- ID:
- ivo://CDS.VizieR/J/other/PASA/33.45
- Title:
- FRBCAT: The Fast Radio Burst (FRB) Catalog
- Short Name:
- J/other/PASA/33.
- Date:
- 06 Dec 2021 20:29:39
- Publisher:
- CDS
- Description:
- Here, we present a catalogue of known Fast Radio Burst sources in the form of an online catalogue, FRBCAT. The catalogue includes information about the instrumentation used for the observations for each detected burst, the measured quantities from each observation, and model-dependent quantities derived from observed quantities. To aid in consistent comparisons of burst properties such as width and signal-to-noise ratios, we have re-processed all the bursts for which we have access to the raw data, with software which we make available. The originally derived properties are also listed for comparison.
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- ID:
- ivo://CDS.VizieR/J/A+A/609/A1
- Title:
- FR0CAT. a FIRST catalog of FR 0 radio galaxies
- Short Name:
- J/A+A/609/A1
- Date:
- 04 Jan 2022 14:18:36
- Publisher:
- CDS
- Description:
- With the aim of exploring the properties of the class of FR 0 radio galaxies, we selected a sample of 108 compact radio sources, called FR0CAT, by combining observations from the NVSS, FIRST, and SDSS surveys. We included in the catalog sources with redshift <=0.05, with a radio size <=5kpc, and with an optical spectrum characteristic of low-excitation galaxies. Their radio luminosities at 1.4GHz are in the range 10^38^<={nu}L_1.4_<=10^40^erg/s. The FR0CAT hosts are mostly (86%) luminous (-21>=M_r_>=-23) red early-type galaxies with black hole masses 10^8^<=M_BH_<=10^9^M_{sun}_. These properties are similar to those seen for the hosts of FR I radio galaxies, but they are on average a factor ~1.6 less massive. The number density of FR0CAT sources is ~5 times higher than that of FR Is, and thus they represent the dominant population of radio sources in the local Universe. Different scenarios are considered to account for the smaller sizes and larger abundance of FR 0s with respect to FR Is. An age-size scenario that considers FR 0s as young radio galaxies that will all eventually evolve into extended radio sources cannot be reconciled with the large space density of FR 0s. However, the radio activity recurrence, with the duration of the active phase covering a wide range of values and with short active periods strongly favored with respect to longer ones, might account for their large density number. Alternatively, the jet properties of FR 0s might be intrinsically different from those of the FR Is, the former class having lower bulk Lorentz factors, possibly due to lower black hole spins. Our study indicates that FR 0s and FR I/IIs can be interpreted as two extremes of a continuous population of radio sources that is characterized by a broad distribution of sizes and luminosities of their extended radio emission, but shares a single class of host galaxies.
- ID:
- ivo://CDS.VizieR/J/MNRAS/446/683
- Title:
- Free-form lensing grid solution for A1689
- Short Name:
- J/MNRAS/446/683
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We examine Abell 1689 non-parametrically, combining strongly lensed Hubble Space Telescope images and weak distortions from wider field Subaru imaging. Our model incorporates member galaxies to improve the lens solution. By adding luminosity-scaled member galaxy deflections to our smooth grid, we can derive meaningful solutions with sufficient accuracy to permit the identification of our own strongly lensed images, so our model becomes self-consistent. We identify 11 new multiply lensed system candidates and clarify previously ambiguous cases, in the deepest optical and near-infrared data to date from Hubble and Subaru. Our improved spatial resolution brings up new features not seen when the weak and strong lensing effects are used separately, including clumps and filamentary dark matter around the main halo. Our treatment means we can obtain an objective mass ratio between the cluster and galaxy components. We find a typical mass-to-light ratios of M/L_B_=21+/-14 inside the r<1arcmin region. Our model independence means we can objectively evaluate the competitiveness of stacking cluster lenses for defining the geometric lensing-distance-redshift relation in a model-independent way.
