J/A+A/632/A74 Extended main-sequence turn-offs isochrones (Johnston+, 2019)
Isochrone-cloud fitting of the extended main-sequence turn-off of young
clusters.
Johnston C., Aerts C., Pedersen M.G., Bastian N.
<Astron. Astrophys. 632, A74 (2019)>
=2019A&A...632A..74J 2019A&A...632A..74J (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, CCD ; Models
Keywords: asteroseismology - stars: interiors - stars: oscillations -
stars: rotation - galaxies: star clusters: general
Abstract:
Extended main-sequence turn-offs (eMSTO) are a commonly observed
property of young clusters. A global theoretical interpretation for
the eMSTOs is still lacking, but stellar rotation is considered a
necessary ingredient to explain the eMSTO. We aim to assess the
importance of core-boundary and envelope mixing in stellar interiors
for the interpretation of eMSTOs in terms of one coeval population. We
construct isochrone-clouds based on interior mixing profiles of stars
with a convective core calibrated from asteroseismology of isolated
galactic field stars. We fit these isochrone-clouds to the measured
eMSTO to estimate the age and core mass of the stars in the two young
clusters NGC 1850 and NGC 884, assuming one coeval population and
fixing the metallicity to the one measured from spectroscopy. We
assess the correlations between the interior mixing properties of the
cluster members and their rotational and pulsational properties. We
find that stellar models based on asteroseismically-calibrated
interior mixing profiles lead to enhanced core masses of eMSTO stars
and can explain a good fraction of the observed eMSTOs of the two
considered clusters in terms of one coeval population of stars, with
similar ages to those in the literature, given the large
uncertainties. The rotational and pulsational properties of the stars
in NGC 884 are not sufficiently well known to perform asteroseismic
modelling, as it is achieved for field stars from space photometry.
The stars in NGC 884 for which we have vsini and a few pulsation
frequencies show no correlation between these properties and the core
masses of the stars that set the cluster age. Future cluster space
asteroseismology may allow to interpret the values of the core masses
in terms of the physical processes that cause them, based on the
modelling of the interior mixing profiles for the individual member
stars with suitable identified modes.
Description:
Isochrone clouds for three metalicities. For each metalicity, we
provide the absolute magnitude, bolometric correction, and luminosity
in Johnson UBVRIJKLL'M, and Hubble F170W, F218W, F255W, F300W, F336W,
F439W, F450W, F555W, F606W, F702W, F814W, and F850Lp filters, as well
as the physical properties Age, mixing length parameter, core hydrogen
and helium content, overshooting parameter, convective core mass,
helium core mass, envelope mixing parameter, the log radius, log
temperature, log luminosity, and log surface gravity, and the seismic
parameters nu_max and the asymptotic period spacing value.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
z00060ic.dat 1086 3186065 Isochrone-clouds for Z=0.0060
z00100ic.dat 1086 3419453 Isochrone-clouds for Z=0.0100
z00140ic.dat 1086 3368575 Isochrone-clouds for Z=0.0140
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Byte-by-byte Description of file: z00060ic.dat z00100ic.dat z00140ic.dat
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Bytes Format Units Label Explanations
