- ID:
- ivo://CDS.VizieR/I/206
- Title:
- Bright Stars Supplement to PPM
- Short Name:
- I/206
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A number of bright stars is missing from the PPM Star Catalogue, both on the northern <I/146> and on the southern <I/193> hemisphere. The Bright Stars Supplement described here makes PPM complete down to V=7.5 mag. For this purpose it lists all missing stars brighter than V=7.6 mag that we could find in published star lists. Their total number is 275. Only 2 of them are brighter than V=3.5. This replaces the December 1992 edition (catalogue I/194) of the Bright Stars Supplement which inadvertently contained 46 duplicates of stars already contained in the main parts of PPM.
Number of results to display per page
Search Results
- ID:
- ivo://CDS.VizieR/J/MNRAS/472/4173
- Title:
- Bright white dwarfs for high-speed photometry
- Short Name:
- J/MNRAS/472/4173
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- The upcoming NASA Transiting Exoplanet Survey Satellite (TESS) will obtain space-based uninterrupted light curves for a large sample of bright white dwarfs distributed across the entire sky, providing a very rich resource for asteroseismological studies and the search for transits from planetary debris. We have compiled an all-sky catalogue of ultraviolet, optical and infrared photometry as well as proper motions, which we propose as an essential tool for the preliminary identification and characterization of potential targets. We present data for 1864 known white dwarfs and 305 high-probability white dwarf candidates brighter than 17mag. We describe the spectroscopic follow-up of 135 stars, of which 82 are white dwarfs and 25 are hot subdwarfs. The new confirmed stars include six pulsating white dwarf candidates (ZZ Cetis), and nine white dwarf binaries with a cool main- sequence companion. We identify one star with a spectroscopic distance of only 25pc from the Sun. Around the time TESS is launched, we foresee that all white dwarfs in this sample will have trigonometric parallaxes measured by the ESA Gaia mission next year.
- ID:
- ivo://CDS.VizieR/J/MNRAS/459/1415
- Title:
- Bright white dwarfs IRAC photometry
- Short Name:
- J/MNRAS/459/1415
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We cross-correlate several sources of archival photometry for 1265 bright (V~16mag) white dwarfs (WDs) with available high signal-to-noise spectroscopy. We find 381 WDs with archival Spitzer+IRAC data and investigate this subsample for infrared excesses due to circumstellar dust. This large data set reveals 15 dusty WDs, including three new debris discs and the hottest WD known to host dust (WD 0010+280). We study the frequency of debris discs at WDs as function of mass. The frequency peaks at 12.5 per cent for 0.7-0.75M_{sun}_ WDs (with 3M_{sun}_ main-sequence star progenitors) and falls off for stars more massive than this, which mirrors predicted planet occurrence rates for stars of different masses.
- ID:
- ivo://CDS.VizieR/J/AJ/123/2206
- Title:
- BRI photometry of 3 QSO fields
- Short Name:
- J/AJ/123/2206
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- This paper describes the acquisition and analysis of imaging data for the identification of galaxies associated with z~4 damped Ly{alpha} systems. We present deep BRI images of three fields known to contain four z~4 damped systems. We discuss the reduction and calibration of the data, detail the color criteria used to identify z~4 galaxies, and present a photometric redshift analysis to complement the color selection. We have found no galaxy candidates closer to the QSO than 7" that could be responsible for the damped Ly{alpha} systems. Assuming that at least one of the galaxies is not directly beneath the QSO, we set an upper limit on this damped Ly {alpha} system of L<L^*^_LBG_/4. Finally, we have established a Web site to release these imaging data to the public, at http://kingpin.ucsd.edu/~dlaimg/papers/refern.html . The observations where made with LRIS on the Keck II telescope, on 13 Jan 1999 for PSS 0132+1341 and BR 0951-0450, and 23 Jan 1999 for PSS 1443+2724.
