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5231. PM2000 Bordeaux Proper Motion catalogue
ID:
ivo://CDS.VizieR/I/300
Title:
PM2000 Bordeaux Proper Motion catalogue
Short Name:
I/300
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a proper motion catalogue of 2 670 974 stars, covering the declination zone +11{deg}<{delta}<+18{deg}. The catalogue has a limiting magnitude V=16.2 (Bordeaux CCD meridian circle magnitude) and is complete down to V=15.4. Depending on magnitude, the positional precision at mean epoch ranges from 50 to 70mas and the precision of proper motions varies from 1.5mas/yr to 6mas/yr. Meridian V magnitudes are provided for all objects together with additional photometry from the 2MASS catalogue when available (99.5% of objects). Positions and proper motions are on the ICRS (International Celestial Reference System). Proper motions are derived from the comparison of the positional M2000 catalogue (systematic observations of the Bordeaux Carte du Ciel Zone with the meridian circle, completed in 2000) with positions derived from the reduction of 512 Carte du Ciel plates of the Bordeaux zone (scanned at the APM Cambridge), the AC2000.2 catalogue, the USNO-A2.0 catalogue and the unpublished Yellow Sky (YS) USNO catalogue. Systematic offsets in 2MASS positions and in UCAC2 proper motions were revealed from comparisons with PM2000.
5232. PM J22299+3024 and LP 119-10 light curves
ID:
ivo://CDS.VizieR/J/A+A/651/A14
Title:
PM J22299+3024 and LP 119-10 light curves
Short Name:
J/A+A/651/A14
Date:
22 Feb 2022
Publisher:
CDS
Description:
We continued our ground-based observing project with the season-long observations of ZZ Ceti stars at the Konkoly Observatory. Our present targets are the newly discovered PM J22299+3024 and the already known LP 119-10 variables. LP 119-10 was also observed by the TESS space telescope in 120-second cadence mode. Our main aims are to characterise the pulsation properties of the targets and extract pulsation modes from the data for asteroseismic investigations. We performed a standard Fourier analysis of the daily, weekly, and entire data sets, together with test data of different combinations of weekly observations. We then performed asteroseismic fits utilising the observed and the calculated pulsation periods. For the calculations of model grids necessary for the fits, we applied the 2018 version of the White Dwarf Evolution Code. We derived six possible pulsation modes for PM J22299+3024 and five plus two TESS pulsation frequencies for LP 119-10. We note that further pulsation frequencies may be present in the data sets, but we found their detection ambiguous, so we omitted them from the final frequency list. Our asteroseismic fits of PM J22299+3024 give 11400K and 0.46M_{sun}_ for the effective temperature and the stellar mass, respectively. The temperature is ~800K higher, while the mass of the model star is exactly the same as was earlier derived by spectroscopy. Our model fits of LP 119-10 put the effective temperature in the range of 11800-11900K, which is again higher than the spectroscopic 11290K value. Moreover, our best model solutions give M*=0.70M_{sun}_ mass for this target, which is near to the spectroscopic value of 0.65M_{sun}_ and likewise in the case of PM J22299+3024. The seismic distances of our best-fit model stars agree with the Gaia astrometric distances of PM J22299+3024 and LP 119-10 within the errors, validating our model results.
5233. PMN J0948+0022 radio-to-gamma-ray monitoring
ID:
ivo://CDS.VizieR/J/A+A/548/A106
Title:
PMN J0948+0022 radio-to-gamma-ray monitoring
Short Name:
J/A+A/548/A106
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present more than three years of observations at different frequencies, from radio to high-energy gamma-rays, of the Narrow-Line Seyfert 1 (NLS1) Galaxy PMN J0948+0022 (z=0.585). This source is the first NLS1 detected at energies above 100 MeV and therefore can be considered the prototype of this emerging new class of gamma-ray emitting active galactic nuclei (AGN). The observations performed from 2008 August 1 to 2011 December 31 confirmed that PMN J0948+0022 generates a powerful relativistic jet, able to develop an isotropic luminosity at gamma-rays of the order of 10^48^erg/s, at the level of powerful quasars. The evolution of the radiation emission of this source in 2009 and 2010 followed the canonical expectations of relativistic jets, with correlated multiwavelength variability (gamma-rays followed by radio emission after a few months), but it was difficult to retrieve a similar pattern in the light curves of 2011. The comparison of gamma-ray spectra before and including 2011 data suggested that there was a softening of the high-energy spectral slope. We selected five specific epochs to be studied by modelling the broad-band spectrum, characterised by an outburst at gamma-rays or very low/high flux at other wavelengths. The observed variability can largely be explained either by changes in the injected power, the bulk Lorentz factor of the jet or the electron spectrum. The characteristic time scale of doubling/halving flux ranges from a few days to a few months, depending on the frequency and the sampling rate. The shortest doubling time scale at gamma-rays is 2.3+/-0.5days. These small values underline the need of highly-sampled multiwavelength campaigns to better understand the physics of these sources.
