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18 results for “LAMOST”
The stellar parameters and the quantities of the residual emissions of the detected active stars in the LAMOST-K2 survey
<p>The full Table 1 in <em>Investigation of stellar magnetic activity using variational autoencoder based on low-resolution spectroscopic survey</em> (Xiang, Gu & Cao, 2022, MNRAS, 514, 4781; <a href="https://arxiv.org/abs/2206.07257">arXiv:2206.07257</a>). The columns are LAMOST obsid, K2 ID, Teff, logg, [Fe/H], EW_res_Halpha, EW_res_Ca II 8498, EW_res_Ca II 8542, EW_res_Ca II 8662, log F_Halpha, log F_Ca, log R'_Halpha, log R'_Ca. The chromospheric emissions were detected and measured with the spectral subtraction technique, which removes the inactive template spectra (photospheric contribution) from the observed stellar spectra. In this work, we used the variational autoencoder neural networks to efficiently generate the proper template spectra in a data-driven manner. More details can be found in the associated paper (<a href="https://arxiv.org/abs/2206.07257">https://arxiv.org/abs/2206.07257</a>). The demo code can be found on GitHub (<a href="https://github.com/xylib/vae-for-spectroscopic-survey">https://github.com/xylib/vae-for-spectroscopic-survey</a>).</p>
2m Perek telescope images of symmetrical object LAMOST J053944.81+531825.7
<p>The pictures of the object LAMOST J053944.81+531825.7 showing the unusual symmetric triple star configuration and complex emission line profiles. Images were taken by newly commissioned photometric camera G2 Mark II 3200 of Ondrejov 2m Perek telescope in primary focus. Plate scale 0.2 arcsec /pixel . The whole field is 7x5 arcmin. The distance of both satellites from the central bright star is 6.7 arcsec. The zoomed composed image is 16x16arcsec in SDSS spectral filter g' (left) and r' (right).</p> <p>Exposure time 300 s. Observed on 15th April 2020, 19:13 and 19:19 UTC respectively.</p> <p>The same region was observed by PanSTARRS-1 in the years 2011 to 2014. See for reference <a href="https://ps1images.stsci.edu/cgi-bin/ps1cutouts?pos=05+39+44.81+%2B53+18+25.7">PS1 image web service</a></p>
Dynamical Parameters and Clustering Results for Four-hundred Very Metal-Poor Stars Studied with LAMOST and Subaru
<p>This is the data associated with the paper "Four-hundred Very Metal-Poor Stars Studied with LAMOST and Subaru. III. Dynamically Tagged Groups and Chemodynamical Properties" by Zhang, Matsuno, Li et al. 2024. Table "LSVMP_HRdata_dynamics.csv" contains the dynamical parameters and clustering results of the HR sample in this paper. File "readme.txt" describes the meaning of each column in the table and the notes for the flag of stars. </p> <p>This sample is obtained by the LAMOST/Subaru joint project. See our paper I (DOI: 10.3847/1538-4357/ac6515) for detailed descriptions of target selection and observations, paper II (DOI: 10.3847/1538-4357/ac6514) for the chemical abundance analysis, and paper III (DOI: 10.3847/1538-4357/ad31a6) for clustering and chemodynamical analysis.</p> <p>If you have any questions about this data, please contact lhn@nao.cas.cn or rz.richie.zhang@gmail.com for more information.</p>
LAMOST–Gaia–Kepler Stellar Kinematic catalog
<p>In the second part of the Planets Across the Space and Time (PAST) series, by combining the data from the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) DR4 and Gaia DR2 and then applying the revised kinematic methods from PAST I, we present a catalog of kinematic properties (i.e., Galactic positions, velocities, and the relative membership probabilities among the thin disk, thick disk, Hercules stream, and the halo) as well as other basic stellar parameters for 35,835 Kepler stars.</p> <p>The new version combing LAMOST DR8 and Gaia eDR3 will be released soon.</p>
Stellar chromospheric activity database of solar-like stars based on the Ca II H and K lines of LAMOST Low-Resolution Spectroscopic Survey: the bolometric and photospheric calibration