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1- 5 F5.1 Myr Age Age in Mega years (Age)
7- 17 F11.6 1/d AsympdP Asymptotic period spacing value
(Asymptotic_dP)
19- 29 F11.6 --- Zini Mass fraction of metals (Zini)
31- 41 F11.6 mag BMAG Absolute magnitude in the Johnson B
filter (absmagB)
43- 53 F11.6 mag F170WMAG Absolute magnitude in the Hubble F170W
filter (absmagF170W)
55- 65 F11.6 mag F218WMAG Absolute magnitude in the Hubble F218W
filter (absmagF218W)
67- 77 F11.6 mag F255WMAG Absolute magnitude in the Hubble F255W
filter (absmagF255W)
79- 89 F11.6 mag F300WMAG Absolute magnitude in the Hubble F300W
filter (absmagF300W)
91- 101 F11.6 mag F336WMAG Absolute magnitude in the Hubble F336W
filter (absmagF336W)
103- 113 F11.6 mag F439WMAG Absolute magnitude in the Hubble F439W
filter (absmagF439W)
115- 125 F11.6 mag F450WMAG Absolute magnitude in the Hubble F450W
filter (absmagF450W)
127- 137 F11.6 mag F555WMAG Absolute magnitude in the Hubble F555W
filter (absmagF555W)
139- 149 F11.6 mag F606WMAG Absolute magnitude in the Hubble F606W
filter (absmagF606W)
151- 161 F11.6 mag F702WMAG Absolute magnitude in the Hubble F702W
filter (absmagF702W)
163- 173 F11.6 mag F814WMAG Absolute magnitude in the Hubble F814W
filter (absmagF814W)
175- 185 F11.6 mag F850LPMAG Absolute magnitude in the Hubble F850LP
filter (absmagF850LP)
187- 197 F11.6 mag HMAG Absolute magnitude in the Johnson H
filter (absmagH)
199- 209 F11.6 mag IMAG Absolute magnitude in the Johnson I
filter (absmagI)
211- 221 F11.6 mag JMAG Absolute magnitude in the Johnson J
filter (absmagJ)
223- 233 F11.6 mag KMAG Absolute magnitude in the Johnson K
filter (absmagK)
235- 245 F11.6 mag LMAG Absolute magnitude in the Johnson L
filter (absmagL)
247- 257 F11.6 mag LpMAG Absolute magnitude in the Johnson L'
filter (absmagLprime)
259- 269 F11.6 mag MMAG Absolute magnitude in the Johnson M
filter (absmagM)
271- 281 F11.6 mag RMAG Absolute magnitude in the Johnson R
filter (absmagR)
283- 293 F11.6 mag UMAG Absolute magnitude in the Johnson U
filter (absmagU)
295- 305 F11.6 mag VMAG Absolute magnitude in the Johnson V
filter (absmagV)
307- 317 F11.6 --- alphamlt Mixing length alpha parameter
(alpha_mlt)
319- 329 F11.6 mag BCB Bolometric Correction in the Johnson B
filter (bc_B)
331- 341 F11.6 mag BCF170W Bolometric Correction in the Hubble F170W
filter (bc_F170W)
343- 353 F11.6 mag BCF218W Bolometric Correction in the Hubble F218W
filter (bc_F218W)
355- 365 F11.6 mag BCF255W Bolometric Correction in the Hubble F255W
filter (bc_F255W)
367- 377 F11.6 mag BCF300W Bolometric Correction in the Hubble F300W
filter (bc_F300W)
379- 389 F11.6 mag BCF336W Bolometric Correction in the Hubble F336W
filter (bc_F336W)
391- 401 F11.6 mag BCF439W Bolometric Correction in the Hubble F439W
filter (bc_F439W)
403- 413 F11.6 mag BCF450W Bolometric Correction in the Hubble F450W
filter (bc_F450W)
415- 425 F11.6 mag BCF555W Bolometric Correction in the Hubble F555W
filter (bc_F555W)
427- 437 F11.6 mag BCF606W Bolometric Correction in the Hubble F606W
filter (bc_F606W)
439- 449 F11.6 mag BCF702W Bolometric Correction in the Hubble F702W
filter (bc_F702W)
451- 461 F11.6 mag BCF814W Bolometric Correction in the Hubble F814W
filter (bc_F814W)
463- 473 F11.6 mag BCF850LP Bolometric Correction in the Hubble
F850LP filter (bc_F850LP)
475- 485 F11.6 mag BCH Bolometric Correction in the Johnson H
filter (bc_H)
487- 497 F11.6 mag BCI Bolometric Correction in the Johnson I
filter (bc_I)
499- 509 F11.6 mag BCJ Bolometric Correction in the Johnson J
