- ID:
- ivo://CDS.VizieR/J/ApJ/690/163
- Title:
- The first Swift UV-Opt GRB afterglow catalog
- Short Name:
- J/ApJ/690/163
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first Swift Ultraviolet/Optical Telescope (UVOT) gamma-ray burst (GRB) afterglow catalog. The catalog contains data from over 64000 independent UVOT image observations of 229 GRBs first detected by Swift, the High Energy Transient Explorer 2 (HETE2), the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), and the Interplanetary Network (IPN). The catalog covers GRBs occurring during the period from 2005 January 17 to 2007 June 16 and includes ~86% of the bursts detected by the Swift Burst Alert Telescope (BAT). The catalog provides detailed burst positional, temporal, and photometric information extracted from each of the UVOT images. Positions for bursts detected at the 3{sigma} level are provided with a nominal accuracy, relative to the USNO-B1 catalog, of ~0.25". Photometry for each burst is given in three UV bands, three optical bands, and a "white" or open filter. Upper limits for magnitudes are reported for sources detected below 3{sigma}. General properties of the burst sample and light curves, including the filter-dependent temporal slopes, are also provided.
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- ID:
- ivo://CDS.VizieR/J/ApJ/874/150
- Title:
- The first 3yrs of DES-SN (DES-SN3YR)
- Short Name:
- J/ApJ/874/150
- Date:
- 08 Dec 2021
- Publisher:
- CDS
- Description:
- We present the analysis underpinning the measurement of cosmological parameters from 207 spectroscopically classified SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program (DES-SN), spanning a redshift range of 0.017<z<0.849. We combine the DES-SN sample with an external sample of 122 low-redshift (z<0.1) SNe Ia, resulting in a "DES-SN3YR" sample of 329 SNe Ia. Our cosmological analyses are blinded: after combining our DES-SN3YR distances with constraints from the Cosmic Microwave Background, our uncertainties in the measurement of the dark energy equation-of-state parameter, w, are 0.042 (stat) and 0.059 (stat+syst) at 68% confidence. We provide a detailed systematic uncertainty budget, which has nearly equal contributions from photometric calibration, astrophysical bias corrections, and instrumental bias corrections. We also include several new sources of systematic uncertainty. While our sample is less than one-third the size of the Pantheon sample, our constraints on w are only larger by 1.4x, showing the impact of the DES-SN Ia light-curve quality. We find that the traditional stretch and color standardization parameters of the DES-SNe Ia are in agreement with earlier SN Ia samples such as Pan-STARRS1 and the Supernova Legacy Survey. However, we find smaller intrinsic scatter about the Hubble diagram (0.077mag). Interestingly, we find no evidence for a Hubble residual step (0.007+/-0.018mag) as a function of host-galaxy mass for the DES subset, in 2.4{sigma} tension with previous measurements. We also present novel validation methods of our sample using simulated SNe Ia inserted in DECam images and using large catalog-level simulations to test for biases in our analysis pipelines.
- ID:
- ivo://CDS.VizieR/J/A+A/639/A136
- Title:
- The Fornax Deep Survey with the VST. IX.
