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23 results for “Spectroscopic survey”
HETDEX Public Source Catalog 1: 220 K Sources including over 50K Lyman Alpha Emitters From an Untargeted Wide-area Spectroscopic Survey
<p>We present the first publicly released catalog of sources obtained from the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). HETDEX is an integral field spectroscopic survey designed to measure the Hubble expansion parameter and angular diameter distance at 1.88 < z < 3.52 by using the spatial distribution of more than a million Lyα-emitting galaxies over a total target area of 540 deg2. The catalog comes from contiguous fiber spectra coverage of 25 deg2 of sky from January 2017 through June 2020, where object detection is performed through two complementary detection methods: one designed to search for line emission and the other a search for continuum emission. The HETDEX public release catalog is dominated by emission-line galaxies and includes 51,863 Lyα-emitting galaxy (LAE) identifications and 123,891 [O II]-emitting galaxies at z < 0.5. Also included in the catalog are 37,916 stars, 5,274 low-redshift (z < 0.5) galaxies without emission lines, and 4,976 active galactic nuclei. The catalog provides sky coordinates, redshifts, line identifications, classification information, line fluxes, [O II] and Lyα line luminosities where applicable, and spectra for all identified sources processed by the HETDEX detection pipeline. Extensive testing demonstrates that HETDEX redshifts agree to within ∆z < 0.02, 96.1% of the time to those in external spectroscopic catalogs. We measure the photometric counterpart fraction in deep ancillary Hyper Suprime-Cam imaging and find that only 55.5% of the LAE sample has an r-band continuum counterpart down to a limiting magnitude of r ∼ 26.2 mag (AB) indicating that an LAE search of similar sensitivity with photometric pre-selection would miss nearly half of the HETDEX LAE catalog sample.<br> <br> Two catalogs make up HETDEX Source Catalog 1:<br> <br> 1. The Source Observation Table: hetdex_sc1_vX.dat/.fits/.ecsv<br> With SPECTRA arrays included: hetdex_sc1_spec_vX.fits<br> <br> One row per source observation. The table provides basic coordinates/redshift/source information for each observation of a unique astornomical source. The larger file hetdex_sc1_spec_vX.fits contains the same info from the first table plus addition data units of spectral array data.<br> <br> 2. The Detection Information Table: hetdex_sc1_detinfo_vX.fits<br> One row per line or continuum detection. Bright sources can be comprised of multiple line or continuum emission. This catalog provides specific detection information such as line parameter info (S/N, line flux, line width)<br> <br> 3. Jupyter Notebook with access example: HETDEX_source_catalog_1.ipynb/.pdf/.html</p> <p>We request that the following acknowledgement be included in any paper using data or software from HETDEX public data releases:</p> <blockquote> <p>HETDEX is led by the University of Texas at Austin McDonald Observatory and Department of Astronomy with participation from the Ludwig-Maximilians-Universität München, Max-Planck-Institut für Extraterrestrische Physik (MPE), Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Pennsylvania State University, Institut für Astrophysik Göttingen, The University of Oxford, Max-Planck-Institut für Astrophysik (MPA), The University of Tokyo and Missouri University of Science and Technology.</p> <p>Observations for HETDEX were obtained with the Hobby-Eberly Telescope (HET), which is a joint project of the University of Texas at Austin, the Pennsylvania State University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly. The Visible Integral-field Replicable Unit Spectrograph (VIRUS) was used for HETDEX observations. VIRUS is a joint project of the University of Texas at Austin, Leibniz-Institut für Astrophysik Potsdam (AIP), Texas A&M University, Max-Planck-Institut fürExtraterrestrische Physik (MPE), Ludwig-Maximilians-Universität München, Pennsylvania State University, Institut für Astrophysik Göttingen, University of Oxford, and the Max-Planck-Institut fur Astrophysik (MPA).</p> <p>Funding for HETDEX has been provided by the partner institutions, the National Science Foundation, the State of Texas, the US Air Force, and by generous support from private individuals and foundations.</p> </blockquote> <p> </p>
Selection function for spectroscopic surveys (main set).
