- ID:
- ivo://CDS.VizieR/J/ApJ/722/605
- Title:
- A stellar rotation census of B stars
- Short Name:
- J/ApJ/722/605
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Two recent observing campaigns provide us with moderate dispersion spectra of more than 230 cluster and 370 field B stars. Combining them and the spectra of the B stars from our previous investigations (~430 cluster and ~100 field B stars) yields a large, homogeneous sample for studying the rotational properties of B stars. We derive the projected rotational velocity vsini, effective temperature, gravity, mass, and critical rotation speed V_crit_ for each star. We compare the evolutionary trends of rotation (measured according to the polar gravity of the star) with recent models that treat internal mixing.
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- ID:
- ivo://CDS.VizieR/J/PASP/110/863
- Title:
- A Stellar Spectral Flux Library: 1150 - 25000 A
- Short Name:
- J/PASP/110/863
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Available published spectra have been combined to form a library of digital stellar spectra spanning 1150 - 25000 A with a sampling interval of 5 A and a resolution of ~500. The library was constructed to enable synthesis and modeling of the integrated light from composite populations. The library consists of 131 flux-calibrated spectra, encompassing all normal spectral types and luminosity classes at solar abundance, plus metal-weak and metal-rich F-K dwarfs and G-K giants. Each library spectrum was formed by combining data from several sources overlapping in wavelength coverage. The data sources are listed in file srclist.doc, and the specific components used to form each spectrum are identified in file complist.doc. The library has complete spectral coverage from 1150 - 10620 A for all spectra and to 25000 A for about half of them, mainly later types of solar abundance. Missing spectral coverage in the infrared consists of a smooth energy distribution formed from standard colors for the relevant types. The library spectra are each given as normalized F(lambda) vs. wavelength in A: each spectrum is normalized to 1.0 at 5556 A. Spectra are organized in two groups of 131 files each; the files are named according to the spectral type, luminosity class and metallicity. The first group of files, designated UVILIB, contains the final combined spectra from 1150 - 11620 A. The second set of files, UVKLIB, extends the UVILIB spectra out to 25000 A, as described above. The data files contain the wavelength, normalized flux and standard deviation for the final combined spectrum in the first three columns. Subsequent columns contain the normalized flux for component spectra which were used to make the final spectrum. Columns which contain these component spectra are labelled according to a code which specifies the source of that spectrum (see complist.doc for more detail) -- UVILIB component codes Code Occasional Alternate Reference source Codes fsv Sviderskiene 1988, Cat. <VI/50> fi (IUE) Heck et al. 1984, Cat. <III/83> fg Gunn & Stryker 1983, Cat. <III/88> fk Kiehling 1987, Cat. <III/124> fj Jacoby, Hunter & Christian 1984, Cat. <III/92> fs Silva & Cornell 1992, Cat. <III/166> fp Pickles 1985, Cat. <VII/102> fn (N6522) Pickles & van der Kruit 1990 (1990A&AS...84..421P) fr fr1, fr2 Serote Roos, Boisson & Joly 1996, Cat. <J/A+AS/117/93> fd fdd1, fdd2; fd3, fd4 Danks & Dennefeld 1994 (1994PASP..106..382D) UVKLIB component codes Code Reference source fh spectrum from UVILIB fse interpolated spectrum based on standardized flux points fl Lancon & Rocca-Volmerange 1992, Cat. <III/196> fd Dallier, Boisson & Joly 1996, Cat. <J/A+AS/116/239> fk Kleinmann & Hall 1986 (1986ApJS...62..501K) fc Cohen et al. (1995, 1996a, 1996b); Cat. <J/AJ/110/275>, <J/AJ/112/241>, <J/AJ/112/2274> fm Fluks et al. 1994, Cat. <J/A+AS/105/311> M giant spectra in UVKLIB include the synthetic M0-M10 MK type spectra from Fluks et. al. (1994), and are a combination of these and the UVILIB spectra in the range 1150-10620A. M0-M8 III are the only cases where the 1150-10500A data differ between UVILIB and UVKLIB. M9 and M10 III spectra are exclusively synthetic spectra from Fluks et. al. (1994) in both libraries. In addition to the spectrum library itself, synthetic photometry and selected local equivalent widths & magnitude indices are provided in tables synphot.dat and lew.dat. The standard infrared colors used to form the smooth energy curves used in UVKLIB spectra are listed in irstphot.dat. Further documentation details are available in the *.doc files as described below in the table notes in this ReadMe.
