by the HEASARC in June 2004 based on a table supplied by one of the authors. The HEASARC updated the table and added the data products in July 2006. This is a service provided by NASA HEASARC .
COBE DIRBE Point Source Catalog
This table contains the Cosmic Background Explorer (COBE) Diffuse Infrared Background Experiment (DIRBE) Point Source Catalog, an all-sky catalog containing infrared photometry in 10 bands from 1.25 microns to 240 microns for 11,788 of the brightest near and mid-infrared point sources in the sky. Since DIRBE had excellent temporal coverage (100-1900 independent measurements per object during the 10 month cryogenic mission in 1989 to 1990), the catalog also contains information about variability at each wavelength, including amplitudes of variation observed during the mission. Since the DIRBE spatial resolution is relatively poor (0.7 degrees), the authors carefully investigated the question of confusion, and flagged sources with infrared-bright companions within the DIRBE beam. In addition, they filtered the DIRBE light curves for data points affected by companions outside of the main DIRBE beam but within the `sky' portion of the scan. At high Galactic latitudes (|b| > 5 degrees), the catalog contains essentially all of the unconfused sources with flux densities greater than 90, 60, 60, 50, 90, and 165 Jy at 1.25, 2.2, 3.5, 4.9, 12, and 25 microns, respectively, corresponding to magnitude limits of approximately 3.1, 2.6, 1.7, 1.3, -1.3, and -3.5. At longer wavelengths and in the Galactic Plane, the completeness is less certain because of the large DIRBE beam and possible contributions from extended emission. For each source, for comparison, the names of the sources in other catalogs, their spectral types, variability types, IRAS and 2MASS photometry, SIMBAD spectral types and published variability types, and whether or not the sources are known OH/IR stars are also included. Unlike the IRAS and 2MASS Catalogs, the DIRBE Point Source Catalog was not constructed by searching the DIRBE database with a point source template and extracting sources based on S/N and confirmation criteria. The DIRBE Catalog was constructed using a target sample list obtained from other infrared catalogs. Since DIRBE is much less sensitive per scan than IRAS or 2MASS, essentially all of the point sources with high S/N light curves in the DIRBE database are already contained in IRAS, 2MASS, and/or MSX. Thus, for simplicity, the authors used these previous catalogs to select a sample for the DIRBE Point Source Catalog. Their initial sample included a total of 21,335 sources; the final catalog contains 11,788 sources. The initial sample was selected from the IRAS Point Source Catalog (1988), the 2MASS Point Source Catalog (Cutri 2003), and/or the MSX Point Source Catalog Version 1.2 (Egan et al. 1999, A&A, 349, 236) that satisfied at least one of the following criteria: (a) 2MASS J magnitude <= 4.51 (F<sub>1.25</sub> >= 25 Jy), (b) 2MASS K magnitude <= 3.81 (F<sub>2.2</sub> >= 20 Jy), (c) IRAS or MSX F<sub>12</sub> >= 15 Jy, or (d) IRAS or MSX F<sub>25</sub> >= 27.5 Jy. The 1.25 and 2.2 micron limits are equal to the average 1-sigma sensitivity per scan in the raw DIRBE light curves of Smith et al. (2002, AJ, 123, 948), while the 12 and 25 micron limits are 0.5 times the average noise levels per scan in that study. These low limits were selected in order to avoid missing variable stars that may have been faint during the 2MASS, IRAS, or MSX mission and to improve the completeness at 3.5 and 4.9 micron. Since the filtering process improves the average per measurement uncertainty, a sensitive selection criterion is warranted to include as many sources as possible. There were 7872 sources with 2MASS J <= 4.51, 20,492 sources with 2MASS K <= 3.81, 4969 sources with IRAS F12 >= 15 Jy, 40 sources in the MSX IRAS Gaps survey with MSX F12 >= 15 Jy, 2753 sources with IRAS F25 >= 27.5 Jy, and 18 sources in the MSX IRAS Gaps survey with MSX F25 >= 27.5 Jy. Thus, the initial list is dominated by stars selected by the 2MASS criteria. These lists were merged together to make a single target list, containing 21,335 sources. To merge the 2MASS and IRAS/MSX lists, the authors used a 60 arcsecond matching radius. If more than one 2MASS source was within 60 arcseconds of the IRAS position, they assumed that the brightest K band source was the match. Note that the authors did not include sources in their input list based on their 60 and/or 100 micron IRAS flux densities, as extended emission from cirrus becomes more significant at these wavelengths. This means that the DIRBE Point Source Catalog is biased against very cold objects, such as galaxies and molecular clouds. Since the authors only used the point source catalogs of 2MASS, IRAS, and MSX for source selection, their sample is also biased against extended objects. Note also that they are only targeting sources bright enough to detect their possible variability in the DIRBE database (i.e., sources that may be detected in a single DIRBE scan at at least one DIRBE wavelength). By co-adding the full light c
NGC 1893 Chandra X-Ray Point Source Catalog
