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J/MNRAS/440/3809    KIC 10670103 frequency spectrum          (Reed+, 2014)

Analysis of the rich frequency spectrum of KIC 10670103 revealing the most slowly rotating subdwarf B star in the Kepler field. Reed M.D., Foster H., Telting J.H., Ostensen R.H., Farris L.H., Oreiro R., Baran A.S. <Mon. Not. R. Astron. Soc., 440, 3809-3824 (2014)> =2014MNRAS.440.3809R (SIMBAD/NED BibCode)
ADC_Keywords: Stars, variable ; Stars, B-type ; Spectroscopy Keywords: stars: oscillations - subdwarfs Abstract: We analyse 2.75yr of Kepler spacecraft observations of the pulsating subdwarf B star KIC 10670103. These 1.4 million measurements have an impressive duty cycle of 93.8 per cent, a frequency resolution of 0.017µHz, and a 5σ detection limit of 0.1 parts-per-thousand (ppt). We detect 278 periodicities, making KIC 10670103 the richest pulsating subdwarf B star to date. Frequencies range from 23 to 673µHz (0.4 and 11.8h), with amplitudes from the detection limit up to 14 ppt. Follow-up spectroscopic data were obtained from which it was determined that KIC 10670103 does not show significant radial velocity variations. Updated atmospheric model fits determined Teff=21485±540K, logg=5.14±0.05, and logN(He)/N(H) =-2.60±0.04. We identify pulsation modes using asymptotic period spacings and frequency multiplets. The frequency multiplets indicate a spin period of 88±8d. Of the 278 periodicities detected in KIC 10670103, 163 (59 per cent) have been associated with low-degree (l≤2) pulsation modes, providing tight constraints for model fitting. While the data are exquisite, amplitudes (and some frequencies) are not stable over the course of the observations, requiring tools which are non-standard for compact pulsators such as sliding Fourier transforms and Lorentzian fitting. Using the 163 identified pulsation modes, it is possible to make detailed examinations of the pulsation structure; including where the pulsation power is concentrated in radial order, over what frequency range mode trapping is inefficient, and how power switches between multiplet members. Description: From 33 months of nearly continuous Kepler data, we have detected 278 periodicities in KIC 10670103, making it the richest sdBV star observed, so far. The 93.8 per cent duty cycle provided excellent data with a 5σ detection limit of 0.1ppt and a resolution of 0.017uHz. Objects: ------------------------------------------------------------------ RA (2000) DE Designation(s) ------------------------------------------------------------------ 19 34 39.94 +47 58 11.7 KIC 10670103 = 2MASS J19343993+4758117 ------------------------------------------------------------------ File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 99 278 The frequency list as a result of Lorentzian fitting
See also: V/133 : Kepler Input Catalog (Kepler Mission Team, 2009) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- ID Frequency identification 5 A1 --- n_ID [abd] Note on ID (1) 7- 13 F7.3 uHz Freq Frequency 15- 19 F5.3 uHz e_Freq rms uncertainty on Freq (2) 21- 28 F8.2 s Per Period 30- 34 F5.2 s e_Per rms uncertainty on Per (2) 36- 40 F5.2 10-3 Amp Amplitude (in ppt = parts-per-thousand) 42- 47 A6 --- l Best estimate of the mode degree l 49- 55 A7 --- m Azimuthal order m 57- 58 I2 --- n1 ?=- radial overtone n1 fit to Πl,nl,n=0+n.Δπl (3) 60- 62 I3 --- n2 ?=- radial overtone n2 fit to Πl,nl,n=0+n.Δπl (3) 64- 67 F4.2 --- dP/DPi1 ?=- Factional deviation from even period spacing 1 δP/ΔΠ1 69- 72 F4.2 --- dP/DPi2 ?=- Factional deviation from even period spacing 2 δP/ΔΠ2 74- 78 F5.3 uHz Dnu ?=- Δν Frequency splitting from the subsequent frequency, if it may be part of a multiplet 80- 81 A2 --- l_Model [≥ ] Limit flag on Model 82 I1 --- Model ?=- Mode degree l based on frequency multiplets 84- 85 A2 --- l_IDCnl [≥ ] Limit flag on MIDCnl 86 I1 --- IDCnl ?=- Value of the Ledoux constant from the frequency splitting (assuming Δm=1) 88- 94 A7 --- PS Period spacing (4) 96- 99 A4 --- M10 Frequency ID notation from Reed et al. (2010MNRAS.409.1496R)
Note (2): frequency/period errors are the corresponding Lorentzian linewidths. Note (3): where Πl=1,n=0 was estimated to be close to the radial fundamental mode. Note (1): Notes as follows: a = This multiplet was fitted using Quarters 9 through 15 only. b = This multiplet was fitted using Quarters 11 through 15 only. d = The FT peaks in these regions are particularly messy and we only attempted to fit the most obvious ones rather than all of them Note (4): c when More periods exist in this region than can be accomodated by the mode assignment
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 22-May-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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