- ID:
- ivo://CDS.VizieR/J/A+A/336/953
- Title:
- Bp-Ap stars HR-diagram from Hipparcos data
- Short Name:
- J/A+A/336/953
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using Hipparcos (Cat. <I/239>) parallaxes and proper motions together with radial velocity data, the luminosity calibration and kinematics of Bp-Ap stars have been obtained. The used statistical method allows to treat inhomogeneous samples and to identify the different groups. Six types of Bp-Ap stars (He-rich, He-weak, Hg-Mn, Si, Si+ and SrCrEu) have been considered. In most of the samples, with the exception of the He-rich and He-weak stars, two groups have been separated. Individual distances and luminosities are given for the stars belonging to the main groups which contain the largest number of stars. The list of stars in the secondary groups is given
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Search Results
- ID:
- ivo://CDS.VizieR/J/AJ/129/2663
- Title:
- B photometry of M31 variable star candidates
- Short Name:
- J/AJ/129/2663
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A search for variable stars is performed using two epochs of Hubble Space Telescope Advanced Camera for Surveys imaging data for a 9.28arcmin^2^ portion of M31. This data set reveals 254 sources that vary by at least 4{sigma} between epochs. The positions and two-epoch B-band (equivalent) photometry of these sources are presented.
- ID:
- ivo://CDS.VizieR/J/A+A/398/1073
- Title:
- BP Mus Geneva 7-colour light curves
- Short Name:
- J/A+A/398/1073
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The semi-detached eclipsing binary system BP Muscae has been analysed using the Wilson-Devinney program. The physical and orbital parameters have been determined through a self-consistent simultaneous solution of light curves in seven colours and of the radial velocity curves of both components. The 373 photometric measurements of BP Mus in the 7-colour GENEVA system are listed in the table. P and Q are the weights in colours and V magnitude (see Rufener, 1988, Cat. <II/169>).
- ID:
- ivo://CDS.VizieR/J/A+A/622/A209
- Title:
- B2 0258+35 polarisation images
- Short Name:
- J/A+A/622/A209
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The contribution of active galactic nuclei to the magnetisation of the Universe can be constrained by knowing their duty cycles, jet and magnetic field morphologies, and the physical processes dominating their interaction with the surrounding environment. The magnetic field morphology and strength of radio lobes of AGN has an influence on the mechanisms for the propagation of cosmic rays into intergalactic space. Using the source B2 0258+35 we want to investigate the interaction of its radio lobes with the surrounding environment and examine the underlying physical effects. Published HI and radio continuum data at {lambda}21cm were combined with newly reduced archival Westerbork Radio Synthesis Telescope polarisation data at the same wavelength to investigate the polarised emission in the radio lobes of B2 0258+35. We assumed energy equipartition between the cosmic rays and the magnetic field to calculate their pressure and investigate the physical processes leading to the detected emission. We detected a unique S-shaped diffuse polarised structure. The lobes have a pressure of p=1.95+/-0.4x10^-14^dyn/cm^2^. The calculated total magnetic field strengths are low (B_eq_=1.21+/-0.12uG). We observe depolarisation in the northern lobe, which might originate from the HI-disc in the foreground. In addition we see an anti-correlation between the pressure and the fractional polarisation along the S-shaped structure. Therefore we consider magnetic draping and magnetic field compression as possible effects that might have created the observed S-shape. Our results suggest that magnetic draping can be effectively used to explain the observed polarised structures. This is likely due to the combination of a relatively low magnetic field strength, enabling super-Alfvenic motion of the rising lobes (with M_A_=2.47-3.50), and the coherency of the surrounding magnetic field. Moreover, the draped layer tends to suppress any mixing of the material between the radio lobes and the surrounding environment, but can enhance the mixing and re-acceleration efficiencies inside the lobes, providing an explanation for the average flat spectral index observed in the lobes.
- ID:
- ivo://CDS.VizieR/J/other/NewA/32.6
- Title:
- BP Peg times of maximum light
- Short Name:
- J/other/NewA/32.
