J/A+A/703/A104 Improving chemical abundances using star clusters (Kos+, 2025)
The GALAH survey: Improving chemical abundances using star clusters.
Kos J., Buder S., Beeson K.L., Bland-Hawthorn J., De Silva G.M., D'Orazi V.,
Freeman K., Hayden M., Lewis G.F., Lind K., Martell S.L., Sharma S.,
Zucker D.B., Zwitter T., Da Costa G.S., de Grijs R., Howell M., McKenzie M.,
Nordlander T., Saikia S., Stello D., Traven G.
<Astron. Astrophys. 703, A104 (2025)>
=2025A&A...703A.104K 2025A&A...703A.104K (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Associations, stellar ; Clusters, globular ;
Clusters, open ; Abundances ; Spectroscopy
Keywords: methods: data analysis - techniques: spectroscopic - surveys -
stars: abundances - globular clusters: general -
open clusters and associations: general
Abstract:
Large spectroscopic surveys aim to consistently compute stellar
parameters of very diverse stars while minimizing systematic errors.
We explore the use of stellar clusters as benchmarks to verify the
precision of spectroscopic parameters in the fourth data release (DR4)
of the GALAH survey. We examine 58 open and globular clusters and
associations to validate measurements of temperature, gravity,
chemical abundances, and stellar ages. We focus on identifying
systematic errors and understanding trends between stellar parameters,
particularly temperature and chemical abundances. We identify trends
by stacking measurements of chemical abundances against effective
temperature and modelling them with splines. We also refit spectra in
three clusters with the Spectroscopy Made Easy and Korg packages to
reproduce the trends in DR4 and to search for their origin by varying
temperature and gravity priors, linelists, and spectral continuum.
Trends are consistent between clusters of different ages and
metallicities, can reach amplitudes of 0.5dex and differ for dwarfs
and giants. We use the derived trends to correct the DR4 abundances of
24 and 31 chemical elements for dwarfs and giants, respectively, and
publish a detrended catalogue. While the origin of the trends could
not be pinpointed, we found that: i) photometric priors affect derived
abundances, ii) temperature, metallicity, and continuum levels are
degenerate in spectral fitting, and it is hard to break the degeneracy
even by using independent measurements, iii) the completeness of the
linelist used in spectral synthesis is essential for cool stars, and
iv) different spectral fitting codes produce significantly different
iron abundances for stars of all temperatures. We conclude that
clusters can be used to characterise the systematic errors of
parameters produced in large surveys, but further research is needed
to explain the origin of the trends.
Description:
We provide a copy of the main table of GALAH data release four
with detrended measurements of abundances of chemical elements. We
also provide a list of stars in three clusters (Melotte 22,
Melotte 25, and NGC 2632) which we analysed in more details.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
catalog.dat 1678 917588 Detrended GALAH DR4 catalogue
tablee1.dat 105 346 Stars analysed in more details
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See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
J/MNRAS/506/150 : The GALAH+ Survey DR3 (Buder+, 2021)
https://galah-survey.org/ : GALAH Home Page
https://www.galah-survey.org/dr4/overview/ : GALAH DR4
Byte-by-byte Description of file: catalog.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 I15 --- GALAH GALAH identifier (sobject_id)
17- 33 A17 --- 2MASS 2MASS identifier (tmass_id)
35- 53 I19 --- GaiaDR3 Gaia DR3 source_id (gaiadr3sourceid)
55- 71 A17 --- Survey HERMES-2dF Survey/Program/Pointing
(survey_name)
73- 83 I11 --- FieldId GALAH Field ID (field_id)
85- 91 A7 --- setup Analysis setup (setup)
93- 99 F7.1 d MJD Modified Julian Date of observation
(mjd)
101- 115 F15.11 deg RAdeg Right Ascension (J2000)
(propagated from Gaia DR3) (ra)
117- 131 F15.11 deg DEdeg Declination (J2000)
(propagated from Gaia DR3) (dec)
133- 137 I5 --- flagsp Major spectroscopic quality bitmask
flag (flag_sp)
139- 140 I2 --- flagspfit Major spectroscopic fitting quality
bitmask flag (flagspfit)
142- 143 I2 --- optloop Number of optimisation loops used
for fitting (opt_loop)
145- 151 I7 --- flagred Quality bitmask flag of reduction
pipeline (flag_red)
153- 163 F11.6 --- snrpxccd1 ?=- Average signal-to-noise ratio
(per pixel) of CCD1 (snrpxccd1)
165- 175 F11.6 --- snrpxccd2 Average signal-to-noise ratio
(per pixel) of CCD2 (snrpxccd2)
177- 187 F11.6 --- snrpxccd3 ?=- Average signal-to-noise ratio
(per pixel) of CCD3 (snrpxccd3)
189- 200 F12.6 --- snrpxccd4 ?=- Average signal-to-noise ratio
(per pixel) of CCD4 (snrpxccd4)
202- 211 F10.6 --- chi2sp ?=- Chi squared value of spectroscopic
fit (chi2_sp)
213- 215 I3 % pxusedperc Percentage of spectrum used for
spectroscopic fit (pxusedperc)
217- 231 A15 --- ModelName Neural network model used for creating
synthetic spectra (model_name)
233- 247 A15 --- ClosestMod Closest neural network model for
Teff/logg/[Fe/H] combination
(closest_model)
249- 260 F12.6 s CompTime ?=- Computation time spent on spectrum
(comp_time)
262- 266 A5 --- fitglobRV Are spectra coadded (without RV
shifts) and then a global RV fitted ?
