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131 results for “AGN”
A Study to Evaluate AGN-151586 Intramuscular Injections in Adult Participants for Treatment of Glabellar Lines
ClinicalTrials.gov study NCT06308198. IPD Sharing: YES. Countries: 3. Publications: 0.
Merger-free AGN-hosts with GALFIT
<p><strong>History</strong></p> <p>This repository contains the data released in the paper "Structural Decomposition of Merger-Free Galaxies Hosting Luminous AGNs" (<em>DOI to follow on publication</em>).</p> <p>We release GALFIT photometric fitting of bulgeless galaxies hosting luminous, Type 1 AGN imaged with the <em>Hubble Space Telescope</em>.</p> <p>-----------------------------------------------------------------------------------------------------</p> <p>v0.1.0 - made structure more user friendly. Fixed Mbh, renamed some columns.</p> <p>The headings within the dataset are as follows:</p> <table> <tbody> <tr> <th>Column Name</th> <th>Description</th> </tr> <tr> <td>gal_ID</td> <td>Assigned DISKDOM galaxy ID</td> </tr> <tr> <td>name</td> <td>SDSS DR16 ID</td> </tr> <tr> <td>RA_deg</td> <td>Galaxy Right Ascension (decimal)</td> </tr> <tr> <td>Dec_deg</td> <td>Galaxy Declination (decimal)</td> </tr> <tr> <td>RA_hms</td> <td>Galaxy Right Ascension</td> </tr> <tr> <td>Dec_dms</td> <td>Galaxy Declination</td> </tr> <tr> <td>z</td> <td>Galaxy Redshift</td> </tr> <tr> <td>z_source</td> <td>Source for obtaining galaxy redshift</td> </tr> <tr> <td>filter</td> <td>HST filter used to image galaxy</td> </tr> <tr> <td>mag_zp</td> <td>HST filter zeropoint (AB Magnitude)</td> </tr> <tr> <td>exp_time</td> <td>HST image exposure time (seconds)</td> </tr> <tr> <td>L_bol</td> <td>Galaxy bolometric luminosity</td> </tr> <tr> <td>PSF_x</td> <td>GALFIT fitted PSF x coordinate</td> </tr> <tr> <td>PSF_y</td> <td>GALFIT fitted PSF y coordinate</td> </tr> <tr> <td>PSF_mag</td> <td>GALFIT fitted PSF magnitude</td> </tr> <tr> <td>comp_i_type</td> <td>Initially assigned component type for Component i</td> </tr> <tr> <td>comp_i_new_type</td> <td>Final assigned component type for Component i (via Kormendy Relation)</td> </tr> <tr> <td>comp_i_mag</td> <td>GALFIT fitted Component i magnitude</td> </tr> <tr> <td>comp_i_SB</td> <td>GALFIT fitted Component i surface brightness</td> </tr> <tr> <td>comp_i_r_eff</td> <td>GALFIT fitted Component i effective radius</td> </tr> <tr> <td>comp_i_n</td> <td>GALFIT fitted Component i Sérsic index</td> </tr> <tr> <td>comp_i_axis_ratio</td> <td>GALFIT fitted Component i axis ratio</td> </tr> <tr> <td>comp_i_PA</td> <td>GALFIT fitted Component i position angle</td> </tr> <tr> <td>comp_i_fourier_mode_amp</td> <td>GALFIT fitted Component i Fourier Mode amplitude</td> </tr> <tr> <td>comp_i_fourier_mode_phase_angle</td> <td>GALFIT fitted Component i Fourier Mode phase angle</td> </tr> <tr> <td>comp_i_diskyness(neg)/boxyness(pos)</td> <td>GALFIT fitted Component i Diskyness/Boxyness parameter</td> </tr> <tr> <td>comp_i_truncation_x</td> <td>GALFIT fitted Component i truncation x coordinate</td> </tr> <tr> <td>comp_i_truncation_y</td> <td>GALFIT fitted Component i truncation y coordinate</td> </tr> <tr> <td>comp_i_truncation_break_radius</td> <td>GALFIT fitted Component i truncation break radius</td> </tr> <tr> <td>comp_i_softening_length</td> <td>GALFIT fitted Component i truncation softening length</td> </tr> <tr> <td>comp_i_truncation_axis_ratio</td> <td>GALFIT fitted Component i truncation axis ratio</td> </tr> <tr> <td>comp_i_truncation_PA</td> <td>GALFIT fitted Component i truncation position angle</td> </tr> <tr> <td>comp_i_spiral_r_inner</td> <td>GALFIT fitted Component i spiral inner radius</td> </tr> <tr> <td>comp_i_spiral_r_outer</td> <td>GALFIT fitted Component i spiral outer radius</td> </tr> <tr> <td>comp_i_spiral_cumul_rotation_to_outer_radius</td> <td>GALFIT fitted Component i spiral cumulative rotation to outer radius</td> </tr> <tr> <td>comp_i_asymptotic_spiral_powerlaw</td> <td>GALFIT fitted Component i asymptotic spiral power law</td> </tr> <tr> <td>comp_i_spiral_inclination_to_L.O.S.</td> <td>GALFIT fitted Component i spiral inclination to L.O.S.