The outer Galaxy, where the environmental conditions are different from the solar neighbourhood, is a laboratory in which it is possible to investigate the dependence of the star formation process on the environmental parameters. The authors investigate the X-ray properties of NGC 1893, a young cluster (~ 1 - 2 Myr) in the outer part of the Galaxy (galactic radius >= 11 kpc), where they expect differences in the disk evolution and in the mass distribution of the stars, so as to explore the X-ray emission of its members and compare it with that of young stars in star forming regions near to the Sun. The authors analyze 5 deep Chandra ACIS-I observations with a total exposure time of 450 ks. Source events of the 1021 X-ray sources have been extracted with the IDL-based routine ACIS-Extract. Using spectral fitting and quantile analysis of X-ray spectra, they derive X-ray luminosities and compare the respective properties of Class II and Class III members. They also evaluate the variability of sources using the Kolmogorov-Smirnov test and identify flares in the lightcurves. The X-ray luminosity of NGC 1893 X-ray members is in the range 10<sup>29.5</sup> - 10<sup>31.5</sup> erg s<sup>-1</sup>. Diskless stars are brighter in X-rays than disk-bearing stars, given the same bolometric luminosity. The authors find that 34% of the 1021 lightcurves appear variable and that they show 0.16 flares per source, on the average. Comparing their results with those relative to the Orion Nebula Cluster, they find that, after accounting for observational biases, the X-ray properties of NGC 1893 and the Orion stars are very similar. The authors conclude that the X-ray properties of stars in NGC 1893 are not affected by the environment and that the stellar population in the outer Galaxy may have the same coronal properties as nearby star-forming regions. The X-ray luminosity properties and the X-ray luminosity function appear to be universal and can therefore be used for estimating distances and for determining stellar properties. This table was created by the HEASARC in March 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/539/A74">CDS Catalog J/A+A/539/A74</a> file catalog.dat, the catalog of 1021 X-ray sources detected towards NGC 1893. This is a service provided by NASA HEASARC .
Second INTEGRAL AGN Catalog
The INTEGRAL mission provides a large data set for studying the hard X-ray properties of AGN and allows testing the unified scheme for AGN. This table contains some of the results from the analysis of INTEGRAL IBIS/ISGRI, JEM-X, and OMC data for 199 AGN (and 3 clusters of galaxies) that have been reported to be detected by INTEGRAL at energies above 20 keV. The data analyzed therein allowed a significant spectral extraction on 148 objects and optical variability study of 57 AGN. The slopes of the hard X-ray spectra of Seyfert 1 and Seyfert 2 galaxies were found to be consistent within the uncertainties, whereas lower luminosities were measured for the more absorbed/type 2 AGN. The intermediate Seyfert 1.5 objects exhibit hard X-ray spectra consistent with those of Seyfert 1 galaxies. When applying a Compton reflection model, the underlying continua appear still the same in Seyfert 1 and 2 with photon index 2, and the reflection strength is about R = 1, when assuming different inclination angles. A significant correlation is found between the hard X-ray and optical luminosity and the mass of the central black hole, in the sense that the more luminous objects appear to be more massive. There is also a general trend for the absorbed sources and type 2 AGN to have lower Eddington ratios. The black hole mass appears to form a fundamental plane together with the optical and X-ray luminosity of the form L<sub>V</sub> being proportional to L<sub>X</sub><sup>0.6</sup> M<sub>BH</sub><sup>0.2</sup>, similar to that found between radio luminosity L<sub>R</sub>, L<sub>X</sub>, and M<sub>BH</sub>. The unified model for Seyfert galaxies seems to hold, showing in hard X-rays that the central engine is the same in Seyfert 1 and 2 but seen under different inclination angles and absorption. A catalog of 199 IBIS/ISGRI detected AGN is presented. For those 148 objects significantly detected in the data set analyzed here, spectral parameters, fluxes, and luminosities are given. In addition, the photometric table of OMC measurements in the V-band (given for 57 of the AGN) is also included herein. For objects with more complex spectra, notice, the results of a fit to a cut-off power law model were presented in Table 3 of the reference paper, but are not included in this HEASARC table. The JEM-X spectra of the 23 AGN detected by the X-ray monitor were fit with the IBIS/ISGRI data, and the results of this were presented in Table 4 of the reference paper, but are also not included in this HEASARC table. This table was created by the HEASARC in November 2009 based on the electronic version of Tables 1, 2 and 5 from the reference paper which was obtained from the CDS (their catalog J/A+A/505/417 files table1.dat, table2.dat and table5.dat). This is a service provided by NASA HEASARC .
