| Col. . | Name . | Description . |
|---|---|---|
| 1 | spec_id | LAMOST unique spectral ID, in format of date-plateid-spectrographid-fibreid |
| 2 | date | Date of observation |
| 3 | plate | LAMOST plate ID, not necessarily unique |
| 4 | sp_id | LAMOST spectrograph ID, ranging from 1 to 16 |
| 5 | fibre_id | LAMOST fibre ID for a given spectrograph, ranging from 1 to 250 |
| 6 | objid | Object ID in the input catalogues |
| 7 | objtype | Initial object type from the survey input catalogues |
| 8 | ra | Right ascension of J2000.0 (°) |
| 9 | dec | Declination of J2000.0 (°) |
| 10 | l | Galactic longitude (°) |
| 11 | b | Galactic latitude (°) |
| 12 | jd | Julian days at the middle time of the first exposure |
| 13 | moonphase | Moon phase at the middle time of the first exposure |
| 14 | monodis | Moon distance at the middle time of the first exposure |
| 15 | airmass | Airmass at the middle time of the first exposure |
| 16 | alt | Altitude (in degrees) of the telescope at the middle time of the first exposure |
| 17 | az | Azimuth angle (in degrees) of the telescope at the middle time of the first exposure |
| 18 | ha | Hour angle (in degrees) of the telescope at the middle time of the first exposure |
| 19 | badfiber | Is it a bad fibre? (yes – 1, no – 0) |
| 20 | satflag | Is the spectrum saturated? (yes – 1, no – 0) |
| 21 | brightflag | Are there bright stars (snr_b > 300) in the nearby five fibres (yes – 1, no – 0) |
| 22 | brightsnr | Largest snr_b in the nearby five fibres |
| 23 | object_sky_ratio | Object to sky flux ratio |
| 24 | snr_b | S/N(4650 Å) per pixel |
| 25 | snr_r | S/N(7450 Å) per pixel |
| 26 | uqflag | Uniqueness flag. If the target has been observed n times, then uqflag runs from 1 to n, with 1 denoting |
| the spectrum of the highest snr_b | ||
| 27 | vr | Radial velocity yielded by LSP3, after corrected for a systematic offset of −3.1 km s−1 (km s−1) |
| 28 | err_vr | Error of radial velocity yielded by LSP3 (km s−1) |
| 29 | teff | Recommended Teff (K) |
| 30 | err_teff | Error of the recommended Teff |
| 31 | teff_from | Which method is the recommended Teff adopted |
| 32 | logg | Recommended log g (cm s−2) |
| 33 | err_logg | Error of the recommended log g |
| 34 | logg_from | Which method is the recommended log g adopted |
| 35 | mv | Recommended absolute magnitude in V band |
| 36 | err_mv | Error of MV |
| 37 | mv_from | Which method is the recommended MV adopted |
| 38 | mk | Recommended absolute magnitude in Ks band |
| 39 | err_mk | Error of |$M_{K_{\rm s}}$| |
| 40 | mk_from | Which method is the recommended |$M_{K_{\rm s}}$| adopted |
| 41 | feh | Recommended [Fe/H] (dex) |
| 42 | err_feh | Error of the recommended [Fe/H] |
| 43 | feh_from | Which method is the recommended [Fe/H] adopted |
| 44 | afe | Recommended [α/Fe] (dex) |
| 45 | err_afe | Error of the recommended [α/Fe] |
| 46 | afe_from | Which method is the recommended [α/Fe] adopted |
| 47 | am | α-element to metal abundance ratio [α/M] estimated by training the LAMOST-APOGEE stars (dex) |
| 48 | err_am | Error of [α/M] |
| 49 | mh | Metal abundance [M/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 50 | err_mh | Error of [M/H] |
| 51 | ch | Carbon abundance [C/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 52 | err_mh | Error of [C/H] |
| 53 | nh | Nitrogen abundance [N/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 54 | err_nh | Error of [N/H] |
| 55 | ebv | Recommended E(B − V) |
| 56 | dist | Recommended distance (pc) |
| 57 | err_dist | Error of the recommended distance |
| 58 | dist_from | Which method is the recommended distance adopted |
| 59 | vr_peak_corr_coeff | Peak correlation coefficient for radial velocity estimation |
| 60 | vr_flag | Flag to describe value of ‘vr_peak_corr_coeff’, n means the vr_peak_corr_coeff |
| is smaller than the median value of the sample stars with the same snr_b by n ×MAD | ||
| 61 | teff1 | Teff estimated with the weighted-mean algorithm (K) |
| 62 | err_teff1 | Error of teff1 |
| 63 | teff2 | Teff estimated with the KPCA method (K) |
| 64 | err_teff2 | Error of teff2 |
| 65 | logg1 | Log g estimated with the weighted-mean algorithm (cm s−2) |
| 66 | err_logg1 | Error of logg1 |
| 67 | logg2 | Log g estimated with the KPCA method using MILES stars as training set (cm s−2) |
| 68 | err_logg2 | Error of logg2 |
| 69 | logg3 | Log g estimated with the KPCA method using LAMOST-Kepler stars as training set (cm s−2) |
| 70 | err_logg3 | Error of logg3 |
| 71 | mv1 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 72 | err_mv1 | Error of mv1 |
| 73 | mv2 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 74 | err_mv2 | Error of mv2 |
| 75 | mk1 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 76 | err_mk1 | Error of mk1 |
| 77 | mk2 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 78 | err_mk2 | Error of mk2 |
| 79 | feh1 | [Fe/H] estimated with the LSP3 weighted mean algorithm (dex) |
| 80 | err_feh1 | Error of feh1 |
| 81 | feh2 | [Fe/H] estimated with the LSP3 KPCA method by training the MILES stars (dex) |
| 82 | err_feh2 | Error of feh2 |
| 83 | feh3 | [Fe/H] estimated with the LSP3 KPCA method by training the LAMOST-APOGEE stars (dex) |
| 84 | err_feh3 | Error of feh3 |
| 85 | afe1 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 3900–3980, 4400–4600 and 5000–5300 Å (dex) | ||
| 86 | err_afe1 | Error of afe1 |
| 87 | afe2 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 4400–4600 and 5000 – 5300 Å (dex) | ||
| 88 | err_afe2 | Error of afe2 |
| 89 | afe3 | [α/Fe] estimated with the LSP3 KPCA method using the LAMOST-APOGEE training set (dex) |
| 90 | err_afe3 | Error of afe3 |
| 91 | besttemp_chi2 | Name of the best-matching template star with χ2 algorithm |
| 92 | besttemp_corr | Name of the best-matching template star with correlation algorithm |
| 93 | typeflag_chi2 | Stellar types of the best-matching template star with χ2 algorithm |
| 94 | typeflag_corr | Stellar types of the best-matching template star with correlation algorithm |