(fitglobalrv)
268- 279 F12.6 km/s RV1 ?=- Radial velocity of primary source
(rvcomp1)
281- 292 E12.6 km/s e_RV1 ?=- Uncertainty of rvcomp1
(ervcomp_1)
294- 305 F12.6 km/s RV2 ?=- Radial velocity of potential
secondary source (rvcomp2
307- 316 F10.6 km/s e_RV2 ?=- Uncertainty of rvcomp2
(ervcomp_2)
318- 328 F11.6 km/s RVGaiaDR3 ?=- Radial velocity in Gaia DR3
(rvgaiadr3)
330- 338 F9.6 km/s e_RVGaiaDR3 ?=- Uncertainty of rvgaiadr3
(ervgaia_dr3)
340- 349 F10.6 km/s Vbaryeff ?=- Barycentric velocity applied to
reduced spectra (vbaryeff)
351- 357 F7.2 K Teff ?=- Spectroscopic effective
temperature (used for fitting) (teff)
359- 370 E12.6 K e_Teff ?=- Uncertainty of teff (e_teff)
372- 380 F9.6 [cm/s2] logg ?=- Surface gravity adjusted via
parallax information (logg)
382- 389 F8.6 [cm/s2] e_logg ?=- Uncertainty of logg (e_logg)
391- 399 F9.6 --- [Fe/H] ?=- Abundance of Fe and all other
elements not fitted in GALAH
(Fe: 1D-NLTE) (fe_h)
401- 412 E12.6 --- e_[Fe/H] ?=- Uncertainty of fe_h (efeh)
414- 416 I3 --- f_[Fe/H] Quality flag of fe_h (flagfeh)
418- 425 F8.6 km/s vmic ?=- Microturbulence velocity (fitted)
(vmic)
427- 438 E12.6 km/s e_vmic ?=- Uncertainty of vmic (e_vmic)
440- 447 F8.5 km/s vsini ?=- Broadening velocity (combines
rotational and macroturbulence
velocities) (vsini)
449- 460 E12.6 km/s e_vsini ?=- Uncertainty of vsini (e_vsini)
462- 470 F9.6 --- [Li/Fe] ?=- Elemental abundance for [Li/Fe]
(li_fe)
472- 483 E12.6 --- e_[Li/Fe] ?=- Uncertainty of [Li/Fe] (elife)
485- 487 I3 --- f_[Li/Fe] Quality bitmask flag of [Li/Fe]
(flaglife)
489- 497 F9.6 --- [C/Fe] ?=- Elemental abundance for [C/Fe]
(c_fe)
499- 510 E12.6 --- e_[C/Fe] ?=- Uncertainty of [C/Fe] (ecfe)
512- 514 I3 --- f_[C/Fe] Quality bitmask flag of [C/Fe]
(flagcfe)
516- 524 F9.6 --- [N/Fe] ?=- Elemental abundance for [N/Fe]
(n_fe)
526- 534 F9.6 --- e_[N/Fe] ?=- Uncertainty of [N/Fe] (enfe)
536- 538 I3 --- f_[N/Fe] Quality bitmask flag of [N/fe]
(flagnfe)
540- 548 F9.6 --- [O/Fe] ?=- Elemental abundance for [O/Fe]
(o_fe)
550- 561 E12.6 --- e_[O/Fe] ?=- Uncertainty of [O/Fe] (eofe)
563- 565 I3 --- f_[O/Fe] Quality bitmask flag of [O/Fe]
(flagofe)
567- 575 F9.6 --- [Na/Fe] ?=- Elemental abundance for [Na/Fe]
(na_fe)
577- 586 F10.6 --- e_[Na/Fe] ?=- Uncertainty of na_fe (enafe)
588- 590 I3 --- f_[Na/Fe] Quality bitmask flag of [Na/Fe]
(flagnafe)
592- 600 F9.6 --- [Mg/Fe] ?=- Elemental abundance for [Mg/Fe]
(mg_fe)
602- 613 E12.6 --- e_[Mg/Fe] ?=- Uncertainty of [Mg/Fe] (emgfe)
615- 617 I3 --- f_[Mg/Fe] Quality bitmask flag of [Mg/Fe]
(flagmgfe)
619- 627 F9.6 --- [Al/Fe] ?=- Elemental abundance for [Al/Fe]