</td> </tr> <tr> <td>comp_1_spiral_sky_PA</td> <td>GALFIT fitted Component i spiral sky position angle</td> </tr> <tr> <td>L_tot</td> <td>Total galaxy luminosity (including PSF contribution)</td> </tr> <tr> <td>min_L_tot</td> <td>Minimum total galaxy luminosity (including PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>max_L_tot</td> <td>Maximum total galaxy luminosity (including PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>L_host</td> <td>Total galaxy luminosity (excluding PSF contribution)</td> </tr> <tr> <td>min_L_host</td> <td>Minimum total galaxy luminosity (excluding PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>max_L_host</td> <td>Maximum total galaxy luminosity (excluding PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>L_PSF</td> <td>Galaxy PSF luminosity</td> </tr> <tr> <td>L_ratio_PSF</td> <td>Galaxy PSF luminosity ratio (PSF_Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>min_L_ratio_PSF</td> <td>Minimum galaxy PSF luminosity ratio</td> </tr> <tr> <td>max_L_ratio_PSF</td> <td>Maximum galaxy PSF luminosity ratio</td> </tr> <tr> <td>L_ratio_bulge</td> <td>Galaxy bulge luminosity ratio (Total Bulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>min_L_ratio_bulge</td> <td>Minimum galaxy bulge luminosity ratio</td> </tr> <tr> <td>max_L_ratio_bulge</td> <td>Maximum galaxy bulge luminosity ratio</td> </tr> <tr> <td>L_ratio_pseudobulge</td> <td>Galaxy pseudobulge luminosity ratio (Total Pseudobulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>min_L_ratio_pseudobulge</td> <td>Minimum galaxy pseudobulge luminosity ratio</td> </tr> <tr> <td>max_L_ratio_pseudobulge</td> <td>Maximum galaxy pseudobulge luminosity ratio</td> </tr> <tr> <td>L_ratio_compact_comp</td> <td>Galaxy compact component luminosity ratio (Total Bulge Luminosity + Total Pseudobulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>min_L_ratio_compact_comp</td> <td>Minimum galaxy compact component luminosity ratio</td> </tr> <tr> <td>max_L_ratio_compact_comp</td> <td>Maximum galaxy compact component luminosity ratio</td> </tr> <tr> <td>u_PSF</td> <td>SDSS DR16 galaxy PSF magnitude (u band)</td> </tr> <tr> <td>r_PSF</td> <td>SDSS DR16 galaxy PSF magnitude (r band)</td> </tr> <tr> <td>u_galaxy</td> <td>SDSS DR16 galaxy magnitude (u band)</td> </tr> <tr> <td>r_galaxy</td> <td>SDSS DR16 galaxy magnitude (r band)</td> </tr> <tr> <td>Mstar</td> <td>Galaxy stellar mass (using SDSS DR16 u-r colours)</td> </tr> <tr> <td>Mbh</td> <td>Galaxy black hole mass</td> </tr> </tbody> </table> <p> </p> <p>-----------------------------------------------------------------------------------------------------</p> <p> </p> <p>v0.0.1 - closed pre-release for internal review</p> <p>The headings within the dataset are as follows:</p> <table> <tbody> <tr> <th>Column Name</th> <th>Description</th> </tr> </tbody> <tbody> <tr> <td>Galaxy_ID</td> <td>Assigned DISKDOM galaxy ID</td> </tr> <tr> <td>name</td> <td>SDSS DR16 ID</td> </tr> <tr> <td>RA_deg</td> <td>Galaxy Right Ascension (decimal)</td> </tr> <tr> <td>Dec_deg</td> <td>Galaxy Declination (decimal)</td> </tr> <tr> <td>RA_hms</td> <td>Galaxy Right Ascension</td> </tr> <tr> <td>Dec_dms</td> <td>Galaxy Declination</td> </tr> <tr> <td>z</td> <td>Galaxy Redshift</td> </tr> <tr> <td>z_source</td> <td>Source for obtaining galaxy redshift</td> </tr> <tr> <td>Filter</td> <td>HST filter used to image galaxy</td> </tr> <tr> <td>Magnitude_zeropoint</td> <td>HST filter zeropoint (AB Magnitude)</td> </tr> <tr> <td>Exposure_time</td> <td>HST image exposure time (seconds)</td> </tr> <tr> <td>Bolometric_Luminosity</td> <td>Galaxy bolometric luminosity</td> </tr> <tr> <td>PSF_x_coordinate</td> <td>GALFIT fitted PSF x coordinate</td> </tr> <tr> <td>PSF_y_coordinate</td> <td>GALFIT fitted PSF y coordinate</td> </tr> <tr> <td>PSF_magnitude</td> <td>GALFIT fitted PSF magnitude</td> </tr> <tr> <td>Component_i_type</td> <td>Initially assigned component type for Component i</td> </tr> <tr> <td>Component_i_new_type</td> <td>Final assigned component type for Component i (via Kormendy Relation)</td> </tr> <tr> <td>Component_i_magnitude</td> <td>GALFIT fitted Component i magnitude</td> </tr> <tr> <td>Component_i_surface_brightness</td> <td>GALFIT fitted Component i surface brightness</td> </tr> <tr> <td>Component_i_effective_radius</td> <td>GALFIT fitted Component i effective radius</td> </tr> <tr> <td>Component_i_sersic_index</td> <td>GALFIT fitted Component i Sérsic index</td> </tr> <tr> <td>Component_i_axis_ratio</td> <td>GALFIT fitted Component i axis ratio</td> </tr> <tr> <td>Component_i_position_angle</td> <td>GALFIT fitted Component i position angle</td> </tr> <tr> <td>Component_i_fourier_mode_amplitude</td> <td>GALFIT fitted Component i Fourier Mode amplitude</td> </tr> <tr> <td>Component_i_fourier_mode_phase_angle</td> <td>GALFIT fitted Component i Fourier Mode phase angle</td> </tr> <tr> <td>Component_i_Diskyness(neg)/Boxyness(pos)</td> <td>GALFIT fitted Component i Diskyness/Boxyness parameter</td> </tr> <tr> <td>Component_i_truncation_x_coordinate</td> <td>GALFIT fitted Component i truncation x coordinate</td> </tr> <tr> <td>Component_i_truncation_y_coordinate</td> <td>GALFIT