| Issue |
A&A
Volume 602, June 2017
|
|
|---|---|---|
| Article Number | C2 | |
| Number of page(s) | 7 | |
| Section | Catalogs and data | |
| DOI | https://doi.org/10.1051/0004-6361/201525666e | |
| Published online | 14 June 2017 | |
The catalogue of radial velocity variable hot subluminous stars from the MUCHFUSS project (Corrigendum)
1 European Southern Observatory, Karl-Schwarzschild-Str. 2, 85748 Garching, Germany
e-mail: sgeier@eso.org
2 Dr. Karl Remeis-Observatory & ECAP, Astronomical Institute, Friedrich-Alexander University Erlangen-Nuremberg, Sternwartstr. 7, 96049 Bamberg, Germany
3 Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
4 Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria
5 Department of Physics, High Point University, One University Parkway, High Point, NC 27268, USA
6 Institute of Astronomy, KU Leuven, Celestijnenlaan 200D, 3001 Heverlee, Belgium
7 Australian Astronomical Observatory, PO Box 915, North Ryde NSW 1670, Australia
8 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK
9 Department of Physics, University of Warwick, Conventry CV4 7AL, UK
10 Centre of Astrophysics Research, University of Hertfordshire, College Lane, Hatfield AL10 9AB, UK
Key words: binaries: spectroscopic / subdwarfs / stars: horizontal branch / stars: atmospheres / errata, addenda
The function we used to calculate the logarithm of the false-detection probability provides the natural logarithm lnp and not the decadal logarithm as incorrectly assumed in the paper. This mildy affects the number of radial velocity (RV) variable stars and significantly the number of RV variable candidates in our sample. The conclusions of the paper essentially remain the same.
We consider the detection of RV variability to be significant, if the false-detection probability p is smaller than 0.01% (lnp< −9.2). The fraction of such significant detections in our initial sample of 196 is now 39% (76 objects). Objects with false-detection probabilities between 0.01% and 5% (lnp = −9.2 to lnp = −3.0) are regarded as candidates for RV variability and constitute 27% of the initial sample (53 objects). About 34% (lnp> −3.0, 67 objects) are regarded as non-detections. Removing those non-detections we end up with a sample of 129 stars, which show RV variability with probabilites between 95% and 99.9% (see Table 1).
Tables 3−5 and A.1 as well as Figures 1−6 of the original paper have been updated (Tables 2−5, Figs. 1−4).
The corrected upper limit for the fraction of extremely close binary sdB+NS/BH binaries is 1.5% instead of 1.3%.
The RV-variable sample now contains 18 helium-rich hot subdwarf stars. 6 of them show significant RV variations while 12 qualify as candidates (see Table 3). The He-sdOB J160450.44+051909.2 discussed in the paper is not regarded as RV-variable candidate any more.
Sample statistics.
 |
Fig. 1 Left panel: Teff−log g diagram of the full sample of hot, subluminous, RV-variable stars. The size of the symbols scales with ΔRVmax. The black circles mark stars with hydrogen dominated atmospheres (log y< 0), while the red diamonds mark stars with helium dominated atmospheres. The helium main sequence (HeMS) and the HB band are superimposed with HB evolutionary tracks (dashed lines) for subsolar metallicity (log z = −1.48) from Dorman et al. (1993). The three tracks in the high temperature range correspond to helium core masses of 0.488, 0.490 and 0.495 M⊙ (from bottom-left to top-right). Those tracks mark the EHB evolution, since the stars do not reascend the giant branch in the helium shell-burning phase. The two tracks in the upper right correspond to core masses of 0.53 and 0.54 M⊙. Blue horizontal branch stars following those tracks are expected to experience a second giant phase. The solid line marks the relevant part of the zero-age main sequence for solar metallicity taken from Schaller et al. (1992). The two dotted lines are post-AGB tracks for hydrogen-rich stars with masses of 0.546 (lower line) and 0.565 M⊙ (upper line) taken from Schönberner (1983). The two long-dashed lines are post-AGB tracks for helium-rich stars with masses of 0.53 (lower line) and 0.609 M⊙ (upper line) taken from Althaus et al. (2009). Right panel: Teff−log g diagram of RV variable hydrogen-rich sdB and sdOB stars. The two dotted lines mark post-RGB tracks (Driebe et al. 1998) for core masses of 0.234 (left) and 0,259 M⊙ (right). |
 |
Fig. 2 Left panel: highest RV shift between individual spectra plotted against time difference between the corresponding observing epochs. The filled red diamonds mark sdB binaries with known orbital parameters (Kupfer et al. 2015), while the filled black circles mark the rest of the hydrogen-rich sdB sample of RV variable stars. Right panel: the same plot for the hydrogen-rich sdOB and sdO sample of RV variable stars. |
 |
Fig. 3 ΔRVmax distribution of RV-variable sdB stars (left panel) as well as sdOB and sdO stars with hydrogen-rich atmospheres (right panel). |
 |
Fig. 4 Left panel: Teff−log g diagram of RV variable helium-rich sdOB and sdO stars (see Fig. 1). The size of the symbols scales with ΔRVmax. The helium main sequence (HeMS) and the HB band are superimposed with HB evolutionary tracks (dashed lines) for subsolar metallicity (log z = −1.48) from Dorman et al. (1993). The three tracks correspond to helium core masses of 0.488, 0.490 and 0.495 M⊙ (from bottom-left to top-right). Right panel: highest RV shift between individual spectra plotted against time difference between the corresponding observing epochs for helium-rich sdO and sdOB stars (see Fig. 2). |
Parameters of 101 hydrogen-rich hot subdwarfs (65 RV variable, 36 RV variable candidates).