| 95 | min_chi2 | Minimum χ2 yielded by LSP3 from template matching with the MILES library |
| 96 | chi2_flag | The ‘min_chi2’ is smaller than the median value of the sample stars in the same SNR and |
| atmospheric parameter bin by n ×MAD | ||
| 97 | dg_miles_tm | Maximum value of the kernel function for estimation of Teff and [Fe/H] with KPCA method |
| via training the MILES stars | ||
| 98 | dg_miles_g | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the MILES stars | ||
| 99 | dg_lm_kep | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the LAMOST-Kepler stars | ||
| 100 | dg_lm_hip | Maximum value of the kernel function for estimation of absolute magnitudes with KPCA method |
| via training the LAMOST-Hipparcos stars | ||
| 101 | dg_lm_apo | Maximum value of the kernel function for estimation of abundances with KPCA method via training |
| the LAMOST-APOGEE stars | ||
| 102 | fuv | GALEXFUV-band magnitude (mag) |
| 103 | err_fuv | Error of fuv |
| 104 | nuv | GALEXNUV-band magnitude (mag) |
| 105 | err_nuv | Error of nuv |
| 106 | g | XSTPS-GAC g-band magnitude (mag) |
| 107 | err_g | Error of g |
| 108 | r | XSTPS-GAC r-band magnitude (mag) |
| 109 | err_r | Error of r |
| 110 | i | XSTPS-GAC i-band magnitude (mag) |
| 111 | err_i | Error of i |
| 112 | J | 2MASS J-band magnitude (mag) |
| 113 | err_J | Error of J |
| 114 | H | 2MASS H-band magnitude (mag) |
| 115 | err_H | Error of H |
| 116 | Ks | 2MASS Ks-band magnitude (mag) |
| 117 | err_Ks | Error of Ks |
| 118 | w1 | WISEW1-band magnitude (mag) |
| 119 | err_w1 | Error of w1 |
| 120 | w2 | WISEW2-band magnitude (mag) |
| 121 | err_w2 | Error of w2 |
| 122 | w3 | WISEW3-band magnitude (mag) |
| 123 | err_w3 | Error of w3 |
| 124 | w4 | WISEW4-band magnitude (mag) |
| 125 | err_w4 | Error of w3 |
| 126 | ph_qual_2mass | 2MASS photometric quality flag |
| 127 | ph_qual_wise | WISE photometric quality flag |
| 128 | var_flag_wise | WISE variability flag |
| 129 | ext_flag_wise | WISE extended source flag |
| 130 | cc_flag_wise | WISE contamination and confusion flag |
| 131 | ebv_sfd | E(B − V) from the SFD extinction map (mag) |
| 132 | ebv_sp | E(B − V) derived from the star pair method (mag) |
| 133 | err_ebv_sp | Error of ebv_sp |
| 134 | ebv_mod | E(B − V) derived by comparing the observed and synthetic model atmosphere colours (mag) |
| 135 | ebv_phot | E(B − V) derived by fitting multiband photometry to the empirical stellar loci (Chen et al. 2014) (mag) |
| 136 | dist_em1 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the recommended atmospheric parameters | ||
| 137 | err_dist_em1 | Error of dist_em1 |
| 138 | dist_em2 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the weighted-mean atmospheric parameters | ||
| 139 | err_dist_em2 | Error of dist_em2 |
| 140 | dist_sp1 | Distance inferred from absolute magnitudes estimated with KPCA method using 300 PCs (pc) |
| 141 | err_dist_sp1 | Error of dist_sp1 |
| 142 | dist_sp2 | Distance inferred from absolute magnitudes estimated with KPCA method using 100 PCs (pc) |
| 143 | err_dist_sp2 | Error of dist_sp2 |
| 144 | dist_phot | Distance derived from the photometric parallax method (Chen et al. 2014) (pc) |
| 145 | err_dist_phot | Error of dist_phot |
| 146 | pmra_ppmxl | Proper motion in RA from the PPMXL catalogues (mas yr−1) |
| 147 | epmra_ppmxl | Error of pmra_ppmxl |
| 148 | pmdec_ppmxl | Proper motion in Dec. from the PPMXL catalogues (mas yr−1) |
| 149 | epmdec_ppmxl | Error of pmdec_ppmxl |
| 150 | pmra_ucac4 | Proper motion in RA from the UCAC4 catalogues (mas yr−1) |
| 151 | epmra_ucac4 | Error of pmra_ucac4 |
| 152 | pmdec_ucac4 | Proper motion in Dec. from the UCAC4 catalogues (mas yr−1) |
| 153 | epmdec_ucac4 | Error of pmdec_ucac4 |
| 154 | pmra_xuyi2mass | Proper motion in RA derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 155 | pmdec_xuyi2mass | Proper motion in Dec. derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 156 | x | x-coordinate in a Galactocentric Cartesian reference system, positive towards the Galactic Centre (kpc) |
| 157 | err_x | Error of x |
| 158 | y | y-coordinate in a Galactocentric Cartesian reference system, positive in the direction of disc rotation (kpc) |
| 159 | err_y | Error of y |
| 160 | z | z-coordinate in a Galactocentric Cartesian reference system, positive towards the North Galactic Pole (kpc) |
| 161 | err_z | Error of z |
| 162 | u[2] | Galactic space velocities in the x-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the Galactic Centre (km s−1) | ||
| 163 | err_u[2] | Error of u[2] |
| 164 | v[2] | Galactic space velocities in the y-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive in the direction of Galactic rotation (km s−1) | ||
| 165 | err_v[2] | Error of v[2] |
| 166 | w[2] | Galactic space velocities in the z-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the north Galactic pole (km s−1) | ||
| 167 | err_w[2] | Error of w[2] |
| 168 | v_r[2] | Galactic space velocities in the r-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively (km s−1) | ||
| 169 | err_v_r[2] | Error of v_r[2] |
| 170 | v_phi[2] | Galactic space velocities in the Φ-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive in the direction of counter disc rotation (km s−1) | ||
| 171 | err_v_phi[2] | Error of v_phi[2] |
| 172 | v_z[2] | Galactic space velocities in the z-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive towards the north Galactic pole (km s−1) | ||
| 173 | err_v_z[2] | Error of v_z[2] |
| 174 | e[2] | Orbital eccentricities computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively |
| 175 | Rapo[2] | Maximum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 176 | Rperi[2] | Minimum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 177 | zmin[2] | Minimum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 178 | zmax[2] | Maximum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| Col. . | Name . | Description . |
|---|---|---|
| 1 | spec_id | LAMOST unique spectral ID, in format of date-plateid-spectrographid-fibreid |