fitted Component i truncation y coordinate</td> </tr> <tr> <td>Component_i_truncation_break_radius</td> <td>GALFIT fitted Component i truncation break radius</td> </tr> <tr> <td>Component_i_truncation_softening_length</td> <td>GALFIT fitted Component i truncation softening length</td> </tr> <tr> <td>Component_i_truncation_axis_ratio</td> <td>GALFIT fitted Component i truncation axis ratio</td> </tr> <tr> <td>Component_i_truncation_position_angle</td> <td>GALFIT fitted Component i truncation position angle</td> </tr> <tr> <td>Component_i_spiral_inner_radius</td> <td>GALFIT fitted Component i spiral inner radius</td> </tr> <tr> <td>Component_i_spiral_outer_radius</td> <td>GALFIT fitted Component i spiral outer radius</td> </tr> <tr> <td>Component_i_spiral_cumulative_rotation_to_outer_radius</td> <td>GALFIT fitted Component i spiral cumulative rotation to outer radius</td> </tr> <tr> <td>Component_i_asymptotic_spiral_power_law</td> <td>GALFIT fitted Component i asymptotic spiral power law</td> </tr> <tr> <td>Component_i_spiral_inclination_to_L.O.S.</td> <td>GALFIT fitted Component i spiral inclination to L.O.S.</td> </tr> <tr> <td>Component_1_spiral_sky_position_angle</td> <td>GALFIT fitted Component i spiral sky position angle</td> </tr> <tr> <td>Total_Galaxy_Luminosity</td> <td>Total galaxy luminosity (including PSF contribution)</td> </tr> <tr> <td>Total_Galaxy_Luminosity_Min</td> <td>Minimum total galaxy luminosity (including PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>Total_Galaxy_Luminosity_Max</td> <td>Maximum total galaxy luminosity (including PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>Total_Host_Galaxy_Luminosity</td> <td>Total galaxy luminosity (excluding PSF contribution)</td> </tr> <tr> <td>Total_Host_Galaxy_Luminosity_Min</td> <td>Minimum total galaxy luminosity (excluding PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>Total_Host_Galaxy_Luminosity_Max</td> <td>Maximum total galaxy luminosity (excluding PSF contribution) using errors from GALFIT fits</td> </tr> <tr> <td>PSF_Luminosity</td> <td>Galaxy PSF luminosity</td> </tr> <tr> <td>PSF_Luminosity_Ratio</td> <td>Galaxy PSF luminosity ratio (PSF_Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>PSF_Luminosity_Ratio_Min</td> <td>Minimum galaxy PSF luminosity ratio</td> </tr> <tr> <td>PSF_Luminosity_Ratio_Max</td> <td>Maximum galaxy PSF luminosity ratio</td> </tr> <tr> <td>Bulge_Luminosity_Ratio</td> <td>Galaxy bulge luminosity ratio (Total Bulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>Bulge_Luminosity_Ratio_Min</td> <td>Minimum galaxy bulge luminosity ratio</td> </tr> <tr> <td>Bulge_Luminosity_Ratio_Max</td> <td>Maximum galaxy bulge luminosity ratio</td> </tr> <tr> <td>Pseudobulge_Luminosity_Ratio</td> <td>Galaxy pseudobulge luminosity ratio (Total Pseudobulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>Pseudobulge_Luminosity_Ratio_Min</td> <td>Minimum galaxy pseudobulge luminosity ratio</td> </tr> <tr> <td>Pseudobulge_Luminosity_Ratio_Max</td> <td>Maximum galaxy pseudobulge luminosity ratio</td> </tr> <tr> <td>Compact_Component_Luminosity_Ratio</td> <td>Galaxy compact component luminosity ratio (Total Bulge Luminosity + Total Pseudobulge Luminosity / Total_Host_Galaxy_Luminosity)</td> </tr> <tr> <td>Compact_Component_Luminosity_Ratio_Min</td> <td>Minimum galaxy compact component luminosity ratio</td> </tr> <tr> <td>Compact_Component_Luminosity_Ratio_Max</td> <td>Maximum galaxy compact component luminosity ratio</td> </tr> <tr> <td>upmag_cone</td> <td>SDSS DR16 galaxy PSF magnitude (u band)</td> </tr> <tr> <td>rpmag_cone</td> <td>SDSS DR16 galaxy PSF magnitude (r band)</td> </tr> <tr> <td>e_upmag_cone</td> <td>SDSS DR16 galaxy PSF magnitude error (u band)</td> </tr> <tr> <td>e_rpmag_cone</td> <td>SDSS DR16 galaxy PSF magnitude error (r band)</td> </tr> <tr> <td>umag</td> <td>SDSS DR16 galaxy magnitude (u band)</td> </tr> <tr> <td>rmag</td> <td>SDSS DR16 galaxy magnitude (r band)</td> </tr> <tr> <td>e_umag</td> <td>SDSS DR16 galaxy magnitude error (u band)</td> </tr> <tr> <td>e_rmag</td> <td>SDSS DR16 galaxy magnitude error (r band)</td> </tr> <tr> <td>Stellar_Mass</td> <td>Galaxy stellar mass (using SDSS DR16 u-r colours)</td> </tr> <tr> <td>Err_Stellar_Mass</td> <td>Galaxy stellar mass error (using SDSS DR16 u-r colours)</td> </tr> <tr> <td>MBH</td> <td>Galaxy black hole mass</td> </tr> <tr> <td>Err_MBH</td> <td>Galaxy black hole mass error</td> </tr> </tbody> </table>
Using AGN-190584 in Subjects Utilizing Single -Use Daily, Contact Lenses
ClinicalTrials.gov study NCT05624320. IPD Sharing: NO. Countries: 0. Publications: 0.