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- New CCD photometric monitoring on the high-amplitude delta Scuti variable BP Peg was carried out on November 4, 2013 by using the 1.0-m reflecting telescope of Yunnan Observatories in China as well as on December 29, 2013 by using the 85-cm telescope at Xinglong Station of National Astronomical Observatory in China. BP Peg is a new high-amplitude delta Scuti variable with a period of 0.10954357-day. We have collected all the times of light maximum from the literature together with our data, and the pulsation period changes are analyzed through Observed-Calculated (O-C) method. With the available data, we discover that the pulsating period of BP Peg shows a cyclic oscillation with a period of 24.5-years and an amplitude of 0.0060-days. If the cyclic period changes are caused by light-time effect in a binary system, the reckoned mass of the hidden companion could be 0.20M_{sun}_ and possibly, it is an M-type star.
2006. BRAVA Catalog
- ID:
- ivo://irsa.ipac/BRAVA/Catalog
- Title:
- BRAVA Catalog
- Short Name:
- BRAVA Catalog
- Date:
- 01 Oct 2018 20:27:21
- Publisher:
- NASA/IPAC Infrared Science Archive
- Description:
- The Bulge Radial Velocity Assay (BRAVA) consists of spectra of approximately 8500 red giants in the Galactic bulge.
- ID:
- ivo://CDS.VizieR/J/A+A/608/A127
- Title:
- Breaks in disc galaxy abundance gradients
- Short Name:
- J/A+A/608/A127
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We examine the relation between breaks in the surface brightness profiles and radial abundance gradients within the optical radius in the discs of 134 spiral galaxies from the CALIFA survey. The distribution of the radial abundance (in logarithmic scale) in each galaxy was fitted by simple and broken linear relations. The surface brightness profile was fitted assuming pure and broken exponents for the disc. We find that the maximum absolute difference between the abundances in a disc given by broken and pure linear relations is less than 0.05dex in the majority of our galaxies and exceeds the scatter in abundances for 26 out of 134 galaxies considered. The scatter in abundances around the broken linear relation is close (within a few percent) to that around the pure linear relation. The breaks in the surface brightness profiles are more prominent. The scatter around the broken exponent in a number of galaxies is lower by a factor of two or more than that around the pure exponent. The shapes of the abundance gradients and surface brightness profiles within the optical radius in a galaxy may be different. A pure exponential surface brightness profile may be accompanied by a broken abundance gradient and vise versa. There is no correlation between the break radii of the abundance gradients and surface brightness profiles. Thus, a break in the surface brightness profile does not need to be accompanied by a break in the abundance gradient.
- ID:
- ivo://CDS.VizieR/J/A+A/625/A36
- Title:
- Breaks in surf. brightness prof. of galaxy disks
- Short Name:
- J/A+A/625/A36
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Using a sample of 175 low-inclination galaxies from the S^4^G, we investigate the origins of up-bending (Type III) breaks in the 3.6{mu}m surface brightness profiles of disk galaxies. We reanalyzed a sample of previously identified Type III disk break-hosting galaxies using a new, unbiased break-finding algorithm, which uncovered many new, sometimes subtle disk breaks across the whole sample. We classified each break by its likely origin through close examination of the galaxy images across wavelengths, and compare samples of galaxies separated by their outermost identified break types in terms of their stellar populations and local environments. We find that more than half of the confirmed Type III breaks in our sample can be attributed to morphological asymmetry in the host galaxies. As these breaks are mostly an artifact of the azimuthal averaging process, their status as physical breaks is questionable. Such galaxies occupy some of the highest density environments in our sample, implying that much of this asymmetry is the result of tidal disturbance. We also find that Type III breaks related to extended spiral arms or star formation often host down-bending (Type II) breaks at larger radius which were previously unidentified. Such galaxies reside in the lowest density environments in our sample, in line with previous studies that found a lack of Type II breaks in clusters. Galaxies occupying the highest density environments most often show Type III breaks associated with outer spheroidal components. We find that Type III breaks in the outer disks of galaxies arise most often through environmental influence: either tidal disturbance (resulting in disk asymmetry) or heating through, for example, galaxy harrassment (leading to spheroidal components). Galaxies hosting the latter break types also show bimodal distributions in central g-r color and morphological type, with more than half of such galaxies classified as Sa or earlier; this suggests these galaxies may be evolving into early-type galaxies. By contrast, we find that Type III breaks related to apparently secular features (e.g., spiral arms) may not truly define their hosts' outer disks, as often in such galaxies additional significant breaks can be found at larger radius. Given this variety in Type III break origins, we recommend in future break studies making a more detailed distinction between break subtypes when seeking out, for example, correlations between disk breaks and environment, to avoid mixing unlike physical phenomena.