| 2 | date | Date of observation |
| 3 | plate | LAMOST plate ID, not necessarily unique |
| 4 | sp_id | LAMOST spectrograph ID, ranging from 1 to 16 |
| 5 | fibre_id | LAMOST fibre ID for a given spectrograph, ranging from 1 to 250 |
| 6 | objid | Object ID in the input catalogues |
| 7 | objtype | Initial object type from the survey input catalogues |
| 8 | ra | Right ascension of J2000.0 (°) |
| 9 | dec | Declination of J2000.0 (°) |
| 10 | l | Galactic longitude (°) |
| 11 | b | Galactic latitude (°) |
| 12 | jd | Julian days at the middle time of the first exposure |
| 13 | moonphase | Moon phase at the middle time of the first exposure |
| 14 | monodis | Moon distance at the middle time of the first exposure |
| 15 | airmass | Airmass at the middle time of the first exposure |
| 16 | alt | Altitude (in degrees) of the telescope at the middle time of the first exposure |
| 17 | az | Azimuth angle (in degrees) of the telescope at the middle time of the first exposure |
| 18 | ha | Hour angle (in degrees) of the telescope at the middle time of the first exposure |
| 19 | badfiber | Is it a bad fibre? (yes – 1, no – 0) |
| 20 | satflag | Is the spectrum saturated? (yes – 1, no – 0) |
| 21 | brightflag | Are there bright stars (snr_b > 300) in the nearby five fibres (yes – 1, no – 0) |
| 22 | brightsnr | Largest snr_b in the nearby five fibres |
| 23 | object_sky_ratio | Object to sky flux ratio |
| 24 | snr_b | S/N(4650 Å) per pixel |
| 25 | snr_r | S/N(7450 Å) per pixel |
| 26 | uqflag | Uniqueness flag. If the target has been observed n times, then uqflag runs from 1 to n, with 1 denoting |
| the spectrum of the highest snr_b | ||
| 27 | vr | Radial velocity yielded by LSP3, after corrected for a systematic offset of −3.1 km s−1 (km s−1) |
| 28 | err_vr | Error of radial velocity yielded by LSP3 (km s−1) |
| 29 | teff | Recommended Teff (K) |
| 30 | err_teff | Error of the recommended Teff |
| 31 | teff_from | Which method is the recommended Teff adopted |
| 32 | logg | Recommended log g (cm s−2) |
| 33 | err_logg | Error of the recommended log g |
| 34 | logg_from | Which method is the recommended log g adopted |
| 35 | mv | Recommended absolute magnitude in V band |
| 36 | err_mv | Error of MV |
| 37 | mv_from | Which method is the recommended MV adopted |
| 38 | mk | Recommended absolute magnitude in Ks band |
| 39 | err_mk | Error of |$M_{K_{\rm s}}$| |
| 40 | mk_from | Which method is the recommended |$M_{K_{\rm s}}$| adopted |
| 41 | feh | Recommended [Fe/H] (dex) |
| 42 | err_feh | Error of the recommended [Fe/H] |
| 43 | feh_from | Which method is the recommended [Fe/H] adopted |
| 44 | afe | Recommended [α/Fe] (dex) |
| 45 | err_afe | Error of the recommended [α/Fe] |
| 46 | afe_from | Which method is the recommended [α/Fe] adopted |
| 47 | am | α-element to metal abundance ratio [α/M] estimated by training the LAMOST-APOGEE stars (dex) |
| 48 | err_am | Error of [α/M] |
| 49 | mh | Metal abundance [M/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 50 | err_mh | Error of [M/H] |
| 51 | ch | Carbon abundance [C/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 52 | err_mh | Error of [C/H] |
| 53 | nh | Nitrogen abundance [N/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 54 | err_nh | Error of [N/H] |
| 55 | ebv | Recommended E(B − V) |
| 56 | dist | Recommended distance (pc) |
| 57 | err_dist | Error of the recommended distance |
| 58 | dist_from | Which method is the recommended distance adopted |
| 59 | vr_peak_corr_coeff | Peak correlation coefficient for radial velocity estimation |
| 60 | vr_flag | Flag to describe value of ‘vr_peak_corr_coeff’, n means the vr_peak_corr_coeff |
| is smaller than the median value of the sample stars with the same snr_b by n ×MAD | ||
| 61 | teff1 | Teff estimated with the weighted-mean algorithm (K) |
| 62 | err_teff1 | Error of teff1 |
| 63 | teff2 | Teff estimated with the KPCA method (K) |
| 64 | err_teff2 | Error of teff2 |
| 65 | logg1 | Log g estimated with the weighted-mean algorithm (cm s−2) |
| 66 | err_logg1 | Error of logg1 |
| 67 | logg2 | Log g estimated with the KPCA method using MILES stars as training set (cm s−2) |
| 68 | err_logg2 | Error of logg2 |
| 69 | logg3 | Log g estimated with the KPCA method using LAMOST-Kepler stars as training set (cm s−2) |
| 70 | err_logg3 | Error of logg3 |
| 71 | mv1 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 72 | err_mv1 | Error of mv1 |
| 73 | mv2 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 74 | err_mv2 | Error of mv2 |
| 75 | mk1 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 76 | err_mk1 | Error of mk1 |
| 77 | mk2 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 78 | err_mk2 | Error of mk2 |
| 79 | feh1 | [Fe/H] estimated with the LSP3 weighted mean algorithm (dex) |
| 80 | err_feh1 | Error of feh1 |
| 81 | feh2 | [Fe/H] estimated with the LSP3 KPCA method by training the MILES stars (dex) |
| 82 | err_feh2 | Error of feh2 |
| 83 | feh3 | [Fe/H] estimated with the LSP3 KPCA method by training the LAMOST-APOGEE stars (dex) |
| 84 | err_feh3 | Error of feh3 |
| 85 | afe1 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 3900–3980, 4400–4600 and 5000–5300 Å (dex) | ||
| 86 | err_afe1 | Error of afe1 |
| 87 | afe2 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 4400–4600 and 5000 – 5300 Å (dex) | ||
| 88 | err_afe2 | Error of afe2 |
| 89 | afe3 | [α/Fe] estimated with the LSP3 KPCA method using the LAMOST-APOGEE training set (dex) |
| 90 | err_afe3 | Error of afe3 |
| 91 | besttemp_chi2 | Name of the best-matching template star with χ2 algorithm |
| 92 | besttemp_corr | Name of the best-matching template star with correlation algorithm |
| 93 | typeflag_chi2 | Stellar types of the best-matching template star with χ2 algorithm |
| 94 | typeflag_corr | Stellar types of the best-matching template star with correlation algorithm |
| 95 | min_chi2 | Minimum χ2 yielded by LSP3 from template matching with the MILES library |
| 96 | chi2_flag | The ‘min_chi2’ is smaller than the median value of the sample stars in the same SNR and |
