- ID:
- ivo://nasa.heasarc/maghmxbcat
- Title:
- Magellanic Clouds High-Mass X-Ray Binaries Catalog
- Short Name:
- MCHMXRB
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This database table contains a catalog of high-mass X-ray binaries (HMXBs) in the Small and Large Magellanic Clouds (SMC and LMC). The catalog lists source name(s), coordinates, apparent magnitudes, orbital parameters, and X-ray luminosities for 128 HMXBs, together with the stellar parameters of the components, other characteristic properties and a comprehensive selection of the relevant literature. The aim of this catalog is to provide easy access to the basic information on the X-ray sources and their counterparts in other wavelength ranges (UV, optical, IR, radio). Most of the sources have been identified as Be/X-ray binaries. Some sources, however, are only tentatively identified as HMXBs on the basis of a transient character and/or a hard X-ray spectrum. Further identification in other wavelength bands is needed to finally determine the nature of these sources. In cases where there is some doubt about the high-mass nature of the X-ray binary this is mentioned. Literature published before 1 May 2005 has, as far as possible, been taken into account. Information on the numbers used to code references is available at <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/refs.dat">CDS</a>. Individual notes on each HMXB are also available for <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/notes1.dat">SMC systems</a> and for <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135/notes2.dat">LMC systems</a> at the same site. This Browse table contains the combination of 92 HMXBs in the SMC and 36 HMXBs in the LMC which were listed in Tables 1 and 2, respectively, of the published version of this catalog. The HEASARC has added a parameter called cloud_id which can be used to identify which Magellanic Cloud any specified HMXB belongs to (the SMC or the LMC). This database was created by the HEASARC in December 2005 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/442/1135">CDS Catalog J/A+A/442/1135</a>, table1.dat and table2.dat. This is a service provided by NASA HEASARC .
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- ID:
- ivo://nasa.heasarc/maranoxmm
- Title:
- Marano Field XMM-Newton X-Ray Source Optical Counterparts
- Short Name:
- MARANOXMM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains some of the results from a medium deep XMM-Newton survey of the Marano Field and optical follow-up observations. The mosaicked XMM-Newton pointings in this optical quasar survey field cover 0.6 deg<sup>2</sup> with a total of 120 ks good observation time. 328 X-ray sources were detected in total with detection likelihoods ML >= 5. The X-ray fluxes are in the range f<sub>X</sub> = (0.16 - 54) x 10<sup>-14</sup> erg cm<sup>-2</sup> s<sup>-1</sup> (0.2 - 10 keV). The turnover flux of this sample is f<sub>X</sub> ~ 5 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in this same energy band. With VLT FORS1 and FORS2 spectroscopy 96 new X-ray counterparts have been classified. The central 0.28 deg<sup>2</sup> region, where detailed optical follow-up observations were performed, contains ~ 170 X-ray sources (detection likelihood ML > 10), out of which 48 had already been detected by ROSAT. In this region 23 out of 29 optically selected quasars have been recovered. With a total of 110 classifications in their core sample, the authors have reached a completeness of ~65%. About one-third of the XMM-Newton sources are classified as type II AGN with redshifts mostly below 1.0. Furthermore, five high redshift type II AGN (2.2 <= z <= 2.8) have been detected. This table contains the list of the 195 optical counterparts for 172 of the XMM-Newton X-ray sources given in Table 8 of the reference paper. It does not contain the full list of 328 X-ray sources given in Table A1 of the reference paper, nor the lists of marginal X-ray sources given in Appendix B of the reference paper. This table was created by the HEASARC in May 2007 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/466/41">CDS catalog J/A+A/466/41</a> file table8.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/markarian2
- Title:
- Markarian Galaxies Optical Database
- Short Name:
- MARKARIAN2