- ID:
- ivo://CDS.VizieR/J/A+A/506/471
- Title:
- Frequency analysis of CoRoT B stars
- Short Name:
- J/A+A/506/471
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We search for new variable B-type pulsators in the CoRoT data assembled primarily for planet detection, as part of CoRoT's Additional Programme. We aim to explore the properties of newly discovered B-type pulsators from the uninterrupted CoRoT spacebased photometry and to compare them with those of known members of the beta Cep and slowly pulsating B star (SPB) classes. We developed automated data analysis tools which include algorithms for jump correction, light curve detrending, frequency detection, frequency combination search and frequency and period spacing search. Besides numerous new classical slowly pulsating B stars, we find evidence for a new class of low-amplitude B-type pulsators between the SPB and delta Sct instability strips, with a very broad range of frequencies and low amplitudes, as well as several slowly pulsating B stars with residual excess power at frequencies typically a factor three above their expected g-mode frequencies. The frequency data we obtained for numerous new B-type pulsators represent an appropriate starting point for further theoretical analyses of these stars, once their effective temperature, gravity, rotation velocity and abundances will be derived spectroscopically in the framework of an ongoing FLAMES survey at VLT.
- ID:
- ivo://CDS.VizieR/J/ApJ/598/597
- Title:
- Frequency analysis of fundamental-mode RR Lyrae
- Short Name:
- J/ApJ/598/597
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have frequency-analyzed 6391 variables classified earlier as fundamental-mode RR Lyrae (RR0) stars in the MACHO database on the Large Magellanic Cloud (LMC). The overwhelming majority (i.e., 96%) of these variables have been proved to be indeed RR0 stars, whereas the remaining ones have fallen into one of the following categories: single- and double-mode Cepheids, binaries, first-overtone and double-mode RR Lyrae stars, and nonclassified variables. Special attention has been paid to the properties of the amplitude- and phase-modulated RR0 stars (the Blazhko stars). We found altogether 731 Blazhko variables showing either a doublet or an equidistant triplet pattern at the main pulsation component in their frequency spectra. This sample overwhelmingly exceeds the number of Blazhko stars known in all other systems combined. The incidence rate of the Blazhko variables among the RR0 stars in the LMC is 11.9%, which is 3 times higher than their rate among the first-overtone RR Lyrae stars. No difference is found in the average brightness between the single-mode and Blazhko variables. However, the latter ones show a somewhat lower degree of skewness in their average light curves and a concomitant lower total amplitude in their modulation-free light curves.
- ID:
- ivo://CDS.VizieR/J/ApJS/224/41
- Title:
- Frequency spacing of {delta} Scuti stars. II.
- Short Name:
- J/ApJS/224/41
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A sequence search method was developed for searching for regular frequency spacing in {delta} Scuti stars by visual inspection (VI) and algorithmic search. The sample contains 90 {delta} Scuti stars observed by CoRoT. An example is given to represent the VI. The algorithm (SSA) is described in detail in section 3.2. The data treatment of the CoRoT light curves, the criteria for frequency filtering, and the spacings derived by two methods (i.e., three approaches: VI, SSA, and FT (Fourier Transform)) are given for each target. Echelle diagrams are presented for 77 targets for which at least one sequence of regular spacing was identified. Comparing the spacing and the shifts between pairs of echelle ridges revealed that at least one pair of echelle ridges is shifted to midway between the spacing for 22 stars. The estimated rotational frequencies compared to the shifts revealed rotationally split doublets, triplets, and multiplets not only for single frequencies, but for the complete echelle ridges in 31 {delta} Scuti stars. Using several possible assumptions for the origin of the spacings, we derived the large separation ({Delta}_nu_) that are distributed along the mean density versus large separations relation derived from stellar models.
- ID:
- ivo://CDS.VizieR/J/A+A/598/A49
- Title:
- FRICAT. FIRST catalog of FR I radio galaxies
- Short Name:
- J/A+A/598/A49
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We built a catalog of 219 FR I radio galaxies (FR Is), called FRICAT, selected from a published sample and obtained by combining observations from the NVSS, FIRST, and SDSS surveys. We included in the catalog the sources with an edge-darkened radio morphology, redshift >=0.15, and extending (at the sensitivity of the FIRST images) to a radius r larger than 30kpc from the center of the host. We also selected an additional sample (sFRICAT) of 14 smaller (10<r<30kpc) FR Is, limiting to z<0.05. The hosts of the FRICAT sources are all luminous (-21>=M_r_>=-24), red early-type galaxies with black hole masses in the range 10^8^<=M_BH_<=3x10^9^M_{sun}_; the spectroscopic classification based on the optical emission line ratios indicates that they are all low excitation galaxies. Sources in the FRICAT are then indistinguishable from the FR Is belonging to the Third Cambridge Catalogue of Radio Sources (3C) on the basis of their optical properties. Conversely, while the 3C-FR Is show a strong positive trend between radio and [O III] emission line luminosity, these two quantities are unrelated in the FRICAT sources; at a given line luminosity, they show radio luminosities spanning about two orders of magnitude and extending to much lower ratios between radio and line power than 3C-FR Is. Our main conclusion is that the 3C-FR Is just represent the tip of the iceberg of a much larger and diverse population of FR Is.