| atmospheric parameter bin by n ×MAD | ||
| 97 | dg_miles_tm | Maximum value of the kernel function for estimation of Teff and [Fe/H] with KPCA method |
| via training the MILES stars | ||
| 98 | dg_miles_g | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the MILES stars | ||
| 99 | dg_lm_kep | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the LAMOST-Kepler stars | ||
| 100 | dg_lm_hip | Maximum value of the kernel function for estimation of absolute magnitudes with KPCA method |
| via training the LAMOST-Hipparcos stars | ||
| 101 | dg_lm_apo | Maximum value of the kernel function for estimation of abundances with KPCA method via training |
| the LAMOST-APOGEE stars | ||
| 102 | fuv | GALEXFUV-band magnitude (mag) |
| 103 | err_fuv | Error of fuv |
| 104 | nuv | GALEXNUV-band magnitude (mag) |
| 105 | err_nuv | Error of nuv |
| 106 | g | XSTPS-GAC g-band magnitude (mag) |
| 107 | err_g | Error of g |
| 108 | r | XSTPS-GAC r-band magnitude (mag) |
| 109 | err_r | Error of r |
| 110 | i | XSTPS-GAC i-band magnitude (mag) |
| 111 | err_i | Error of i |
| 112 | J | 2MASS J-band magnitude (mag) |
| 113 | err_J | Error of J |
| 114 | H | 2MASS H-band magnitude (mag) |
| 115 | err_H | Error of H |
| 116 | Ks | 2MASS Ks-band magnitude (mag) |
| 117 | err_Ks | Error of Ks |
| 118 | w1 | WISEW1-band magnitude (mag) |
| 119 | err_w1 | Error of w1 |
| 120 | w2 | WISEW2-band magnitude (mag) |
| 121 | err_w2 | Error of w2 |
| 122 | w3 | WISEW3-band magnitude (mag) |
| 123 | err_w3 | Error of w3 |
| 124 | w4 | WISEW4-band magnitude (mag) |
| 125 | err_w4 | Error of w3 |
| 126 | ph_qual_2mass | 2MASS photometric quality flag |
| 127 | ph_qual_wise | WISE photometric quality flag |
| 128 | var_flag_wise | WISE variability flag |
| 129 | ext_flag_wise | WISE extended source flag |
| 130 | cc_flag_wise | WISE contamination and confusion flag |
| 131 | ebv_sfd | E(B − V) from the SFD extinction map (mag) |
| 132 | ebv_sp | E(B − V) derived from the star pair method (mag) |
| 133 | err_ebv_sp | Error of ebv_sp |
| 134 | ebv_mod | E(B − V) derived by comparing the observed and synthetic model atmosphere colours (mag) |
| 135 | ebv_phot | E(B − V) derived by fitting multiband photometry to the empirical stellar loci (Chen et al. 2014) (mag) |
| 136 | dist_em1 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the recommended atmospheric parameters | ||
| 137 | err_dist_em1 | Error of dist_em1 |
| 138 | dist_em2 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the weighted-mean atmospheric parameters | ||
| 139 | err_dist_em2 | Error of dist_em2 |
| 140 | dist_sp1 | Distance inferred from absolute magnitudes estimated with KPCA method using 300 PCs (pc) |
| 141 | err_dist_sp1 | Error of dist_sp1 |
| 142 | dist_sp2 | Distance inferred from absolute magnitudes estimated with KPCA method using 100 PCs (pc) |
| 143 | err_dist_sp2 | Error of dist_sp2 |
| 144 | dist_phot | Distance derived from the photometric parallax method (Chen et al. 2014) (pc) |
| 145 | err_dist_phot | Error of dist_phot |
| 146 | pmra_ppmxl | Proper motion in RA from the PPMXL catalogues (mas yr−1) |
| 147 | epmra_ppmxl | Error of pmra_ppmxl |
| 148 | pmdec_ppmxl | Proper motion in Dec. from the PPMXL catalogues (mas yr−1) |
| 149 | epmdec_ppmxl | Error of pmdec_ppmxl |
| 150 | pmra_ucac4 | Proper motion in RA from the UCAC4 catalogues (mas yr−1) |
| 151 | epmra_ucac4 | Error of pmra_ucac4 |
| 152 | pmdec_ucac4 | Proper motion in Dec. from the UCAC4 catalogues (mas yr−1) |
| 153 | epmdec_ucac4 | Error of pmdec_ucac4 |
| 154 | pmra_xuyi2mass | Proper motion in RA derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 155 | pmdec_xuyi2mass | Proper motion in Dec. derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 156 | x | x-coordinate in a Galactocentric Cartesian reference system, positive towards the Galactic Centre (kpc) |
| 157 | err_x | Error of x |
| 158 | y | y-coordinate in a Galactocentric Cartesian reference system, positive in the direction of disc rotation (kpc) |
| 159 | err_y | Error of y |
| 160 | z | z-coordinate in a Galactocentric Cartesian reference system, positive towards the North Galactic Pole (kpc) |
| 161 | err_z | Error of z |
| 162 | u[2] | Galactic space velocities in the x-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the Galactic Centre (km s−1) | ||
| 163 | err_u[2] | Error of u[2] |
| 164 | v[2] | Galactic space velocities in the y-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive in the direction of Galactic rotation (km s−1) | ||
| 165 | err_v[2] | Error of v[2] |
| 166 | w[2] | Galactic space velocities in the z-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the north Galactic pole (km s−1) | ||
| 167 | err_w[2] | Error of w[2] |
| 168 | v_r[2] | Galactic space velocities in the r-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively (km s−1) | ||
| 169 | err_v_r[2] | Error of v_r[2] |
| 170 | v_phi[2] | Galactic space velocities in the Φ-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive in the direction of counter disc rotation (km s−1) | ||
| 171 | err_v_phi[2] | Error of v_phi[2] |
| 172 | v_z[2] | Galactic space velocities in the z-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive towards the north Galactic pole (km s−1) | ||
| 173 | err_v_z[2] | Error of v_z[2] |
| 174 | e[2] | Orbital eccentricities computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively |
| 175 | Rapo[2] | Maximum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 176 | Rperi[2] | Minimum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 177 | zmin[2] | Minimum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 178 | zmax[2] | Maximum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| Col. . | Name . | Description . |
|---|---|---|
| 1 | spec_id | LAMOST unique spectral ID, in format of date-plateid-spectrographid-fibreid |
| 2 | date | Date of observation |
| 3 | plate | LAMOST plate ID, not necessarily unique |
| 4 | sp_id | LAMOST spectrograph ID, ranging from 1 to 16 |