<p>This database contains the stellar chromospheric activity parameters of solar-like stars based on the Ca II H and K lines from the spectra of the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). We extract 1,122,495 LRS spectra of solar-like stars from the LAMOST Data Release 8 v2.0 and provide the chromospheric activity parameters $S_{\rm tri}$, $S_{\rm MWO}$, $R_{\rm HK}$ and $R'_{\rm HK}$, as well as their uncertainties in the database. $R_{\rm HK}$ and $R'_{\rm HK}$ are derived from the method in the classic literature (denoted with classic) and the method based on the PHOENIX model (denoted with PHOENIX). These stellar chromospheric activity indexes and their uncertainties, along with the relevant spectroscopic parameters from the LAMOST catalogs, are saved in a CSV-format file (name: CaIIHK_Activity_Indexes_LAMOST_DR8_LRS.csv).</p> <p> </p> <p>Columns in the catalog of the database:</p> <p>obsid - Unique observation identifier of LAMOST LRS spectrum</p> <p>obsdate-Spectral observation date</p> <p>fitsname - FITS file name of LAMOST LRS spectrum</p> <p>snrg - Signal-to-noise ratio in the $g$ band ($\mathrm{S/N}_g$) of LAMOST LRS spectrum</p> <p>snrr - Signal-to-noise ratio in the $r$ band ($\mathrm{S/N}_r$) of LAMOST LRS spectrum</p> <p>teff - Effective temperature ($T_\mathrm{eff}$) derived from the LASP (unit: K)</p> <p>teff_err - Uncertainty of $T_\mathrm{eff}$ derived from the LASP (unit: K)</p> <p>logg - Surface gravity ($\log\,g$) derived from the LASP (unit: dex)</p> <p>logg_err - Uncertainty of $\log\,g$ derived from the LASP (unit: dex)</p> <p>feh - Metallicity ([Fe/H]) derived from the LASP (unit: dex)</p> <p>feh_err - Uncertainty of [Fe/H] derived from the LASP (unit: dex)</p> <p>rv - Radial velocity ($V_r$) derived from the LASP (unit: km/s)</p> <p>rv_err - Uncertainty of $V_r$ derived from the LASP (unit: km/s)</p> <p>ra_obs - Right ascension (RA) of fiber pointing (unit: degree)</p> <p>dec_obs - Declination (DEC) of fiber pointing (unit: degree) </p> <p>gaia_source_id - Source identifier in Gaia DR3 catalog</p> <p>gaia_g_mean_mag - $G$ magnitude in Gaia DR3 catalog</p> <p>S_tri* - $S_{\rm tri}$ index of LAMOST LRS </p> <p>S_tri_err* - Uncertainty of $S_{\rm tri}$ </p> <p>S_MWO* - $S_{\rm MWO}$ </p> <p>S_MWO_err* - Uncertainty of $S_{\rm MWO}$ </p> <p>log_R_HK_classic* - $\log\,R_{\rm HK,classic}$ </p> <p>log_R_HK_classic_err* - Uncertainty of $\log\,R_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic* - $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_p_HK_classic_err* - Uncertainty of $\log\,R'_{\rm HK,classic}$ </p> <p>log_R_HK_PHOENIX* - $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_HK_PHOENIX_err* - Uncertainty of $\log\,R_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX* - $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>log_R_p_HK_PHOENIX_err* - Uncertainty of $\log\,R'_{\rm HK,PHOENIX}$ </p> <p>(Note: The columns denoted by an asterisk represent the parameters provided by this database, and the remaining columns are collected from the data release of LAMOST DR8 V2.0. If the values are not available, they will be filled with '-9999' in this database.)</p>
Dataset of hydrogen Balmer line indexes for stellar chromospheric activity of solar-like stars based on the LAMOST spectroscopic surveys
<p><span>This dataset consists of three catalogs of the data of the hydrogen Balmer line indexes of solar-like stars for stellar chromospheric activity based on the LAMOST Low-Resolution Spectroscopic Survey (LRS) and Medium-Resolution Spectroscopic Survey (MRS): (1) LRS spectral catalog, (2) MRS spectral catalog, and (3) stellar source catalog. These catalogs are stored as three CSV-format data files. The columns contained in the catalogs are described below. The observational and spectroscopic parameters of the spectral samples in the dataset are from LAMOST DR9 v2.0. Unavailable values in the dataset are marked as −9999.0.