- Short Name:
- J/A+A/639/A136
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A possible pathway for understanding the events and the mechanisms involved in galaxy formation and evolution is an in-depth comprehension of the galactic and inter-galactic fossil sub-structures with long dynamical times-scales: stars in the field and in stellar clusters. This paper continues the series of the Fornax Deep Survey (FDS). Following the previous studies dedicated to extended Fornax cluster members, in this paper we present the catalogs of compact stellar systems in the Fornax cluster as well as extended background sources and point-like sources. We derive ugri photometry of ~1.7 million sources over the ~21 square degree area of FDS centered on the bright central galaxy NGC1399. For a wider area, of ~27 square degrees extending in the direction of NGC1316, we provide gri photometry for ~3.1 million sources. To improve the morphological characterization of sources we generate multi-band image stacks by coadding the best seeing gri-band single exposures with a cut at FWHM<=0.9". We use the multi-band stacks as master detection frames, with a FWHM improved by ~15% and a FWHM variability from field to field reduced by a factor of ~2.5 compared to the pass-band with best FWHM, namely the r-band. The identification of compact sources, in particular of globular clusters (GC), is obtained from a combination of photometric (e.g. colors, magnitudes) and morphometric (e.g. concentration index, elongation, effective radius) selection criteria, by also taking as reference the properties of sources with well-defined classification from spectroscopic or high-resolution imaging data. Using the FDS catalogs, we present a preliminary analysis of globular cluster (GC) distributions in the Fornax area. The study confirms and extends further previous results which were limited to a smaller survey area. We observe the inter-galactic population of GCs, a population of mainly blue GCs centered on NGC1399, extends over ~0.9Mpc, with an ellipticity ~0.65 and a small tilt in the direction of NGC1336. Several sub-structures extend over ~0.5Mpc along various directions. Two of these structures do not cross any bright galaxy; one of them appears to be connected to NGC1404, a bright galaxy close to the cluster core and particularly poor of GCs. Using the gri catalogs we analyze the GC distribution over the extended FDS area, and do not find any obvious GC sub-structure bridging the two brightest cluster galaxies, NGC1316 and NGC1399. Although NGC1316 is more than twice brighter of NGC1399 in optical bands, using gri data, we estimate a factor of ~3-4 richer GC population around NGC1399 compared to NGC1316, out to galactocentric distances of ~40' or ~230kpc
- ID:
- ivo://CDS.VizieR/J/MNRAS/505/5164
- Title:
- The Gaia view of the Cepheus flare
- Short Name:
- J/MNRAS/505/5164
- Date:
- 25 Oct 2021 10:05:07
- Publisher:
- CDS
- Description:
- We present a new census of candidate pre-main-sequence stars in the Cepheus flare star-forming region, based on Gaia EDR3 parallaxes, proper motions, and colour-magnitude diagrams. We identified new candidate members of the previously known young stellar groups associated with NGC 7023, L1177, L1217/L1219, L1228, L1235, and L1251. We studied the 3D structure of the star-forming complex and the distribution of tangential velocities of the young stars. The young stellar groups are located between 330 and 368pc from the Sun, divided into three kinematic subgroups, and have ages between 1 and 5 million yr. The results confirm the scenario of propagating star formation, suggested by previous studies. In addition to the bulk pre-main-sequence star population between 330 and 370pc, there is a scattered and more evolved pre-main-sequence population around 150-180pc. We found new candidate members of the nearby Cepheus Association, and identified a new moving group of 46, 15-20 million yr old pre-main-sequence stars located at a distance of 178pc, around the A0-type star HD 190833. A few pre-main-sequence stars are located at 800-900 pc, indicative of star-forming regions associated with the Galactic local arm above the Galactic latitude of +10{deg}.
- ID:
- ivo://CDS.VizieR/J/ApJS/236/37
- Title:
- The Gaia-WISE extragalactic astrometric catalog
- Short Name:
- J/ApJS/236/37
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The Gaia mission has detected a large number of active galactic nuclei (AGNs) and galaxies, but these objects must be identified among the thousandfold more numerous stars. Extant astrometric AGN catalogs do not have the uniform sky coverage required to detect and characterize the all-sky, low-multipole proper motion signals produced by the barycenter motion, gravitational waves, and cosmological effects. To remedy this, we present an all-sky sample of 567,721 AGNs in Gaia Data Release 1, selected using WISE two-color criteria. The catalog has fairly uniform sky coverage beyond the Galactic plane, with a mean density of 12.8 AGNs per square degree. The objects have magnitudes ranging from G=8.8 down to Gaia's magnitude limit, G=20.7. The catalog is approximately 50% complete but suffers from low stellar contamination, roughly 0.2%. We predict that the end-of-mission Gaia proper motions for this catalog will enable detection of the secular aberration drift to high significance (23{sigma}) and will place an upper limit on the anisotropy of the Hubble expansion of about 2%.