XMM-Newton Bright Serendipitous Survey: AGN X-Ray Spectral Properties
X-ray surveys are a key instrument in the study of active galactic nuclei (AGN). Thanks to their penetrating ability, X-rays are able to map the innermost regions close to the central super massive black hole (SMBH) as well as to detect and characterize its emission up to high redshift. This table contains results from a detailed X-ray spectral analysis of the AGN belonging to the XMM-Newton Bright Serendipitous Survey (XBS, the HEASARC Browse XMMBSS table, <a href="https://cdsarc.cds.unistra.fr/ftp/cats/IX/41">CDS Cat. IX/41</a>). The XBS is composed of two flux-limited samples selected in the complementary 0.5 to 4.5 and 4.5 to 7.5 keV energy bands and comprising more than 300 AGN up to redshift ~2.4. The authors have performed an X-ray analysis following two different approaches: by analyzing individually each AGN X-ray spectrum and by constructing average spectra for different AGN types. From the individual analysis, the authors find that there seems to be an anticorrelation between the spectral index and the sources' hard X-ray luminosity, such that the average photon index for the higher luminosity sources (>10<sup>44</sup> erg s<sup>-1</sup>) is significantly (>2 sigma) flatter than the average for the lower luminosity sources. They also find that the intrinsic column density distribution agrees with AGN unified schemes, although a number of exceptions are found (3% of the whole sample), which are much more common among optically classified type 2 AGN. The authors also find that the so-called "soft-excess", apart from the intrinsic absorption, constitutes the principal deviation from a power-law shape in AGN X-ray spectra and it clearly displays different characteristics, and likely a different origin, for unabsorbed and absorbed AGN. Regarding the shape of the average spectra, they find that it is best reproduced by a combination of an unabsorbed (absorbed) power law, a narrow Fe K-alpha emission line and a small (large) amount of reflection for unabsorbed (absorbed) sources. This table was created by the HEASARC in November 2011 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/530/A42">CDS Catalog J/A+A/530/A42</a> files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
Tartarus: Reduced ASCA AGN Data (Version 3.1)
The Tartarus database contains the results of a detailed but systematic analysis of ASCA observations of active galactic nuclei (AGN). It contains source and background events files, spectra, ancillary response files and response matrices, images, and assorted light curves for a large number of ASCA AGN observations. Spectral fit results are done by automatic XSPEC fitting. This database table allows easy access to reduced AGN data for the whole community, allowing the maximum scientific return from the data. Availability of publishable light curves, images, and spectra (which can also be readily re-fitted) should be particularly valuable to astronomers with little direct experience in the reduction of X-ray data. Version 3.1 has been created by analyzing all ASCA observing sequences with targets designated as AGN, as indicated by a leading "7" in the ASCA observing sequence number. Version 3.1 contains products for all 611 observing sequences designated as AGN observations. This is a significant improvement over Versions 1 and 2. Moreover, the 611 sequences for which products are available are complete in the sense that either the target object was not detected (in which case an upper limit on GIS2 source counts is given) or the intended AGN target was detected and the data were fully analyzed. In order to obtain the most accurate background subtraction and minimize contamination from any nearby sources, version 3.1 makes more use of custom extraction regions than previous versions. It is expected that version 3.1 will be replaced when the final ASCA calibration is completed. This database table has been created by the Tartarus Team, and they, rather than Imperial College London or the HEASARC, are responsible for the contents. It was ingested by the HEASARC in August, 2005. 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 .
CHAMP (Chandra Multiwavelength Project) Hard X-Ray Emitting AGN
This table contains the results from an X-ray and optical analysis of 188 active galactic nuclei (AGN) identified from 497 hard X-ray (observed flux in the (2.0 - 8.0 keV) band > 2.7 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s) sources in 20 Chandra fields (1.5 square degrees) forming part of the Chandra Multiwavelength Project (ChaMP). These medium-depth X-ray observations enable the detection of a representative subset of those sources responsible for the bulk of the 2 - 8 keV cosmic X-ray background. Brighter than the survey's optical spectroscopic limit, the authors achieve a reasonable degree of completeness (77% of X-ray sources with counterparts r' < 22.5 have been classified): broad emission-line AGNs (62%), narrow emission-line galaxies (24%), absorption-line galaxies (7%), stars (5%), or clusters (2%). To construct a pure AGN sample, the authors required the rest-frame 2.0-8.0 keV luminosity (uncorrected for intrinsic absorption) to exceed 10<sup>42</sup> erg s<sup>-1</sup>, thereby excluding any sources that may contain a significant stellar or hot ISM component. The most luminous known star-forming or elliptical galaxies attain at most L<sub>X</sub> = 10<sup>42</sup> erg s<sup>-1</sup>. Since many of the traditional optical AGN signatures are not present in obscured sources, high X-ray luminosity becomes the authors' single discriminant for supermassive black hole accretion. They believe that almost all of the NELGs and ALGs harbor accreting SMBHs based on their X-ray luminosity. They find that 90% of the identified ChaMP sources have luminosities above this threshold. These selection criteria yield a sample of 188 AGNs from 20 Chandra fields with f(2-8 keV) > 2.7 x 10<sup>-15</sup> erg cm<sup>-2</sup> s<sup>-1</sup>, r' < 22.5, and L<sub>X</sub> > 10<sup>42</sup> erg s<sup>-1</sup>. The authors removed five objects identified as clusters based on their extended X-ray emission. This table was created by the HEASARC in March 2007 based on the CDS table J/ApJ/618/123, file table4.dat. This is a service provided by NASA HEASARC .
CHAMP/SDSS Nearby Low-Luminosity AGN Catalog
The combination of the Sloan Digital Sky Survey (SDSS) and the Chandra Multiwavelength Project (ChaMP; Green et al. 2004, ApJS, 150, 43) currently offers the largest and most homogeneously selected sample of nearby galaxies for investigating the relations between X-ray nuclear emission, nebular line emission, black hole masses, and the properties of the associated stellar populations. The authors provide X-ray spectral fits and valid uncertainties for all the galaxies with counts ranging from 2 to 1325 (mean 76, median 19). They present in their paper novel constraints that both X-ray luminosity L<sub>X</sub> and X-ray spectral energy distribution bring to the galaxy evolutionary sequence HII -> Seyfert/Transition Object -> LINER -> Passive suggested by optical data. In particular, the authors show that both L<sub>X</sub> and Gamma, the slope of the power law that best fits the 0.5 - 8 keV spectra, are consistent with a clear decline in the accretion power along the sequence, corresponding to a softening of their spectra. This implies that, at z ~ 0, or at low-luminosity active galactic nucleus (AGN) levels, there is an anticorrelation between Gamma and L/L<sub>Edd</sub>, opposite to the