no detailed study of the Kepler data; the survey papers mention it, but a survey is not a study
No detailed study. An orbital period of 0.60513 d is recorded in the target list, and the class there is sdB+WD. Three mean spectra -- KPNO, NOT and WHT, reduced onto one wavelength scale in January 2012 -- came from J. Telting in September 2026 and are fitted here. Nothing about them is published.
| what it probably is | PROBABLY A COMPOSITE, and probably not sdB+WD. The spectroscopy and the photometry both carry a cool star: Mg I b is 3.6 sigma deep in the LAMOST spectrum, the continuum runs a sixth above a pure-subdwarf model by 8800 A, and the SED can only be fitted by inventing three times the reddening the dust maps allow, which is what drives its radius to an impossible 0.94 Msun. See the SED section below for all of it. |
| what that would mean | If there is a cool companion, the 0.60513 d signal does not have to be an orbit at all. Spots on a rotating star produce it just as well, and then nothing requires a white dwarf -- the beaming-plus-ellipsoidal reading is the one that needs the compact companion, not the data. That would make this sdB+MS. |
| was an orbit ever found? | And J. Telting's own file names bear on it. He corrected for the orbit wherever he had one: Hamfast, Primula, Rudigar and Will all arrived as '-noOrbit' means, and every one of those four has a published orbit with a measured K1. Lobelia's three are plain means with no such suffix, which says there was no orbit solution for this star in January 2012 -- consistent with none being findable now. |
| the two readings | The logic then runs: if the means really are plain, the system is sdB+MS and the photometric period is rotation. If it turns out they were orbit-corrected after all, both companions are needed and the system is a hierarchical triple, sdB+WD+MS. J. Telting's individual spectra would settle it outright; the mean spectra here cannot. |
| observation | telescope | date | n | S/N | FWHM [Å] | Teff [K] | log g | log n(He)/n(H) | residual | χ² |
|---|---|---|---|---|---|---|---|---|---|---|
| KPNO | kp4m / test | 2010-08-15 | 3 | 80.2 | 1.69 | 29047 ± 268 | 5.511 ± 0.040 | -2.42 ± 0.06 | 2.36% | 2.01 |
| LAMOST | LAMOST | 1 | 75.9 | 2.50 | 28452 ± 402 | 5.597 ± 0.063 | -2.40 ± 0.10 | 2.65% | 0.98 | |
| NOT | NOT / ALFOSC_FASU | 2011-08-29 | 3 | 90.9 | 2.36 | 27332 ± 176 | 5.603 ± 0.030 | -2.42 ± 0.06 | 1.82% | 1.51 |
| WHT ★ | WHT / ISIS blue arm | 2010-08-26 | 6 | 236.0 | 1.67 | 27769 ± 68 | 5.610 ± 0.011 | -2.47 ± 0.03 | 0.82% | 1.60 |
| WHT-2009 | WHT / ISIS blue arm | 2009-04-13 | 1 | 90.8 | 4.00 | 27740 ± 133 | 5.518 ± 0.023 | -2.41 ± 0.09 | 2.04% | 2.57 |
★ 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] | 1529 |
| parallax error [%] | 5.2 (per cent; the mass error is twice this) |
| E(44−55) [mag] | 0.087 (= E(44-55); R(55) = 3.03; HELD at this value for the two-component fit, not fitted) |
| … the dust map | 0.0866 (SFD×disk(f=0.92)) |
| log Θ [rad] | — |
| R [R☉] | 0.189 +0.010 −0.009 |
| M [M☉] | 0.532 +0.090 −0.075 |
| L [L☉] | 19.2 +2.2 −1.9 |
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 27769 K and log g 5.610 from WHT, with 32 of the fitted bands and reduced χ² 0.16. 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:Ks, 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, 2MASS:J, 2MASS:H, WISE:W1, WISE:W2.