(al_fe)
629- 637 F9.6 --- e_[Al/Fe] ?=- Uncertainty of [Al/Fe] (ealfe)
639- 641 I3 --- f_[Al/Fe] Quality bitmask flag of [Al/Fe]
(flagalfe)
643- 651 F9.6 --- [Si/Fe] ?=- Elemental abundance for [Si/Fe]
(si_fe)
653- 661 F9.6 --- e_[Si/Fe] ?=- Uncertainty of [Si/Fe] (esife)
663- 665 I3 --- f_[Si/Fe] Quality bitmask flag of [Si/Fe]
(flagsife)
667- 675 F9.6 --- [K/Fe] ?=- Elemental abundance for [K/Fe]
(k_fe)
677- 685 F9.6 --- e_[K/Fe] ?=- Uncertainty of [K/Fe] (ekfe)
687- 689 I3 --- f_[K/Fe] Quality bitmask flag of [K/Fe]
(flagkfe)
691- 699 F9.6 --- [Ca/Fe] ?=- Elemental abundance for [Ca/Fe]
(ca_fe)
701- 712 E12.6 --- e_[Ca/Fe] ?=- Uncertainty of [Ca/Fe] (ecafe)
714- 716 I3 --- f_[Ca/Fe] Quality bitmask flag of [Ca/Fe]
(flagcafe)
718- 726 F9.6 --- [Sc/Fe] ?=- Elemental abundance for [Sc/Fe]
(sc_fe)
728- 739 E12.6 --- e_[Sc/Fe] ?=- Uncertainty of [Sc/Fe] (escfe)
741- 743 I3 --- f_[Sc/Fe] Quality bitmask flag of [Sc/Fe]
(flagscfe)
745- 753 F9.6 --- [Ti/Fe] ?=- Elemental abundance for [Ti/Fe]
(ti_fe)
755- 766 E12.6 --- e_[Ti/Fe] ?=- Uncertainty of [Ti/Fe] (etife)
768- 770 I3 --- f_[Ti/Fe] Quality bitmask flag of [Ti/Fe]
(flagtife)
772- 780 F9.6 --- [V/Fe] ?=- Elemental abundance for [V/Fe]
(v_fe)
782- 791 F10.6 --- e_[V/Fe] ?=- Uncertainty of [V/Fe] (evfe)
793- 795 I3 --- f_[V/Fe] Quality bitmask flag of [V/Fe]
(flagvfe)
797- 805 F9.6 --- [Cr/Fe] ?=- Elemental abundance for [Cr/Fe]
(cr_fe)
807- 818 E12.6 --- e_[Cr/Fe] ?=- Uncertainty of [Cr/Fe] (ecrfe)
820- 822 I3 --- f_[Cr/Fe] Quality bitmask flag of [Cr/Fe]
(flagcrfe)
824- 832 F9.6 --- [Mn/Fe] ?=- Elemental abundance for [Mn/Fe]
(mn_fe)
834- 843 F10.6 --- e_[Mn/Fe] ?=- Uncertainty of [Mn/Fe] (emnfe)
845- 847 I3 --- f_[Mn/Fe] Quality bitmask flag of [Mn/Fe]
(flagmnfe)
849- 857 F9.6 --- [Co/Fe] ?=- Elemental abundance for [Co/Fe]
(co_fe)
859- 868 F10.6 --- e_[Co/Fe] ?=- Uncertainty of [Co/Fe] (ecofe)
870- 872 I3 --- f_[Co/Fe] Quality bitmask flag of [Co/Fe]
(flagcofe)
874- 882 F9.6 --- [Ni/Fe] ?=- Elemental abundance for [Ni/Fe]
(ni_fe)
884- 895 E12.6 --- e_[Ni/Fe] ?=- Uncertainty of [Ni/Fe] (enife)
897- 899 I3 --- f_[Ni/Fe] Quality bitmask flag of [Ni/Fe]
(flagnife)
901- 909 F9.6 --- [Cu/Fe] ?=- Elemental abundance for [Cu/Fe]
(cu_fe)
911- 920 F10.6 --- e_[Cu/Fe] ?=- Uncertainty of [Cu/Fe] (ecufe)
922- 924 I3 --- f_[Cu/Fe] Quality bitmask flag of [Cu/Fe]
(flagcufe)
926- 934 F9.6 --- [Zn/Fe] ?=- Elemental abundance for [Zn/Fe]
(zn_fe)
936- 945 F10.6 --- e_[Zn/Fe] ?=- Uncertainty of [Zn/Fe] (eznfe)
947- 949 I3 --- f_[Zn/Fe] Quality bitmask flag of [Zn/Fe]
(flagznfe)
951- 959 F9.6 --- [Rb/Fe] ?=- Elemental abundance for [Rb/Fe]