| 5 | fibre_id | LAMOST fibre ID for a given spectrograph, ranging from 1 to 250 |
| 6 | objid | Object ID in the input catalogues |
| 7 | objtype | Initial object type from the survey input catalogues |
| 8 | ra | Right ascension of J2000.0 (°) |
| 9 | dec | Declination of J2000.0 (°) |
| 10 | l | Galactic longitude (°) |
| 11 | b | Galactic latitude (°) |
| 12 | jd | Julian days at the middle time of the first exposure |
| 13 | moonphase | Moon phase at the middle time of the first exposure |
| 14 | monodis | Moon distance at the middle time of the first exposure |
| 15 | airmass | Airmass at the middle time of the first exposure |
| 16 | alt | Altitude (in degrees) of the telescope at the middle time of the first exposure |
| 17 | az | Azimuth angle (in degrees) of the telescope at the middle time of the first exposure |
| 18 | ha | Hour angle (in degrees) of the telescope at the middle time of the first exposure |
| 19 | badfiber | Is it a bad fibre? (yes – 1, no – 0) |
| 20 | satflag | Is the spectrum saturated? (yes – 1, no – 0) |
| 21 | brightflag | Are there bright stars (snr_b > 300) in the nearby five fibres (yes – 1, no – 0) |
| 22 | brightsnr | Largest snr_b in the nearby five fibres |
| 23 | object_sky_ratio | Object to sky flux ratio |
| 24 | snr_b | S/N(4650 Å) per pixel |
| 25 | snr_r | S/N(7450 Å) per pixel |
| 26 | uqflag | Uniqueness flag. If the target has been observed n times, then uqflag runs from 1 to n, with 1 denoting |
| the spectrum of the highest snr_b | ||
| 27 | vr | Radial velocity yielded by LSP3, after corrected for a systematic offset of −3.1 km s−1 (km s−1) |
| 28 | err_vr | Error of radial velocity yielded by LSP3 (km s−1) |
| 29 | teff | Recommended Teff (K) |
| 30 | err_teff | Error of the recommended Teff |
| 31 | teff_from | Which method is the recommended Teff adopted |
| 32 | logg | Recommended log g (cm s−2) |
| 33 | err_logg | Error of the recommended log g |
| 34 | logg_from | Which method is the recommended log g adopted |
| 35 | mv | Recommended absolute magnitude in V band |
| 36 | err_mv | Error of MV |
| 37 | mv_from | Which method is the recommended MV adopted |
| 38 | mk | Recommended absolute magnitude in Ks band |
| 39 | err_mk | Error of |$M_{K_{\rm s}}$| |
| 40 | mk_from | Which method is the recommended |$M_{K_{\rm s}}$| adopted |
| 41 | feh | Recommended [Fe/H] (dex) |
| 42 | err_feh | Error of the recommended [Fe/H] |
| 43 | feh_from | Which method is the recommended [Fe/H] adopted |
| 44 | afe | Recommended [α/Fe] (dex) |
| 45 | err_afe | Error of the recommended [α/Fe] |
| 46 | afe_from | Which method is the recommended [α/Fe] adopted |
| 47 | am | α-element to metal abundance ratio [α/M] estimated by training the LAMOST-APOGEE stars (dex) |
| 48 | err_am | Error of [α/M] |
| 49 | mh | Metal abundance [M/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 50 | err_mh | Error of [M/H] |
| 51 | ch | Carbon abundance [C/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 52 | err_mh | Error of [C/H] |
| 53 | nh | Nitrogen abundance [N/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 54 | err_nh | Error of [N/H] |
| 55 | ebv | Recommended E(B − V) |
| 56 | dist | Recommended distance (pc) |
| 57 | err_dist | Error of the recommended distance |
| 58 | dist_from | Which method is the recommended distance adopted |
| 59 | vr_peak_corr_coeff | Peak correlation coefficient for radial velocity estimation |
| 60 | vr_flag | Flag to describe value of ‘vr_peak_corr_coeff’, n means the vr_peak_corr_coeff |
| is smaller than the median value of the sample stars with the same snr_b by n ×MAD | ||
| 61 | teff1 | Teff estimated with the weighted-mean algorithm (K) |
| 62 | err_teff1 | Error of teff1 |
| 63 | teff2 | Teff estimated with the KPCA method (K) |
| 64 | err_teff2 | Error of teff2 |
| 65 | logg1 | Log g estimated with the weighted-mean algorithm (cm s−2) |
| 66 | err_logg1 | Error of logg1 |
| 67 | logg2 | Log g estimated with the KPCA method using MILES stars as training set (cm s−2) |
| 68 | err_logg2 | Error of logg2 |
| 69 | logg3 | Log g estimated with the KPCA method using LAMOST-Kepler stars as training set (cm s−2) |
| 70 | err_logg3 | Error of logg3 |
| 71 | mv1 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 72 | err_mv1 | Error of mv1 |
| 73 | mv2 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 74 | err_mv2 | Error of mv2 |
| 75 | mk1 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 76 | err_mk1 | Error of mk1 |
| 77 | mk2 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 78 | err_mk2 | Error of mk2 |
| 79 | feh1 | [Fe/H] estimated with the LSP3 weighted mean algorithm (dex) |
| 80 | err_feh1 | Error of feh1 |
| 81 | feh2 | [Fe/H] estimated with the LSP3 KPCA method by training the MILES stars (dex) |
| 82 | err_feh2 | Error of feh2 |
| 83 | feh3 | [Fe/H] estimated with the LSP3 KPCA method by training the LAMOST-APOGEE stars (dex) |
| 84 | err_feh3 | Error of feh3 |
| 85 | afe1 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 3900–3980, 4400–4600 and 5000–5300 Å (dex) | ||
| 86 | err_afe1 | Error of afe1 |
| 87 | afe2 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 4400–4600 and 5000 – 5300 Å (dex) | ||
| 88 | err_afe2 | Error of afe2 |
| 89 | afe3 | [α/Fe] estimated with the LSP3 KPCA method using the LAMOST-APOGEE training set (dex) |
| 90 | err_afe3 | Error of afe3 |
| 91 | besttemp_chi2 | Name of the best-matching template star with χ2 algorithm |
| 92 | besttemp_corr | Name of the best-matching template star with correlation algorithm |
| 93 | typeflag_chi2 | Stellar types of the best-matching template star with χ2 algorithm |
| 94 | typeflag_corr | Stellar types of the best-matching template star with correlation algorithm |
| 95 | min_chi2 | Minimum χ2 yielded by LSP3 from template matching with the MILES library |
| 96 | chi2_flag | The ‘min_chi2’ is smaller than the median value of the sample stars in the same SNR and |
| atmospheric parameter bin by n ×MAD | ||
| 97 | dg_miles_tm | Maximum value of the kernel function for estimation of Teff and [Fe/H] with KPCA method |