</span></p> <p><span> </span></p> <p><span>(1) LRS spectral catalog (Balmer_line_indexes_LRS_spectral_catalog_LAMOST_DR9.csv)</span></p> <p><span>obsid - unique LAMOST observation identifier of LRS</span></p> <p><span>obsdate - date of LRS observation (UTC)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source in LRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source in LRS catalog (unit: degree)</span></p> <p><span>sn_g - LRS g-band signal-to-noise ratio</span></p> <p><span>sn_r - LRS r-band signal-to-noise ratio</span></p> <p><span>teff - stellar effective temperature determined from LRS data (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity determined from LRS data (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity determined from LRS data (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>rv - radial velocity determined from LRS data (unit: km/s)</span></p> <p><span>rv_err - uncertainty of rv (unit: km/s)</span></p> <p><span>L_halpha - Hα activity index of LRS data</span></p> <p><span>L_halpha_err - uncertainty of L_halpha</span></p> <p><span>L_hbeta - Hβ activity index of LRS data</span></p> <p><span>L_hbeta_err - uncertainty of L_hbeta</span></p> <p><span>L_hgamma - Hγ activity index of LRS data</span></p> <p><span>L_hgamma_err - uncertainty of L_hgamma</span></p> <p><span>L_hdelta - Hδ activity index of LRS data</span></p> <p><span>L_hdelta_err - uncertainty of L_hdelta</span></p> <p><span> </span></p> <p><span>(2) MRS spectral catalog (Balmer_line_indexes_MRS_spectral_catalog_LAMOST_DR9.csv)</span></p> <p><span>obsid - unique LAMOST observation identifier of MRS</span></p> <p><span>obsdate - date of MRS observation (UTC)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source in MRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source in MRS catalog (unit: degree)</span></p> <p><span>sn_B - MRS blue-band signal-to-noise ratio</span></p> <p><span>sn_R - MRS red-band signal-to-noise ratio</span></p> <p><span>teff - stellar effective temperature determined from MRS data (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity determined from MRS data (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity determined from MRS data (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>rv_r0 - radial velocity determined from the red band data of MRS (unit: km/s)</span></p> <p><span>rv_r0_err - uncertainty of rv_r0 (unit: km/s)</span></p> <p><span>M_halpha – Hα activity index of MRS data</span></p> <p><span>M_halpha_err - uncertainty of M_halpha</span></p> <p><span> </span></p> <p><span>(3) stellar source catalog (Balmer_line_indexes_stellar_source_catalog_LAMOST_DR9.csv)</span></p> <p><span>uid - unique LAMOST source identifier</span></p> <p><span>ra - right ascension of stellar source from LRS catalog (unit: degree)</span></p> <p><span>dec - declination of stellar source from LRS catalog (unit: degree)</span></p> <p><span>teff - stellar effective temperature from LRS catalog (unit: K)</span></p> <p><span>teff_err - uncertainty of teff (unit: K)</span></p> <p><span>logg - stellar surface gravity from LRS catalog (unit: dex)</span></p> <p><span>logg_err - uncertainty of logg (unit: dex)</span></p> <p><span>feh - stellar metallicity from LRS catalog (unit: dex)</span></p> <p><span>feh_err - uncertainty of feh (unit: dex)</span></p> <p><span>L_halpha - Hα activity index of LRS data</span></p> <p><span>L_halpha_err - uncertainty of L_halpha</span></p> <p><span>L_hbeta - Hβ activity index of LRS data</span></p> <p><span>L_hbeta_err - uncertainty of L_hbeta</span></p> <p><span>L_hgamma - Hγ activity index of LRS data</span></p> <p><span>L_hgamma_err - uncertainty of L_hgamma</span></p> <p><span>L_hdelta - Hδ activity index of LRS data</span></p> <p><span>L_hdelta_err - uncertainty of L_hdelta</span></p> <p><span>M_halpha - Hα activity index of MRS data</span></p> <p><span>M_halpha_err - uncertainty of M_halpha</span></p> <p><span>l_halpha - Hα absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_halpha_err - uncertainty of l_halpha (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hbeta - Hβ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hbeta_err - uncertainty of l_hbeta (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hgamma - Hγ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hgamma_err - uncertainty of l_hgamma (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hdelta - Hδ absolute flux index of LRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>l_hdelta_err - uncertainty of l_hdelta (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>m_halpha</span><span> - Hα absolute flux index of MRS data (unit: 1/</span><span>Å</span><span>)</span></p> <p><span>m_halpha_err - uncertainty of m_halpha (unit: 1/</span><span>Å</span><span>)</span></p> <p><span> </span></p> <p><span> </span></p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey(disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with <em>T</em><sub>eff</sub> ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> using the rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> using the triangular bandpass, are evaluated based on the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p> <p> </p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey (disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with effective temperature ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> based on the 1 Å rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> based on the 1.09 Å FWHM triangular bandpass, are evaluated from the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p>
Stellar chromospheric activity spectral database of solar-type stars based on the LAMOST Low-Resolution Spectroscopic Survey(disused)
<p>A stellar chromospheric activity spectral database of solar-type stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains 1,330,654 high-quality LRS spectra of solar-type stars with effective temperature ranging from 4800 K to 6800 K. We measure the mean fluxes at line cores of the Ca II H&K lines using a 1 Å rectangular bandpass as well as a 1.09 Å full width at half maximum (FWHM) triangular bandpass, and the mean fluxes of two 20 Å pseudo-continuum bands on the two sides of the lines. Three chromospheric activity indexes, <em>S</em><sub>rec</sub> based on the 1 Å rectangular bandpass, and <em>S</em><sub>tri</sub> and <em>S</em><sub>MWL</sub> based on the 1.09 Å FWHM triangular bandpass, are evaluated from the measured fluxes. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H&K lines for all the spectra in the database. This database with more than one million high-quality LAMOST LRS spectra and basal chromospheric activity parameters can be further used for investigating activity characteristics of solar-type stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv</p> <p>(2) Library of Spectrum Diagrams<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-199.zip (49 subfolders)<br> spectrum_diagrams_200-249.zip (47 subfolders)<br> spectrum_diagrams_250-299.zip (45 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-399.zip (39 subfolders)<br> spectrum_diagrams_400-449.zip (45 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p>
Interesting spectra discovered by Active Deep Learning in LAMOST DR2
<p>PDF previews of interesting spectra found by Active Deep Learning in LAMOST DR2 spectra survey. These are referred to in an article Škoda,Podsztavek&Tvrdík "Active deep learning method for the discovery of objects of interest in large spectroscopic surveys" submitted to Astronomy and Astrophysics. Previews show both the whole LAMOST spectrum created from original FITS file and its zoomed part around Halpha line used for machine learning.</p>
Stellar chromospheric activity database of solar-like stars based on the LAMOST Low-Resolution Spectroscopic Survey