(rb_fe)
961- 969 F9.6 --- e_[Rb/Fe] ?=- Uncertainty of [Rb/Fe] (erbfe)
971- 973 I3 --- f_[Rb/Fe] Quality bitmask flag of [Rb/Fe]
(flagrbfe)
975- 983 F9.6 --- [Sr/Fe] ?=- Elemental abundance for [Sr/Fe]
(sr_fe)
985- 993 F9.6 --- e_[Sr/Fe] ?=- Uncertainty of [Sr/Fe] (esrfe)
995- 997 I3 --- f_[Sr/Fe] Quality bitmask flag of [Sr/Fe]
(flagsrfe)
999-1007 F9.6 --- [Y/Fe] ?=- Elemental abundance for [Y/Fe]
(y_fe)
1009-1020 E12.6 --- e_[Y/Fe] ?=- Uncertainty of [Y/Fe] (eyfe)
1022-1024 I3 --- f_[Y/Fe] Quality bitmask flag of [Y/Fe]
(flagyfe)
1026-1034 F9.6 --- [Zr/Fe] ?=- Elemental abundance for [Zr/Fe]
(zr_fe)
1036-1045 F10.6 --- e_[Zr/Fe] ?=- Uncertainty of [Zr/Fe] (ezrfe)
1047-1049 I3 --- f_[Zr/Fe] Quality bitmask flag of [Zr/Fe]
(flagzrfe)
1051-1059 F9.6 --- [Mo/Fe] ?=- Elemental abundance for [Mo/Fe]
(mo_fe)
1061-1069 F9.6 --- e_[Mo/Fe] ?=- Uncertainty of [Mo/Fe] (emofe)
1071-1073 I3 --- f_[Mo/Fe] Quality bitmask flag of [Mo/Fe]
(flagmofe)
1075-1083 F9.6 --- [Ru/Fe] ?=- Elemental abundance for [Ru/Fe]
(ru_fe)
1085-1093 F9.6 --- e_[Ru/Fe] ?=- Uncertainty of [Ru/Fe] (erufe)
1095-1097 I3 --- f_[Ru/Fe] Quality bitmask flag of [Ru/Fe]
(flagrufe)
1099-1107 F9.6 --- [Ba/Fe] ?=- Elemental abundance for [Ba/Fe]
(ba_fe)
1109-1120 E12.6 --- e_[Ba/Fe] ?=- Uncertainty of [Ba/Fe] (ebafe)
1122-1124 I3 --- f_[Ba/Fe] Quality bitmask flag of [Ba/Fe]
(flagbafe)
1126-1134 F9.6 --- [La/Fe] ?=- Elemental abundance for [La/Fe]
(la_fe)
1136-1145 F10.6 --- e_[La/Fe] ?=- Uncertainty of [La/Fe] (elafe)
1147-1149 I3 --- f_[La/Fe] Quality bitmask flag of [La/Fe]
(flaglafe)
1151-1159 F9.6 --- [Ce/Fe] ?=- Elemental abundance for [Ce/Fe]
(ce_fe)
1161-1170 F10.6 --- e_[Ce/Fe] ?=- Uncertainty of [Ce/Fe] (ecefe)
1172-1174 I3 --- f_[Ce/Fe] Quality bitmask flag of [Ce/Fe]
(flagcefe)
1176-1184 F9.6 --- [Nd/Fe] ?=- Elemental abundance for [Nd/Fe]
(nd_fe)
1186-1195 F10.6 --- e_[Nd/Fe] ?=- Uncertainty of [Nd/Fe] (endfe)
1197-1199 I3 --- f_[Nd/Fe] Quality bitmask flag of [Nd/Fe]
(flagndfe)
1201-1209 F9.6 --- [Sm/Fe] ?=- Elemental abundance for [Sm/Fe]
(sm_fe)
1211-1219 F9.6 --- e_[Sm/Fe] ?=- Uncertainty of [Sm/Fe] (esmfe)
1221-1223 I3 --- f_[Sm/Fe] Quality bitmask flag of [Sm/Fe]
(flagsmfe)
1225-1233 F9.6 --- [Eu/Fe] ?=- Elemental abundance for [Eu/Fe]
(eu_fe)
1235-1242 F8.6 --- e_[Eu/Fe] ?=- Uncertainty of [Eu/Fe] (eeufe)
1244-1246 I3 --- f_[Eu/Fe] Quality bitmask flag of [Eu/Fe]
(flageufe)
1248-1255 F8.6 Msun Mass ?=- Mass used for calculating
logg(plx) (mass)
1257-1265 F9.6 Gyr Age ?=- Age estimated when calculating
mass (age)
1267-1274 F8.6 mag BCks ?=- Bolometric Correction of Ks,
BC(Ks), used for calculating