<p>Selection function values for large spectroscopic surveys. Supplementary material for A&A paper Minst&Hekker 2018 (https://ui.adsabs.harvard.edu/#abs/2018arXiv181012296M/abstract). Main set (all stars in each survey)</p>
JWST Advanced Deep Extragalactic Survey: Thumbnail Images of Spectroscopically-Confirmed Galaxies at z>10.
<p>JWST NIRCam FITS image thumbnails for the spectroscopically-confirmed high-redshift galaxy sample in Robertson et al., arXiv:2212.04480. The tar file expands into the following directories:</p> <p>JADES-GS-z10-0/</p> <p>JADES-GS-z11-0/</p> <p>JADES-GS-z12-0/</p> <p>JADES-GS-z13-0/</p> <p>Each directory contains the F090W, F115W, F150W, F200W, F277W, F335M, F356W, F410M, and F444W FITS images of the galaxies. The FITS headers contain information about the observations, the units of the data, and the locations of the objects on the sky.</p>
Data and software: 'Survey Operations for the Dark Energy Spectroscopic Instrument'
<p>Supplementary material to the DESI publication "Survey Operations for the Dark Energy Spectroscopic Instrument".</p><p>The main "figures.py" script generates the figures in the paper from the included data files. The software relies on the DESI software stack available at github.com/desihub, and conveniently available at NERSC in the default DESI environment.</p><p>Some documentation on the code implementing the survey and for running the survey simulations is available here:</p><ul><li>https://desisurvey.readthedocs.io/en/latest/</li><li>https://surveysim.readthedocs.io/en/latest/</li></ul><p>Contents:</p><ul><li>Configuration files<ul><li>config-main-actual.yaml: a yaml file giving the configuration for the survey simulation software (https://github.com/desihub/surveysim/releases/tag/0.12.5), specifying things like interexposure times and downtime, using the actual long shutdowns we had.</li><li>config-main-nominal.yaml: a yaml file giving the configuration for the survey simulation software, using the nominal long shutdowns we planned for.</li><li>config-main.yaml: same as config-main-nominal.yaml, except with the default name looked for by the survey simulation software.</li><li>rules-main.yaml: configuration rules file controlling how the next tile selector selects files for observation, implementing our depth-first strategy.</li></ul></li><li>Software files<ul><li>figures.py: main routines for generating the plots in this publication. Running `python figures.py` will create all of the figures used in this paper.</li><li>precess.py: set of routines implementing the precession of the Earth's pole used by figures.py for accurate airmass calculations.</li><li>downtime.py: routines used by figures.py for computing statistics about DESI's time usage, in particular the downtime.</li><li>util_efs.py: utility routines, primarily for making plots used by figures.py</li><li>util_efs_c.pyx: cython routines used by util_efs.py</li><li>margincomputations.py: routines for computing survey margin; i.e., how well we did relative to how much time was available.</li></ul></li><li>Data files<ul><li>Survey<ul><li>exposures-daily-main-20220614.ecsv: list of main survey exposures taken through 2022-06-14, following processing by the offline pipeline.</li><li>exposures-20220614.ecsv: list of main survey exposures taken through 2022-06-14, before processing by the offline pipeline. This largely duplicates exposures-daily, but contains much less information and contains more records for rare cases when exposures cannot be processed by the offline pipeline.</li><li>tiles-4112-packing-20210405-decorated-fixed.fits: file giving the geometry of DESI tile centers on the sky, plus associated information, like the extinction and stellar density at those locations.</li><li>tiles-daily.csv</li></ul></li><li>Simulation<ul><li>ephem_2019-01-01_2027-12-31.fits: ephemerides for DESI site for 2019 through 2027, generated by the desisurvey software ephemerides module. https://github.com/desihub/desisurvey</li><li>desi-status-end-nominal.ecsv: tile file giving completion of each DESI tile, for a survey simulation using the nominal configuration file.</li><li>desi-status-end-actual-noslew.ecsv: tile file giving completion of each DESI tile, for a survey simulation using the actual configuration file, without slew optimization</li><li>desi-status-end-actual.ecsv: tile file giving the completion of each DESI tile, for a survey simulation using the actual configuration file.