trend which is exhibited by high-z AGN (quasars). The turning point in the Gamma - L/L<sub>Edd</sub> LLAGN + quasars relation occurs near Gamma ~ 1.5 and L/L<sub>Edd</sub> ~ 0.01. Interestingly, this is identical to what stellar mass X-ray binaries exhibit, indicating that the authors have probably found the first empirical evidence for an intrinsic switch in the accretion mode, from advection-dominated flows to standard (disk/corona) accretion modes in supermassive black hole accretors, similar to what has been seen and proposed to happen in stellar mass black hole systems. The anticorrelation the authors find between Gamma and L/L<sub>Edd</sub> may instead indicate that stronger accretion correlates with greater absorption. Therefore, the trend for softer spectra toward more luminous, high-redshift, and strongly accreting (L/L<sub>Edd</sub> >~ 0.01) AGNs/quasars could simply be the result of strong selection biases reflected in the dearth of type 2 quasar detections. The cross-match of all ChaMP sky regions imaged by Chandra/ACIS with the SDSS DR4 spectroscopic footprint results in a parent sample of 15,955 galaxies on or near a chip and a subset of 199 sources that are X-ray detected. Among those, only 107 sources have an off-axis angle (OAA) Theta <0.2 degrees and avoid ccd=8 due to high serial readout noise; these 107 objects comprise the main sample that the authors employ for this study and that are listed in this table. The authors performed direct spectral fits to the X-ray counts distribution using the full instrument calibration, known redshift, and Galactic 21-cm column nH<sub>Gal</sub>. Source spectra were extracted from circular regions with radii corresponding to energy encircled fractions of ~90%, while the background region encompasses a 20 arcsec annulus, centered on the source, with separation 4 arcsecs, from the source region. Any nearby sources were excised, from both the source and the background regions. The spectral fitting was done via yaxx ('Yet Another X-ray eXtractor': Aldcroft 2006, BAAS, 38, 376), an automated script that employs the CIAO Sherpa tool. Each spectrum was fitted in the range 0.5 - 8 keV by two different models: (1) a single power law plus absorption fixed at the Galactic 21-cm value (model 'PL'), and (2) a fixed power law of photon index Gamma = 1.9 plus intrinsic absorption of column nH (model 'PLfix'). For the nine objects with more than 200 counts, the authors employed a third model in which both the slope of the power law and the intrinsic absorption were free to vary (model 'PL_abs'). This table was created by the HEASARC in January 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJ/705/1336/">CDS Catalog J/ApJ/705/1336/</a> file table1.dat. This is a service provided by NASA HEASARC .
Chandra COSMOS Radio-Selected Star-Forming Galaxies and AGN Catalog
X-ray surveys contain sizable numbers of star-forming galaxies, beyond the AGN which usually make up the majority of detections. Many methods to separate the two populations are used in the literature, based on X-ray and multi-wavelength properties. The authors aim at a detailed test of the classification schemes and to study the X-ray properties of the resulting samples. They build on a sample of galaxies selected at 1.4 GHz in the VLA-COSMOS survey, classified by Smolcic et al. (2008, ApJS, 177, 14) according to their optical colors and also observed by Chandra. A similarly selected control sample of AGN is also used for comparison. The authors review some X-ray based classification criteria and check how they affect the sample composition. The efficiency of the classification scheme devised by Smolcic et al. (2008) is such that ~30% of composite/misclassified objects are expected because of the higher X-ray brightness of AGN with respect to galaxies. The latter fraction is actually 50% in the X-ray detected sources, while it is expected to be much lower among X-ray undetected sources. Indeed, the analysis of the stacked spectrum of undetected sources shows, consistently, strongly different properties between the AGN and galaxy samples. X-ray based selection criteria are then used to refine both samples. The radio/X-ray luminosity correlation for star-forming (SF) galaxies is found to hold with the same X-ray/radio ratio valid for nearby galaxies. Some evolution of the ratio may be possible for sources at high redshift or high luminosity, though it is likely explained by a bias arising from the radio selection. Finally, in their paper the authors discuss the X-ray number counts of star-forming galaxies from the VLA- and C-COSMOS surveys according to different selection criteria, and compare them to the similar determination from the Chandra Deep Fields. The classification scheme proposed here may find application in future works and surveys. This table contains the catalogs of radio-selected SF- and AGN-candidate sources with an X-ray detection in C-COSMOS which were contained in Tables 2 and 3 of the reference paper, respectively. The HEASARC has merged these into a single table, adding a new parameter sample which is set to 'SFG' for radio-selected SF-candidate sources from Table 2 and to 'AGN' for the AGN-candidate sources from Table 3. This table was created by the HEASARC in June 2012 based on CDS table J/A+A/542/A16 files table2.dat and table3.dat. This is a service provided by NASA HEASARC .
X-Ray Selected High-z AGN Catalog
This table contains the results from an analysis of the largest high-redshift (z > 3) X-ray-selected active galactic nucleus (AGN) sample to date, combining the Chandra Cosmological Evolution Survey and Chandra Multi-wavelength Project surveys and doubling the previous samples. The sample comprises 209 X-ray-detected AGNs, over a wide range of rest-frame 2-10 keV luminosities log L<sub>X</sub> = 43.3 - 46.0 erg/s. X-ray hardness ratios show that ~39 per cent of the sources are highly obscured, N<sub>H</sub> > 10<sup>22</sup> cm<sup>-2</sup>, in agreement with the ~37 per cent of type-2 AGNs found in this sample based on their optical classification. For ~26 per cent of objects, there are mismatched optical and X-ray classifications. Utilizing the 1/V<sub>max</sub> method, the authors confirm that the comoving space density of all luminosity ranges of AGNs decreases with redshift above z > 3 and up to z ~ 7. With a significant sample of AGNs (N = 27) at z > 4, it is found that both source number counts in the 0.5-2 keV band and comoving space density are consistent with the expectation of a luminosity-dependent density evolution (LDDE) model at all redshifts, while they exclude the luminosity and density evolution (LADE) model. The measured comoving space density of type-1 and type-2 AGNs shows a constant ratio between the two types at z > 3. These results for both AGN types at these redshifts are consistent with the expectations of LDDE model. The high-redshift AGN sample used in this work has been selected from the C-COSMOS X-ray catalog, combining the spectroscopic and photometric information available from the identification catalogue of X-ray C-COSMOS sources (Civano et al. 2011, ApJ, 741, 91; 2012, ApJS, 201, 30) and the ChaMP (Chandra Multi-wavelength Project) X-ray catalog using only the 323 ChaMP ObsIDs overlapping with Sloan Digital Sky Survey (SDSS; Richards et al. 2006, AJ, 131, 2766) DR5 imaging. This table was created by the HEASARC in March 2016 based on the <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/445/1430">CDS catalog J/MNRAS/445/1430</a> file tablea1.dat. This is a service provided by NASA HEASARC .
