J/MNRAS/510/5623 Study of Kepler's FGKM stars (Masuda+, 2022)
Inferring the rotation period distribution of stars from their projected
rotation velocities and radii Application to late-F/early-G Kepler stars.
Masuda K., Petigura E.A., Hall O.J.
<Mon. Not. R. Astron. Soc., 510, 5623-5638 (2022)>
=2022MNRAS.510.5623M 2022MNRAS.510.5623M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, F-type ; Stars, G-type ; Stars, K-type ; Stars, M-type ;
Photometry ; Spectroscopy ; Optical ; Effective temperatures ;
Abundances, [Fe/H] ; Rotational velocities ; Stars, diameters ;
Stars, distances ; Infrared ; Positional data ;
Parallaxes, trigonometric ; Proper motions ; Combined data
Keywords: methods: data analysis - methods: statistical -
techniques: spectroscopic - stars: rotation
Abstract:
While stellar rotation periods Prot may be measured from broad-band
photometry, the photometric modulation becomes harder to detect for
slower rotators, which could bias measurements of the long-period tail
of the Prot distribution. Alternatively, the Prot distribution of
stars can be inferred from their projected rotation velocities vsin i
and radii R, without being biased against photometrically quiet stars.
We solve this inference problem using a hierarchical Bayesian
framework, which (i) is applicable to heteroscedastic measurements of
vsin(i) and R with non-Gaussian uncertainties and (ii) does not
require a simple parametric form for the true Prot distribution. We
test the method on simulated data sets and show that the true Prot
distribution can be recovered from ~> 100 sets of vsin i and R
measured with precisions of 1 km.s-1 and 4 per cent, respectively,
unless the true distribution includes sharp discontinuities. We apply
the method to a sample of 144 late-F/early-G dwarfs in the Kepler
field with vsin(i) measured from Keck/HIRES spectra, and find that the
typical rotation periods of these stars are similar to the photometric
periods measured from Kepler light curves: we do not find a large
population of slow rotators that are missed in the photometric sample,
although we find evidence that the photometric sample is biased for
young, rapidly rotating stars. Our results also agree with
asteroseismic measurements of Prot for Kepler stars with similar
ages and effective temperatures, and show that ≃ 1.1 M☉ stars
beyond the middle of their main-sequence lifetimes rotate faster than
predicted by standard magnetic braking laws.
Description:
The study of stellar rotation has been revolutionized by
high-precision, continuous, and long-term photometry made available by
the Kepler mission (Borucki et al. 2010Sci...327..977B 2010Sci...327..977B; Koch et al.
2010ApJ...713L..79K 2010ApJ...713L..79K). Quasi-periodic brightness variations due to
active regions on the surface enabled rotation period measurements for
tens of thousands of FGKM stars, including those with longer period
and/or lower amplitude variabilities than can be studied with the
ground-based photometry. The data from the ongoing space missions such
as TESS (Ricker et al. 2014SPIE.9143E..20R 2014SPIE.9143E..20R) and Gaia (Gaia
Collaboration 2016A&A...595A...1G 2016A&A...595A...1G) will further expand the capability
of the photometry-based measurements (e.g. Lanzafame et al.
2018A&A...616A..16L 2018A&A...616A..16L; Claytor et al. 2021tsc2.confE.120C), (i.e see
introduction section).
A challenge to this inference is that the Prot of individual stars
with individual measurements of vsin(i) and R constrain as in the
equation 2 in the section 2 method where we present a mathematical
framework. Further in our study, we apply the mentionned method to
actual measurements of vsin(i) obtained from Keck/HIRES spectra for
late-F/early-G stars in the Kepler field (from Louden et al.