| via training the MILES stars | ||
| 98 | dg_miles_g | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the MILES stars | ||
| 99 | dg_lm_kep | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the LAMOST-Kepler stars | ||
| 100 | dg_lm_hip | Maximum value of the kernel function for estimation of absolute magnitudes with KPCA method |
| via training the LAMOST-Hipparcos stars | ||
| 101 | dg_lm_apo | Maximum value of the kernel function for estimation of abundances with KPCA method via training |
| the LAMOST-APOGEE stars | ||
| 102 | fuv | GALEXFUV-band magnitude (mag) |
| 103 | err_fuv | Error of fuv |
| 104 | nuv | GALEXNUV-band magnitude (mag) |
| 105 | err_nuv | Error of nuv |
| 106 | g | XSTPS-GAC g-band magnitude (mag) |
| 107 | err_g | Error of g |
| 108 | r | XSTPS-GAC r-band magnitude (mag) |
| 109 | err_r | Error of r |
| 110 | i | XSTPS-GAC i-band magnitude (mag) |
| 111 | err_i | Error of i |
| 112 | J | 2MASS J-band magnitude (mag) |
| 113 | err_J | Error of J |
| 114 | H | 2MASS H-band magnitude (mag) |
| 115 | err_H | Error of H |
| 116 | Ks | 2MASS Ks-band magnitude (mag) |
| 117 | err_Ks | Error of Ks |
| 118 | w1 | WISEW1-band magnitude (mag) |
| 119 | err_w1 | Error of w1 |
| 120 | w2 | WISEW2-band magnitude (mag) |
| 121 | err_w2 | Error of w2 |
| 122 | w3 | WISEW3-band magnitude (mag) |
| 123 | err_w3 | Error of w3 |
| 124 | w4 | WISEW4-band magnitude (mag) |
| 125 | err_w4 | Error of w3 |
| 126 | ph_qual_2mass | 2MASS photometric quality flag |
| 127 | ph_qual_wise | WISE photometric quality flag |
| 128 | var_flag_wise | WISE variability flag |
| 129 | ext_flag_wise | WISE extended source flag |
| 130 | cc_flag_wise | WISE contamination and confusion flag |
| 131 | ebv_sfd | E(B − V) from the SFD extinction map (mag) |
| 132 | ebv_sp | E(B − V) derived from the star pair method (mag) |
| 133 | err_ebv_sp | Error of ebv_sp |
| 134 | ebv_mod | E(B − V) derived by comparing the observed and synthetic model atmosphere colours (mag) |
| 135 | ebv_phot | E(B − V) derived by fitting multiband photometry to the empirical stellar loci (Chen et al. 2014) (mag) |
| 136 | dist_em1 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the recommended atmospheric parameters | ||
| 137 | err_dist_em1 | Error of dist_em1 |
| 138 | dist_em2 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the weighted-mean atmospheric parameters | ||
| 139 | err_dist_em2 | Error of dist_em2 |
| 140 | dist_sp1 | Distance inferred from absolute magnitudes estimated with KPCA method using 300 PCs (pc) |
| 141 | err_dist_sp1 | Error of dist_sp1 |
| 142 | dist_sp2 | Distance inferred from absolute magnitudes estimated with KPCA method using 100 PCs (pc) |
| 143 | err_dist_sp2 | Error of dist_sp2 |
| 144 | dist_phot | Distance derived from the photometric parallax method (Chen et al. 2014) (pc) |
| 145 | err_dist_phot | Error of dist_phot |
| 146 | pmra_ppmxl | Proper motion in RA from the PPMXL catalogues (mas yr−1) |
| 147 | epmra_ppmxl | Error of pmra_ppmxl |
| 148 | pmdec_ppmxl | Proper motion in Dec. from the PPMXL catalogues (mas yr−1) |
| 149 | epmdec_ppmxl | Error of pmdec_ppmxl |
| 150 | pmra_ucac4 | Proper motion in RA from the UCAC4 catalogues (mas yr−1) |
| 151 | epmra_ucac4 | Error of pmra_ucac4 |
| 152 | pmdec_ucac4 | Proper motion in Dec. from the UCAC4 catalogues (mas yr−1) |
| 153 | epmdec_ucac4 | Error of pmdec_ucac4 |
| 154 | pmra_xuyi2mass | Proper motion in RA derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 155 | pmdec_xuyi2mass | Proper motion in Dec. derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 156 | x | x-coordinate in a Galactocentric Cartesian reference system, positive towards the Galactic Centre (kpc) |
| 157 | err_x | Error of x |
| 158 | y | y-coordinate in a Galactocentric Cartesian reference system, positive in the direction of disc rotation (kpc) |
| 159 | err_y | Error of y |
| 160 | z | z-coordinate in a Galactocentric Cartesian reference system, positive towards the North Galactic Pole (kpc) |
| 161 | err_z | Error of z |
| 162 | u[2] | Galactic space velocities in the x-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the Galactic Centre (km s−1) | ||
| 163 | err_u[2] | Error of u[2] |
| 164 | v[2] | Galactic space velocities in the y-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive in the direction of Galactic rotation (km s−1) | ||
| 165 | err_v[2] | Error of v[2] |
| 166 | w[2] | Galactic space velocities in the z-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the north Galactic pole (km s−1) | ||
| 167 | err_w[2] | Error of w[2] |
| 168 | v_r[2] | Galactic space velocities in the r-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively (km s−1) | ||
| 169 | err_v_r[2] | Error of v_r[2] |
| 170 | v_phi[2] | Galactic space velocities in the Φ-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive in the direction of counter disc rotation (km s−1) | ||
| 171 | err_v_phi[2] | Error of v_phi[2] |
| 172 | v_z[2] | Galactic space velocities in the z-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive towards the north Galactic pole (km s−1) | ||
| 173 | err_v_z[2] | Error of v_z[2] |
| 174 | e[2] | Orbital eccentricities computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively |
| 175 | Rapo[2] | Maximum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 176 | Rperi[2] | Minimum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 177 | zmin[2] | Minimum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 178 | zmax[2] | Maximum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| Col. . | Name . | Description . |
|---|---|---|
| 1 | spec_id | LAMOST unique spectral ID, in format of date-plateid-spectrographid-fibreid |
| 2 | date | Date of observation |
| 3 | plate | LAMOST plate ID, not necessarily unique |
| 4 | sp_id | LAMOST spectrograph ID, ranging from 1 to 16 |
| 5 | fibre_id | LAMOST fibre ID for a given spectrograph, ranging from 1 to 250 |
| 6 | objid | Object ID in the input catalogues |
