a detailed study with both a full pulsation analysis and dedicated spectroscopy
The published spectrum is not on disk here. Telting et al. used KPNO 4m (RC-Spec/F3KB, kpc-22b), NOT/ALFOSC grism #16 and WHT/ISIS. Only the WHT mean is here. The KPNO and NOT means behind the published 27910/5.410/-3.116 have not been found on disk -- ask J. H. Telting.
| reference | Telting et al. 2012, A&A 544, A1; Kern et al. 2018, MNRAS 474, 5186 |
| title | Three ways to solve the orbit of KIC 11558725: a 10-day beaming sdB+WD binary with a pulsating subdwarf |
| Kepler data used | the near-continuous 2010-2011 light curve |
| pulsations | Rich g-mode spectrum with a few low-amplitude p-modes |
| orbit | P = 10.05 d, K = 58 km/s; companion minimum mass 0.63 Msun, so an unseen white dwarf; Doppler beaming detected at 238 ppm consistent with the spectroscopic amplitude |
| spectra behind it | ground-based low-resolution spectroscopy in the Balmer-line region across the 2010 and 2011 seasons |
| the spectrum behind it | Telting et al. used KPNO 4m (RC-Spec/F3KB, kpc-22b), NOT/ALFOSC grism #16 and WHT/ISIS. Only the WHT mean is here. The KPNO and NOT means behind the published 27910/5.410/-3.116 have not been found on disk -- ask J. H. Telting. |
| survey archive | A LAMOST DR11 spectrum exists and is here as LAMOST/, fitted in the LAMOST sample: 27483 +- 138 / 5.525 +- 0.021, agreeing with the WHT-c fit here to 34 K and 0.003 dex. Two further DR11 epochs are available. |
| note | Kern et al. (2018) is a later study; no copy here. |
Paper: Telting12b.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 |
|---|---|---|---|---|---|---|---|---|---|---|
| LAMOST | LAMOST | 1 | 240.7 | 2.50 | 27483 ± 138 | 5.525 ± 0.021 | -3.16 ± 0.06 | 1.09% | 0.97 | |
| WHT-c ★ | WHT / ISIS blue arm | 2010-07-28 | 14 | 396.6 | 1.86 | 27517 ± 33 | 5.522 ± 0.006 | -3.31 ± 0.06 | 0.55% | 2.08 |
★ 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] | 1273 |
| parallax error [%] | 3.5 (per cent; the mass error is twice this) |
| E(44−55) [mag] | 0.018 (0.010–0.028) |
| … the dust map | 0.0563 (SFD×disk(f=0.93)) |
| log Θ [rad] | -11.159 +0.005 −0.005 |
| R [R☉] | 0.196 +0.007 −0.007 |
| M [M☉] | 0.466 +0.068 −0.060 |
| L [L☉] | 19.8 +1.7 −1.5 |
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 27517 K and log g 5.522 from WHT-c, with 34 of the fitted bands and reduced χ² 0.24. 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:Ks, WISE:W2, WISE:W3, WISE:W4, 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, PAN-STARRS/PS1:y — the last of these was not excluded by rule but clipped, sitting beyond five sigma of a model that fits its neighbours.
wht/ is the original 2011 fitprof22 working directory, kept as it was run, with the line list of its own era. It holds no sp.spek, so fitk1 does not read it. The live directory is WHT-c/, extracted from the same meanallc.fits and linked to the master. Only the continuum-corrected mean exists for this target, which is what the -c says; there is no raw twin.