- ID:
- ivo://CDS.VizieR/J/ApJS/226/21
- Title:
- ASTEP catalog of EB* and variable stars
- Short Name:
- J/ApJS/226/21
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We used the large photometric database of the ASTEP program, whose primary goal was to detect exoplanets in the southern hemisphere from Antarctica, to search for eclipsing binaries (EcBs) and variable stars. 673 EcBs and 1166 variable stars were detected, including 31 previously known stars. The resulting online catalogs give the identification, the classification, the period, and the depth or semi-amplitude of each star. Data and light curves for each object are available at http://astep-vo.oca.eu/.
- ID:
- ivo://CDS.VizieR/J/A+A/423/381
- Title:
- Asteroidal I, J, K in the DENIS Survey
- Short Name:
- J/A+A/423/381
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- I, J, K magnitudes of 767 asteroids (numbered between 1 and 8000) are presented here. These asteroids have been recovered in the DENIS Survey (Deep European Near-Infrared southern sky Survey) on the basis of their predicted ephemerides. The observations were performed with the 1m-telescope at ESO, La Silla (Chile). The limiting magnitudes of the three bands I, J, K centered at 0.8, 1.25 and 2.15 microns are respectively 18.5, 16.5 and 13.5.
- ID:
- ivo://CDS.VizieR/J/A+A/375/275
- Title:
- Asteroidal I, J, K in the DENIS Survey
- Short Name:
- J/A+A/375/275
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- I, J, K magnitudes of 1233 asteroids (numbered between 1 and 8000) are presented here. These asteroids have been recovered in the DENIS Survey (Deep European Near-Infrared southern sky Survey) on the basis of their predicted ephemerides. The observations were performed with the 1m-telescope at ESO, La Silla (Chile). The limiting magnitudes of the three bands I, J, K centered at 0.8, 1.25 and 2.15 microns are respectively 18.5, 16.5 and 13.5.
- ID:
- ivo://CDS.VizieR/J/A+A/465/331
- Title:
- Asteroid brightness and geometry
- Short Name:
- J/A+A/465/331
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present physical models of ten asteroids obtained by means of lightcurve inversion. A substantial part of the photometric data was observed by amateur astronomers. We emphasize the importance of a coordinated network of observers that will be of extreme importance for future all-sky asteroids photometric surveys.
- ID:
- ivo://CDS.VizieR/J/PASJ/63/1117
- Title:
- Asteroid catalog using AKARI (AcuA). V1.
- Short Name:
- J/PASJ/63/1117
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The AKARI Infrared Astronomical Satellite observed the whole sky in the far infrared (50-180{mu}m) and the mid-infrared (9 and 18{mu}m) between May 2006 and August 2007 (Murakami et al. 2007PASJ...59S.369M). The Asteroid catalog using AKARI (AcuA) version 1.0 is the first asteroid catalog produced based on the AKARI/IRC Mid-Infrared Survey. The catalog provides the size and albedo of 5120 asteroids.