| 7 | objtype | Initial object type from the survey input catalogues |
| 8 | ra | Right ascension of J2000.0 (°) |
| 9 | dec | Declination of J2000.0 (°) |
| 10 | l | Galactic longitude (°) |
| 11 | b | Galactic latitude (°) |
| 12 | jd | Julian days at the middle time of the first exposure |
| 13 | moonphase | Moon phase at the middle time of the first exposure |
| 14 | monodis | Moon distance at the middle time of the first exposure |
| 15 | airmass | Airmass at the middle time of the first exposure |
| 16 | alt | Altitude (in degrees) of the telescope at the middle time of the first exposure |
| 17 | az | Azimuth angle (in degrees) of the telescope at the middle time of the first exposure |
| 18 | ha | Hour angle (in degrees) of the telescope at the middle time of the first exposure |
| 19 | badfiber | Is it a bad fibre? (yes – 1, no – 0) |
| 20 | satflag | Is the spectrum saturated? (yes – 1, no – 0) |
| 21 | brightflag | Are there bright stars (snr_b > 300) in the nearby five fibres (yes – 1, no – 0) |
| 22 | brightsnr | Largest snr_b in the nearby five fibres |
| 23 | object_sky_ratio | Object to sky flux ratio |
| 24 | snr_b | S/N(4650 Å) per pixel |
| 25 | snr_r | S/N(7450 Å) per pixel |
| 26 | uqflag | Uniqueness flag. If the target has been observed n times, then uqflag runs from 1 to n, with 1 denoting |
| the spectrum of the highest snr_b | ||
| 27 | vr | Radial velocity yielded by LSP3, after corrected for a systematic offset of −3.1 km s−1 (km s−1) |
| 28 | err_vr | Error of radial velocity yielded by LSP3 (km s−1) |
| 29 | teff | Recommended Teff (K) |
| 30 | err_teff | Error of the recommended Teff |
| 31 | teff_from | Which method is the recommended Teff adopted |
| 32 | logg | Recommended log g (cm s−2) |
| 33 | err_logg | Error of the recommended log g |
| 34 | logg_from | Which method is the recommended log g adopted |
| 35 | mv | Recommended absolute magnitude in V band |
| 36 | err_mv | Error of MV |
| 37 | mv_from | Which method is the recommended MV adopted |
| 38 | mk | Recommended absolute magnitude in Ks band |
| 39 | err_mk | Error of |$M_{K_{\rm s}}$| |
| 40 | mk_from | Which method is the recommended |$M_{K_{\rm s}}$| adopted |
| 41 | feh | Recommended [Fe/H] (dex) |
| 42 | err_feh | Error of the recommended [Fe/H] |
| 43 | feh_from | Which method is the recommended [Fe/H] adopted |
| 44 | afe | Recommended [α/Fe] (dex) |
| 45 | err_afe | Error of the recommended [α/Fe] |
| 46 | afe_from | Which method is the recommended [α/Fe] adopted |
| 47 | am | α-element to metal abundance ratio [α/M] estimated by training the LAMOST-APOGEE stars (dex) |
| 48 | err_am | Error of [α/M] |
| 49 | mh | Metal abundance [M/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 50 | err_mh | Error of [M/H] |
| 51 | ch | Carbon abundance [C/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 52 | err_mh | Error of [C/H] |
| 53 | nh | Nitrogen abundance [N/H] estimated by training the LAMOST-APOGEE stars (dex) |
| 54 | err_nh | Error of [N/H] |
| 55 | ebv | Recommended E(B − V) |
| 56 | dist | Recommended distance (pc) |
| 57 | err_dist | Error of the recommended distance |
| 58 | dist_from | Which method is the recommended distance adopted |
| 59 | vr_peak_corr_coeff | Peak correlation coefficient for radial velocity estimation |
| 60 | vr_flag | Flag to describe value of ‘vr_peak_corr_coeff’, n means the vr_peak_corr_coeff |
| is smaller than the median value of the sample stars with the same snr_b by n ×MAD | ||
| 61 | teff1 | Teff estimated with the weighted-mean algorithm (K) |
| 62 | err_teff1 | Error of teff1 |
| 63 | teff2 | Teff estimated with the KPCA method (K) |
| 64 | err_teff2 | Error of teff2 |
| 65 | logg1 | Log g estimated with the weighted-mean algorithm (cm s−2) |
| 66 | err_logg1 | Error of logg1 |
| 67 | logg2 | Log g estimated with the KPCA method using MILES stars as training set (cm s−2) |
| 68 | err_logg2 | Error of logg2 |
| 69 | logg3 | Log g estimated with the KPCA method using LAMOST-Kepler stars as training set (cm s−2) |
| 70 | err_logg3 | Error of logg3 |
| 71 | mv1 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 72 | err_mv1 | Error of mv1 |
| 73 | mv2 | MV estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 74 | err_mv2 | Error of mv2 |
| 75 | mk1 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 300 PCs (mag) |
| 76 | err_mk1 | Error of mk1 |
| 77 | mk2 | |$M_{K_{\rm s}}$| estimated with the KPCA method taking LAMOST-Hipparcos stars as training set using 100 PCs (mag) |
| 78 | err_mk2 | Error of mk2 |
| 79 | feh1 | [Fe/H] estimated with the LSP3 weighted mean algorithm (dex) |
| 80 | err_feh1 | Error of feh1 |
| 81 | feh2 | [Fe/H] estimated with the LSP3 KPCA method by training the MILES stars (dex) |
| 82 | err_feh2 | Error of feh2 |
| 83 | feh3 | [Fe/H] estimated with the LSP3 KPCA method by training the LAMOST-APOGEE stars (dex) |
| 84 | err_feh3 | Error of feh3 |
| 85 | afe1 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 3900–3980, 4400–4600 and 5000–5300 Å (dex) | ||
| 86 | err_afe1 | Error of afe1 |
| 87 | afe2 | [α/Fe] estimated by template matching with synthetic spectra using spectral segments |
| of 4400–4600 and 5000 – 5300 Å (dex) | ||
| 88 | err_afe2 | Error of afe2 |
| 89 | afe3 | [α/Fe] estimated with the LSP3 KPCA method using the LAMOST-APOGEE training set (dex) |
| 90 | err_afe3 | Error of afe3 |
| 91 | besttemp_chi2 | Name of the best-matching template star with χ2 algorithm |
| 92 | besttemp_corr | Name of the best-matching template star with correlation algorithm |
| 93 | typeflag_chi2 | Stellar types of the best-matching template star with χ2 algorithm |
| 94 | typeflag_corr | Stellar types of the best-matching template star with correlation algorithm |
| 95 | min_chi2 | Minimum χ2 yielded by LSP3 from template matching with the MILES library |
| 96 | chi2_flag | The ‘min_chi2’ is smaller than the median value of the sample stars in the same SNR and |
| atmospheric parameter bin by n ×MAD | ||
| 97 | dg_miles_tm | Maximum value of the kernel function for estimation of Teff and [Fe/H] with KPCA method |