5234. PM-selected stars of Hercules galaxy
ID:
ivo://CDS.VizieR/J/A+A/570/A61
Title:
PM-selected stars of Hercules galaxy
Short Name:
J/A+A/570/A61
Date:
21 Oct 2021
Publisher:
CDS
Description:
Discovered in the last decade as overdensities of resolved stars, the ultra-faint dwarfs (UFDs) are among the least luminous, most dark-matter dominated, and most metal-poor galaxies known today. They appear as sparse, loose objects with high mass-to-light ratios. Hercules is the prototype of the UFD galaxies. To date, there are still no firm constraints on its total luminosity due to the difficulty of disentangling Hercules bona-fide stars from the severe Galactic field contamination. To better constrain Hercules properties, we aim at removing foreground and background contaminants in the galaxy field using the proper motions of the Milky Way stars and the colour-colour diagram. We have obtained images of Hercules in the r_Sloan_ , B_Bessel_ and U_spec_ bands with the Large Binocular Telescope (LBT) and LBC-BIN mode capabilities. The r_Sloan_ new dataset combined with data from the LBT archive span a time baseline of about 5yr, allowing us to measure proper motions of stars in the Hercules direction for the first time. The U_spec_ data along with existing LBT photometry allowed us to use colour-colour diagram to further remove the field contamination. Description: The Hercules ultra-faint dwarf (UFD) galaxy (J2000 position 16:31:02.0+12:47:25.6) was observed with the Large Binocular Camera (LBC) at the LBT located on Mount Graham in Arizona. The LBC is a wide field imager (4 CCDs, 2Kx4.5K pixels each) with a FoV of ~23'x 23' and a resolution of 0.225"/pix. We employed both archival and proprietary data to have the longest available time baseline. File table2 contains the final catalogue of 528 PM-selected sources. From left to right we report: the source identity (Col. 1), right ascension and declination (Col. 2-3), U_spec_, B_Bessel_ and r_Sloan_ magnitudes with their uncertainty (Col. 4-6), displacement with its uncertainty (Col. 7)
5235. PMS stars in open clusters: the DAY-I Catalogue
ID:
ivo://CDS.VizieR/J/A+A/467/1397
Title:
PMS stars in open clusters: the DAY-I Catalogue
Short Name:
J/A+A/467/1397
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the basic ideas and first results from the project we are carrying out at present, the search for and characterisation of pre-main sequence (PMS) stars among the members of Galactic young clusters. The observations of 10 southern clusters, nine of them located in the Carina-Sagittarius spiral arm of the Milky Way are presented. We aim at listing candidate PMS member stars in young clusters. The catalogued stars will serve as a basis for future spectroscopic studies of individual objects to determine the properties of stellar formation in the last phases before the main sequence stage. Properties such as the presence of residual envelopes or disks, age spread among PMS members, and the possible presence of several episodes of star formation in the clusters, are to be addressed. Multicolour photometry in the UBVRcIc system has been obtained for 10 southern young clusters in the fourth Galactic quadrant, located between Galactic longitudes l=238 and l=310. For six clusters in the sample, the observations presented here provide the first published study based on CCD photometry. A quantitative comparison is performed with post-MS isochrones, and PMS isochrones from three different evolutionary models are used in the photometric membership analysis for possible PMS stars. The observations produce photometric indices in the Johnson-Cousins photometric systems for a total of 26962 stars. The matching of our pixel coordinates with corresponding fields in the 2MASS data base provides astrometric calibration for all catalogued stars and JHK 2MASS photometric indices for 60% of them. Post-MS cluster ages range from 4 to 60Myr, whereas the photometric membership analysis assigns PMS membership assignment to a total of 842 stars, covering an age range between 1 and 10Myr. This information on the PMS candidate members has been collected into a catalogue, named DAY-I, which contains 16 entries for 842 stars in the field of 10 southern clusters.
5236. PMS stars in the Cepheus flare region
ID:
ivo://CDS.VizieR/J/ApJS/185/451
Title:
PMS stars in the Cepheus flare region
Short Name:
J/ApJS/185/451
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present results of optical spectroscopic and BVR_C_I_C_ photometric observations of 77 pre-main-sequence (PMS) stars in the Cepheus flare region. A total of 64 of these are newly confirmed PMS stars, originally selected from various published candidate lists. We estimate effective temperatures and luminosities for the PMS stars, and comparing the results with PMS evolutionary models, we estimate stellar masses of 0.2-2.4M_{sun}_ and stellar ages of 0.1-15Myr. Among the PMS stars, we identify 15 visual binaries with separations of 2-10". From archival IRAS, Two Micron All Sky Survey, and Spitzer data, we construct their spectral energy distributions (SEDs) and classify 5% of the stars as Class I, 10% as Flat SED, 60% as Class II, and 3% as Class III young stellar objects. We identify 12 classical T Tauri stars and two weak-line T Tauri stars as members of NGC 7023, with a mean age of 1.6Myr. The 13 PMS stars associated with L1228 belong to three small aggregates: RNO 129, L1228A, and L1228S. The age distribution of the 17 PMS stars associated with L1251 suggests that star formation has propagated with the expansion of the Cepheus flare shell. We detect sparse aggregates of ~6-7Myr old PMS stars around the dark clouds L1177 and L1219, at a distance of ~400pc. Three T Tauri stars appear to be associated with the Herbig Ae star SV Cep at a distance of 600pc. Our results confirm that the molecular complex in the Cepheus flare region contains clouds of various distances and star-forming histories.