Australia Telescope-PMN Catalog of Southern Radio Sources
This table contains a source catalog of 9040 radio sources derived from high-resolution observations of a selection of 8385 Parkes-MIT-NRAO (PMN) sources made with the Australia Telescope Compact Array (ATCA). The catalog lists flux density and structural measurements at 4.8 and 8.6 GHz, derived from observations of all PMN sources in the declination range -87 degrees < Dec < -38.5 degrees (exclusive of galactic latitudes |b| < 2 degrees) with PMN flux density S<sub>4850</sub> > 70mJy (> 50 mJy south of Dec = -73 degrees). The authors assess the quality of the data, which was gathered in the 1992-1994 time period, and the resulting source parameters. They describe the population of catalogued sources, and compare it to samples from complementary catalogs. In particular, they find 122 radio sources with highly probable association with gamma-ray sources observed by the orbiting Fermi Large Area Telescope (LAT), and 11 more radio sources with possible associations with Fermi LAT sources. This Australia Telescope PMN (ATPMN) catalog lists the source measurements of flux density, position and structure of a selection of sources from the PMN catalog. Each catalog entry corresponds to a discrete source observed by the ATCA. In many cases, a single PMN source yields several ATPMN sources. Apart from the name of the parent PMN source, there is no indication of physical association: multiple sources in the one field may be aligned by chance, or may be components of the one object. This catalog contains the following information for each source: position; the flux density at 4.8 and 8.6 GHz; uncertainties in each flux density; the source size modelled as an ellipse (major axes, minor axes, position angle) of the best fit for a Gaussian brightness distribution; the spectral index computed between 4.8 and 8.6 GHz; the uncertainty in the spectral index; a code denoting the epoch of the observation. In the table as given in the original reference, the positions were given with varying degrees of precision, from 0.001 to 1 second of time in RA and from 0.01 to 1 arcsecond in Declination. The authors state in Section 4 of the reference paper that the error in a position coordinate is less than 10 times the final digit given in the coordinate. The positions as displayed in this table do not reflect this system: e.g., a Dec value displayed as '-79 58 34.00' may have been given in the original table as '-79 58 34.00' or '-79 58 34.0' or '-79 58 34'. To recover this information about positional precision the HEASARC has created two additional parameters ra_accuracy and dec_accuracy which list the number of digits after the decimal point given in the original table for the RA and Dec, respectively. Thus, if ra_accuracy = 3, the RA was given to a precision of 0.001 s in the original table, implying that the actual error in RA was less than 10 * 0.001 = 0.01 s. This table was created by the HEASARC in July 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/422/1527">CDS Catalog J/MNRAS/422/1527</a> file atpmncat.dat. This is a service provided by NASA HEASARC .