| via training the MILES stars | ||
| 98 | dg_miles_g | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the MILES stars | ||
| 99 | dg_lm_kep | Maximum value of the kernel function for estimation of log g with KPCA method via training |
| the LAMOST-Kepler stars | ||
| 100 | dg_lm_hip | Maximum value of the kernel function for estimation of absolute magnitudes with KPCA method |
| via training the LAMOST-Hipparcos stars | ||
| 101 | dg_lm_apo | Maximum value of the kernel function for estimation of abundances with KPCA method via training |
| the LAMOST-APOGEE stars | ||
| 102 | fuv | GALEXFUV-band magnitude (mag) |
| 103 | err_fuv | Error of fuv |
| 104 | nuv | GALEXNUV-band magnitude (mag) |
| 105 | err_nuv | Error of nuv |
| 106 | g | XSTPS-GAC g-band magnitude (mag) |
| 107 | err_g | Error of g |
| 108 | r | XSTPS-GAC r-band magnitude (mag) |
| 109 | err_r | Error of r |
| 110 | i | XSTPS-GAC i-band magnitude (mag) |
| 111 | err_i | Error of i |
| 112 | J | 2MASS J-band magnitude (mag) |
| 113 | err_J | Error of J |
| 114 | H | 2MASS H-band magnitude (mag) |
| 115 | err_H | Error of H |
| 116 | Ks | 2MASS Ks-band magnitude (mag) |
| 117 | err_Ks | Error of Ks |
| 118 | w1 | WISEW1-band magnitude (mag) |
| 119 | err_w1 | Error of w1 |
| 120 | w2 | WISEW2-band magnitude (mag) |
| 121 | err_w2 | Error of w2 |
| 122 | w3 | WISEW3-band magnitude (mag) |
| 123 | err_w3 | Error of w3 |
| 124 | w4 | WISEW4-band magnitude (mag) |
| 125 | err_w4 | Error of w3 |
| 126 | ph_qual_2mass | 2MASS photometric quality flag |
| 127 | ph_qual_wise | WISE photometric quality flag |
| 128 | var_flag_wise | WISE variability flag |
| 129 | ext_flag_wise | WISE extended source flag |
| 130 | cc_flag_wise | WISE contamination and confusion flag |
| 131 | ebv_sfd | E(B − V) from the SFD extinction map (mag) |
| 132 | ebv_sp | E(B − V) derived from the star pair method (mag) |
| 133 | err_ebv_sp | Error of ebv_sp |
| 134 | ebv_mod | E(B − V) derived by comparing the observed and synthetic model atmosphere colours (mag) |
| 135 | ebv_phot | E(B − V) derived by fitting multiband photometry to the empirical stellar loci (Chen et al. 2014) (mag) |
| 136 | dist_em1 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the recommended atmospheric parameters | ||
| 137 | err_dist_em1 | Error of dist_em1 |
| 138 | dist_em2 | Distance derived using the empirical relations of absolute magnitudes as a function of stellar atmospheric |
| parameters as yielded by the MILES stars using the weighted-mean atmospheric parameters | ||
| 139 | err_dist_em2 | Error of dist_em2 |
| 140 | dist_sp1 | Distance inferred from absolute magnitudes estimated with KPCA method using 300 PCs (pc) |
| 141 | err_dist_sp1 | Error of dist_sp1 |
| 142 | dist_sp2 | Distance inferred from absolute magnitudes estimated with KPCA method using 100 PCs (pc) |
| 143 | err_dist_sp2 | Error of dist_sp2 |
| 144 | dist_phot | Distance derived from the photometric parallax method (Chen et al. 2014) (pc) |
| 145 | err_dist_phot | Error of dist_phot |
| 146 | pmra_ppmxl | Proper motion in RA from the PPMXL catalogues (mas yr−1) |
| 147 | epmra_ppmxl | Error of pmra_ppmxl |
| 148 | pmdec_ppmxl | Proper motion in Dec. from the PPMXL catalogues (mas yr−1) |
| 149 | epmdec_ppmxl | Error of pmdec_ppmxl |
| 150 | pmra_ucac4 | Proper motion in RA from the UCAC4 catalogues (mas yr−1) |
| 151 | epmra_ucac4 | Error of pmra_ucac4 |
| 152 | pmdec_ucac4 | Proper motion in Dec. from the UCAC4 catalogues (mas yr−1) |
| 153 | epmdec_ucac4 | Error of pmdec_ucac4 |
| 154 | pmra_xuyi2mass | Proper motion in RA derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 155 | pmdec_xuyi2mass | Proper motion in Dec. derived by comparing the XSTPS-GAC and 2MASS positions (mas yr−1) |
| 156 | x | x-coordinate in a Galactocentric Cartesian reference system, positive towards the Galactic Centre (kpc) |
| 157 | err_x | Error of x |
| 158 | y | y-coordinate in a Galactocentric Cartesian reference system, positive in the direction of disc rotation (kpc) |
| 159 | err_y | Error of y |
| 160 | z | z-coordinate in a Galactocentric Cartesian reference system, positive towards the North Galactic Pole (kpc) |
| 161 | err_z | Error of z |
| 162 | u[2] | Galactic space velocities in the x-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the Galactic Centre (km s−1) | ||
| 163 | err_u[2] | Error of u[2] |
| 164 | v[2] | Galactic space velocities in the y-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive in the direction of Galactic rotation (km s−1) | ||
| 165 | err_v[2] | Error of v[2] |
| 166 | w[2] | Galactic space velocities in the z-direction computed from dist_em and the corrected PPMXL and UCAC4 |
| proper motions, respectively, positive towards the north Galactic pole (km s−1) | ||
| 167 | err_w[2] | Error of w[2] |
| 168 | v_r[2] | Galactic space velocities in the r-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively (km s−1) | ||
| 169 | err_v_r[2] | Error of v_r[2] |
| 170 | v_phi[2] | Galactic space velocities in the Φ-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive in the direction of counter disc rotation (km s−1) | ||
| 171 | err_v_phi[2] | Error of v_phi[2] |
| 172 | v_z[2] | Galactic space velocities in the z-direction in a Galactocentric cylindrical polar coordinate system, |
| computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively, | ||
| positive towards the north Galactic pole (km s−1) | ||
| 173 | err_v_z[2] | Error of v_z[2] |
| 174 | e[2] | Orbital eccentricities computed from dist_em and the corrected PPMXL and UCAC4 proper motions, respectively |
| 175 | Rapo[2] | Maximum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 176 | Rperi[2] | Minimum Galactic radii reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 177 | zmin[2] | Minimum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
| 178 | zmax[2] | Maximum height reached by the orbits computed with PPMXL and UCAC4 proper motions, respectively (kpc) |
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