- ID:
- ivo://CDS.VizieR/J/A+A/567/A1
- Title:
- BVJH photometry of Andrews-Lindsay 1 field
- Short Name:
- J/A+A/567/A1
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Andrews-Lindsay 1 is a pertinent open cluster because it may host the planetary nebula (PN) PHR 1315-6555, yet ambiguities linger concerning its fundamental parameters (>50% scatter). New multiband BVJHW_1-4_ photometry for cluster and field stars, in concert with observations of recently discovered classical Cepheids, were used to constrain the reddening and velocity-distance profiles along the sightline. That analysis yielded the following parameters for the cluster: E(J-H)=0.24+/-0.03, d=10.0+/-0.4kpc (d_JH_=9.9+/-0.6kpc, d_BV_=10.1+/-0.5kpc), and log{tau}=8.90+/-0.15. The steep velocity-distance gradient along l~305{deg} indicates that two remote objects sharing spatial and kinematic parameters (i.e., PHR 1315-6555 and Andrews-Lindsay 1) are associated, thus confirming claims that the PN is a cluster member. The new distance for PHR 1315-6555 is among the most precise established yet for a Galactic PN ({sigma}/d=4%).
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Search Results
- ID:
- ivo://CDS.VizieR/J/A+A/629/A58
- Title:
- B2 0258+35 VLA and VLBI HI absorption spectra
- Short Name:
- J/A+A/629/A58
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Low-luminosity radio-loud active galactic nuclei (AGN) are of importance in studies concerning feedback from radio AGN since a dominant fraction of AGN belong to this class. We report high-resolution Very Large Array (VLA) and European VLBI Network (EVN) observations of HI 21cm absorption from a young, compact steep-spectrum radio source, B2 0258+35, nested in the early-type galaxy NGC 1167, which contains a 160kpc HI disc. Our VLA and EVN HI absorption observations, modelling, and comparison with molecular gas data suggest that the cold gas in the centre of NGC 1167 is very turbulent (with a velocity dispersion of ~90km/s) and that this turbulence is induced by the interaction of the jets with the interstellar medium (ISM). Furthermore, the ionised gas in the galaxy shows evidence of shock heating at a few kpc from the radio source. These findings support the results from numerical simulations of radio jets expanding into a clumpy gas disc, which predict that the radio jets in this case percolate through the gas disc and drive shocks into the ISM at distances much larger than their physical extent. These results expand the number of low-luminosity radio sources found to impact the surrounding medium, thereby highlighting the possible relevance of these AGN for feedback.
2233. B3-VLA CSS sample
- ID:
- ivo://CDS.VizieR/J/A+A/426/463
- Title:
- B3-VLA CSS sample
- Short Name:
- J/A+A/426/463
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results of VLBA observations at 6 and 3.6cm for eighteen Compact Steep Spectrum radio sources (CSS) from the B3-VLA CSS sample. In most cases these VLBA images display a "Double/Triple" morphology, and the core is unambiguously detected in seven sources. Multifrequency images allow us to study the spectral properties of the individual source components and to constrain the spectral age. In lobe-dominated sources the radiative ages deduced from the synchrotron theory are in the range of up 5x10^3^ years, if equipartition magnetic field is assumed. Polarized emission is detected at a few percent level for two sources only. They were the only two sources displaying polarized emission in VLA A configuration data, and this implies that beam depolarization is not effective in reducing the integrated fractional polarization for these sources.
- ID:
- ivo://CDS.VizieR/J/A+AS/133/129
- Title:
- B3-VLA sample. I. 10.6 GHz data
- Short Name:
- J/A+AS/133/129
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 1 presents the 10.6GHz fluxes of B3-VLA sample and an updated list of the Optical Identification of the sample.
- ID:
- ivo://CDS.VizieR/J/A+A/406/579
- Title:
- B3-VLA sample. III. Polarisation
- Short Name:
- J/A+A/406/579
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Polarisation parameters are presented for 192 radiosources of the B3-VLA sample at 1.4, 2.7, 4.8, 10.5GHz. The polarisation has been measured with Effelsberg radiotelescope for 2.7, 4.8, 10.5GHz, while the 1.4 polarization is from NVSS (Cat. <VIII/65>) survey. Rotation Measures (RM) are presented for 143 radiosources.