2021AJ....161...68L 2021AJ....161...68L, Cat. J/AJ/161/68) to infer the rotation period
distribution that is not conditioned on the detectable photometric
modulation, (i.e see introduction section). We focus on the latter
control stars that were selected without regard to the presence of
transiting planets, for which spin orientations can be assumed to be
isotropic. We used their 2MASS IDs to find the corresponding Gaia EDR3
sources (Gaia Collaboration 2021) as well as other nearby sources
within 10 arcsec. We removed stars with bad astrometry and/or
potential binary companions, apply log g < 3.9 cut-off from the
sample that satisfy criteria exposed in the section 4.1 Stellar sample
and parameters. We thus obtain the final sample of 144 stars as
presented in table4.dat with their corresponding Teff, surface gravity
log g, metallicity [Fe/H], vsin(i), R* and also GaiaEDR3/2MASS
parameters.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table4.dat 1513 144 Information on 144 stars used for main analysis
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See also:
J/AJ/161/68 : Obliquities of 150 hot Kepler hosting stars (Louden+, 2021)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
I/350 : Gaia EDR3 (Gaia Collaboration, 2020)
I/352 : Distances to 1.47 billion stars in Gaia EDR3
(Bailer-Jones+, 2021)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
J/AJ/154/107 : California-Kepler Survey (CKS). I. 1305 stars (Petigura+, 2017)
https://github.com/kemasuda/prot_from_vsini : Data underlying this article
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler Input Catalog identifier
(kepid)
10- 20 F11.6 K Teff Effective temperature (teff)
22- 24 I3 K e_Teff Mean error on Teff (teff_err)
26- 36 F11.9 [cm/s2] logg Surface gravity (logg)
38- 40 F3.1 [cm/s2] e_logg Mean error on logg (logg_err)
42- 53 F12.9 [Sun] [Fe/H] Iron to hydrogen abundance ratio (fe)
55- 58 F4.2 [Sun] e_[Fe/H] Mean error on [Fe/H] (fe_err)
60- 71 F12.9 km/s Vsini Rotational velocity (vsini)
73- 103 A31 --- Comments Comments on spectroscopic fit
(comments)
105- 109 A5 --- Binflag [False] The flag Binflag value
(binflag)
111- 128 F18.16 Rsun R* Stellar radius (rad)
130- 147 F18.16 Rsun E_R* Upper error on R* (radep)
149- 166 F18.16 Rsun e_R* Lower error on R* (radem)
168- 187 F20.18 Rsun s_R* Mean error on R* (rade)
189- 206 F18.14 pc D* Stellar distance (dis)
208- 226 F19.16 pc E_D* Upper error on D* (disep)
228- 246 F19.16 pc e_D* Lower error on D* (disem)
248- 270 A23 --- 2MASS 2MASS source designation as
(2MASS Jhhmmssss+ddmmsss)
(tm_designation)
272- 289 F18.15 --- Kepmag Estimated magnitude in Kepler band
(kepmag)
291- 308 F18.15 --- Jmag 2MASS J magnitude (jmag)
310- 314 F5.3 --- e_Jmag Mean error on Jmag (jmag_err)
316- 333 F18.15 --- Hmag 2MASS H magnitude (hmag)
335- 339 F5.3 --- e_Hmag Mean error on Hmag (hmag_err)
341- 358 F18.15 --- Kmag 2MASS K magnitude (kmag)
360- 364 F5.3 --- e_Kmag Mean error on Kmag (kmag_err)
366- 384 I19 --- SolID GaiaDR3 solution identifier
(solution_id)
386- 414 A29 --- NameGaiaEDR3 GaiaDR3 name idenfifier (designation)
416- 434 I19 --- GaiaEDR3 GaiaDR3 unique source identifier
(source_id)
436- 445 I10 --- RandomI GaiaDR3 random index used to select
subsets (random_index)
447- 452 F6.1 --- Epoch Reference epoch (ref_epoch)
454- 471 F18.14 deg RAdeg Barycentric right ascension of the
source (ICRS) at Ep=2016.0 (ra)
473- 484 F12.10 mas e_RAdeg Standard error eRA=eRA*cosDE of the
right ascension of the source in
ICRS at Ep=2016.0 (ra_error)
486- 503 F18.15 deg DEdeg Barycentric declination of the
source (ICRS) at Ep=2016.0 (dec)
505- 516 F12.10 mas e_DEdeg Standard error of the declination of
the source in ICRS at at Ep=2016.0
(dec_error)
518- 536 F19.16 mas Plx Absolute stellar parallax of the
source at the Ep=2016.0 (parallax)
538- 549 F12.10 mas e_Plx Standard error of the stellar
parallax at Ep=2016.0
(parallax_error)
551- 560 F10.6 --- RPlx Parallax divided by its standard
error (parallaxovererror)
562- 571 F10.7 mas/yr PM Total proper motion (pm)
573- 592 F20.16 mas/yr pmRA Proper motion in right ascension