XTE All-Sky Slew Survey AGN Catalog
This table contains the RXTE All-Sky Slew Survey Catalog of AGN and AGN candidates. The catalog authors compiled a sample of 95 AGNs which were serendipitously detected in the 3-20 keV band at Galactic latitude |b| > 10 degrees during the RXTE Slew Survey (XSS, Revnivtsev et al., CDS Cat. <J/A+A/418/927>), and utilized it to study the statistical properties of the local population of AGN, including the X-ray luminosity function and absorption distribution. They find that among low X-ray luminosity (L<sub>X</sub> < 10<sup>43.5</sup> erg/s) AGN, the ratio of absorbed (characterized by intrinsic absorption in the range 10<sup>22</sup> cm<sup>-2</sup> < N<sub>H</sub> < 10<sup>24</sup> cm<sup>-2</sup>) and unabsorbed (N<sub>H</sub> < 10<sup>22</sup> cm<sup>-2</sup>) objects is 2:1, while this ratio drops to less than 1:5 for higher luminosity AGN. The summed X-ray output of AGN with L<sub>X</sub> > 10<sup>41</sup> erg/s estimated here is smaller than the earlier estimated total X-ray volume emissivity in the local Universe, suggesting that a comparable X-ray flux may be produced together by lower luminosity AGN, non-active galaxies and clusters of galaxies. The authors also presented a sample of 35 AGN candidates, composed of unidentified XSS sources. Most of these AGN belong to the local population (z < 0.1). For each confirmed AGN source, the following information is provided: AGN class, the count rate in two energy bands (3-8 keV and 8-20 keV), the observed and intrinsic (absorption-corrected) luminosity in the 3 - 20keV band, and the intrinsic absorption column density. For the AGN candidates, composed of unidentified XSS sources, the following information is provided: the count rate in two energy bands (3-8 keV and 8-20 keV), the estimated intrinsic absorption column density, and information about RASS Bright Source Catalog and HEAO A-1 X-ray source counterparts. This table was created by the HEASARC in December 2004 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/423/469">CDS Catalog J/A+A/423/469</a>, table1.dat and table2.dat (the corrected version of 01-Dec-2004). This is a service provided by NASA HEASARC .
WISE/2MASS/RASS (W2R) AGN Sample Catalog
The authors of this catalog have developed the S<sub>IX</sub> statistic to identify bright, highly likely active galactic nucleus (AGN) candidates solely on the basis of Wide-field Infrared Survey Explorer (WISE), Two-Micron All-Sky Survey (2MASS), and ROSAT All-Sky Survey (RASS) data. This statistic was optimized with data from the preliminary WISE survey and the Sloan Digital Sky Survey, and tested with Lick 3 m Kast spectroscopy. The authors find that sources with S<sub>IX</sub> < 0 have a >~ 95% likelihood of being an AGN (defined in this paper as a Seyfert 1, quasar, or blazar). This statistic was then applied to the full WISE/2MASS/RASS dataset, including the final WISE data release, to yield the "W2R" sample of 4316 sources with S<sub>IX</sub> < 0. Only 2209 of these sources are currently in the Veron-Cetty and Veron (VCV) Catalog of spectroscopically confirmed AGNs, indicating that the W2R sample contains nearly 2000 new, relatively bright (J <~ 16) AGNs. The authors utilize the W2R sample to quantify biases and incompleteness in the VCV Catalog. They find that it is highly complete for bright (J < 14), northern AGNs, but the completeness drops below 50% for fainter, southern samples and for sources near the Galactic plane. This approach also led to the spectroscopic identification of 10 new AGNs in the Kepler field, more than doubling the number of AGNs being monitored by Kepler. The W2R sample contains better than 1 bright AGN every 10 deg<sup>2</sup>, permitting construction of AGN samples in any sufficiently large region of sky. This table contains the 4316 sources comprising the W2R sample. This table was created by the HEASARC in June 2012 based on an electronic version of Table 3 from the reference paper which was obtained from the ApJ website. This is a service provided by NASA HEASARC .
ROSAT All-Sky Survey and SDSS DR5 Sample of X-Ray Emitting AGN
This table contains further results of a program aimed at yielding ~ 10<sup>4</sup> fully characterized optical identifications of ROSAT X-ray sources. The program employs X-ray data from the ROSAT All Sky Survey (RASS) and both optical imaging and spectroscopic data from the Sloan Digital Sky Survey (SDSS). RASS/SDSS data from 5740 deg<sup>2</sup> of sky spectroscopically covered in SDSS Data Release 5 (DR5) provide an expanded catalog of 7000 confirmed quasars and other active galactic nuclei (AGN) that are probable RASS identifications. Again, in this expanded catalog the identifications as X-ray sources are statistically secure, with only a few percent of the SDSS AGNs likely to be randomly superposed on unrelated RASS X-ray sources. Most identifications continue to be quasars and Seyfert 1 galaxies with 15 < m < 21 and 0.01 < z < 4, but the total sample size has grown to include very substantial numbers of even quite rare AGN, e.g., it now includes several hundreds of candidate X-ray-emitting BL Lac objects and narrow-line Seyfert 1 galaxies. In addition to exploring rare subpopulations, such a large total sample may be useful when considering correlations between the X-ray and the optical and may also serve as a resource list from which to select the ``best'' object (e.g., the X-ray-brightest AGN of a certain subclass at a preferred redshift or luminosity) for follow-up X-ray spectral or alternate detailed studies. Much more information on the SDSS is available at the project's web site at <a href="http://www.sdss.org/">http://www.sdss.org/</a>. This table was created by the HEASARC in February 2007 based on the combination of the electronic versions of tables 1 through 6 from the above reference which were obtained from the electronic AJ website. It replaces a previous version containing the results presented by Anderson et al. (2003, AJ, 126, 2209) which were based on a cross-correlation of the RASS with optical data from very early on in the SDSS program, e.g., extending back to the 'Early Data Release' before SDSS photometric calibrations were complete. This is a service provided by NASA HEASARC .