- ID:
- ivo://CDS.VizieR/J/A+AS/118/65
- Title:
- BRI & redshifts in Cl0939+472 & Cl0016+161
- Short Name:
- J/A+AS/118/65
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present results of a study of the galaxy population of Cl 0939+472 (z=0.41) and Cl 0016+161 (z=0.54). We have used narrow-band filters (FWHM=~90-200A) and broad band B, R, I filters covering the range from 3800A to 9200A obtain low resolution spectra for all galaxies brighter than R=22.5mag in a 5'x5' (Cl 0939+472) and a 3.5'x5' (Cl 0016+161) field. Template spectra for classical Hubble type and E+A galaxies were fitted to the low-resolution spectral energy distribution in order to determine the galaxies' redshift and the morphological type. We detected 160 cluster members in Cl 0939+472 and 100 in Cl 0016+161, with a success rate of about 80% in the determination of redshifts and corresponding classification of morphological types from spectral energy distributions. These results constitute a statistical improvement of at least a factor of 4 over the most complete study to date of these clusters. In particular, we provide a large sample of elliptical galaxies with secure membership, well suited for a study of evolutionary effects. The same E+A templates developed for the analysis of Cl 0939+472 were successful in recognizing almost all of the spectroscopically already known E+A galaxies in Cl 0016+161 and in identifying 10 new ones. Our results show that in this cluster, too, the fraction of E+A galaxies represents about 20% of the total galaxy population. This outlines the importance of taking into account galaxies with signs of recent star formation for a correct evaluation of the Butcher-Oemler effect in distant galaxy clusters.
- ID:
- ivo://CDS.VizieR/J/A+AS/124/283
- Title:
- BR magnitude and redshift of A1300
- Short Name:
- J/A+AS/124/283
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the first results of an optical follow-up of X-ray bright clusters of galaxies located between 0.15<=z<=0.31: B and R photometry as well as medium resolution spectroscopy of the galaxies. The cluster studied here - A1300 - is found to have a redshift of 0.3072 and a velocity dispersion of 1210km/s, based on 52 cluster members. Structures are observed in the galaxy number counts but the velocity histogram shows no significant departure from a Gaussian distribution.
- ID:
- ivo://CDS.VizieR/J/AJ/125/1711
- Title:
- Broad Absorption Line Quasars from SDSS
- Short Name:
- J/AJ/125/1711
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a catalog of 224 broad absorption line quasars (BALQSOs) from the Sloan Digital Sky Survey's Early Data Release Quasar Catalog, (Schneider et al., 2002, Cat. <J/AJ/123/567>) including a relatively complete and homogeneous subsample of 131 BALQSOs. Since the identification of BALQSOs is subject to considerable systematic uncertainties, we attempt to create a complete sample of SDSS BALQSOs by combining the results of two automated selection algorithms and a by-eye classification scheme. One of these automated algorithms finds broad absorption line troughs by comparing with a composite quasar spectrum. We present the details of this algorithm and compare this method with one that uses a power-law fit to the continuum. The BALQSOs in our sample are further classified as high-ionization BALQSOs (HiBALs), low-ionization BALQSOs (LoBALs), and BALQSOs with excited iron absorption features (FeLoBALs); composite spectra of each type are presented. We further present a study of the properties of the BALQSOs in terms of the balnicity distribution, which rises with decreasing balnicity. This distribution of balnicities suggests that the fraction of quasars with intrinsic outflows may be significantly underestimated. The balnicity index defined by Weymann et al. (1991ApJ...373...23W) amounts to a sort of equivalent width: a quasar is declared to be a BAL when its balnicity index is >=0.