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- A database for the entire Markarian (First Byurakan Spectral Sky Survey or FBS) Catalog is presented that combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. The authors provide accurate coordinates, morphological type, spectral and activity classes, red and blue apparent magnitudes, apparent diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. Special attention was paid to the individual descriptions of the galaxies in the original Markarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems, larger galaxies with knots of star formation, possible stars, and cases of stars projected on galaxies. The total number of individual Markarian objects in the database is now 1544. The authors also have included redshifts which are now available for 1524 of the objectswith UV-excess radiation, as well as Galactic color excess E(B-V) values and their 2MASS or DENIS infrared magnitudes. The table also includes extensive notes that summarize information about the membership of Markarian galaxies in different systems of galaxies and about new and revised activity classes and redshifts. The new optical information on Markarian galaxies was obtained from images extracted from the STScI Digitized Sky Survey (DSS) of F_pg (red) and J_pg (blue) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. This table was created by the HEASARC in November 2009 based on the electronic version of the optical database of Markarian galaxies which was obtained from the CDS (their catalog J/ApJS/170/33 file table1.dat). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mashpncat
- Title:
- MASH Catalogs of MASH Planetary Nebulae
- Short Name:
- MASHPNCAT
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The first part of the Macquarie/AAO/Strasbourg H-alpha Planetary Nebula Catalog (MASH) contains 903 new true, likely and possible Galactic planetary nebulae (PNe) discovered in the AAO/UKST H-alpha survey of the southern Galactic Plane. The combination of depth, resolution, uniformity, and areal coverage of the H-alpha survey has opened up an hitherto unexplored region of parameter space permitting the detection of this significant new PN sample. The second part, MASH-II, consists of over 300 true, likely and possible new Galactic PNe found after re-examination of the entire AAO/UKST H-alpha survey of the Southern Galactic Plane in digital form. Over 240 of these new candidates were confirmed as bona fide PNe on the basis of spectroscopic observations. This HEASARC table contains all 1238 objects from the combined MASH and MASH-II catalogs. This table was created by the HEASARC in April 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/V/127A">CDS Catalog V/127A</a> files mash1.dat and mash2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/moxc
- Title:
- Massive Star-Forming Regions Omnibus X-Ray Catalog
- Short Name:
- MOXC
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table contains the Massive Star-forming Regions (MSFRs) Omnibus X-ray Catalog (MOXC), a compendium of X-ray point sources from Chandra/ACIS observations of a selection of MSFRs across the Galaxy, plus 30 Doradus in the Large Magellanic Cloud. MOXC consists of 20,623 X-ray point sources from 12 MSFRs with distances ranging from 1.7 kpc to 50 kpc, and comprises Table 3 of the reference paper. In their paper, the authors show the morphology of the unresolved X-ray emission that remains after the cataloged X-ray point sources are excised from the ACIS data, in the context of Spitzer and WISE observations that trace the bubbles, ionization fronts, and photon-dominated regions that characterize MSFRs. In previous work, they have found that this unresolved X-ray emission is dominated by hot plasma from massive star wind shocks. This diffuse X-ray emission is found in every MOXC MSFR, clearly demonstrating that massive star feedback (and the several-million-degree plasmas that it generates) is an integral component of MSFR physics. The Chandra observations used for the Massive Star-forming Regions Omnibus X-ray Catalog (MOXC) are summarized in Table 2 of the reference paper and have dates ranging from 2000-04-03 to 2013-01-31 for the 12 MSFRs: the 7 MYStIX targets NGC 6334, NGC 6357, M 16, M 17, W 3, W 4 and NGC 3576, and the 5 "beyond-MYStIX" targets G333.6-0.2, W 51A, G29.96-0.02, NGC 3603 and 30 Doradus. A similar table to MOXC for other MYStIX targets was presented by Kuhn et al. (2013, ApJS, 209, 27, available as the HEASARC MYSTIXXRAY table). The main difference between that table and the MOXC version is that the present authors have chosen to omit absorption-corrected X-ray source luminosities from the XPHOT algorithm (Getman et al. 2010, ApJ, 708, 1760) herein, because those quantities are given