SAGE-SMC MIPS 160 micron Combined Epoch Catalog
The SAGE-SMC pro ject is a Cycle 4 legacy program on the Spitzer Space Telescope, entitled, SAGE-SMC: Surveying the Agents of Galaxy Evolution in the Tidally-Disrupted, Low-Metallicity Small Magellanic Cloud, with Karl Gordon (STScI) as the PI. The project overview and initial results are described in a paper by Gordon et al. (2010, in prep). The SMC was mapped at two different epochs dubbed Epochs 1 and 2 separated by 3 (IRAC) and 9 (MIPS) months, as this provides a 90-degree roll angle in the orientation of the detectors, which optimally removes the striping artifacts in MIPS and artifacts along columns and rows in the IRAC image data. In addition, these two epochs are useful constraints of source variability expected for evolved stars and some young stellar ob jects (YSOs). The IRAC and MIPS observations from the S3MC pathfinder survey of the inner 3 sq. deg. of the SMC (PI: Bolatto, referred to as Epoch 0) have been reduced using the same software. To be included in each single epoch catalog, each 24 um source has to meet a number of criteria. The source had to be nearly point like with a correlation value >0.89. This removed approximately 2/3 of the entries in the single epoch source lists. In regions where there is a significant structure in the surrounding region (identified as having a sigma > 0.25 in a 120" width square box), the source had to have a correlation value >0.91. This requirement removed a small number of sources (70). Finally, all sources had to have signal-to-noise (S/N) values >5. The S/N used was that estimated from the StarFinder code using the mosaic uncertainty image added in quadrature with an 0.6% error due to the background subtraction. This removed 700 sources. The final Epoch 1 catalog likely has a few remaining unreliable sources, estimated to be at less than the 1% level. The Full List contains ALL sources extracted from the MIPS 24 um mosaics, thus a user should be aware that it contains spurious sources. For more details, see Section 4.1 of the SAGE-SMC Data Delivery Document.
LALA Cetus Field Chandra X-Ray Point Source Catalog
The 174 ks Chandra Advanced CCD Imaging Spectrometer (ACIS) exposure of the Large Area Lyman Alpha Survey (LALA) Cetus field is the second of the two deep Chandra images on LALA fields. In their paper, the authors present the Chandra X-ray sources detected in the Cetus field, along with an analysis of X-ray source counts, the stacked X-ray spectrum, and the optical identifications. A total of 188 X-ray sources were detected: 174 in the 0.5-7.0 keV band, 154 in the 0.5-2.0 keV band, and 113 in the 2.0-7.0 keV band. The X-ray source counts were derived and compared with the 172 ks exposure LALA Bootes field (available as the LALABOOCXO table in Browse). Interestingly, the authors find consistent hard-band X-ray source density, but a (36 +/- 12)% higher soft-band X-ray source density in the Cetus field. The weighted stacked spectrum of the detected X-ray sources can be fitted by a power law with photon index Gamma = 1.55. Based on the weighted stacked spectrum, the authors find that the resolved fraction of the X-ray background drops from (72 +/- 1)% at 0.5-1.0 keV to (63 +/- 4)% at 6.0-8.0 keV. The unresolved spectrum can be fitted by a power law over the range 0.5-7 keV, with a photon index Gamma = 1.22. Optical counterparts are also presented for 154 of the X-ray sources, down to a limiting magnitude of r' = 25.9 (Vega), using a deep r'-band image obtained with the MMT. This table was created by the HEASARC in October 2010 based on the CDS table J/ApJ/669/765 file table1.dat This is a service provided by NASA HEASARC .
Giant Metrewave Radio Telescope VVDS-VLA Deep Field 610-MHz Radio Source Catalog
This table contains the 5-sigma catalog at 610 MHz of the VIMOS VLT Deep Survey-Very Large Array (VVDS-VLA) deep field obtained from Giant Metrewave Radio Telescope (GMRT) observations. The field is located at RA, Dec = 02:26:00, -04:30:00 (J2000) and covers a 1-square degree area. The GMRT observations imaged the whole 1 square degree field with an angular resolution of 6 arcseconds and an average sensitivity of about 50 µJy/beam. The catalog lists 514 radio sources, 17 of which are fitted with multiple components (between 2 and 5). For these multiple sources, each component (A, B, etc.) is listed separately, and the entire source (indicated by the suffix T in the name) is also listed. Thus, there are 557 entries in this table, 43 of which correspond to multiple components. This table was created by the HEASARC in February 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/463/519">CDS Catalog J/A+A/463/519</a> file table.dat. This is a service provided by NASA HEASARC .