- ID:
- ivo://CDS.VizieR/J/AJ/153/259
- Title:
- The GAMBLES extension of the SLoWPoKES catalog
- Short Name:
- J/AJ/153/259
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The formation and evolution of binary star systems are some of the remaining key questions in modern astronomy. Wide binary pairs (separations >10^3^au) are particularly intriguing because their low binding energies make it difficult for the stars to stay gravitationally bound over extended timescales, and thus to probe the dynamics of binary formation and dissolution. Our previous SLoWPoKES catalogs, I and II, provided the largest and most complete sample of wide-binary pairs of low masses. Here we present an extension of these catalogs to a broad range of stellar masses: the Gaia Assorted Mass Binaries Long Excluded from SloWPoKES (GAMBLES), comprising 8660 statistically significant wide pairs that we make available in a living online database. Within this catalog we identify a subset of 543 long-lived (dissipation timescale >1.5Gyr) candidate binary pairs, of assorted mass, with typical separations between 10^3^ and 10^5.5^ au (0.002-1.5pc), using the published distances and proper motions from the Tycho-Gaia Astrometric Solution and Sloan Digital Sky Survey photometry. Each pair has at most a false positive probability of 0.05; the total expectation is 2.44 false binaries in our sample. Among these, we find 22 systems with 3 components, 1 system with 4 components, and 15 pairs consisting of at least 1 possible red giant. We find the largest long-lived binary separation to be nearly 3.2pc; even so, >76% of GAMBLES long-lived binaries have large binding energies and dissipation lifetimes longer than 1.5Gyr. Finally, we find that the distribution of binary separations is clearly bimodal, corroborating the findings from SloWPoKES and suggesting multiple pathways for the formation and dissipation of the widest binaries in the Galaxy.
- ID:
- ivo://CDS.VizieR/J/AJ/155/116
- Title:
- The globular cluster M14.II. Variable stars
- Short Name:
- J/AJ/155/116
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present time-series BVI photometry for the Galactic globular cluster NGC 6402 (M14). The data consist of ~137 images per filter, obtained using the 0.9 and 1.0 m SMARTS telescopes at the Cerro Tololo Inter-American Observatory. The images were obtained during two observing runs in 2006-2007. The image-subtraction package ISIS, along with DAOPHOT II/ALLFRAME, was used to perform crowded-field photometry and search for variable stars. We identified 130 variables, eight of which are new discoveries. The variable star population is comprised of 56 ab-type RR Lyrae stars, 54 c-type RR Lyrae, 6 type II Cepheids, 1 W UMa star, 1 detached eclipsing binary, and 12 long-period variables. We provide Fourier decomposition parameters for the RR Lyrae, and discuss the physical parameters and photometric metallicity derived therefrom. The M14 distance modulus is also discussed, based on different approaches for the calibration of the absolute magnitudes of RR Lyrae stars. The possible presence of second-overtone RR Lyrae in M14 is critically addressed, with our results arguing against this possibility. By considering all of the RR Lyrae stars as members of the cluster, we derive <P_ab_>=0.589 days. This, together with the position of the RR Lyrae stars of both Bailey types in the period-amplitude diagram, suggests an Oosterhoff-intermediate classification for the cluster. Such an intermediate Oosterhoff type is much more commonly found in nearby extragalactic systems, and we critically discuss several other possible indications that may point to an extragalactic origin for this cluster.