- ID:
- ivo://CDS.VizieR/J/A+A/657/A80
- Title:
- Asteroides phase curves using SLOAN MOC
- Short Name:
- J/A+A/657/A80
- Date:
- 22 Feb 2022
- Publisher:
- CDS
- Description:
- Large photometric surveys are producing, and will continue doing it, massive amounts of data on small bodies. Usually,these data will be sparsely obtained at arbitrary (and unknown) rotational phases. Therefore, new methods to process such data need to be developed to make the most of those large catalogs. We aim to produce a method to create phase curves of small bodies considering the uncertainties introduced not only by the nominal errors in the magnitudes, but also the effect introduced by rotational variations.We use as a benchmark the data from the SLOAN Moving Objects Catalog with the objective to construct phase curves of all small bodies in there, in the u, g, r, i, and z, filters. We will obtain from the phase curves the absolute magnitudes and set up with them the absolute colors, which are the colors of the asteroids not affected by changes in phase angle. We select objects with >3 observations taken in, at least, one filter and spanned over a minimum of 5 degrees in phase angle. We developed a method that combines Monte Carlo simulations and Bayesian inference to estimate the absolute magnitudes using the HG12 photometric system. We obtained almost 15000 phase curves, about 12000 including all five filters. The absolute magnitudes and absolute colors are compatible with previously published data, supporting our method.Conclusions. The method we developed is fully automatic and well suited to be run on large amounts of data. Moreover, it includes the nominal uncertainties in the magnitudes and the whole distribution of possible rotational states of the objects producing, possibly,less precise values, i.e., larger uncertainties, but more accurate, i.e., closer to the real value. To the best of our knowledge, this work is the first to include the effect of rotational variations in such a way.
- ID:
- ivo://CDS.VizieR/J/A+A/641/A80
- Title:
- Asteroid (31) Euphrosyne R-band images
- Short Name:
- J/A+A/641/A80
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Asteroid (31) Euphrosyne is one of the biggest objects in the asteroid main belt and it is also the largest member of its namesake family. The Euphrosyne family occupies a highly inclined region in the outer main belt and contains a remarkably large number of members, which is interpreted as an outcome of a disruptive cratering event.The goals of this adaptive-optics imaging study are threefold: to characterize the shape of Euphrosyne, to constrain its density, and to search for the large craters that may be associated with the family formation event. We obtained disk-resolved images of Euphrosyne using SPHERE/ZIMPOL at the ESO 8.2m VLT as part of our large program (ID: 199.C-0074, PI: Vernazza). We reconstructed its 3D shape via the ADAM shape modeling algorithm based on the SPHERE images and the available light curves of this asteroid. We analyzed the dynamics of the satellite with the \genoid meta-heuristic algorithm. Finally, we studied the shape of Euphrosyne using hydrostatic equilibrium models. Our SPHERE observations show that Euphrosyne has a nearly spherical shape with the sphericity index of 0.9888 and its surface lacks large impact craters. Euphrosyne's diameter is 268+/-6km, making it one of the top ten largest main belt asteroids. We detected a satellite of Euphrosyne - S/2019 (31) 1 - that is about 4 km across, on a circular orbit. The mass determined from the orbit of the satellite together with the volume computed from the shape model imply a density of 1665+/-242kg/m^-3^, suggesting that Euphrosyne probably contains a large fraction of water ice in its interior. We find that the spherical shape of Euphrosyne is a result of the reaccumulation process following the impact, as in the case of (10)Hygiea. However, our shape analysis reveals that, contrary to Hygiea, the axis ratios of Euphrosyne significantly differ from those suggested by fluid hydrostatic equilibrium following reaccumulation.
- ID:
- ivo://CDS.VizieR/J/A+A/561/A45
- Title:
- Asteroid (341843) 2008 EV5 WISE light curves
- Short Name:
- J/A+A/561/A45
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We derive the thermal inertia of 2008 EV5, the baseline target for the Marco Polo-R mission proposal, and infer information about the size of the particles on its surface. Values of thermal inertia were obtained by fitting an asteroid thermophysical model to NASA's Wide-field Infrared Survey Explorer (WISE) infrared data. Grain size was derived from the constrained thermal inertia and a model of heat conductivity that accounts for different values of the packing fraction (a measure of the degree of compaction of the regolith particles).