INTEGRAL IBIS AGN Catalog
In this work, the authors present the most comprehensive INTEGRAL active galactic nucleus (AGN) sample. It lists 272 AGN for which they have secure optical identifications, precise optical spectroscopy and measured redshift values plus X-ray spectral information, i.e. 2-10 and 20-100 keV fluxes plus column densities. In their paper, the authors mainly use this sample to study the absorption properties of active galaxies, to probe new AGN classes and to test the AGN unification scheme. The authors find that half (48%) of the sample is absorbed, while the fraction of Compton-thick AGN is small (~7%). In line with their previous analysis, they have however shown that when the bias towards heavily absorbed objects which are lost if weak and at large distance is removed, as is possible in the local Universe, the above fractions increase to become 80% and 17%, respectively. The authors also find that absorption is a function of source luminosity, which implies some evolution in the obscuration properties of AGN. A few peculiar classes, so far poorly studied in the hard X-ray band, have been detected and studied for the first time such as 5 X-ray bright optically normal galaxies (XBONGs), 5 type 2 QSOs and 11 low-ionization nuclear emission regions. In terms of optical classification, this sample contains 57% type 1 and 43% type 2 AGN; this subdivision is similar to that found in X-rays if unabsorbed versus absorbed objects are considered, suggesting that the match between optical and X-ray classifications is on the whole good. Only a small percentage of sources (12%) does not fulfill the expectation of the unified theory as the authors find 22 type 1 AGN which are absorbed and 10 type 2 AGN which are unabsorbed. Studying in depth these outliers they found that most of the absorbed type 1 AGN have X-ray spectra characterized by either complex or warm/ionized absorption more likely due to ionized gas located in an accretion disc wind or in the bi-conical structure associated with the central nucleus, therefore unrelated to the toroidal structure. Among the 10 type 2 AGN which are unabsorbed, at most 3-4% are still eligible to be classified as 'true' type 2 AGN. In the fourth INTEGRAL/IBIS survey (Bird et al. 2010, ApJS, 186, 1, available in the HEASARC database as the IBISCAT4 table), there are 234 objects which have been identified with AGN. To this set of sources, the present authors then added 38 galaxies listed in the INTEGRAL all-sky survey by Krivonos et al. (2007, A&A, 475, 775, available in the HEASARC database as the INTIBISASS table) updated on the website (<a href="http://hea.iki.rssi.ru/integral/survey/catalog.php">http://hea.iki.rssi.ru/integral/survey/catalog.php</a>) but not included in the Bird et al. catalog due to the different sky coverage (these latter sources are indicated with hard_flag = 'h' values in this HEASARC table). The final data set presented and discussed in the reference paper and constituting this table therefore comprises 272 AGN and was last updated in March 2011 March. It represents the most complete view of the INTEGRAL extragalactic sky as of the date of publication in 2012. This table was created by the HEASARC in October 2014 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/MNRAS/426/1750">CDS Catalog J/MNRAS/426/1750</a> files tablea1.dat and refs.dat. This is a service provided by NASA HEASARC .
XMM-COSMOS Catalog of X-Ray Selected Type 1 AGN
This table contains the results from a study of the X-ray to optical properties of a sample of 545 X-ray selected Type 1 AGN, from the XMM-Newton Cosmic Evolution (XMM-COSMOS) survey, over a wide range of redshifts (0.04 < z < 4.25) and X-ray luminosities (40.6 <= log(L<sub>2-10keV</sub>) <= 45.3). About 60% of them are spectroscopically identified Type 1 AGN, while the others have a reliable photometric redshift and are classified as Type 1 AGN on the basis of their multi-band Spectral Energy Distributions (SEDs). In the reference, the authors discuss the relationship between UV and X-ray luminosity, as parametrized by the X-ray to optical-UX alpha<sub>ox</sub> spectral slope, and its dependence on redshift and luminosity. Herein optical and X-ray properties for 545 Type 1 AGN in XMM-COSMOS are presented. For each source, X-ray ID, spectroscopic redshift, photometric redshift, upper error on the photometric redshift, lower error on the photometric redshift, logarithm of the monochromatic luminosity at 2500 Angstroms, logarithm of the monochromatic luminosity at 2 keV, alpha<sub>ox</sub>, logarithm of the 2-10 keV luminosity, logarithm of the bolometric luminosity in solar units, bolometric correction, photometric classification, logarithm of the Eddington ratio, logarithm of the black hole mass in solar masses, and a flag for the 2-10 keV detection (flag = 1 [343 entries] means a detection in the 2-10 keV band, while flag = 0 is for 2-10 keV upper limits) are given. This table was created by the HEASARC in May 2010 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/512/A34">CDS catalog J/A+A/512/A34</a> file table2.dat. This is a service provided by NASA HEASARC .
Fermi LAT Fourth AGN Catalog
This is the third update to the fourth catalog of active galactic nuclei (AGNs) detected by the Fermi Large Area Telescope (LAT). This version (4LAC-DR3) derives from the third data release of the 4FGL catalog based on 12 years of gamma-ray data with energies greater than 50 MeV. The spectral parameters, spectral energy distributions (SEDs), yearly light curves, and associations have been updated for all sources. The catalog contains includes 3407 AGN located at high Galactic latitudes (|b| > 10 degrees). This database table was first ingested by the HEASARC in February 2010. It was last updated (to the 4LAC-DR3 version) in June 2023 using electronic data obtained from the Fermi Science Support Center (FSSC). That data is available at <a href="https://fermi.gsfc.nasa.gov/ssc/data/access/lat/4LACDR3/">https://fermi.gsfc.nasa.gov/ssc/data/access/lat/4LACDR3/</a>. Note that this table does not contain the low-latitude sources given in a separate file there, which are not formally a part of the catalog. This is a service provided by NASA HEASARC .