- ID:
- ivo://CDS.VizieR/J/A+A/286/444
- Title:
- The globular cluster NGC 6652
- Short Name:
- J/A+A/286/444
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- (no description available)
- ID:
- ivo://CDS.VizieR/J/ApJ/797/31
- Title:
- The G+M eclipsing binary V530 Orionis photometry
- Short Name:
- J/ApJ/797/31
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We report extensive photometric and spectroscopic observations of the 6.1 day period, G+M-type detached double-lined eclipsing binary V530 Ori, an important new benchmark system for testing stellar evolution models for low-mass stars. We determine accurate masses and radii for the components with errors of 0.7% and 1.3%, as follows: M_A_=1.0038+/-0.0066 M_{sun}_, M_B_=0.5955+/-0.0022 M_{sun}_, R_A_=0.980+/-0.013 R_{sun}_, and R_B_=0.5873+/-0.0067 R_{sun}_. The effective temperatures are 5890+/-100 K (G1 V) and 3880+/-120 K (M1 V), respectively. A detailed chemical analysis probing more than 20 elements in the primary spectrum shows the system to have a slightly subsolar abundance, with [Fe/H]=-0.12+/-0.08. A comparison with theory reveals that standard models underpredict the radius and overpredict the temperature of the secondary, as has been found previously for other M dwarfs. On the other hand, models from the Dartmouth series incorporating magnetic fields are able to match the observations of the secondary star at the same age as the primary (~3 Gyr) with a surface field strength of 2.1+/-0.4 kG when using a rotational dynamo prescription, or 1.3+/-0.4 kG with a turbulent dynamo approach, not far from our empirical estimate for this star of 0.83+/-0.65 kG. The observations are most consistent with magnetic fields playing only a small role in changing the global properties of the primary. The V530 Ori system thus provides an important demonstration that recent advances in modeling appear to be on the right track to explain the long-standing problem of radius inflation and temperature suppression in low-mass stars.
3770. The GPM catalog
- ID:
- ivo://CDS.VizieR/I/285
- Title:
- The GPM catalog
- Short Name:
- I/285
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- GPM is the newer version of the General Compiled Catalogue of Absolute Proper Motions, derived with respect to galaxies within the plan called Catalogue of Faint Stars (KSZ, Deutch, 1952, Trans. IAU, Vol. 8, 789). The programme was proposed for several observatories of the former Soviet Union, China, Rumania and Spain. There are some resulting individual catalogues of absolute proper motions of stars compiled at five observatories (Kiev, Pulkovo, Moscow, Tashkent and Shanghai). The GPM combines these catalogues and comprises absolute proper motions for 52805 stars from 8 to 15.5mag in 185 fields north of -25 degrees of declination. The size of each region is nearly 1.5 square degrees. The mean standard error of proper motion is 8 mas/yr on average. Detailed information on the construction methodology and input data can be found in (Rybka & Yatsenko, 1997KFNT...13e..70R). In addition to absolute proper motions the GPM contains accurate equatorial coordinates and three-colour B V R photometry for the vast majority of its stars (Rybka 2000KFNT...16e..60R). Additional information was selected from all available sources. Usage of the ACT catalog should provide improved positions (mostly in removing of systematic errors) and improved photometry (because the brightest stars in each GPM region had B and V magnitudes measured by the Tycho experiment on the Hipparcos satellite). The mean accuracies achived, as demonstrated by comparison with above catalogue, are 250 mas for the positions and 0.22mag for B magnitude and 0.26mag for B-V colour. The GPM gives right ascensions and declinations for equinox J2000.0 and epoch copied from available sources. They were only presented to identify the GPM stars with those from other catalogues. The compiled catalogue also presents B magnitudes and B-V colours. They were converted to be close to Johnson system. The Tycho stars were also identified in the GPM catalogue. A search area with a radius of 2 arcseconds was used to search for multiple entries of the same star, which may be appeared in the region overlap areas. The detected entries were then removed from the final catalogue. The procedure decreased the number of stars in the catalogue by about 0.4 %. The adopted catalogue organization includes data in 185 regions sorted according the KSZ region numbers. The data were then sorted nearly in right ascension order within each GPM region. All information needed to associate a point on the sky with region number and provide a more rapid access to that region are given in file region.dat.