filter (bc_J)
511- 521 F11.6 mag BCK Bolometric Correction in the Johnson K
filter (bc_K)
523- 533 F11.6 mag BCL Bolometric Correction in the Johnson L
filter (bc_L)
535- 545 F11.6 mag BCLp Bolometric Correction in the Johnson L'
filter (bc_Lprime)
547- 557 F11.6 mag BCM Bolometric Correction in the Johnson M
filter (bc_M)
559- 569 F11.6 mag BCR Bolometric Correction in the Johnson R
filter (bc_R)
571- 581 F11.6 mag BCU Bolometric Correction in the Johnson U
filter (bc_U)
583- 593 F11.6 mag BCV Bolometric Correction in the Johnson V
filter (bc_V)
595- 605 F11.6 --- centerH1 Mass fraction of hydrogen left in the
core burning region (center_h1)
607- 617 F11.6 --- centerHe4 Mass fraction of helium left in the core
burning region (center_he4)
619- 629 F11.6 muHz deltanu Asymptotic large frequency spacing for
p-modes (delta_nu)
631- 641 F11.6 --- fov Overshooting parameter (fov)
643- 653 F11.6 Msun HecoreMass Helium core mass (hecoremass)
655- 665 F11.6 Rsun HecoreRads Helium core radius (hecoreradius)
667- 677 F11.6 [-] logDext logarithm of the D_ext mixing parameter
(logDext)
679- 689 F11.6 [Lsun] logL logarithm of the luminosity (log_L)
691- 701 F11.6 [Rsun] logR logarithm of the radius (log_R)
703- 713 F11.6 [K] logTeff logarithm of the effective temperature
(log_Teff)
715- 725 F11.6 [cm/s2] logg logarithm of the surface gravity (log_g)
727- 739 E13.6 W LumB Luminosity in the Johnson B filter
(lumbandB)
741- 753 E13.6 W LumF170W Luminosity in the Hubble F170W filter
(lumbandF170W)
755- 767 E13.6 W LumF218W Luminosity in the Hubble F218W filter
(lumbandF218W)
769- 781 E13.6 W LumF255W Luminosity in the Hubble F255W filter
(lumbandF255W)
783- 795 E13.6 W LumF300W Luminosity in the Hubble F300W filter
(lumbandF300W)
797- 809 E13.6 W LumF336W Luminosity in the Hubble F336W filter
(lumbandF336W)
811- 823 E13.6 W LumF439W Luminosity in the Hubble F439W filter
(lumbandF439W)
825- 837 E13.6 W LumF450W Luminosity in the Hubble F450W filter
(lumbandF450W)
839- 851 E13.6 W LumF555W Luminosity in the Hubble F555W filter
(lumbandF555W)
853- 865 E13.6 W LumF606W Luminosity in the Hubble F606W filter
(lumbandF606W)
867- 879 E13.6 W LumF702W Luminosity in the Hubble F702W filter
(lumbandF702W)
881- 893 E13.6 W LumF814W Luminosity in the Hubble F814W filter
(lumbandF814W)
895- 907 E13.6 W LumF850LP Luminosity in the Hubble F850LP filter
(lumbandF850LP)
909- 921 E13.6 W LumH Luminosity in the Johnson H filter
(lumbandH)
923- 935 E13.6 W LumI Luminosity in the Johnson I filter
(lumbandI)
937- 949 E13.6 W LumJ Luminosity in the Johnson J filter
(lumbandJ)
951- 963 E13.6 W LumK Luminosity in the Johnson K filter
(lumbandK)
965- 977 E13.6 W LumL Luminosity in the Johnson L filter
(lumbandL)
979- 991 E13.6 W LumLp Luminosity in the Johnson L' filter
(lumbandLprime)
993-1005 E13.6 W LumM Luminosity in the Johnson M filter
(lumbandM)
1007-1019 E13.6 W LumR Luminosity in the Johnson R filter
(lumbandR)
1021-1033 E13.6 W LumU Luminosity in the Johnson U filter
(lumbandU)
1035-1047 E13.6 W LumV Luminosity in the Johnson V filter
(lumbandV)
1049-1059 F11.6 Msun MassConvCore Mass of the convective core
(massconvcore)
1061-1074 F14.6 muHz nuMax Frequency of highest amplitude (nu_max)
1076-1086 F11.6 Msun Mstar Stellar mass (star_mass)
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Acknowledgements:
Cole Johnston, colecampbell.johnston(at)kuleuven.be
(End) Cole Johnston [KU Leuven, Belgium], Patricia Vannier [CDS] 21-Oct-2019