- ID:
- ivo://CDS.VizieR/J/A+A/633/A54
- Title:
- B0355+508 reduced spectra
- Short Name:
- J/A+A/633/A54
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Phosphorus-bearing species are essential to the formation of life on Earth, however they have barely been detected in the interstellar medium. In particular, towards star-forming regions only PN and PO have been identified so far. Since only a small number of detections of P-bearing molecules are available, their chemical formation pathways are not easy to constrain and are thus highly debatable. An important factor still missing in the chemical models is the initial elemental abundance of phosphorus, that is, the depletion level of P at the start of chemical models of dense clouds. In order to overcome this problem, we study P-bearing species in diffuse and translucent clouds. In these objects phosphorus is expected to be mainly in the gas phase and therefore the elemental initial abundance needed in our chemical simulations corresponds to the cosmic one and is well constrained. For the study of P-bearing chemistry we used an advanced chemical model. We updated and significantly extended the P-chemistry network based on chemical databases and previous literature. We performed single-pointing observations with the IRAM 30m telescope in the 3mm range towards the line of sight to the strong continuum source B0355+508 aiming for the (2-1) transitions of PN, PO, HCP, and CP. This line of sight incorporates five diffuse and/or translucent clouds. The (2-1) transitions of the PN, PO, HCP, and CP were not detected. We report high signal-to-noise-ratio detections of the (1-0) lines of ^13^CO, HNC, and CN along with a first detection of C^34^S towards this line of sight. We have attempted to reproduce the observations of HNC, CN, CS, and CO in every cloud with our model by applying typical physical conditions for diffuse or translucent clouds. We find that towards the densest clouds with v_LSR_= -10, -17 km/s the best-fit model is given by the parameters (n_H_, A_V_, T_gas_) = (300cm^-3^, 3mag, 40K). According to our best-fit model, the most abundant P-bearing species are HCP and CP (1e-10). The molecules PN, PO, and PH_3_ also show relatively high predicted abundances of 1e-11. We show that the abundances of these species are sensitive to visual extinction, cosmic-ray ionization rate, and the diffusion-to-desorption energy ratio on dust grains. The production of P-bearing species is favored towards translucent rather than diffuse clouds, where the environment provides a stronger shielding from the interstellar radiation. Based on our improved model, we show that the (1-0) transitions of HCP, CP, PN, and PO are expected to be detectable with estimated intensities of up to ~200mK.
- ID:
- ivo://CDS.VizieR/J/ApJS/188/32
- Title:
- Breit-Pauli transition probabilities for SII
- Short Name:
- J/ApJS/188/32
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- New improved calculations are reported for transition probabilities and electron impact excitation collision strengths for the astrophysically important lines in SII. The collision strengths have been calculated in the close-coupling approximation using the B-spline Breit-Pauli R-matrix method. The multiconfiguration Hartree-Fock method with term-dependent non-orthogonal orbitals is employed for an accurate representation of the target wave functions. The close-coupling expansion includes 70 bound levels of SII covering all possible terms of the ground 3s^2^3p^3^ and singly excited 3s3p^4^, 3s^2^3p^2^3d, 3s^2^3p^2^4s, and 3s^2^3p^2^4p configurations. The present calculations are more extensive than previous ones, leading to a total 2415 transitions between fine-structure levels. The effective collision strengths are obtained by averaging the electron collision strengths over a Maxwellian distribution of velocities and these are tabulated for all fine-structure transitions at electron temperatures in the range from 5000 to 100000K. The present results are compared with a variety of other close-coupling calculations and available experimental data. There is an overall good agreement with the recent 18-state calculations by Ramsbottom, Bell, & Stafford and with the 19-state calculations by Tayal for the most part, but some significant differences are also noted for some transitions.
