- ID:
- ivo://CDS.VizieR/J/ApJ/825/25
- Title:
- Narrow absorption lines of lensed QSO J1029+2623
- Short Name:
- J/ApJ/825/25
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We exploit the widely separated images of the lensed quasar SDSSJ1029+2623 (z_em_=2.197, {theta}=22.5") to observe its outflowing wind through two different sightlines. We present an analysis of three observations, including two with the Subaru telescope in 2010 February and 2014 April, separated by four years, and one with the Very Large Telescope, separated from the second Subaru observation by ~2 months. We detect 66 narrow absorption lines (NALs), of which 24 are classified as intrinsic NALs that are physically associated with the quasar based on partial coverage analysis. The velocities of intrinsic NALs appear to cluster around values of {nu}_ej_~59000, 43000, and 29000km/s, which is reminiscent of filamentary structures obtained by numerical simulations. There are no common intrinsic NALs at the same redshift along the two sightlines, implying that the transverse size of the NAL absorbers should be smaller than the sightline distance between two lensed images. In addition to the NALs with large ejection velocities of {nu}_ej_>1000km/s, we also detect broader proximity absorption lines (PALs) at z_abs_~z_em_. The PALs are likely to arise in outflowing gas at a distance of r<=620pc from the central black hole with an electron density of n_e_>=8.7x10^3^/cm^3^. These limits are based on the assumption that the variability of the lines is due to recombination. We discuss the implications of these results on the three-dimensional structure of the outflow.
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Search Results
- ID:
- ivo://CDS.VizieR/J/ApJS/229/39
- Title:
- Narrow line Seyfert 1 galaxies from SDSS-DR12
- Short Name:
- J/ApJS/229/39
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a new catalog of narrow-line Seyfert 1 (NLSy1) galaxies from the Sloan Digital Sky Survey Data Release 12 (SDSS DR12). This was obtained by a systematic analysis through modeling of the continuum and emission lines of the spectra of all the 68859 SDSS-DR12 objects that are classified as "QSO" by the SDSS spectroscopic pipeline with z<0.8 and a median signal-to-noise ratio (S/N)>2/pixel. This catalog contains a total of 11101 objects, which is about 5 times larger than the previously known NLSy1 galaxies. Their monochromatic continuum luminosity at 5100{AA} is found to be strongly correlated with H{beta}, H{alpha}, and [OIII] emission line luminosities. The optical FeII strength in NLSy1 galaxies is about two times larger than the broad-line Seyfert 1 (BLSy1) galaxies. About 5% of the catalog sources are detected in the FIRST survey. The Eddington ratio ({xi}_Edd_) of NLSy1 galaxies has an average of log({xi}_Edd_) of -0.34, much higher than -1.03 found for BLSy1 galaxies. Their black hole masses (M_BH_) have an average of log(M_BH_) of 6.9M_{sun}_, which is less than BLSy1 galaxies, which have an average of log(M_BH_) of 8.0M_{sun}_. The M_BH_ of NLSy1 galaxies is found to be correlated with their host galaxy velocity dispersion. Our analysis suggests that geometrical effects playing an important role in defining NLSy1 galaxies and their M_BH_ deficit is perhaps due to their lower inclination compared to BLSy1 galaxies.
- ID:
- ivo://CDS.VizieR/J/ApJS/166/128
- Title:
- Narrow line Seyfert 1 galaxies from SDSS-DR3
- Short Name:
- J/ApJS/166/128
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We carried out a systematic search for narrow line Seyfert 1 galaxies (NLS1s) from objects assigned as "QSOs" or "galaxies" in the spectroscopic sample of the Sloan Digital Sky Survey Data Release 3 (SDSS DR3) by a careful modeling of their emission lines and continua. The result is a uniform sample comprising ~2000 NLS1s. This sample dramatically increases the number of known NLS1s by a factor of ~10 over previous compilations. This paper presents the parameters of the prominent emission lines and continua, which were measured accurately with typical uncertainties <10%. Taking advantage of such an unprecedented large and uniform sample with accurately measured spectral parameters, we carried out various statistical analyses, some of which were only possible for the first time.