Herschel Stripe 82 Survey (HerS) Point Source Catalog
This study presents the first set of maps and band-merged catalog from the Herschel Stripe 82 Survey (HerS). Observations at 250, 350, and 500 micron (µm) were taken with the Spectral and Photometric Imaging Receiver (SPIRE) instrument onboard the Herschel Space Observatory. HerS covers 79 square degrees along the SDSS Stripe 82 to an average depth of 13.0, 12.9, and 14.8 mJy beam<sup>-1</sup> (including confusion) at 250, 350, and 500 um, respectively. HerS was designed to measure correlations with external tracers of the dark matter density field, either point-like (i.e., galaxies selected from radio to X-ray) or extended (i.e., clusters and gravitational lensing), in order to measure the bias and redshift distribution of intensities of infrared-emitting dusty star-forming galaxies and active galactic nuclei. By locating HerS in Stripe 82, the authors maximize the overlap with available and upcoming cosmological surveys. The band-merged catalog contains 3.3 x 10<sup>4</sup> sources detected at a significance of >~ 3 sigma (including confusion noise). The maps and catalog are available at <a href="http://www.astro.caltech.edu/hers/">http://www.astro.caltech.edu/hers/</a>. This table contains the first HerS band-merged point source catalog based on observations covering 79 deg<sup>2</sup> in the equatorial Stripe 82, spanning 13 to 37 degrees (0<sup>h</sup> 54<sup>m</sup> to 2<sup>h</sup> 24<sup>m</sup> ) in RA, and -2 to +2 degrees in Declination. The SPIRE beams are 18.1, 25.2 and 36.6 arcseconds at 250, 350 and 500 um, respectively. The band-merged catalog was constructed, after filtering, with DESPHOT (Roseboom et al. 2010, MNRAS, 409, 48), using 250-um sources (extracted with STARFINDER: Diolaiti et al. 2000, A&AS, 147, 335) as positional priors. The authors included sources with S/N greater than 3, whose completeness is estimated to be 50% (see Figure 7 of the reference paper), with a false detection rate less than 1%, and which had reasonable residuals (i.e., chi<sup>2</sup> < 10). Next, they identified obviously extended sources - 24 in total - where their extended nature resulted in them being broken up into multiple components by the filter, and removed them. This results in a catalog with 32,815 sources at 250 um, of which 13,300 and 3,276 have similarly defined 3-sigma detections at 350 and 500 um, respectively. The authors expect a false positive rate of 1.2 +/- 0.2 deg<sup>-2</sup> : thus, across the 79 deg<sup>2</sup> of HerS, they expect 96 +/- 16 spurious sources. The following local extended sources were removed: <pre> Name, RA, DEC NGC 0493,20.537458,0.945361 UGC 00890,20.283333,1.373333 UGC 00892,20.319166,-0.544491 NGC 0428,18.232125,0.981556 NGC 0799,30.551407,-0.100629 NGC 0800,30.549358,-0.130432 NGC 0450,18.876840,-0.860973 NGC 0497,20.599064,-0.875207 NGC 0867,34.269910,1.244202 UGC 01725,33.607833,1.469833 NGC 0570,22.244325,-0.948996 UGC 00711,17.153750,1.641667 UGC 00726,17.489833,-1.749694 NGC 0550,21.677292,2.022361 NGC 0585,22.9255833,-0.9333056 UGC 01123,23.533209,-1.032286 2MASX J01434929-0048547,25.955091,-0.815256 NGC 0856,33.409831,-0.717287 UGC 01698,33.082019,-0.811513 CGCG 385-007,17.256708,1.378194 UGC 00790,18.657792,1.180167 2MFGC 01002,19.930083,1.630778 2MFGC 00979,19.642792,1.747889 UGC 00847,19.768317,-0.138572 </pre> This database table was created by the HEASARC in March 2014 based on a FITS file (v2.0, uploaded Nov 18, 2013, of hers.catalogue_3sig250_no_extended.fits) containing the catalog which was obtained from the HerS web site, viz., <a href="http://www.astro.caltech.edu/hers/Catalogs.html">http://www.astro.caltech.edu/hers/Catalogs.html</a>. Some of the values for the name parameter in the HEASARC's implementation of this table were corrected in April 2018. This is a service provided by NASA HEASARC .
ScienceDex guides
Understand access before you commit
These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.