- ID:
- ivo://CDS.VizieR/J/A+AS/139/359
- Title:
- B3-VLA sample. II. The database
- Short Name:
- J/A+AS/139/359
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Table 2 presents flux densities at 151, 327 and 408MHz and 1.4, 4.8 and 10.6GHz of B3-VLA sample and an updated list of the Optical Identifications of the sample.
- ID:
- ivo://CDS.VizieR/J/A+A/435/863
- Title:
- B3-VLA sample. IV: 74MHz flux densities
- Short Name:
- J/A+A/435/863
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- 74MHz flux densities are presented for 365 radiosources of the B3-VLA sample. Data were obtained as a by-product of the VLA A-array 74MHz survey of Tschager et al. (2003, Cat. <J/A+A/402/171>). These A-array data provide the first morphological information at this low frequency.
- ID:
- ivo://CDS.VizieR/J/A+A/483/263
- Title:
- BV light curve of V570 Per
- Short Name:
- J/A+A/483/263
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The orbit and physical parameters of the previously unsolved double-lined eclipsing binary V570 Per are derived using Asiago Echelle high-resolution and high S/N spectroscopy, and B, V photo-electric photometry. Effective temperatures, gravities, rotational velocities, and metallicities of both components are also obtained from atmospheric chi^2^ analysis. The observed properties of V570 Per components are compared to available families of stellar evolutionary tracks, in particular to BaSTI models computed on purpose for exactly the observed masses and varied chemical compositions.
- ID:
- ivo://CDS.VizieR/J/A+A/452/959
- Title:
- BV light curve of V781 Tau
- Short Name:
- J/A+A/452/959
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We analyze light curves of the W UMa type eclipsing binary V781 Tauri from three epochs and radial velocity curves from two epochs simultaneously, including previously unpublished B and V data. The overall time span is from 1983 to 2000 and the solution is done coherently in time (not phase) with five light curves and two sets of primary and secondary velocity curves. Minor systematic differences among the individual light curves are not large enough to undermine the value of a coherent solution that represents 18 years of observations. Times of minima confirm a period of 0.34491d and the general solution finds a small period change, dP/P, of (5.08+/-04)*10^-11^ that represents recent behavior. The eclipse timings cover the last half-century and find dP/P about four times smaller, corresponding to a period change time scale, P/(dP/dt) of about 6 million years. The system is over-contact with a filling factor of 0.205. The solution produces a temperature difference of about 260K between the components, an inclination of 65.9{deg}, and a mass ratio M_2_/M_1_=2.47. Separate solutions of the several light curves that incorporate dark spots find parameters that differ little from curve to curve. Absolute masses, luminosities, radii and the distance are derived, with luminosities and distance based on star 1 being of type G0V. The orbital angular momentum is compared with those of other W UMa type binaries and is normal. The star to star mass flow that one can infer from dP/dt is opposite to that expected from TRO (Thermal Relaxation Oscillator) theory, but pertains to a time span that is very short compared to the time scale of TRO oscillations.
- ID:
- ivo://CDS.VizieR/J/PAZh/35/44
- Title:
- BV light curves of 33 ASAS-3 Cepheids
- Short Name:
- J/PAZh/35/44
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- Cepheids, the principal distance indicators, point to the existence of two inner Galactic spiral arms in the immediate solar neighborhood (within 5kpc). However, the available Cepheids are clearly insufficient for a detailed study of the structure of these arms. Fortunately, southern-sky monitoring (the ASAS project) has led to the discovery of many new variable stars, more than one thousand of which have been identified as possible Cepheids. To improve the classification and to construct reliable light curves for new Cepheids, we have begun their regular photometric observations. Here, we present the first results: 1192 photoelectric BVIc observations were performed for 33 classicalCepheidswith the 76-cm telescope of the South-African Astronomical Observatory (SAAO, the South-African Republic) from December 2006 to January 2008.We provide tables of observations and V light and B-V and V-Ic color curves. The new observations together with ASAS-3 data have been used to improve the elements of the light variations.
