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81. Baryon Acoustic Oscillations in LRGs
ID:
ivo://CDS.VizieR/J/A+A/542/A34
Title:
Baryon Acoustic Oscillations in LRGs
Short Name:
J/A+A/542/A34
Date:
21 Oct 2021
Publisher:
CDS
Description:
Baryon Acoustic Oscillations (BAO) have been previously detected using correlation functions and power spectra of the galaxy distribution. In this work, we present a new method for the detection of the real-space structures associated with this feature. These baryon acoustic structures are spherical shells with a relatively small density contrast, surrounding high density central regions. We design a specific wavelet adapted to the search for shells, and exploit the physics of the process by making use of two different mass tracers, introducing a specific statistic to detect the BAO features. We apply our method to the detection of BAO in a galaxy sample drawn from the Sloan Digital Sky Survey (SDSS). We use the 'Main' catalogue to trace the shells, and the Luminous Red Galaxies (LRG) as tracers of the high density central regions.
82. Basic galaxy data for spiral-rich group members
ID:
ivo://CDS.VizieR/J/ApJ/791/128
Title:
Basic galaxy data for spiral-rich group members
Short Name:
J/ApJ/791/128
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope, the COS Science Team has conducted a high signal-to-noise survey of 14 bright QSOs. In a previous paper (Savage et al., 2014ApJS..212....8S), these far-UV spectra were used to discover 14 "warm" (T >= 10^5^ K) absorbers using a combination of broad Ly{alpha} and broad O VI absorptions. A reanalysis of a few of this new class of absorbers using slightly relaxed fitting criteria finds as many as 20 warm absorbers could be present in this sample. A shallow, wide spectroscopic galaxy redshift survey has been conducted around these sight lines to investigate the warm absorber environment, which is found to be spiral-rich groups or cluster outskirts with radial velocity dispersions {sigma}=250-750 km/s. While 2{sigma} evidence is presented favoring the hypothesis that these absorptions are associated with the galaxy groups and not with the individual, nearest galaxies, this evidence has considerable systematic uncertainties and is based on a small sample size so it is not entirely conclusive. If the associations are with galaxy groups, the observed frequency of warm absorbers (idN/dz = 3.5-5 per unit redshift) requires them to be very extended as an ensemble on the sky (~1 Mpc in radius at high covering factor). Most likely these warm absorbers are interface gas clouds whose presence implies the existence of a hotter (T ~ 10^6.5^ K), diffuse, and probably very massive (>10^11^ M_{sun}_) intra-group medium which has yet to be detected directly.
83. BATSE occultation catalog of Gamma-Ray sources
ID:
ivo://CDS.VizieR/J/ApJS/127/79
Title:
BATSE occultation catalog of Gamma-Ray sources
Short Name:
J/ApJS/127/79
Date:
21 Oct 2021
Publisher:
CDS
Description:
Using the powerful Earth-occultation technique, long-term, nearly continuous monitoring of the entire low-energy gamma-ray sky is now possible with the advent of BATSE, the Burst and Transient Source Experiment on board the Compton Gamma Ray Observatory (CGRO). In this paper, we present a catalog of 34 moderately strong gamma-ray sources measured by BATSE. It consists of 0.03 - 1.8 MeV photon spectra averaged over weeks and months, and light curves of the 35 - 200 keV flux, with 1 day resolution, covering the first three phases of the CGRO mission (1991 May through 1994 October). This database contains a complete record of {~}1200 daily source count rates in 14 energy channels along with the corresponding Poisson and systematic errors.