<p>A stellar chromospheric activity database of solar-like stars is constructed based on the Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) Low-Resolution Spectroscopic Survey (LRS). The database contains spectral bandpass fluxes and indexes of Ca II H and K lines derived from 1,330,654 high-quality LRS spectra of solar-like stars. We measure the mean fluxes at line cores of the Ca II H and K lines using a 1 Å rectangular bandpass and a 1.09 Å FWHM triangular bandpass, as well as the mean fluxes of two 20 Å wide pseudocontinuum bands on the two sides of the lines. Three activity indexes of Ca II H and K lines, <em>S</em><sub>rec</sub> based on the 1 Å rectangular bandpass and <em>S</em><sub>tri</sub> and <em>S<sub>L</sub></em> based on the 1.09 Å FWHM triangular bandpass, are evaluated from the measured fluxes to quantitatively indicate the chromospheric activity level. The uncertainties of all the obtained parameters are estimated. We also produce spectrum diagrams of Ca II H and K lines for all the spectra in the database. This database, with more than one million high-quality LAMOST LRS spectra of Ca II H and K lines and basal chromospheric activity parameters, can be further used for investigating activity characteristics of solar-like stars and solar-stellar connection.</p> <p> </p> <p>The entity of the database is composed of (1) a catalog of spectral sample and activity parameters, and (2) a library of spectrum diagrams of Ca II H and K lines.</p> <p>(1) Catalog of Spectral Sample and Activity Parameters<br> CaIIHK_Sindex_LAMOST_DR7_LRS.csv<br> (see Table3 in the paper 2022_ApJS_263_12 for description of the columns)</p> <p>(2) Library of Spectrum Diagrams of Ca II H and K lines<br> spectrum_diagrams_000-049.zip (46 subfolders)<br> spectrum_diagrams_050-099.zip (40 subfolders)<br> spectrum_diagrams_100-149.zip (47 subfolders)<br> spectrum_diagrams_150-174.zip (25 subfolders)<br> spectrum_diagrams_175-199.zip (24 subfolders)<br> spectrum_diagrams_200-224.zip (24 subfolders)<br> spectrum_diagrams_225-249.zip (23 subfolders)<br> spectrum_diagrams_250-259.zip (10 subfolders)<br> spectrum_diagrams_260-274.zip (12 subfolders)<br> spectrum_diagrams_275-299.zip (23 subfolders)<br> spectrum_diagrams_300-349.zip (41 subfolders)<br> spectrum_diagrams_350-374.zip (20 subfolders)<br> spectrum_diagrams_375-399.zip (19 subfolders)<br> spectrum_diagrams_400-424.zip (23 subfolders)<br> spectrum_diagrams_425-449.zip (22 subfolders)<br> spectrum_diagrams_450-499.zip (35 subfolders)<br> spectrum_diagrams_500-549.zip (27 subfolders)<br> spectrum_diagrams_550-599.zip (38 subfolders)<br> spectrum_diagrams_600-649.zip (32 subfolders)<br> spectrum_diagrams_650-699.zip (26 subfolders)<br> spectrum_diagrams_700-749.zip (28 subfolders)</p>
Dataset of H-alpha activity indices of F-, G-, and K-type stars observed by the LAMOST Medium-Resolution Spectroscopic Survey
<p>This dataset of H-alpha activity indices is for investigation of stellar H-alpha chromospheric activity based on the LAMOST Medium-Resolution Spectroscopic Survey (MRS). High signal-to-noise ratio MRS coadded spectra of F-, G-, and K-type stars (4000-7000 K) from LAMOST Data Release 8 are utilized in the dataset (329,294 spectra in total). The H-alpha activity index (I_halpha) and the H-alpha R-index (R_halpha) are evaluated for the MRS spectra. The values of the H-alpha indices and their uncertainties, as well as the related spectroscopic parameters from the LAMOST catalogs, are stored in a CSV-format file (file name: Halpha_activity_indices_LAMOST_MRS_DR8.csv).