- ID:
- ivo://CDS.VizieR/J/ApJS/221/32
- Title:
- Narrow MgII absorption lines from SDSS-DR9Q
- Short Name:
- J/ApJS/221/32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using the Data Release 9 Quasar spectra from the Baryonic Oscillation Spectroscopic Survey, which does not include quasar spectra from the Sloan Digital Sky Survey Data Release 7, we detect narrow MgII{lambda}{lambda}2796,2803 absorption doublets in the spectral data redward of 1250{AA} (quasar rest frame) until the red wing of the MgII{lambda}2800 emission line. Our survey is limited to quasar spectra with a median signal-to-noise ratio <S/N>{>=}4/pixel in the surveyed spectral region, resulting in a sample that contains 43260 quasars. We have detected a total of 18598 MgII absorption doublets with 0.2933<=z_abs_<=2.6529. About 75% of absorbers have an equivalent width at rest frame of W_r_^{lambda}2796^. About 75% of absorbers have doublet ratios (DR=W_r_^{lambda}2796^/W_r_^{lambda}2803^) in the range of 1<=DR<=2, and about 3.2% lie outside the range of 1-{sigma}_DR_<=DR<=2+{sigma}_DR_. We characterize the detection false positives/negatives by the frequency of detected MgII absorption doublets in the limits of the S/N of the spectral data. The S/N=4.5 limit is assigned a completeness fraction of 53% and tends to be complete when the S/N is greater than 4.5. The redshift number densities of all of the detected MgII absorbers moderately increase from z~0.4 to z~1.5, which parallels the evolution of the cosmic star formation rate density. Limiting our investigation to those quasars whose emission redshift can be determined from narrow emission lines, the relative velocities ({beta}) of MgII absorbers have a complex distribution which probably consists of three classes of MgII absorbers: (1) cosmologically intervening absorbers; (2) environmental absorbers that reside within the quasar host galaxies or galaxy clusters; (3) quasar outflow absorbers. After subtracting contributions from cosmologically intervening absorbers and environmental absorbers, the {beta} distribution of the MgII might mainly be contributed by the quasar outflow absorbers and peaks at {upsilon}~1500km/s. This peak velocity is lower than the value of 2000km/s found in statistical analysis of CIV absorbers.
- ID:
- ivo://CDS.VizieR/J/ApJS/207/36
- Title:
- 2nd MAXI/GSC catalog in high galactic-latitude sky
- Short Name:
- J/ApJS/207/36
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of high Galactic-latitude (|b|>10{deg}) X-ray sources detected in the first 37 months of data of the Monitor of All-sky X-ray Image/Gas Slit Camera (MAXI/GSC). To achieve the best sensitivity, we develop a background model of the GSC that well reproduces the data based on the detailed on-board calibration. Source detection is performed through image fits with a Poisson likelihood algorithm. The catalog contains 500 objects detected with significances of s_D,4-10keV_>=7 in the 4-10keV band. The limiting sensitivity is ~7.5x10^-12^erg/cm2/s (~0.6mCrab) in the 4-10keV band for 50% of the survey area, which is the highest ever achieved in an all-sky survey mission covering this energy band. We summarize the statistical properties of the catalog and results from cross matching with the Swift/BAT 70 month catalog (Cat. J/ApJS/207/19), the meta-catalog of X-ray detected clusters of galaxies (MCXC; Cat. J/A+A/534/A109), and the MAXI/GSC 7 month catalog (Cat. J/PASJ/63/S677). Our catalog lists the source name (2MAXI), position and its error, detection significances and fluxes in the 4-10keV and 3-4keV bands, the hardness ratio, and the basic information of the likely counterpart available for 296 sources.
- ID:
- ivo://CDS.VizieR/J/ApJ/814/40
- Title:
- Nearby galaxy filaments with UV obs.
- Short Name:
- J/ApJ/814/40
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Simulations of the formation of large-scale structures predict that dark matter, low density highly ionized gas, and galaxies form 10 to 40Mpc scale filaments. These structures are easily recognized in the distribution of galaxies. Here we use Ly{alpha} absorption lines to study the gas in 30x6Mpc filament at cz~3500km/s, defined using a new catalog of nearby (cz<10000km/s) galaxies, which is complete down to a luminosity of about 0.05L_*_ for the region of space analyzed here. Using Hubble Space Telescope spectra of 24 active galactic nuclei, we sample the gas in this filament. All of our sightlines pass outside the virial radius of any known filament galaxy. Within 500kpc of the filament axis the detection rate is ~80%, but no detections are seen more than 2.1Mpc from the filament axis. The width of the Ly{alpha} lines correlates with filament impact parameter and the four BLAs in our sample occur within 400kpc of the filament axis, indicating increased temperature and/or turbulence. Comparing to simulations, we find that the recent Haardt & Madau extragalactic ionizing background predicts a factor of 3-5 too few ionizing photons. Using a more intense radiation field matches the hydrogen density profile within 2.1Mpc of the filament axis, but the simulations still overpredict the detection rate between 2.1 and 5Mpc from the axis. The baryonic mass inside filament galaxies is 1.4x10^13^M_{sun}_, while the mass of filament gas outside galaxy halos is found to be 5.2x10^13^M_{sun}_.