pmRA*cosDE of the source in ICRS at
Ep=2016.0 (pmra)
594- 605 F12.10 mas/yr e_pmRA Standard error of proper motion in
right ascension direction
(pmra_error)
607- 626 F20.16 mas/yr pmDE Proper motion in declination
direction (pmdec)
628- 639 F12.10 mas/yr e_pmDE Standard error of proper motion in
declination direction (pmdec_error)
641- 654 F14.11 --- RADEcor Correlation between right ascension
and declination (radeccorr)
656- 669 E14.13 --- RAPlxcor Correlation between right ascension
and parallax (raparallaxcorr)
671- 683 F13.10 --- RApmRAcor Correlation between right ascension
and proper motion in right ascension
(rapmracorr)
685- 697 F13.10 --- RApmDEcor Correlation between right ascension
and proper motion in declination
(rapmdeccorr)
699- 711 F13.10 --- DEPlxcor Correlation between declination and
parallax (decparallaxcorr)
713- 725 F13.10 --- DEpmRAcor Correlation between declination and
proper motion in right ascension
(decpmracorr)
727- 739 F13.10 --- DEpmDEcor Correlation between declination and
proper motion in declination
(decpmdeccorr)
741- 753 F13.10 --- PlxpmRAcor Correlation between parallax and
proper motion in right ascension
(parallaxpmracorr)
755- 768 F14.11 --- PlxpmDEcor Correlation between parallax and
proper motion in declination
(parallaxpmdeccorr)
770- 782 F13.10 --- pmRApmDEcor Correlation between proper motion in
right ascension and proper motion in
declination (pmrapmdeccorr)
784- 786 I3 --- NAL Total number of observations AL
(astrometricnobs_al)
788- 790 I3 --- NAC Total number of observations AC
(astrometricnobs_ac)
792- 794 I3 --- NgAL Number of good observations AL
(astrometricngoodobsal)
796- 797 I2 --- NbAL Number of bad observations AL
(astrometricnbadobsal)
799- 811 F13.9 --- gofAL Goodness of fit statistic of model
wrt along-scan observations
(astrometricgofal)
813- 824 F12.5 --- chi2AL AL chi-square value
(astrometricchi2al)
826- 836 F11.9 mas epsi Excess noise of the source
(astrometricexcessnoise)
838- 849 F12.7 --- sepsi Significance of excess noise
(astrometricexcessnoise_sig)
851- 852 I2 --- Solved Which parameters have been solved
for? (astrometricparamssolved)
854- 858 A5 --- APF Primary or secondary
(astrometricprimaryflag)
860- 868 F9.7 um-1 nueff ? Effective wavenumber of the source
used in the astrometric solution
(nueffusedinastrometry)
870- 878 F9.7 um pscol ? Astrometrically estimated
pseudocolour of the source
(pseudocolour)
880- 891 F12.10 um e_pscol ? Standard error of the pseudocolour
of the source (pseudocolour_error)
893- 905 F13.10 --- RApscolCorr ? Correlation between right
ascension and pseudocolour
(rapseudocolourcorr)
907- 918 F12.9 --- DEpscolCorr ? Correlation between declination
and pseudocolour
(decpseudocolourcorr)
920- 931 F12.9 --- PlxpscolCorr ? Correlation between parallax and
pseudocolour
(parallaxpseudocolourcorr)
933- 944 F12.9 --- pmRApscolCorr ? Correlation between proper motion
in right ascension and pseudocolour
(pmrapseudocolourcorr)
946- 957 F12.9 --- pmDEpscolCorr ? Correlation between proper motion
in declination and pseudocolour
(pmdecpseudocolourcorr)
959- 960 I2 --- MatchObsA Matched FOV transits used in the
AGIS solution
(astrometricmatchedtransits)
962- 963 I2 --- Nper Number of visibility periods used in
Astrometric solution
(visibilityperiodsused)
965- 975 F11.9 mas amax The longest semi-major axis of the
-5-10 error ellipsoid
(astrometricsigma5dmax)
977- 978 I2 --- MatchObs The total number of field-of-view
transits matched to this source
(matched_transits)
980- 981 I2 --- NewMatchObs The number of transits newly
incorporated into an existing source
in th (newmatchedtransits)
983 I1 --- MatchObsrm The number of transits removed from
an existing source in the current c
(matchedtransitsremoved)
985- 997 F13.11 --- IPDgofha Amplitude of the IPD GoF versus
position angle of scan
(ipdgofharmonic_amplitude)
999-1010 F12.8 deg IPDgofhp Phase of the IPD GoF versus position
angle of scan
(ipdgofharmonic_phase)
1012 I1 --- IPDfmp Percent of successful-IPD windows
with more than one peak
(ipdfracmulti_peak)
1014 I1 --- IPDfow Percent of transits with truncated