84. Bayesian group finder applied to the 2MRS data
ID:
ivo://CDS.VizieR/J/A+A/618/A81
Title:
Bayesian group finder applied to the 2MRS data
Short Name:
J/A+A/618/A81
Date:
21 Oct 2021
Publisher:
CDS
Description:
We propose a probabilistic galaxy group detection algorithm based on marked point processes with interactions. The pattern of galaxy groups in a catalogue is seen as a random set of interacting objects. The positions and the interactions of these objects are governed by a probability density. The parameters of the probability density are chosen using a priori knowledge. The estimator of the unknown cluster pattern is given by the configuration of objects maximising the proposed probability density. Adopting the Bayesian framework, the proposed probability density is maximised using a simulated annealing (SA) algorithm. At fixed temperature, the SA algorithm is a Monte Carlo sampler of the probability density. Hence, the method provides "for free" additional information such as the probabilities that a point or two points in the observation domain belong to the cluster pattern, respectively. These supplementary tools allow the construction of tests and techniques to validate and to refine the detection result. To test the feasibility of the proposed methodology, we applied it to the well-studied 2MASS Redshift Survey (2MRS) data set. Compared to previously published Friends-of-Friends (FoF) group finders, the proposed Bayesian group finder gives overall similar results. However, for specific applications, like the reconstruction of the local Universe, the details of the grouping algorithms are important.
85. Belgrade meridian circle catalog
ID:
ivo://CDS.VizieR/J/other/BOBeo/155.3
Title:
Belgrade meridian circle catalog
Short Name:
J/other/BOBeo/15
Date:
21 Oct 2021
Publisher:
CDS
Description:
The authors present an observational catalogue containing the positions of 351 stars situated in the vicinity of radio sources (RRS2, Tel'nyuk-Adamchuk & Kumkova, 1991, IAU Colloq. 127, 363) worked out by differential method in the FK5 system. The (O-C) corrections to the positions of 267 fundamental stars used in the determination of the instrument parameters are also presented. The star positions are derived from the observations with the Belgrade Large Meridian Circle during 1991-1993.
86. BH masses & host galaxy dispersion vel.
ID:
ivo://CDS.VizieR/J/ApJ/831/134
Title:
BH masses & host galaxy dispersion vel.
Short Name:
J/ApJ/831/134
Date:
21 Oct 2021
Publisher:
CDS
Description:
According to the virial theorem, all gravitational systems in equilibrium sit on a plane in the three-dimensional parameter space defined by their mass, size, and second moment of the velocity tensor. While these quantities cannot be directly observed, there are suitable proxies: the luminosity L_k_, half-light radius R_e_, and dispersion {sigma}_e_. These proxies indeed lie on a very tight fundamental plane (FP). How do the black holes (BHs) in the centers of galaxies relate to the FP? Their masses are known to exhibit no strong correlation with total galaxy mass, but they do correlate weakly with bulge mass (when present), and extremely well with the velocity dispersion through the M_{bullet}_{propto}{sigma}_e_^5.4^ relation. These facts together imply that a tight plane must also exist defined by BH mass, total galaxy mass, and size. Here, I show that this is indeed the case using a heterogeneous set of 230 BHs. The sample includes BHs from zero to 10 billion solar masses and host galaxies ranging from low surface brightness dwarfs, through bulgeless disks, to brightest cluster galaxies. The resulting BH-size-luminosity relation M_{bullet}_{propto}(L_k_/R_e_)^3.8^ has the same amount of scatter as the M_*_-{sigma} relation and is aligned with the galaxy FP, such that it is just a reprojection of {sigma}_e_. The inferred BH-size-mass relation is M_{bullet}_{propto}(M_*_/R_e_)^2.9^. These relationships are universal and extend to galaxies without bulges. This implies that the BH is primarily correlated with its global velocity dispersion and not with the properties of the bulge. I show that the classical bulge-mass relation is a projection of the M_*_-{sigma} relation. When the velocity dispersion cannot be measured (at high z or low dispersions), the BH-size-mass relation should be used as a proxy for BH mass in favor of just galaxy or bulge mass.