logg(plx) (bc_ks)
1276-1283 F8.6 mag AKs ?=- Attenuation in Ks-band A(Ks) used
for calculating logg(plx) (a_k)
1285-1296 E12.6 Lsun Lbol ?=- Bolometric Luminosity used for
calculating logg(plx) (lbol)
1298-1308 F11.5 pc rmed ?=- Median Distance used for
calculating logg(plx) (r_med)
1310-1320 F11.5 pc rlo ?=- Lower Limit Distance used for
calculating logg(plx) (r_lo)
1322-1332 F11.5 pc rhi ?=- Higher Limit Distance used for
calculating logg(plx) (r_hi)
1334-1344 F11.6 km/s sb2RV16 ?=- 16th percentile radial velocity of
fit to syn-obs residuals (sb2rv16)
1346-1356 F11.6 km/s sb2RV50 ?=- 50th perc. radial velocity of fit
to syn-obs residuals (sb2rv50)
1358-1368 F11.6 km/s sb2RV84 ?=- 84th perc. radial velocity of fit
to syn-obs residuals (sb2rv84)
1370-1380 F11.6 0.1nm EWHbeta ?=- Equivalent width of observed
Hbeta core (ewhbeta)
1382-1393 F12.6 0.1nm EWHalpha ?=- Equivalent width of observed
Halpha core (ewhalpha)
1395-1405 F11.6 0.1nm resHbeta ?=- Residual equivalent width of
syn-obs residuals at Hbeta core
(reshbeta)
1407-1418 F12.6 0.1nm resHalpha ?=- Residual equivalent width of
syn-obs residuals at Halpha core
(reshalpha)
1420-1427 F8.6 0.1nm EWKis ?=- Equivalent width of fit for K7699
interstellar Line (ewkis)
1429-1436 F8.6 0.1nm sigmaKis ?=- Sigma of Gaussian fit for K7699
interstellar Line (sigmakis)
1438-1448 F11.6 km/s RVKis ?=- Radial velocity of fit to syn-obs
residuals around K7699 line (rvkis)
1450-1458 F9.6 0.1nm EWdib5780 ?=- Equivalent Width of fit for 5780
diffuse interstellar band
(ew_dib5780)
1460-1467 F8.6 0.1nm sigmadib5780 ?=- Sigma of Gaussian fit for 5780
diffuse interstellar band
(sigma_dib5780)
1469-1480 F12.6 km/s RVdib5780 ?=- Radial velocity of fit to syn-obs
residuals around 5780 diffuse
interstellar band (rv_dib5780)
1482-1490 F9.6 0.1nm EWdib5797 ?=- Equivalent Width of fit for 5797
diffuse interstellar band
(ew_dib5797)
1492-1499 F8.6 0.1nm sigmadib5797 ?=- Sigma of Gaussian fit for 5797
diffuse interstellar band
(sigma_dib5797)
1501-1512 F12.6 km/s RVdib5797 ?=- Radial velocity of fit to syn-obs
residuals around 5797 diffuse
interstellar band (rv_dib5797)
1514-1522 F9.6 0.1nm EWdib6613 ?=- Equivalent Width of fit for 6613
diffuse interstellar band
(ew_dib6613)
1524-1531 F8.6 0.1nm sigmadib6613 ?=- Sigma of Gaussian fit for 6613
diffuse interstellar band
(sigma_dib6613)
1533-1544 F12.6 km/s RVdib6613 ?=- Radial velocity of fit to syn-obs
residuals around 6613 diffuse
interstellar band (rv_dib6613)
1546-1555 F10.6 mag E(B-V) ?=- Color excess E(B-V) (ebv)
1557-1564 F8.5 mag Gmag ?=- Mean Gaia DR3 G-band apparent
magnitude (photgmean_mag)