| how they compare | The fit wants E(44-55) = 0.261 where the dust maps say 0.087, and the radius that follows makes the mass 0.94 Msun -- twice what an sdB should be. Both point the same way: something red is in this aperture that the model does not have. The 2MASS points, drawn but not fitted, sit well above the photosphere. |
| what the classifier says | The classifier is suggestive and short of a verdict. On the LAMOST spectrum it returns sdB with the note "Mg I b suggests a companion but Ca II does not (0.5 sigma)"; on the 2009 WHT spectrum it flags "possible composite (4.4 sigma) -- worth an SED", though that one also carries a wavy-continuum warning. WHT and NOT give a plain sdB, and the KPNO CV call is a four-sigma He II 4686 "emission" in the noisiest spectrum of the five -- ignore it. |
| the cool-star lines | Measured directly against a local continuum on LAMOST: Mg I b 1.5 per cent deep at 3.6 sigma, Ca II 8542 2.9 per cent at 2.9 sigma -- both about what a K star diluted to a sixth of the light would give. But Ca II 8662, which should be four fifths of 8542, is absent (-1.6 sigma), Ca II 8498 comes out in apparent EMISSION (-3.5 sigma), and Fe I 5270 is not there at all. Na I D is strong (5.6 sigma) and proves nothing: at E(B-V) 0.087 it is interstellar. Two of the three triplet lines failing is not a detection. |
| the red excess | Against a pure-sdB model at the map's reddening the LAMOST spectrum runs 1.00 from 4000 to 7400 A and then climbs -- 1.046 by 7600-8000, 1.115 by 8200-8500, 1.158 by 8700-9000, on 0.4 per cent errors. A red excess of a sixth by 8800 A is what the SED turned into extra reddening. Whether it is real is the open question: 8498 coming out in emission says LAMOST's red arm is not to be trusted here. |
| photometry against spectrum | And the two data sets disagree over the same wavelengths. Put the LAMOST spectrum through the g, r, i, z filters and the catalogue is redder than it by 16, 21 and 17 per cent in r, i and z relative to g -- about 0.17 mag in g-i, which is exactly the extra reddening the SED fit invented. One of the two is wrong, and the SED believes the photometry. |
| what the two-component fit adds | 2026-09-13, with the per-band survey limits in: the blanket "past depth" call above is WRONG band by band. 2MASS J at 15.32 against the 15.8 the survey reaches, H at 14.93 against 15.1, WISE W1 at 14.87 against 17.1 and W2 at 14.91 against 15.7 are all comfortably inside their limits; only Ks (14.86 against 14.3) is genuinely past, with W3 and W4. So the "J/H/K photometry deep enough to matter" the verdict below asks for was already on disk, discarded by a V<15 gate applied to the whole infrared at once. With those four bands back and 31 Gaia XP bins added, a one-star fit HELD at the dust map's reddening gives reduced chi-square 30; a two-component fit gives 0.18, better by dchi2 433, with an 11.6 sigma excess on W1. R1 = 0.189, M1 = 0.530 (+0.090 -0.075) against the 0.79-0.94 the one-star fit gave: canonical at last. BUT IT DOES NOT SETTLE THE CONFLICT ABOVE -- it takes the photometry's side of it, which is the side under suspicion. The companion it wants is T2 = 4000 K with R2 = 0.80 Rsun, which is 1.46 times the main-sequence radius at that temperature, and it predicts a red excess of 1.21 by 7800 A, 1.27 by 8350 and 1.31 by 8800 where the LAMOST spectrum measures 1.046, 1.115 and 1.158 -- about half. Two independent signs, the oversized radius and the over-predicted excess, that the photometry-driven companion is too luminous. So the disagreement is now quantified rather than resolved: the infrared says a companion is there more firmly than before, and says it is smaller than the optical catalogue implies. |
| a test that failed | One test that promised to settle it and did not. If the 0.605 d signal were an orbit, a plain mean of spectra taken across it would have smeared lines, and the fit would want a broader instrumental profile than the interstellar Ca II K line gives. It does: the WHT mean prefers 2.20 A against Ca II K's 1.67, the NOT mean 2.90 against 2.36, the KPNO mean 2.50 against 1.69 -- 1.4 to 1.8 A of extra width, which read as orbital motion would be K1 of 60 to 75 km/s. But run the same test on the controls and it falls apart. Will's means, which WERE shifted to rest before co-adding, show no excess at all -- as they should. Pippin's plain 18-spectrum NOT mean shows 1.28 A, nearly as much as Lobelia, and Kern et al. (2017) measured its radial velocities: rms 9.5 km/s with no periodic signal. So most of that width is exposure-to-exposure scatter in the wavelength solution, not the star, and shifting to rest removes both at once. The test cannot separate an orbit from a co-add, and nothing should be concluded from Lobelia's being the largest of them. |
| verdict | So: consistent with the sdB+G/K composite the target list does not claim, not established by it. What would settle it is a red spectrum from an instrument whose flux calibration can be trusted past 8000 A, or J/H/K photometry deep enough to matter -- at V = 15.5 the 2MASS points here are past the survey's depth, which is why they are drawn and not fitted. Until then the class in the target list stays sdB+WD and the 0.94 Msun stays flagged. [Superseded in part, 2026-09-13 -- see above. The mass quoted is now 0.530 from the two-component fit, and the claim that the 2MASS points are past survey depth was wrong for J and H. What still stands: a red spectrum with trustworthy calibration past 8000 A is what would settle it, and the class stays as the target list has it until one exists.] |
A cool companion and extra reddening both redden the model, so the reddening is HELD rather than fitted -- at the one-star value where that agreed with the dust map, and at the map's value where it did not, since there the disagreement IS the companion.