87. Bibliography of Surface Photometry of galaxies
ID:
ivo://CDS.VizieR/VII/39A
Title:
Bibliography of Surface Photometry of galaxies
Short Name:
VII/39A
Date:
21 Oct 2021
Publisher:
CDS
Description:
(adapted from the "Documentation for the Machine-Readable Version of the Detailed bibliography of the surface photometry of galaxies by Lee E. Brotzman and Robert S. Hill (ADC), SASC-T-1-5810-5006-84, July 1984) The bibliography supplies coded information about the methods of observation and reduction, types of photometric data, limiting surface brightness, and the general purpose of each paper for about 650 galaxies and 300 references.
88. Bordeaux AC Zone Data Reduced to ACRS
ID:
ivo://CDS.VizieR/I/228
Title:
Bordeaux AC Zone Data Reduced to ACRS
Short Name:
I/228
Date:
21 Oct 2021
Publisher:
CDS
Description:
The U.S. Naval Observatory is in the process of making new reductions of the Astrographic Catalogue (AC) using a modern reference system, the ACRS, which represents the system of the FK5. The data from the Bordeaux Zone, whose plates are centered between declinations +11 and +17 degrees (eq. 1900), have been analyzed for scale, rotation, tilt, coma, magnitude equation, radial distortion and distortions introduced by the use of reseaux in the Carte du Ciel program. The result is a positional catalog of over 223,000 stars on eq. J2000.0, epoch of observation. Additionally, all stars have been matched with the Tycho Input Catalog (revised); those numbers have been added for additional identification purposes.
89. Box- and peanut-shaped bulges. I.
ID:
ivo://CDS.VizieR/J/A+AS/145/405
Title:
Box- and peanut-shaped bulges. I.
Short Name:
J/A+AS/145/405
Date:
21 Oct 2021
Publisher:
CDS
Description:
NIR observations reveal that dust extinction does almost not influence the shape of bulges. There is no substantial difference between the shape of bulges in the optical and in the NIR. Our analysis reveals that 45% of all bulges are box- and peanut-shaped (b/p). The frequency of b/p bulges for all morphological types from S0 to Sd is >40%. In particular, this is for the first time that such a large frequency of b/p bulges is reported for galaxies as late as Sd. The fraction of the observed b/p bulges is large enough to explain the origin of b/p bulges by a barred potential (Luetticke et al., 2000, A&A, accepted).
90. Boxy/peanut-shaped bulges in barred galaxies
ID:
ivo://CDS.VizieR/J/MNRAS/468/2058
Title:
Boxy/peanut-shaped bulges in barred galaxies
Short Name:
J/MNRAS/468/2058
Date:
21 Oct 2021
Publisher:
CDS
Description:
From a sample of 84 local barred, moderately inclined disc galaxies, we determine the fraction that hosts boxy or peanut-shaped (B/P) bulges (the vertically thickened inner parts of bars). We find that the frequency of B/P bulges in barred galaxies is a very strong function of stellar mass: 79 per cent of the bars in galaxies with log (M*/M_{sun}_)w>=10.4 have B/P bulges, while only 12 per cent of those in lower mass galaxies do. (We find a similar dependence in data published by Yoshino & Yamauchi for edge-on galaxies.) There are also strong trends with other galaxy parameters - e.g. Hubble type: 77 per cent of S0-Sbc bars, but only 15 per cent of Sc-Sd bars, have B/P bulges - but these appear to be side effects of the correlations of these parameters with stellar mass. In particular, despite indications from models that a high gas content can suppress bar buckling, we find no evidence that the (atomic) gas mass ratio M_HI+He_/M* affects the presence of B/P bulges, once the stellar-mass dependence is controlled for. The semimajor axes of B/P bulges range from one-quarter to three-quarters of the full bar size, with a mean of R_box_/L_bar_=0.42+/-0.09 and R_box_/a_{epsilon}_=0.53+/-0.12 (where R_box_ is the size of the B/P bulge and a_{epsilon}_ and L_bar_ are lower and upper limits on the size of the bar).

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