</p> <p> </p> <p>Columns included in the dataset:</p> <p>obsid - unique observation identifier of LAMOST MRS</p> <p>ra - right ascension of the observed object (unit: degree)</p> <p>dec - declination of the observed object (unit: degree)</p> <p>obsdate - UTC date of the observation (format: YYYY-MM-DD)</p> <p>fitsname - MRS FITS data file name</p> <p>sn_B - signal-to-noise ratio of the blue band of MRS</p> <p>sn_R - signal-to-noise ratio of the red band of MRS</p> <p>band_para - indicating which band of MRS is used by the LASP to determine the stellar atmospheric parameters; ‘B’ representing the blue band and ‘R’ representing the red band</p> <p>teff - effective temperature determined by the LASP (unit: K)</p> <p>teff_err - uncertainty of teff (unit: K)</p> <p>logg - surface gravity determined by the LASP (unit: dex)</p> <p>logg_err - uncertainty of logg (unit: dex)</p> <p>feh - metallicity determined by the LASP (unit: dex)</p> <p>feh_err - uncertainty of feh (unit: dex)</p> <p>rv_r0 - radial velocity determined based on the red band data of MRS (unit: km/s)</p> <p>rv_r0_err - uncertainty of rv_r0 (unit: km/s)</p> <p>category* - ‘main-sequence’ or ‘giant’ or ‘intermediate-zone’</p> <p>I_halpha* - H-alpha activity index</p> <p>I_halpha_err* - uncertainty of I_halpha</p> <p>chi* - χ factor for calculating R_halpha from I_halpha (unit: 1/Å)</p> <p>chi_err* - uncertainty of chi (unit: 1/Å)</p> <p>R_halpha* - H-alpha R-index</p> <p>R_halpha_err* - uncertainty of R_halpha</p> <p>(Note: The columns marked with an asterisk are provided by this dataset. Other columns are from the catalogs of LAMOST DR8 v1.1. LASP is an acronym for the LAMOST Stellar Parameter Pipeline. A value of -9999.0 in the dataset indicates that it is not available.)</p> <p> </p> <p> </p>
Hot subdwarf stars observed in Gaia DR2 and LAMOST DR5
<p>Table2.txt: Atmospheric parameters and space positions for 892 non-composite spectra hot subdwarf stars selected from Gaia DR2 and LAMOST DR5.</p> <p>Table3.txt: Orbital parameters, galactic velocities for 747 hot subdwarf stars selected from Gaia DR2 and LAMOST DR5</p>
Tables of Emission Line Spectra discovered by Active Deep Learning in LAMOST DR2
<p>Tables of emission line spectra discovered by Active Deep Learning in LAMOST DR2 spectra survey. These are referred to in an article Škoda,Podsztavek&Tvrdík "Active deep learning method for the discovery of objects of interest in large spectroscopic surveys" submitted to Astronomy and Astrophysics.</p> <p>The zipped files contain both CSV and VOTable formats, the HTML version may be opened directly in a browser. A link to an interactive spectrum plot at Strasbourg datacenter (CDS) Vizier archive may be activated from it as well in most common browsers.</p> <p>The detailed description of tables is in attached README file.</p>
LAMOST RVM and wavelength data.
<p>LAMOST RVM and wavelength data.</p>
Search-for-Barium-Candidates-in-LAMOST-using-the-MEASNet-model
<p>This repository is for the paper MEASNet: A Model for Barium Stars Identification and s-process Abundance Estimation from LAMOST DR10 Low-resolution Survey. I. by Shengjun Song. It is associated with the manuscript number AAS51558.</p>
Stellar Parameter Estimation for Half a Million LAMOST M Dwarfs based on Cycle-StarNet
Open the record for dataset details and reuse information.
Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement
<p>MESA (r12115) inlist files used in the preparation of the paper "Age of FGK Dwarfs Observed with LAMOST and GALAH: Considering the Oxygen Enhancement ".</p> <p>The '<a href="https://zenodo.org/api/files/7cd5636b-f6f5-4baa-be00-b248a0a93018/inlist_project_MIST_sun">inlist_project_MIST_sun</a>' file evolves the model from pre-main sequence to the TAMS '. </p> <p>This '<a href="https://zenodo.org/api/files/7cd5636b-f6f5-4baa-be00-b248a0a93018/inlist_project_MIST_sun">inlist_project_MIST_sun</a>' file is an example file for an O-enhanced stellar model, with an input [α/Fe] value of 0.1 and a [O/Fe] value of 0.5. We use a Python code to drive the calculations of the stellar model grid, by modifying the initial y and z values, as well as the initial mass of the '<a href="https://zenodo.org/api/files/7cd5636b-f6f5-4baa-be00-b248a0a93018/inlist_project_MIST_sun">inlist_project_MIST</a>' file, to obtain the '<a href="https://zenodo.org/api/files/7cd5636b-f6f5-4baa-be00-b248a0a93018/inlist_project_MIST_sun">inlist_project_MIST_sun</a>' file.</p>
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