in Broos et al. (2013, ApJS, 209, 32, available as the HEASARC MYSTIXMPCM table) for relevant MYStIX X-ray sources (those classified as pre-main sequence stars). For beyond-MYStIX targets, the authors chose to postpone XPHOT calculations until the X-ray sources were classified, since XPHOT estimates are only appropriate for pre-MS stars. The XPHOT code is available (Getman et al. 2012, Astrophysics Source Code Library, record ascl.soft12002) if others wish to use it on MOXC sources. All photometric quantities in this table are apparent (not corrected for absorption). The HEASARC has used prefixes 'fb_', 'sb_' and 'hb_' (replacing the suffixes '_t', '_s' and '_h' used in the reference paper) on the names of the X-ray photometric quantities which designate the full (total, 0.5 - 8 keV), soft (0.5 - 2.0 keV) and hard (2-8 keV) energy bands. Correction for finite extraction apertures is applied to the ancillary reference file (ARF) calibration products (see Broos et al. 2010, ApJ, 714, 1582, Section 5.3); the total_counts and counts quantities characterize the extraction and are not aperture-corrected. The only calibrated quantities presented are the apparent photon fluxes, in units of photon cm<sup>-2</sup> s<sup>-1</sup> (see Broos et al. 2010, ApJ, 714, 1582, Section 7.4), and estimates for the apparent energy fluxes, in units of erg cm<sup>-2</sup> s<sup>-1</sup> (Getman et al. 2010, ApJ, 708, 1760). This table was created by the HEASARC in October 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/213/1">CDS Catalog J/ApJS/213/1</a> files table3.dat (the MOXC X-ray Source Catalog) and table6.dat (the list of MOXC sources in previously published Chandra catalogs). This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixmpcm
- Title:
- MassiveYoungStar-FormingComplexStdyinIR&X-Rays:MYStIXProbComplexMbrs
- Short Name:
- MYSTIXMPCM
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-forming complex Study in Infrared and X-rays (MYStIX) project requires samples of young stars that are likely members of 20 nearby Galactic massive star-forming regions. Membership is inferred from statistical classification of X-ray sources, from detection of a robust infrared excess that is best explained by circumstellar dust in a disk or infalling envelope and from published spectral types that are unlikely to be found among field stars. This table contains the MYStIX membership lists, which total 31,549 probable complex members. In their reference paper, the authors describe in detail the statistical classification of X-ray sources via a "Naive Bayes Classifier". These membership lists provide the empirical foundation for subsequent MYStIX science studies. The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26), seeks to identify and study samples of young stars in 20 nearby (0.4 < D < 3.6kpc) Galactic massive star-forming regions (MSFRs). These samples are derived using X-ray data from the Chandra X-ray Observatory, near-infrared (NIR) photometry from the United Kingdom InfraRed Telescope (UKIRT) and from the Two Micron All Sky Survey (2MASS), mid-infrared (MIR) photometry from the Spitzer Space Telescope, and from published spectroscopically-identified massive stars. The purpose of this study is to describe the authors' efforts to minimize contaminants in the MYStIX catalogs of young stars. They refer to these latter objects as the "MYStIX Probable Complex Members" or MPCMs. This table contains the combined MPCM catalog for all 20 of the MYStIX MSFRs. This MPCM catalog is the union of three sets of probable members identified by three different established methods for identifying young stars (see Feigelson et al. 2013, ApJS, 209, 26, Fig. 3). Most of the X-ray information on the MPCMs (with the exception of the X-ray luminosities and absorbing column densities obtained using XPHOT) was produced by the ACIS Extract (AE) software package (Broos et al. 2010, ApJ, 714, 1582 and 2012, Astrophysics Source Code Library, 1203.001). The AE software and User's Guide are available at <a href="http://www.astro.psu.edu/xray/acis/acis_analysis.html">http://www.astro.psu.edu/xray/acis/acis_analysis.html</a>. X-ray quantities using the 'fb' prefix are for the full or total energy band from 0.5 - 8.0 keV, those using the 'sb' prefix are for the soft band from 0.5 - 2.0 keV, and those using the 'hb' prefix are for the hard band from 2.0 - 8.0 keV. L. K. Townsley and P. S. Broos (2013, in preparation) and Kuhn et al. (2013, ApJS, 209, 27) identify a few very bright X-ray sources in each region that suffer from a type of instrumental non-linearity known as photon pile-up (<a href="http://cxc.harvard.edu/ciao/why/pileup_intro.html">http://cxc.harvard.edu/ciao/why/pileup_intro.html</a>); X-ray properties reported for those sources are biased and should be used with caution. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/32">CDS Catalog J/ApJS/209/32</a> file mpcm.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixires
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:IR-ExcessSources
- Short Name:
- MYSTIXIRES
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-Forming Complex Study in Infrared and X-rays (MYStIX) project provides a comparative study of 20 Galactic massive star-forming complexes with distances between 0.4 and 3.6 kpc. Probable stellar members in each target complex are identified using X-ray and/or infrared data via two pathways: (1) X-ray detections of young/massive stars with coronal activity/strong winds or (2) infrared excess (IRE) selection of young stellar objects (YSOs) with circumstellar disks and/or protostellar envelopes. In this particular study, the authors present the methodology for the second pathway using Spitzer/IRAC, 2MASS, and UKIRT imaging and photometry. Although IRE selection of YSOs is well-trodden territory, MYStIX presents unique challenges. The target complexes range from relatively nearby clouds in uncrowded fields located toward the outer Galaxy (e.g., NGC 2264, the Flame Nebula) to more distant, massive complexes situated along complicated, inner Galaxy sightlines (e.g., NGC 6357, M 17). The authors combine IR spectral energy distribution (SED) fitting with IR color cuts and spatial clustering analysis to identify IRE sources and to isolate probable YSO members in each MYStIX target field from the myriad types of contaminating sources that can resemble YSOs: extragalactic sources, evolved stars, nebular knots, and even unassociated foreground/background YSOs. Applying their methodology consistently across 18 of the target complexes, they produce the MYStIX IRE Source (MIRES) Catalog comprising 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes. They also classify the SEDs of 9,365 IR counterparts to MYStIX X-ray sources to assist the first pathway, the identification of X-ray-detected stellar members. The MYStIX project, described by Feigelson et al. (2013, ApJS, 209, 26), provides a comprehensive, parallel study of 20 Galactic massive star-forming regions. The basic input data for the MIRES Catalog were near-IR (NIR) and mid-IR (MIR) photometric catalogs. The authors also used NIR and MIR images and mosaics for visualizing the point-source populations with respect to various nebular structures. They provide high-level descriptions of each input catalog in section 2 of the reference paper. This table contains the MYStIX IRE Source (MIRES) Catalog comprising IR data on 20,719 sources, including 8,686 probable stellar members of the MYStIX target complexes, viz., massive star-forming regions (MSFRs), which was given in Table 2 of the reference paper. It does not include the IR data of the above-mentioned 9,365 IR counterparts to MYStIX X-ray sources (the SED Classification of IR Counterparts to MYStIX X-ray sources (SCIM-X Catalog) that were listed in Table 7 of the reference paper. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/31">CDS Catalog J/ApJS/209/31</a> file table2.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixmidi
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:Mid-IRSourceCatalogs
- Short Name:
- MYSTIXMIDI
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Spitzer IRAC observations and stellar photometric catalogs are presented for the Massive Young star-forming complex Study in the Infrared and X-ray (MYStIX). MYStIX is a multi-wavelength census of young stellar members of 20 nearby (distances < 4 kpc), Galactic, star-forming regions (SFRs) that contain at least one O-type star. All regions have data available from the Spitzer Space Telescope consisting of GLIMPSE or other published catalogs for 11 regions and results of the authors' own photometric analysis of archival data for the remaining 9 regions. The authors also reduced the GLIMPSE data for the W 3 SFR using the aperture photometry method in order to compare the results obtained using the two methods (see Section 3.4.2 of the reference paper). The reference paper seeks to construct deep and reliable catalogs of sources from the Spitzer images. Mid-infrared study of these regions faces challenges of crowding and high nebulosity. These