- ID:
- ivo://CDS.VizieR/J/A+A/622/A15
- Title:
- Broad absorption line quasars in LDR1
- Short Name:
- J/A+A/622/A15
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present a study of the low-frequency radio properties of broad absorption line quasars (BALQSOs) from the LOFAR Two-metre Sky-Survey Data Release 1 (LDR1). The value-added LDR1 catalogue contains Pan-STARRS counterparts, which we match with the Sloan Digital Sky Survey (SDSS) DR7 and DR12 quasar catalogues. We find that BALQSOs are twice as likely to be detected at 144MHz than their non-BAL counterparts, and BALQSOs with low-ionisation species present in their spectra are three times more likely to be detected than those with only high-ionisation species. The BALQSO fraction at 144MHz is constant with increasing radio luminosity, which is inconsistent with previous results at 1.4GHz, indicating that observations at the different frequencies may be tracing different sources of radio emission. We cross-match radio sources between the Faint Images of the Radio Sky at Twenty Centimeters (FIRST) survey and LDR1, which provides a bridge via the LDR1 Pan-STARRS counterparts to identify BALQSOs in SDSS. Consequently we expand the sample of BALQSOs detected in FIRST by a factor of three. The LDR1-detected BALQSOs in our sample are almost exclusively radio-quiet (logr<2), with radio sizes at 144$\,$MHz typically less than 200kpc these radio sizes tend to be larger than those at 1.4GHz, suggesting more extended radio emission at low frequencies. We find that although the radio detection fraction increases with increasing balnicity index (BI), there is no correlation between BI and either low-frequency radio power or radio-loudness. This suggests that both radio emission and BI may be linked to the same underlying process, but are spatially distinct phenomena.
- ID:
- ivo://CDS.VizieR/J/MNRAS/469/4034
- Title:
- Broadband polarisation of radio AGN
- Short Name:
- J/MNRAS/469/4034
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- We present the results from a broadband (1 to 3GHz), spectro-polarimetry study of the integrated emission from 100 extragalactic radio sources with the ATCA, selected to be highly linearly polarized at 1.4 GHz. We use a general purpose, polarization model-fitting procedure that describes the Faraday rotation measure (RM) and intrinsic polarization structure of up to three distinct polarized emission regions or 'RM components' of a source. Overall, 37%/52%/11% of sources are best fit by one/two/three RM components. However, these fractions are dependent on the signal-to-noise ratio (S/N) in polarization (more RM components more likely at higher S/N). In general, our analysis shows that sources with high integrated degrees of polarization at 1.4GHz have low Faraday depolarization, are typically dominated by a single RM component, have a steep spectral index, and a high intrinsic degree of polarization. After classifying our sample into radiative-mode and jet-mode AGN, we find no significant difference between the Faraday rotation or Faraday depolarization properties of jet-mode and radiative-mode AGN. However, there is a statistically significant difference in the intrinsic degree of polarization between the two types, with the jet-mode sources having more intrinsically ordered magnetic field structures than the radiative-mode sources. We also find a preferred perpendicular orientation of the intrinsic magnetic field structure of jet-mode AGN with respect to the jet direction, while no clear preference is found for the radiative-mode sources.
- ID:
- ivo://CDS.VizieR/J/ApJ/821/33
- Title:
- Broad H{beta} emission line in 102 Seyfert galaxies
- Short Name:
- J/ApJ/821/33
- Date:
- 21 Oct 2021
- Publisher:
- CDS
- Description:
- A sample of 102 local (0.02=<z=<0.1) Seyfert galaxies with black hole masses M_BH_>10^7^M_{sun}_ was selected from the Sloan Digital Sky Survey (SDSS) and observed using the Keck 10 m telescope to study the scaling relations between M_BH_ and host galaxy properties. We study profile changes of the broad H{beta} emission line within the three to nine year time frame between the two sets of spectra. The variability of the broad H{beta} emission line is of particular interest, not only because it is used to estimate M_BH_, but also because its strength and width are used to classify Seyfert galaxies into different types. At least some form of broad-line variability (in either width or flux) is observed in the majority (~66%) of the objects, resulting in a Seyfert-type change for ~38% of the objects, likely driven by variable accretion and/or obscuration. The broad H{beta} line virtually disappears in 3/102 (~3%) extreme cases. We discuss potential causes for these changing look active galactic nuclei. While similar dramatic transitions have previously been reported in the literature, either on a case-by-case basis or in larger samples focusing on quasars at higher redshifts, our study provides statistical information on the frequency of H{beta} line variability in a sample of low-redshift Seyfert galaxies.