</li><li>exposures_actual-noslew.fits: exposures generated by survey simulation software using the 'actual' configuration, with slew optimization disabled.</li><li>exposures_actual.fits: exposures file generated by survey simulation software using the 'actual' configuration.</li><li>exposures_nominal.fits: exposures file generated by survey simulation software using the 'nominal' configuration.</li><li>stats_actual.fits: statistics file generated by survey simulation software using the 'actual' configuration, containing information about DESI time usage.</li><li>stats_actual-noslew.fits: same as stats_actual.fits, except with slew time optimization disabled.</li><li>stats_nominal.fits: same as stats_actual.fits, except with the nominal survey sim configuration file.</li><li>tiles-daily.csv: tile file with detailed information on all tiles completed by the survey</li><li>tiles-main-20220614.ecsv: tile file with tile completeness information on 20220614</li><li>tiles-main.ecsv: tile file with completeness information on tiles in the survey</li><li>performance_current.csv.gz: performance information detailing state of DESI instrument every second, used for tracking downtime statistics.</li></ul></li></ul></li></ul><p>Dependencies: The included software uses the 'surveysim,' 'desisurvey,' and 'desimodel' packages, available on github through the desihub organization. Otherwise it depends on the usual astronomy software stack: numpy scipy matplotlib astropy. Alternatively, people with access to NERSC can load the default DESI environment and pull in all needed dependencies.</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>
Archetype-Based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
<p>Supplementary material to DESI's publication "Archetype-Based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey" by Anand et al. 2024 to comply with the data management plan. The material includes all the data shown in the figures of the results of the paper.</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>
MMT/Binospec Spectroscopic Survey of Two z~0.8 Galaxy Clusters: Galaxy Spectra Figures and FITS Data
<p>This dataset includes MMT/Binospec spectra of all 371 galaxies observed in 2019 and 2022, which were already discussed in the research paper (J. Di et al.) where you just got this dataset link. To quickly look at our spectra, we reduced our spectra in the JPG format. We also attached the raw FITS format 1D and 2D spectra of two years' observations.</p>
The mock samples for high-z spectroscopic galaxy survey
<p>The mock samples for high-z spectroscopic galaxy survey. The dataset includes zCOSMOS, VIPERS and PFS-like galaxy survey's mock samples. The final design of PFS galaxy survey is not determined. So if you want to get the PFS-like mocks, please contact meng.jiacheng@foxmail.com or go to https://lig.astro.tsinghua.edu.cn/astrodata.</p> <p>The files named as "lu14_zcosmos_mock_index.h5df" are mocks for zCOSMOS survey. The files named as "lu14_w1_mock_index.h5df" and "lu14_w4_mock_index.h5df" are mocks for VIPERS survey, where "w1" and "w4" represent the two fields of VIPERS survey. Index is from 0 to19, representing the 20 mocks with different direction of line-of-sight when constructing mocks. The meanings of the keys in hdf5 files are as follows:</p> <ul> <li>"ra" and "dec": coordiantes;</li> <li>"z_spec" and "z_phot": spectroscopic redshift and photometric redshift;</li> <li>"stellar_mass": stellar mass;</li> <li>"sfr": star formation rate;</li> <li>"halo_mass": halo mass;</li> <li>"group_index": ID of the galaxy group for the given galaxy;</li> <li>"central_flag": 1 for central galaxy, 0 for satellite galaxy;</li> <li>"m_*": apparent magnitude;</li> <li>"M_*": absolute magnitude;</li> <li>"flag": 0 for no observation, 1 for galaxy having spectroscopic redshift, others for galaxy only having photometric redshift;</li> <li>"snap": the snapshot of the model galaxy;</li> <li>"model_index": the ID of the model galaxy;</li> <li>"box_index": the box ID where the model galaxy are in when constructing mocks.</li> </ul>
Spitzer Extragalactic First Look Survey SDSS Spectroscopic Catalog
The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared. This catalog presents the SDSS spectroscopic information from Papovich et al. (2006).