new catalogs typically contain fainter sources than existing Spitzer studies, which improves the match rate to Chandra X-ray sources that are likely to be young stars, but increases the possibility of spurious point-source detections, especially peaks in the nebulosity. IRAC color-color diagrams help distinguish spurious detections of nebular polycyclic aromatic hydrocarbon (PAH) emission from the infrared excess associated with dusty disks around young stars. The distributions of sources on the mid-infrared color-magnitude and color-color diagrams reflect differences between MYStIX regions, including astrophysical effects such as stellar ages and disk evolution. The GLIMPSE (Galactic Legacy Infrared Mid-Plane Survey Extraordinaire) Survey is a Legacy Science Program of the Spitzer Space Telescope to study star formation in the disk of the Milky Way Galaxy. It contains six MYStIX regions - the Lagoon Nebula, the Trifid Nebula, NGC 6334, the Eagle Nebula, M 17, and NGC 6357 - within the 2-degree wide strip along the Galactic equator (GLIMPSE I and II data releases). Furthermore, Spitzer images and photometry for RCW 38 and NGC 3576 come from the Vela-Carina survey (Majewski et al. 2007, Spitzer Proposal 40791), using a similar observing strategy with mosaicking and photometric analysis as performed with the GLIMPSE pipeline. The authors obtained publicly available raw IRAC images from the Spitzer Heritage Archive for nine MYStIX regions without GLIMPSE coverage. The target list and details of the Astronomical Observation Requests (AORs) are provided in Table 1 of the reference paper. The camera spatial resolutions are FWHM = 1.6" to 1.9" from 3.6 to 8.0um. This table contains the combined IRAC source lists from the GLIMPSE photometry of W 3 and the aperture photometry of the 9 SFRs listed in Table 4, part 1 of the reference paper. This table was created by the HEASARC in February 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209/29">CDS Catalog J/ApJS/209/29</a> files table2.dat and table3.dat. To distinguish from which table a source originated, the HEASARC has added a parameter called table_number listing the number of the source table, 2 or 3. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/mystixxray
- Title:
- MassiveYoungStar-FormingComplexStudyinIR&X-Rays:X-RaySourceCatalog
- Short Name:
- MYSTIXXRAY
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The Massive Young Star-forming complex Study in Infrared and X-ray (MYStIX) uses data from the Chandra X-Ray Observatory to identify and characterize the young stellar populations in 20 Galactic (d < 4 kpc) massive star-forming regions. In this present study, the X-ray analysis for Chandra ACIS-I observations of 10 of the MYStIX fields is described, and a catalog of > 10,000 X-ray sources is presented in this table. In comparison to other published Chandra source lists for the same regions, the number of MYStIX-detected faint X-ray sources in a region is often doubled. While the higher catalog sensitivity increases the chance of false detections, it also increases the number of matches to infrared stars. X-ray emitting contaminants include foreground stars, background stars, and extragalactic sources. The X-ray properties of sources in these classes are discussed in the reference paper. The X-ray observations were made with the imaging array on the Advanced CCD Imaging Spectrometer (ACIS-I) on board the Chandra X-Ray Observatory. This array of four CCD detectors subtends 17' x 17' on the sky. The number of different Chandra pointings for each region, the total exposures for these pointings, and details of how the observations were taken are provided in Table 1 of the reference paper. Overall, 29 Chandra ObsIDs are included with typical integration times for a pointing of 40 - 100 ks, sufficient to detect most OB stars and lower-mass pre-main-sequence stars down to ~ 0.5 - 1 solar masses for the MYStIX regions. The 10 MYStIX MSFRs treated herein are listed in Table 2 of the reference paper. The data were acquired from the Chandra Data Archive from 2001 Jan to Mar 2008 for 10 MYStIX fields (the Flame Nebula, RCW 36, NGC 2264, the Rosette Nebula, the Lagoon Nebula, NGC 2362, DR 21, RCW 38, Trifid Nebula and NGC 1893). The X-ray photometry is from Broos et al. (2010, ApJ, 714, 1582; ACIS Extract); see also the CCCP, Broos et al. (2011, ApJS, 194, 2). The source significance quantities (fb_prob_no_src, sb_prob_no_src, hb_prob_no_src and prob_no_src_min) are computed using a subset of each source's extractions chosen