- ID:
- ivo://CDS.VizieR/J/A+A/606/A12
- Title:
- MUSE-Wide survey: 831 emission line galaxies
- Short Name:
- J/A+A/606/A12
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a first instalment of the MUSE-Wide survey, covering an area of 22.2 arcmin^2^ (corresponding to ~20% of the final survey) in the CANDELS/Deep area of the Chandra Deep Field South. We use the MUSE integral field spectrograph at the ESO VLT to conduct a full-area spectroscopic mapping at a depth of 1h exposure time per 1-arcmin^2^ pointing. We searched for compact emission line objects using our newly developed LSDCat software based on a 3-D matched filtering approach, followed by interactive classification and redshift measurement of the sources. Our catalogue contains 831 distinct emission line galaxies with redshifts ranging from 0.04 to 6. Roughly one third (237) of the emission line sources are Lyman{alpha} emitting galaxies with 3<z<6, only four of which had previously measured spectroscopic redshifts. At lower redshifts 351 galaxies are detected primarily by their [OII] emission line (0.3<~z<~1.5), 189 by their [OIII] line (0.21<~z<~0.85), and 46 by their H{alpha} line (0.04<~z<~0.42). Comparing our spectroscopic redshifts to photometric redshift estimates from the literature, we find excellent agreement for z<1.5 with a median {Delta}z of only ~4x10^-4^ and an outlier rate of 6%, however a significant systematic offset of {Delta}z=0.26 and an outlier rate of 23% for Ly{alpha} emitters at z>3. Together with the catalogue we also release 1D PSF-weighted extracted spectra and small 3D datacubes centred on each of the 831 sources.
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- ID:
- ivo://CDS.VizieR/J/ApJ/772/131
- Title:
- Musket Ball Cluster redshift catalog
- Short Name:
- J/ApJ/772/131
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Merging galaxy clusters have become one of the most important probes of dark matter, providing evidence for dark matter over modified gravity and even constraints on the dark matter self-interaction cross-section. To properly constrain the dark matter cross-section it is necessary to understand the dynamics of the merger, as the inferred cross-section is a function of both the velocity of the collision and the observed time since collision. While the best understanding of merging system dynamics comes from N-body simulations, these are computationally intensive and often explore only a limited volume of the merger phase space allowed by observed parameter uncertainty. Simple analytic models exist but the assumptions of these methods invalidate their results near the collision time, plus error propagation of the highly correlated merger parameters is unfeasible. To address these weaknesses I develop a Monte Carlo method to discern the properties of dissociative mergers and propagate the uncertainty of the measured cluster parameters in an accurate and Bayesian manner. I introduce this method, verify it against an existing hydrodynamic N-body simulation, and apply it to two known dissociative mergers: 1ES 0657-558 (Bullet Cluster) and DLSCL J0916.2+2951 (Musket Ball Cluster).
- ID:
- ivo://CDS.VizieR/J/ApJS/115/1
- Title:
- MX northern Abell cluster redshift survey
- Short Name:
- J/ApJS/115/1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The results from the COBE satellite show the existence of structure on scales ~ 10% or more of the horizon scale of the universe. Rich clusters of galaxies from the Abell/Abell, Corwin, & Olowin catalogs (Cat. <VII/110>) show evidence of structure on scales of 100h^-1^Mpc and hold the promise of confirming structure on the scale of the COBE results. An impediment to that promise has been that redshift information has been unavailable for a large percentage of these clusters, so knowledge of their three-dimensional distribution has had large uncertainties. We have been working to greatly expand the sample of Abell clusters with reliable redshifts. Our approach in this effort, through the MX Northern Abell Cluster Redshift Survey, has been to measure redshifts of at least 25 galaxies in each of 95 R>=1 Abell cluster fields with m_10_<=16.8 and zero or one previously measured redshift. Of these 95 observed Abell clusters, 88 new cluster redshifts were obtained with an average of nine cluster member galaxy redshifts per field. Two clusters were found to be chance projections of galaxies along the line of sight, while five cluster observations did not provide enough galaxy redshifts to make a positive identification. This work has resulted in a deeper, 98% complete, and more reliable sample of three-dimensional positions of rich Abell clusters in the northern hemisphere. The primary intent of this survey has been to produce a larger and more complete sample of rich Abell clusters that can be used as tracers for large-scale structure. Through analyses with tools such as the two-point correlation function, power spectrum, and velocity dispersions, this sample can be used to constrain theoretical models better for the formation of structure we see in the universe today.
- ID:
- ivo://CDS.VizieR/J/AJ/124/1918
- Title:
- MX northern Abell cluster redshift survey. II.
- Short Name:
- J/AJ/124/1918
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The MX Northern Abell Cluster Survey II is the final stage of a program designed to observe rich Abell clusters with m10<=17.0. We present 1542 new galaxy redshifts within 117 R>=1 Abell cluster fields that have 16.9<=m10<=17.0, 0h<=RA<=24h, -17{deg}<=DE<=90{deg}, and |b|>=30{deg}. Of the 117 clusters observed for the MX Survey II, 105 new cluster redshifts were obtained with an average of eight cluster member galaxy redshifts.
- 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}_.
- 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.