5237. PN and HII regions of West and East of NGC 3109
ID:
ivo://CDS.VizieR/J/A+A/466/75
Title:
PN and HII regions of West and East of NGC 3109
Short Name:
J/A+A/466/75
Date:
21 Oct 2021
Publisher:
CDS
Description:
Images obtained with the ESO VLT and FORS1 in [O III] 5007 on- and off-band, as well as r_Gunn filters, are analyzed to search for planetary nebula (PN) candidates. In the continuum-subtracted [O III] 5007 on-band images, a large number of emission-line regions were detected. We describe the criteria employed for distinguishing PN candidates from compact HII regions.
5238. PN ETHOS 1 Bgri magnitudes & radial velocities
ID:
ivo://CDS.VizieR/J/MNRAS/498/6005
Title:
PN ETHOS 1 Bgri magnitudes & radial velocities
Short Name:
J/MNRAS/498/6005
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present a detailed study of the binary central star of the planetary nebula ETHOS 1 (PN G068.1+11.0). Simultaneous modelling of light and radial velocity curves reveals the binary to comprise a hot and massive pre-white-dwarf with an M-type main-sequence companion. A good fit to the observations was found with a companion that follows expected mass-temperature-radius relationships for low-mass stars, indicating that despite being highly irradiated it is consistent with not being significantly hotter or larger than a typical star of the same mass. Previous modelling indicated that ETHOS 1 may comprise the first case where the orbital plane of the central binary does not lie perpendicular to the nebular symmetry axis, at odds with the expectation that the common envelope is ejected in the orbital plane. We find no evidence for such a discrepancy, deriving a binary inclination in agreement with that of the nebula as determined by spatio-kinematic modelling. This makes ETHOS 1 the ninth post-common-envelope planetary nebula in which the binary orbital and nebular symmetry axes have been shown to be aligned, with as yet no known counter-examples. The probability of finding such a correlation by chance is now less than 0.00002%.
5239. PN G283.7-05.1 BVRI and RV curves
ID:
ivo://CDS.VizieR/J/A+A/642/A108
Title:
PN G283.7-05.1 BVRI and RV curves
Short Name:
J/A+A/642/A108
Date:
21 Oct 2021
Publisher:
CDS
Description:
We present the discovery and characterisation of the post-common-envelope central star system in the planetary nebula PN G283.7-05.1. Deep images taken as part of the POPIPlaN survey indicate that the nebula may possess a bipolar morphology similar to other post-common-envelope planetary nebulae. Simultaneous light and radial velocity curve modelling reveals the newly discovered binary system to comprise a highly-irradiated, M-type main-sequence star in a 5.9 hour orbit with a hot pre-white-dwarf. The nebular progenitor is found to have a particularly low mass of around 0.4M_{sun}_, making PN G283.7-05.1 one of only a handful of candidate planetary nebulae to be the product of a common-envelope event while still on the red giant branch. Beyond its low mass, the model temperature, surface gravity and luminosity are all found to be consistent with the observed stellar and nebular spectra through comparison with model atmospheres and photoionisation modelling. However, the high temperature (Teff~95kK) and high luminosity of the central star of the nebula are not consistent with post-RGB evolutionary tracks.
5240. PN Ou5 gri and RV curves
ID:
ivo://CDS.VizieR/J/MNRAS/510/3102
Title:
PN Ou5 gri and RV curves
Short Name:
J/MNRAS/510/3102
Date:
19 Jan 2022 08:33:22
Publisher:
CDS
Description:
We present a detailed study of the stellar and orbital parameters of the post-common envelope binary central star of the planetary nebula Ou5. Low-resolution spectra obtained during the primary eclipse - to our knowledge the first isolated spectra of the companion to a post-common-envelope planetary nebula central star - were compared to catalogue spectra, indicating that the companion star is a late K- or early M-type dwarf. Simultaneous modelling of multi-band photometry and time-resolved radial velocity measurements was then used to independently determine the parameters of both stars as well as the orbital period and inclination. The modelling indicates that the companion star is low mass (~0.25M_{sun}_) and has a radius significantly larger than would be expected for its mass. Furthermore, the effective temperature and surface gravity of nebular progenitor, as derived by the modelling, do not lie on single-star post-AGB evolutionary tracks, instead being more consistent with a post-RGB evolution. However, an accurate determination of the component masses is challenging. This is principally due to the uncertainty on the locus of the spectral lines generated by the irradiation of the companion's atmosphere by the hot primary (used to derive companion star's radial velocities), as well as the lack of radial velocities of the primary.