to maximize significance (Broos et al. 2010, ApJ, 714, 1582, Section 6.2). The source position and positional uncertainty quantities are computed using a subset of each source's extractions chosen to minimize the position uncertainty (Broos et al. 2010, ApJ, 714, 1582, Sections 6.2 and 7.1). All other quantities are computed using a subset of each source's extractions chosen to balance the conflicting goals of minimizing photometric uncertainty and of avoiding photometric bias (Broos et al. 2010, ApJ, 714, 1582, Sections 6.2 and 7). The observed and absorption-corrected energy fluxes and their associated errors and the estimated hydrogen column densities and their uncertainties are derived using non-parametric procedures (XPHOT, Getman et al. 2010, ApJ, 708, 1760). XPHOT assumes the X-ray spectral shapes of young, low-mass stars, which come from coronal X-ray emission. XPHOT quantities will therefore be unreliable for high-mass stars, for which X-ray emission is associated with the stellar wind. This table was created by the HEASARC in January 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/209">CDS Catalog J/ApJS/209</a> 27 file xmystix.dat. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/twomassrsc
- Title:
- 2MASS Redshift Survey (2MRS) Catalog
- Short Name:
- TWOMASSRSC
- Date:
- 14 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table is based on the results of the 2MASS Redshift Survey (2MRS), a ten-year project to map the full three-dimensional distribution of galaxies in the nearby universe. The Two Micron All Sky Survey (2MASS) was completed in 2003 and its final data products, including an extended source catalog (XSC), are available online. The 2MASS XSC contains nearly a million galaxies with K<sub>s</sub> <= 13.5 mag and is essentially complete and mostly unaffected by interstellar extinction and stellar confusion down to a galactic latitude of |b| = 5 degrees for bright galaxies. Near-infrared wavelengths are sensitive to the old stellar populations that dominate galaxy masses, making 2MASS an excellent starting point to study the distribution of matter in the nearby universe. The authors selected a sample of 44,599 2MASS galaxies with K<sub>s</sub> <= 11.75 mag and |b| >= 5 degrees (>= 8 degrees toward the Galactic bulge) as the input catalog for their survey. They obtained spectroscopic observations for 11,000 galaxies and used previously obtained velocities for the remainder of the sample to generate a redshift catalog that is 97.6% complete to well-defined limits and covers 91% of the sky. This provides an unprecedented census of galaxy (baryonic mass) concentrations within 300 Mpc. Earlier versions of their survey have been used in a number of publications that have studied the bulk motion of the Local Group, mapped the density and peculiar velocity fields out to 50 h<sup>-1</sup> Mpc, detected galaxy groups, and estimated the values of several cosmological parameters. Additionally, the authors present morphological types for a nearly complete sub-sample of 20,860 galaxies with K<sub>s</sub> <= 11.25 mag and |b| >= 10 degrees. The authors initially selected 45,086 sources which met the following criteria: <pre> K<sub>s</sub> <= 11.75 mag and detected at H, E(B - V) <= 1 mag, |b| >= 5 degrees for 30 degrees < l < 330 degrees, |b| >= 8 degrees otherwise. </pre> They rejected 324 sources of galactic origin (multiple stars, planetary nebulae, and H II regions) or pieces of galaxies detected as separate sources by the 2MASS pipeline. Additionally, they flagged 314 bona fide galaxies with compromised photometry for reprocessing at a future date. Some of these galaxies have bright stars very close to their nuclei which were not detected by the pipeline. Others are in regions of high stellar density and their center positions and/or isophotal radii have been incorrectly measured by the pipeline. Lastly, some are close pairs or multiples but the pipeline only identified a single object. A detailed explanation of the steps taken to reject and reprocess the flagged galaxies is given in the Appendix of the reference paper. In summary, the final input catalog contained here has 44,599 entries (plotted using black symbols in Figure 1 of the reference paper). In this table, redshifts for 43,533 of the selected galaxies, or 97.6% of the sample, are presented. This table was created by the HEASARC in April 2012 based on an electronic version of Table 3 of the reference paper which was obtained from the ApJS website. This is a service provided by NASA HEASARC .