877. Nearby galaxy flows
- ID:
- ivo://CDS.VizieR/J/ApJS/80/479
- Title:
- Nearby galaxy flows
- Short Name:
- J/ApJS/80/479
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Supporting material for an article in the main journal is presented. One table gives measured galaxy distances used to construct a map of observed peculiar velocities, and another table gives a grid of the distribution of light used to construct a map of expected peculiar velocities. A preferred model was developed which gave a best fit between these maps, and this model has been used to generate output kinematic distances which are recorded here for groups and individual galaxies with V_0_<3000km/s.
- ID:
- ivo://CDS.VizieR/J/ApJ/543/178
- Title:
- Nearby Optical Galaxy (NOG) sample
- Short Name:
- J/ApJ/543/178
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- In this paper we describe the Nearby Optical Galaxy (NOG) sample, which is a complete, distance-limited (cz<=6000km/s) and magnitude-limited (B<=14) sample of ~7000 optical galaxies. The sample covers 2/3 (8.27sr) of the sky (|b|>20{deg}) and appears to have a good completeness in redshift (97%). We select the sample on the basis of homogenized corrected total blue magnitudes in order to minimize systematic effects in galaxy sampling. We identify the groups in this sample by means of both the hierarchical and the percolation "friends-of-friends" methods. The resulting catalogs of loose groups appear to be similar and are among the largest catalogs of groups currently available. Most of the NOG galaxies (~60%) are found to be members of galaxy pairs (~580 pairs for a total of ~15% of objects) or groups with at least three members (~500 groups for a total of ~45% of objects). About 40% of galaxies are left ungrouped (field galaxies). We illustrate the main features of the NOG galaxy distribution. Compared to previous optical and IRAS galaxy samples, the NOG provides a denser sampling of the galaxy distribution in the nearby universe. Given its large sky coverage, the identification of groups, and its high-density sampling, the NOG is suited to the analysis of the galaxy density field of the nearby universe, especially on small scales.
- ID:
- ivo://CDS.VizieR/J/AJ/118/2014
- Title:
- Nearby poor clusters of galaxies catalog
- Short Name:
- J/AJ/118/2014
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A catalog of 732 optically selected, nearby poor clusters of galaxies covering the entire sky north of -3{deg} declination is presented. The poor clusters, called WBL clusters, were identified as concentrations of three or more galaxies with photographic magnitudes brighter than 15.7, possessing a galaxy surface overdensity of 10^4/3^. These criteria are consistent with those used in the identification of the original Yerkes poor clusters, and this new catalog substantially increases the sample size of such objects. These poor clusters cover the entire range of galaxy associations up to and including Abell clusters, systematically including poor and rich galaxy systems spanning over 3 orders of magnitude in the cluster mass function. As a result, this new catalog contains a greater diversity of richness and structures than other group catalogs, such as the Hickson and Yerkes catalogs. The information on individual galaxies includes redshifts and cross-references to other galaxy catalogs. The entries for the clusters include redshift (where available) and cross-references to other group and cluster catalogs.
- ID:
- ivo://CDS.VizieR/J/ApJ/750/93
- Title:
- Near-IR observations of XMM-LSS J02182-05102
- Short Name:
- J/ApJ/750/93
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We discuss the structural and morphological properties of galaxies in a z=1.62 proto-cluster using near-IR imaging data from Hubble Space Telescope Wide Field Camera 3 data of the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS). The cluster galaxies exhibit a clear color-morphology relation: galaxies with colors of quiescent stellar populations generally have morphologies consistent with spheroids, and galaxies with colors consistent with ongoing star formation have disk-like and irregular morphologies. The size distribution of the quiescent cluster galaxies shows a deficit of compact (<~1kpc), massive galaxies compared to CANDELS field galaxies at z=1.6. As a result, the cluster quiescent galaxies have larger average effective sizes compared to field galaxies at fixed mass at greater than 90% significance. Combined with data from the literature, the size evolution of quiescent cluster galaxies is relatively slow from z=~1.6 to the present, growing as (1+z)^-0.6+/-0.1^. If this result is generalizable, then it implies that physical processes associated with the denser cluster region seem to have caused accelerated size growth in quiescent galaxies prior to z=1.6 and slower subsequent growth at z<1.6 compared to galaxies in the lower density field. The quiescent cluster galaxies at z=1.6 have higher ellipticities compared to lower redshift samples at fixed mass, and their surface-brightness profiles suggest that they contain extended stellar disks. We argue that the cluster galaxies require dissipationless (i.e., gas-poor or "dry") mergers to reorganize the disk material and to match the relations for ellipticity, stellar mass, size, and color of early-type galaxies in z<1 clusters.