| companion Teff [K] | 4000 |
| … log g (held) | 4.50 |
| R1 [R☉] | 0.1891 |
| R2 [R☉] | 0.7975 |
| main-sequence R at that T [R☉] | 0.550 |
| R2 over that | 1.45 |
| Δχ² over one star | 404.9 |
| reduced χ² | 0.16 |
| excess over one star | 11.5 sigma on WISE:W1 |
| bands put back for it | 2MASS:J, 2MASS:H, WISE:W1, WISE:W2 |
| reddening | 0.087 (held) |
| verdict | kept |
The radius and mass above come from this fit, not from the one-star one. With the companion's red flux unaccounted for, a single star buys the excess as reddening and inflates the scale — here it wanted E(44−55) 0.182 against a sightline carrying 0.0866, and returned a mass no subdwarf has.
means/ holds three mean spectra as they arrived from J. Telting in
September 2026, plus the tarball they came in. They reached me inside
the Saradoc folder and under the name Saradoc.tgz, but the FITS say
OBJECT = KIC10149211 and the coordinates are 19:39:18 +47:08:55, so they
are this star and not Saradoc (KIC 10139564); the archive was renamed
kic10149211-means.tgz and moved here. All three were resampled by the
reducer onto one 3517-5073 A, 0.765 A/px scale so that the telescopes can
be compared pixel for pixel -- the same January 2012 reduction batch that
produced Paladin's and Primula's means.
KPNO/ mean of 3 KPNO 4-m exposures, 2010-08-15, observers M. Reed and
L. Farris. Those exposures did not reach below 3684 A, so the
first 225 pixels of the common grid are exactly zero and mkspek
trims them; left in they would have flattered the sigcont noise
estimate and made the quoted range a lie. The fitted lines stop
at H11, whose bluest continuum anchor is at 3741 A, so nothing is
lost from the fit.
NOT/ mean of 3 NOT/ALFOSC grism #16 exposures at 0.5", 2011-08-29.
WHT/ mean of 6 WHT/ISIS R600B exposures, 2010-08-26. At S/N 236 and
1.67 A resolution this is the best spectrum of the star by a wide
margin, and its fit has a residual of 0.82% against 1.8-2.6% for
everything else, so it is the one the sample table quotes.
WHT-2009/ was called WHT until these arrived: a single 300 s WHT/ISIS
R300B spectrum from 2009-04-13 at 4.0 A resolution, kept because it is a
separate observation and the comparison is the point. wht2009/ is its
2009 fitprof22 working directory, copied from
data/spek/kepler/KepVI/sdB/J19393+4708 and kept as it was run; it holds
no sp.spek, so fitk1 does not read it. Paladin is laid out the same way
and for the same reason.
LAMOST/ is the LAMOST DR11 fit of the same star, copied verbatim from
share/lamost/J19393+4708 and marked "as_run" in spec.info so fitk1 leaves
it alone. It is not refitted here because the two pipelines differ: the
LAMOST one imposes a single radial velocity on every line and interpolates
over thirteen helium grids, fitk1 lets each line find its own shift and
uses six. Re-deriving it under fitk1 gives 28764 K against the 28452 K
quoted in the LAMOST sample. Pippin/lamost is the same case.