a detailed study with both a full pulsation analysis and dedicated spectroscopy
| reference | Baran et al. 2012, MNRAS 424, 2686 |
| title | A pulsation zoo in the hot subdwarf B star KIC 10139564 observed by Kepler |
| Kepler data used | 15 months |
| pulsations | 57 periodicities: ten g modes and the rest p modes, most of them components of multiplets with a common spacing; rotation period 25.6 +- 1.8 d; l >= 2 multiplets detected, which constrain the pulsation inclination and limb darkening |
| spectra behind it | a mean of 10 NOT/ALFOSC grism #16 spectra covering H-beta to H-theta |
| atmospheric parameters | Table 1: Teff 31859(126) K, log g 5.673(26), log N(He)/N(H) -2.201(36), from a mean of 10 NOT/ALFOSC spectra. H-epsilon was excluded from that fit because of interstellar Ca II contamination |
| the spectrum behind it | Found. The mean of ten NOT/ALFOSC spectra behind the published 31859/5.673/-2.201 is here as NOT/, built 2012-01-25 and sent in September 2026 in the working directory it was refitted in for Baran's TESS paper in February 2024. |
| how they compare | Three fits of that one mean. Baran et al. published 31859 +- 126 / 5.673 +- 0.026 / -2.201 +- 0.036 with H-epsilon dropped for the interstellar Ca II. Refitted on Uli's grid in February 2024 for the TESS paper, on fourteen lines down to H13, it gave 32035 +- 118 / 5.659 +- 0.019 / -2.133 +- 0.035. Refitted here on Bamberg v25 and the shared line list, H-epsilon kept and H11 the bluest, it gives 31647 +- 133 / 5.726 +- 0.019 / -2.19 +- 0.02. Three grids and three line lists agree to 388 K and 0.067 dex, which is about as well as this kind of fit ever agrees with itself. |
| note | The 32500 / 5.81 that the target list used to carry is not this paper's value; it was the fit made here from the WHT spectrum, which now gives 32594 +- 241 / 5.803 +- 0.038 on the shared line list. |
Paper: Baran12a.pdf, in /home/roy/sync/old/sddoc.
| observation | telescope | date | n | S/N | FWHM [Å] | Teff [K] | log g | log n(He)/n(H) | residual | χ² |
|---|---|---|---|---|---|---|---|---|---|---|
| NOT ★ | NOT / ALFOSC_FASU | 2011-06-01 | 10 | 158.8 | 2.06 | 31647 ± 133 | 5.726 ± 0.019 | -2.19 ± 0.02 | 1.16% | 2.00 |
| WHT | WHT / ISIS blue arm | 2009-07-15 | 1 | 71.1 | 3.42 | 32594 ± 241 | 5.803 ± 0.038 | -2.20 ± 0.07 | 1.76% | 1.23 |
★ marks the observation adopted for the sample table — the one with the smallest residual, which is what says how well the model reproduces the spectrum. Signal-to-noise does not.
The line fit gives a temperature and a gravity but says nothing about size. Held at those parameters, the broadband spectral energy distribution has one free scale — the angular diameter — and the Gaia parallax turns that into a radius. Then M = gR²/G, which is linear in g: a tenth of a dex in gravity is 26 per cent in mass, so this is where the gravity scale bites hardest.
| distance [pc] | 1956 |
| parallax error [%] | 6.2 (per cent; the mass error is twice this) |
| E(44−55) [mag] | 0.044 (0.032–0.054) |
| … the dust map | 0.0727 (SFD×disk(f=0.98)) |
| log Θ [rad] | -11.434 +0.006 −0.006 |
| R [R☉] | 0.160 +0.011 −0.010 |
| M [M☉] | 0.495 +0.093 −0.078 |
| L [L☉] | 23.0 +3.3 −2.7 |
Bamberg v25 ATLAS12 through the real filter curves, reddened by Fitzpatrick (1999) — its A(5500)/E(B−V) is 3.03, so this E(B−V) and the E(44−55) of Heber's group are the same number to under one per cent. Prescribed at 31647 K and log g 5.726 from NOT, with 32 of the fitted bands and reduced χ² 0.53. The gravity error carried into the mass is 0.050 dex — the scatter between telescopes, not the formal error, because the formal one would claim a two per cent mass.
Bands left out: Johnson:B, GALEX:NUV, GALEX:FUV, 2MASS:H, 2MASS:J, 2MASS:Ks, WISE:W2, GAIA/GAIA3:G, GAIA/GAIA3:Gbp, GAIA/GAIA3:Grp, SDSS:u, SDSS:g, SDSS:r, SDSS:i, SDSS:z, SDSS:u/SDSS:u', SDSS:g/SDSS:g', SDSS:r/SDSS:r', SDSS:i/SDSS:i', SDSS:z/SDSS:z', Johnson:U, Johnson:V, Cousins:U.
means/ holds meanallA.fits -- the mean of 10 NOT/ALFOSC grism #16 spectra that Baran et al. (2012) fitted for their Table 1 -- and Saradoc.tgz, the archive it came in. The mean itself was built on 2012-01-25, on the same 3517-5073 A, 0.765 A/px scale as J. Telting's January 2012 batch; the tarball is from February 2024, when it was refitted for Baran's TESS paper. So it is the newest FIT of the oldest mean, not a new reduction. NOT/ is that mean extracted here and fitted on Bamberg v25. It has the smaller residual of the two spectra, 1.16% against 1.76%, so it is the one the sample table quotes -- and it should be: it is the published spectrum. not2024/ is the February 2024 fitprof22 working directory as it arrived, with its .spek renamed meanallA.spek so that fitk1 does not read it. Two things about it are worth knowing. Its chidel.dat was a symlink to /home/roy/obs/not/setup/chidel.dat, which is not on this machine, so the link was dropped; the windows it used are printed in fit.out anyway, and they are not the shared ones -- it fitted fourteen lines down to H13, where the list here stops at H11, and it kept H-epsilon, which the published fit dropped for the interstellar Ca II. And its sp.spek sits two pixels blueward of its own FITS: 3515.47-5071.48 against 3517.00-5073.00. The FITS scale is the right one -- interstellar Ca II K lands 0.52 A off on it and would land 2.05 A off on the spek scale -- and that 1.53 A is most of why the 2024 per-line shifts came out near +1.8 A. NOT/ is extracted from the FITS, so it does not carry the offset. wht/ is the 2009 fitprof22 working directory, kept as it was run; it holds no sp.spek, so fitk1 does not read it, and the chidel.dat beside it is the 2010 per-star list, linked from the top of this folder. WHT/ is the live directory, extracted from J19249+4707.fits and linked to the master.