1566-1574 F9.6 mag BP-RP ?=- Color of BP-RP bands (bp_rp)
1576-1582 F7.3 mag Jmag ?=- 2MASS J-band magnitude (j_m)
1584-1589 F6.3 mag e_Jmag ?=- Uncertainty of 2MASS J-band
magnitude (j_msigcom)
1591-1597 F7.3 mag Hmag ?=- 2MASS H-band magnitude (h_m)
1599-1604 F6.3 mag e_Hmag ?=- Uncertainty of 2MASS J-band
magnitude (h_msigcom)
1606-1612 F7.3 mag Ksmag ?=- 2MASS Ks-band magnitude (ks_m)
1614-1619 F6.3 mag e_Ksmag ?=- Uncertainty of 2MASS Ks-band
magnitude (ks_msigcom)
1621-1627 F7.3 mag W2mag ?=- AllWISE W2-band magnitude (W2mag)
1629-1634 F6.3 mag e_W2mag ?=- Uncertainty of AllWISE W2-band
magnitude (e_W2mag)
1636-1644 F9.6 --- RUWE ?=- RUWE (propagated from Gaia DR3)
(ruwe)
1646-1655 F10.6 mas plx ?=- Parallax (propagated from Gaia
DR3) (parallax)
1657-1664 F8.6 mas e_plx ?=- Uncertainty of parallax
(propagated from Gaia DR3)
(parallax_error)
1666-1670 A5 --- giants Star is in giants region of the HRD
(giants)
1672-1676 A5 --- dwarfs Star is in dwarfs region if the HRD
(dwarfs)
1678 I1 --- detModel Model used for detrending
(detrend_model) (1)
--------------------------------------------------------------------------------
Note (1): 0 indicates that a model for dwarfs was used for detrending, 1
indicates that model for giants was used, and 2 indicates that a
combination of both was used for detrending.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablee1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 I15 --- GALAH GALAH identifier (sobject_id)
17- 35 I19 --- GaiaDR3 Gaia DR3 source_id (Gaia DR3 source_id)
37- 46 A10 --- Cluster Cluster name
48 A1 --- C-G Is star included in CANTAT-GAUDIN et al.
(2019A&A...621A.115C 2019A&A...621A.115C, Cat. J/A+A/621/A115)
50 A1 --- H+R Is star included in Hunt and Reffert
(2024A&A...686A..42H 2024A&A...686A..42H, Cat. J/A+A/686/A42
52- 57 F6.3 mag GMAG Absolute Gaia G band magnitude
59- 63 F5.3 mag BP-RP Color in Gaia BP-RP bands
65- 69 F5.2 --- RUWE RUWE (propagated from Gaia DR3)
71- 76 F6.1 K Teff ?=- Effective temperature
(propagated from GALAH DR4)
78- 81 F4.2 [cm/s2] logg ?=- Surface gravity
(propagated from GALAH DR4)
83- 88 F6.1 --- S/N ?=- Signal to noise ratio in CCD3 (per pixel,
propagated from GALAH DR4)
90- 93 F4.2 --- chisq ?=- Chi squared value of spectroscopic fit
(propagated from GALAH DR4)
95- 99 F5.2 --- [Fe/H] ?=- Iron abundance (propagated from GALAH DR4)
101-105 A5 --- Rejected Reason for rejection in detailed analysis
--------------------------------------------------------------------------------
Acknowledgements:
Janez Kos, janez.kos(at)gmail.com
(End) Patricia Vannier [CDS] 13-Sep-2025