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10 results for “Stellar activity”
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>
Simulated Solar Spectra for Testing Stellar Activity Mitigation Strategies
<p>Recent and upcoming stabilized spectrographs are pushing the frontier for Doppler spectroscopy to detect and characterize low-mass planets. Specifications for these instruments are so impressive that intrinsic stellar variability is expected to limit their Doppler precision for most target stars (Fischer et al. 2016). In order to realize their full potential, astronomers must develop new strategies for distinguishing true Doppler shifts from intrinsic stellar variability. Stellar variability due to starspots, faculae, and other rotationally-linked variability is particularly concerning, as the stellar rotation period is often included in the range of potential planet orbital periods. In order to robustly detect and accurately characterize low-mass planets via Doppler planet surveys, the exoplanet community must develop statistical models capable of jointly modeling planetary perturbations and intrinsic stellar variability. Towards this effort, we present simulations of extremely high-resolution solar-like spectra created with SOAP 2.0(Dumusque et al. 2014) that includes multiple evolving starspots to aid in developing and testing future statistical methods.</p>
Photometric Activity Cycles in fast-rotating stars: Revisiting the reality of stellar activity cycle branches
<p>The provided files comprise the tables and Activity cycle fits presented in our manuscript titled "Photometric Activity Cycles in fast-rotating Stars". The files are denoted as Table 1 (main-sequence stars), Table 2 (RS CVn candidates) and a folder containing activity cycle fits for all main-sequence and RSCVn candidates listed in the aforementioned tables. DOI: <a href="https://doi.org/10.1093/mnras/staf754" target="_blank" rel="noopener">10.1093/mnras/staf754</a> </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>
Precise and efficient modeling of stellar-activity-affected solar spectra using SOAP-GPU
<p>The simulated spectral time series generated using SOAP-GPU is based on the extraction of active regions from Solar Dynamics Observatory (SDO) data. The positions of sunspots and faculae on the solar disk at each time step are obtained from magnetogram and intensity maps, which are then input into SOAP-GPU to simulate the corresponding spectra. Comparison with HARPS-N solar spectra demonstrates that SOAP-GPU can accurately model the solar RV time series with a precision of 0.9 m/s.</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>
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>
ScienceDex guides
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