- ID:
- ivo://CDS.VizieR/J/A+A/635/A183
- Title:
- Fried Egg Nebula AMBER and GRAVITY observations
- Short Name:
- J/A+A/635/A183
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The objective of this work is to study in detail the nature (i.e., geometry, rates) of the mass-loss episodes associated with the yellow hypergiant IRAS 17163-3907. We analysed a large set of optical/near-infrared data, in spectroscopic, photometric, spectropolarimetric, and interferometric modes. We use the optical observations to determine its spectral type and we present the first model independent reconstructed images of IRAS 17163-3907 at 2 micron tracing milli-arcsecond scales. Lastly, we apply a 2D radiative transfer model to fit the dereddened photometry and the radial profiles of published diffraction limited VISIR images at 8.59um, 11.85um and 12.81um simultaneously, adopting a revised distance determination using the new Gaia measurements (DR2).
- ID:
- ivo://CDS.VizieR/J/A+A/588/A14
- Title:
- Friends-of-friends galaxy group finder
- Short Name:
- J/A+A/588/A14
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We improve the widely used friends-of-friends (FoF) group finding algorithm with membership refinement procedures and apply the method to a combined dataset of galaxies in the local Universe. A major aim of the refinement is to detect subgroups within the FoF groups, enabling a more reliable suppression of the fingers-of-God effect. The FoF algorithm is often suspected of leaving subsystems of groups and clusters undetected. We used a galaxy sample built of the 2MRS, CF2, and 2M++ survey data comprising nearly 80000 galaxies within the local volume of 430Mpc radius to detect FoF groups. We conducted a multimodality check on the detected groups in search for subgroups. We furthermore refined group membership using the group virial radius and escape velocity to expose unbound galaxies. We used the virial theorem to estimate group masses. The analysis results in a catalogue of 6282 galaxy groups in the 2MRS sample with two or more members, together with their mass estimates. About half of the initial FoF groups with ten or more members were split into smaller systems with the multimodality check.
- ID:
- ivo://CDS.VizieR/J/ApJ/756/116
- Title:
- FR II radio galaxies from MaxBCG
- Short Name:
- J/ApJ/756/116
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We have identified and studied a sample of 151 FR IIs found in brightest cluster galaxies (BCGs) in the MaxBCG cluster catalog with data from FIRST and NVSS. We have compared the radio luminosities and projected lengths of these FR IIs to the projected length distribution of a range of mock catalogs generated by an FR II model and estimate the FR II lifetime to be 1.9x10^8^yr. The uncertainty in the lifetime calculation is a factor of two, primarily due to uncertainties in the intracluster medium (ICM) density and the FR II axial ratio. We furthermore measure the jet power distribution of FR IIs in BCGs and find that it is well described by a log-normal distribution with a median power of 1.1x10^37^W and a coefficient of variation of 2.2. These jet powers are nearly linearly related to the observed luminosities, and this relation is steeper than many other estimates, although it is dependent on the jet model. We investigate correlations between FR II and cluster properties and find that galaxy luminosity is correlated with jet power. This implies that jet power is also correlated with black hole mass, as the stellar luminosity of a BCG should be a good proxy for its spheroid mass and therefore the black hole mass. Jet power, however, is not correlated with cluster richness, nor is FR II lifetime strongly correlated with any cluster properties. We calculate the enthalpy of the lobes to examine the impact of the FR IIs on the ICM and find that heating due to adiabatic expansion is too small to offset radiative cooling by a factor of at least six. In contrast, the jet power is approximately an order of magnitude larger than required to counteract cooling. We conclude that if feedback from FR IIs offsets cooling of the ICM, then heating must be primarily due to another mechanism associated with FR II expansion.