Parameters of 18 helium-rich hot subdwarfs (6 RV variable, 12 RV variable candidates).
Parameters of 10 other types of hot stars (5 RV variable, 5 RV variable candidates).
Parameters of 67 stars with non-significant RV variations.
References
- Althaus, L. G., Panei, J. A., Miller Bertolami, M. M., et al. 2009, ApJ, 704, 1605 [NASA ADS] [CrossRef] [Google Scholar]
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- Driebe, T., Schönberner, D., Bloecker, T., & Herwig, F. 1998, A&A, 339, 123 [NASA ADS] [Google Scholar]
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- Schaller, G., Schaerer, D., Meynet, G., & Maeder, A. 1992, A&AS, 96, 269 [Google Scholar]
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© ESO, 2017
All Tables
Parameters of 101 hydrogen-rich hot subdwarfs (65 RV variable, 36 RV variable candidates).
Parameters of 18 helium-rich hot subdwarfs (6 RV variable, 12 RV variable candidates).
Parameters of 10 other types of hot stars (5 RV variable, 5 RV variable candidates).
All Figures
|
Fig. 1 Left panel: Teff−log g diagram of the full sample of hot, subluminous, RV-variable stars. The size of the symbols scales with ΔRVmax. The black circles mark stars with hydrogen dominated atmospheres (log y< 0), while the red diamonds mark stars with helium dominated atmospheres. The helium main sequence (HeMS) and the HB band are superimposed with HB evolutionary tracks (dashed lines) for subsolar metallicity (log z = −1.48) from Dorman et al. (1993). The three tracks in the high temperature range correspond to helium core masses of 0.488, 0.490 and 0.495 M⊙ (from bottom-left to top-right). Those tracks mark the EHB evolution, since the stars do not reascend the giant branch in the helium shell-burning phase. The two tracks in the upper right correspond to core masses of 0.53 and 0.54 M⊙. Blue horizontal branch stars following those tracks are expected to experience a second giant phase. The solid line marks the relevant part of the zero-age main sequence for solar metallicity taken from Schaller et al. (1992). The two dotted lines are post-AGB tracks for hydrogen-rich stars with masses of 0.546 (lower line) and 0.565 M⊙ (upper line) taken from Schönberner (1983). The two long-dashed lines are post-AGB tracks for helium-rich stars with masses of 0.53 (lower line) and 0.609 M⊙ (upper line) taken from Althaus et al. (2009). Right panel: Teff−log g diagram of RV variable hydrogen-rich sdB and sdOB stars. The two dotted lines mark post-RGB tracks (Driebe et al. 1998) for core masses of 0.234 (left) and 0,259 M⊙ (right). |
| In the text | |
|
Fig. 2 Left panel: highest RV shift between individual spectra plotted against time difference between the corresponding observing epochs. The filled red diamonds mark sdB binaries with known orbital parameters (Kupfer et al. 2015), while the filled black circles mark the rest of the hydrogen-rich sdB sample of RV variable stars. Right panel: the same plot for the hydrogen-rich sdOB and sdO sample of RV variable stars. |
| In the text | |
|
Fig. 3 ΔRVmax distribution of RV-variable sdB stars (left panel) as well as sdOB and sdO stars with hydrogen-rich atmospheres (right panel). |
| In the text | |
|
Fig. 4 Left panel: Teff−log g diagram of RV variable helium-rich sdOB and sdO stars (see Fig. 1). The size of the symbols scales with ΔRVmax. The helium main sequence (HeMS) and the HB band are superimposed with HB evolutionary tracks (dashed lines) for subsolar metallicity (log z = −1.48) from Dorman et al. (1993). The three tracks correspond to helium core masses of 0.488, 0.490 and 0.495 M⊙ (from bottom-left to top-right). Right panel: highest RV shift between individual spectra plotted against time difference between the corresponding observing epochs for helium-rich sdO and sdOB stars (see Fig. 2). |
| In the text | |
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