Detection of a time-variable relativistic UV outflow at velocities up to 0.3c in quasar J2318, with estimated mass-loss rate and kinetic luminosity above typical feedback thresholds.
The Eighth Data Release of the Sloan Digital Sky Survey: First Data from SDSS-III
6 Pith papers cite this work. Polarity classification is still indexing.
6
Pith papers citing it
abstract
The Sloan Digital Sky Survey (SDSS) started a new phase in August 2008, with new instrumentation and new surveys focused on Galactic structure and chemical evolution, measurements of the baryon oscillation feature in the clustering of galaxies and the quasar Ly alpha forest, and a radial velocity search for planets around ~8000 stars. This paper describes the first data release of SDSS-III (and the eighth counting from the beginning of the SDSS). The release includes five-band imaging of roughly 5200 deg^2 in the Southern Galactic Cap, bringing the total footprint of the SDSS imaging to 14,555 deg^2, or over a third of the Celestial Sphere. All the imaging data have been reprocessed with an improved sky-subtraction algorithm and a final, self-consistent photometric recalibration and flat-field determination. This release also includes all data from the second phase of the Sloan Extension for Galactic Understanding and Evolution (SEGUE-2), consisting of spectroscopy of approximately 118,000 stars at both high and low Galactic latitudes. All the more than half a million stellar spectra obtained with the SDSS spectrograph have been reprocessed through an improved stellar parameters pipeline, which has better determination of metallicity for high metallicity stars.
representative citing papers
At fixed stellar mass, inner gas mass—not size, SFR, or potential—best predicts gas metallicity, and differences in long-term inflow histories can explain the pattern.
DESI DR1 yields 314k high-mass and 9.6k dwarf AGN, extending the M_BH-M_star relation to log M_star ~7.8 and suggesting two evolutionary pathways for galaxies and black holes.
EP250905a is best explained as a mildly off-axis structured-jet afterglow at z=2.714, possibly weakly magnified by a foreground galaxy at z=0.374.
MSFA-Net applies multi-scale convolutions and soft frequency attention to LAMOST spectra, achieving high-precision BHB identification and adding 3583 new candidates to the catalog.
Asteroid 2024 YR4 has a 19.46-minute rotation period, Sq or K taxonomy, and absolute magnitude H_V of 24.14 with a shallow phase curve slope of G=0.51.
citing papers explorer
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A New Member of the Fast and Furious Family: A Relativistic and Time-Variable UV Outflow in a Luminous Quasar
Detection of a time-variable relativistic UV outflow at velocities up to 0.3c in quasar J2318, with estimated mass-loss rate and kinetic luminosity above typical feedback thresholds.
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Beyond the Fundamental Metallicity Relation: galaxy sizes encode the link between inflow and metallicity
At fixed stellar mass, inner gas mass—not size, SFR, or potential—best predicts gas metallicity, and differences in long-term inflow histories can explain the pattern.
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A New Record Census of Dwarf AGN and a Bimodal $M_{\rm BH}$-$M_{\star}$ Scaling Relation with DESI DR1
DESI DR1 yields 314k high-mass and 9.6k dwarf AGN, extending the M_BH-M_star relation to log M_star ~7.8 and suggesting two evolutionary pathways for galaxies and black holes.
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Multi-wavelength Constraints on the Transient EP250905a
EP250905a is best explained as a mildly off-axis structured-jet afterglow at z=2.714, possibly weakly magnified by a foreground galaxy at z=0.374.
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MSFA-Net: An Advanced Deep Learning Model for Identifying Blue Horizontal-Branch Stars from LAMOST DR12
MSFA-Net applies multi-scale convolutions and soft frequency attention to LAMOST spectra, achieving high-precision BHB identification and adding 3583 new candidates to the catalog.
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Rapid-response characterization of near-Earth asteroid 2024 YR4 during a Torino Scale 3 alert
Asteroid 2024 YR4 has a 19.46-minute rotation period, Sq or K taxonomy, and absolute magnitude H_V of 24.14 with a shallow phase curve slope of G=0.51.