VeronCatalogofQuasars&AGN,13thEdition
This database table contains the 13th edition of the Catalog of Quasars and Active Galactic Nuclei by Veron-Cetty and Veron, and is an update of the previous versions. As in the previous editions, no information about absorption lines or X-ray properties is given, but absolute magnitides are provided, assuming a Hubble constant H<sub>0</sub> = 71 km/s/Mpc and a deceleration parameter q<sub>0</sub> = 0 (notice the change of cosmology from previous editions in which H<sub>0</sub> was assumed to be 50 km/s/Mpc). The present edition of this catalog contains 133336 quasars, 1374 BL Lac objects and 34231 active galaxies (including 15627 Seyfert 1 galaxies), for a grand total of 168941 objects, significantly more than the number of objects listed in the 12th edition (108080). The 13th edition includes positions and redshifts, as well as photometry (U, B, and V) and 6-cm and 20-cm flux densities, when available. 178 objects once proposed but now rejected as quasars are NOT included in the online version of this catalog: their names and positions are listed in the file <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/258/reject.dat">https://cdsarc.cds.unistra.fr/ftp/cats/VII/258/reject.dat</a>. This HEASARC table also does NOT contain the additional information on gravitationally lensed quasars and quasar pairs listed in Tables 3 and 4 of the published paper: these tables are available in electronic form at the CDS <a href="https://cdsarc.cds.unistra.fr/ftp/cats/VII/248/">https://cdsarc.cds.unistra.fr/ftp/cats/VII/248/</a> files table2.dat and table3.dat (sic). The present edition of this catalog contains quasars with measured redshift known prior to July 1st, 2009. This online catalog was created by the HEASARC in April 2010 based on machine-readable tables obtained from the CDS (their catalog VII/258, files qso.dat, bllac.dat, and agn.dat). It was last updated in June 2012 to tweak some class values. This is a service provided by NASA HEASARC .
Lockman Hole AGN Optical and Infrared Properties Catalog
This table contains the observed-frame optical, near-infrared, and mid-infrared properties of X-ray-selected active galactic nuclei (AGN) in the Lockman Hole. Using a likelihood ratio method on optical, near-infrared or mid-infrared catalogs, the authors assigned counterparts to 401 out of the 409 X-ray sources of the XMM-Newton catalog (Brunner et al. 2008, A&A, 479, 283). Accurate photometry was collected for all the sources from U to 24 microns. The authors used X-ray and optical criteria to remove any normal galaxies, galactic stars, or X-ray clusters among them and studied the multi-wavelength properties of the remaining 377 AGN in their paper. They used a mid-IR colour-colour selection to understand the AGN contribution to the optical and infrared emission. Using this selection, they identified different behaviours of AGN-dominated and host-dominated sources in X-ray-optical-infrared color-color diagrams. More specifically, the AGN-dominated sources show a clear trend in the f<sub>x</sub>/f<sub>RC</sub> vs. R<sub>C</sub> - K and f<sub>24um</sub>/f<sub>RC</sub> vs. R<sub>C</sub> - K diagrams, while the hosts follow the behaviour of non-X-ray detected galaxies. In the optical-near-infrared color-magnitude diagram, the known trend of redder objects to be more obscured in X-rays is seen to be stronger for AGN-dominated than for host-dominated systems. This is an indication that the trend is more related to the AGN, which contaminate the overall colors, than to any evolutionary effects, the authors believe. Finally, the authors find that a significant fraction (~30%) of the reddest AGN are not obscured in X-rays. The X-ray observations of the Lockman Hole took place between April 2000 and December 2002 with XMM-Newton. The optical observations of the Lockman Hole were conducted with the Large Binocular Telescope (U, B, V bands) and the Subaru Telescope (R<sub>C</sub>, I<sub>C</sub>, z' bands). The LBT observations were taken from February 2007 to March 2009. The R<sub>C</sub>, I<sub>C</sub>, and z' bands have been observed with the Suprime-Cam of the Subaru telescope between November 2001 and April 2002. This table contains the properties of the counterparts to all 409 X-ray sources listed in the Lockman Hole XMM-Newton source catalog of Brunner et al. (2008, A&A, 479, 283), including the 377 AGN and also the 32 objects classified as Galactic stars, galaxy clusters or galaxies. For 8 (2%) of the 409 X-ray sources no optical or IR counterparts were found. These 8 objects are listed in this table with null positional values. This table was created by the HEASARC in January 2012 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/529/A135">CDS Catalog J/A+A/529/A135</a> file table2.dat. This is a service provided by NASA HEASARC .
XMM-COSMOS X-Ray Selected Type-2 AGN
This table contains the results from a study of the multi-wavelength (from the mid-infrared to the hard X-ray) properties of a sample of 255 spectroscopically identified X-ray selected Type-2 AGN from the XMM-COSMOS survey. Most of them are obscured and the X-ray absorbing column density is determined by either X-ray spectral analyses (for 45% of the sample), or from hardness ratios. Spectral energy distributions (SEDs) were computed for all sources in the sample. The average SEDs in the optical band are dominated by the host-galaxy light, especially at low X-ray luminosities and redshifts. There is also a trend between X-ray and mid-infrared luminosity: the AGN contribution in the infrared is higher at higher X-ray luminosities. The authors have calculated bolometric luminosities, bolometric corrections, stellar masses and star formation rates (SFRs) for these sources using multi-component modeling to properly disentangle the emission associated with stellar light from that due to black hole accretion. For 90% of the sample, they also have the morphological classifications obtained with an upgraded version of the Zurich estimator of structural types (ZEST+). The authors find that, on average, type-2 AGN have lower bolometric corrections than type-1 AGN. Moreover, they confirm that the morphologies of AGN host-galaxies indicate that there is a preference for these type-2 AGN to be hosted in bulge-dominated galaxies with stellar masses greater than 10<sup>10</sup> solar masses. For each source, this table contains the X-ray ID, spectroscopic redshift, logarithm of the 2-10keV luminosity, logarithm of the bolometric luminosity, bolometric correction, logarithm of the stellar mass, star formation rate, absolute magnitude M<sub>U</sub>, absolute magnitude M<sub>V</sub>, absolute magnitude M<sub>J</sub> (Johnson-Kron-Cousin system), and the morphological class. This table was created by the HEASARC in October 2011 based on CDS table J/A+A/534/A110 file table1.dat. 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 .
COSMOS 3GHz AGN Catalog
The VLA-COSMOS 3 GHz AGN catalog includes classification and selected physical properties for the 3 GHz radio sample with optical/NIR counterparts (7 903 sources in total). For more information see Delvecchio et al. (2017).
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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.