SMALL MAIN-BELT ASTEROID SPECTROSCOPIC SURVEY, PHASE II
This data set contains visible-wavelength (0.435-0.925 micron) spectra for 1341 main-belt asteroids observed during the second phase of the Small Main-belt Asteroid Spectroscopic Survey (SMASSII) between August 1993 and March 1999. The purpose of the SMASSII survey was to provide a new basis for studying the compositional diversity and structure of the asteroid belt. Based on experiences gained from the earlier SMASS survey, SMASSII focused on producing an even larger, internally consistent set of CCD spectra for small (D < 20 km) main-belt asteroids. The observing strategies and procedures used during SMASSII roughly parallel those used in the first survey (Xu et al. Icarus 115 1-35, 1995 [XUETAL1995]), though several minor changes were made in instrumentation and in portions of the data reduction process.
SMALL SOLAR SYSTEM OBJECTS SPECTROSCOPIC SURVEY V1.0
This dataset contains the visible spectra of 820 asteroids obtained between November 1996 and May 2001 at the 1.52m telescope at ESO (La Silla). The useful spectral range is between about 4900 and 9200 Angstroms. The global spatial distribution of the objects covers the region between 2.2 and 3.3 AU. Some concentrations are apparent, since part of the survey was focused on particuarly interesting groups or families of asteroids. The observed asteroids have been classified according to the Tholen and the Bus taxonomies, with a good agreement between both in most of the cases.
Spitzer Extragalactic First Look Survey MMT/Hectospec Spectroscopic Catalog
The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared. This catalog allows advanced queries of the MMT/Hectospec ancillary spectra described in Papovich et al. (2006).
Small Main-Belt Asteroid Spectroscopic Survey, Phase II V1.0
This data set contains visible-wavelength (0.435-0.925 micron) spectra for 1341 main-belt asteroids observed during the second phase of the Small Main-belt Asteroid Spectroscopic Survey (SMASSII) between August 1993 and March 1999. The purpose of the SMASSII survey was to provide a new basis for studying the compositional diversity and structure of the asteroid belt. Based on experiences gained from the earlier SMASS survey, SMASSII focused on producing an even larger, internally consistent set of CCD spectra for small (D < 20 km) main-belt asteroids. The observing strategies and procedures used during SMASSII roughly parallel those used in the first survey (Xu et al. Icarus 115 1-35, 1995), though several minor changes were made in instrumentation and in portions of the data reduction process.
Spitzer Extragalactic First Look Survey WIYN/Hydra Spectroscopic Catalog
The Extragalactic First Look Survey is composed of 4 square degrees of imaging with MIPS and IRAC centered at J1718+5930, with extensive ancillary data from ground-based optical and radio telescopes. As one of the first observations made with Spitzer after the completion of Science Verification at the end of 2003 November, the aim of this 67 hr survey was to characterize the extragalactic source populations observed with Spitzer down to sub-millijansky levels in the mid-infrared. This catalog presents data on the WIYN/Hydra spectra described in Marleau et al. (2007).
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These curated guides explain access requirements, typical timelines, costs, and reuse considerations for widely used research datasets.
Allen Brain Atlas
Allen Brain Atlas is an Allen Institute collection of brain map atlases, datasets, APIs, and analysis tools covering mouse, human, and non-human primate brain resources.
Annotated Behaviour and Observability Dataset (ABODe)
ABODe is a University of Edinburgh DataShare dataset for behavior classification in group-housed mice using home-cage video, identities, bounding boxes, ground-plate positions, and annotator labels.
DANDI Archive for NWB datasets
DANDI is a BRAIN Initiative archive for publishing and sharing neurophysiology data, including electrophysiology, optophysiology, and behavioral data packaged as NWB and related standards.
International Brain Laboratory public data
The International Brain Laboratory public data releases expose standardized mouse decision-making experiments, including Neuropixels recordings, widefield calcium imaging, behavior, and session metadata accessed through the ONE API.
OpenNeuro
OpenNeuro is a free, open platform for sharing neuroimaging datasets, with public search, dataset pages, and download paths for web, S3, DataLad, and the OpenNeuro CLI.