windows or multiple gate
(ipdfracodd_win)
1016-1026 F11.8 --- RUWE Renormalised unit weight error (ruwe)
1028-1032 A5 --- Dup Source with multiple source
identifiers (duplicated_source)
1034-1036 I3 --- o_Gmag Number of observations (CCD
transits) that contributed to the G
mean fl (photgn_obs)
1038-1056 F19.11 e-/s FG Mean flux in the G-band
(photgmean_flux)
1058-1068 F11.6 e-/s e_FG Standard deviation of the G-band
fluxes divided by sqrt
(photgmeanfluxerror)
1070-1079 F10.4 --- RFG Mean flux in the G-band divided by
its error
(photgmeanfluxover_error)
1081-1090 F10.7 mag Gmag G-band mean magnitude (Vega)
(photgmean_mag)
1092-1093 I2 --- o_BPmag Number of observations contributing
to BP photometry (photbpn_obs)
1095-1113 F19.11 e-/s FBP Mean flux in the integrated BP band
(photbpmean_flux)
1115-1124 F10.5 e-/s e_FBP Error on the integrated BP mean flux
(photbpmeanfluxerror)
1126-1135 F10.5 --- RFBP Integrated BP mean flux divided by
its error
(photbpmeanfluxover_error)
1137-1146 F10.7 mag BPmag Integrated BP mean magnitude (Vega)
(photbpmean_mag)
1148-1149 I2 --- o_RPmag Number of observations (CCD
transits) that contributed to the
integrated RP mean flux and me
(photrpn_obs)
1151-1169 F19.11 e-/s FRP Mean flux in the integrated RP band
(photrpmean_flux)
1171-1181 F11.6 e-/s e_FRP Error on the integrated RP mean flux
(photrpmeanfluxerror)
1183-1191 F9.4 --- RFRP Integrated RP mean flux divided by
its error
(photrpmeanfluxover_error)
1193-1202 F10.7 mag RPmag Integrated RP mean magnitude (Vega)
(photrpmean_mag)
1204-1206 F3.1 --- NBPcont Number of BP contaminated transits
(photbpncontaminatedtransits)
1208-1211 F4.1 --- NBPblend Number of BP blended transits
(photbpnblendedtransits)
1213-1215 F3.1 --- NRPcont Number of RP contaminated transits
(photrpncontaminatedtransits)
1217-1220 F4.1 --- NRPblend Number of RP blended transits
(photrpnblendedtransits)
1222-1224 F3.1 --- Mode Photometry processing mode
(photprocmode)
1226-1234 F9.7 --- E(BP/RP) BP/RP excess factor
(photbprpexcessfactor)
1236-1245 F10.8 mag BP-RP BP-RP colour (bp_rp)
1247-1256 F10.8 mag BP-G BP-G colour (bp_g)
1258-1267 F10.8 mag G-RP G-RP colour (g_rp)
1269-1280 F12.8 km/s RVDR2 ? Radial velocity from Gaia DR2
(dr2radialvelocity)
1282-1292 F11.8 km/s e_RVDR2 ? Radial velocity error from Gaia
DR2 (dr2radialvelocity_error)
1294-1295 I2 --- o_RVDR2 Number of transits used to compute
radial velocity in Gaia DR2
(dr2rvnb_transits)
1297-1302 F6.1 K Tefftemp ? Teff of the template used to
compute radial velocity in Gaia DR2
(dr2rvtemplate_teff)
1304-1306 F3.1 [cm/s2] loggtemp ? Logg of the template used to
compute radial velocity in Gaia DR2
(dr2rvtemplate_logg)
1308-1312 F5.2 [-] [Fe/H]temp ? Iron to hydrogen abundance of the
template used to compute radial
velocity in Gaia DR2
(dr2rvtemplatefeh)
1314-1330 F17.14 deg GLON Galactic longitude (l)
1332-1349 F18.15 deg GLAT Galactic latitude (b)
1351-1368 F18.14 deg ELON Ecliptic longitude (ecl_lon)
1370-1387 F18.15 deg ELAT Ecliptic latitude (ecl_lat)
1389-1393 A5 --- Sb2flag [False] Sb2 flag value (sb2flag)
1395-1399 A5 --- Visflag [False] Vis flag value (visflag)
1401-1405 A5 --- Astflag [False] Ast flag value (astflag)
1407-1411 A5 --- Parflag [False] Par flag value (parflag)
1413-1421 F9.5 pc rgeo Median of the geometric distance
posterior (rmedgeo)
1423-1432 F10.6 pc b_rgeo 16th percentile of the geometric
distance posterior (rlogeo)
1434-1443 F10.6 pc B_rgeo 84th percentile of the geometric
distance posterior (rhigeo)
1445-1453 F9.5 pc rpgeo Median of the photogeometric
distance posterior (rmedphotogeo)
1455-1464 F10.6 pc b_rpgeo 16th percentile of the
photogeometric distance posterior
(rlophotogeo)
1466-1475 F10.6 pc B_rpgeo 84th percentile of the
photogeometric distance posterior
(rhiphotogeo)
1477-1483 F7.1 --- Flag Flag as from Gaia EDR3 Bailer-Jones
et al. 2021AJ....161..147B 2021AJ....161..147B Cat.
I/352 (flag)
1485-1493 F9.6 mag Zptmag Zero point magnitude used (zpt)
1495-1513 F19.16 mas PlxZP Parallax zero-point used
(parallax_zpcorrected)
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(End) Luc Trabelsi [CDS] 28-Nov-2024