The Apache Point Observatory Galactic Evolution Experiment (APOGEE) will undertake an H-band (1.52-1.68 micron) spectroscopic survey of 1E5 red giant stars spanning the Galactic disk, bulge, and halo, with typical limiting magnitude H 12.5. During the commissioning of APOGEE a number of plates containing stellar clusters were observed. Some of

Context. Siphon flows that are driven by a gas pressure difference between two photospheric footpoints of different magnetic field strength connected by magnetic field lines are a well-studied phenomenon in theory, but observational evidence is scarce. Aims. We investigate the properties of a structure in the solar chromosphere in an active region

We analysed the longest phase-connected photometric data set available for NGC 1313 X-2, looking for the ˜6-day modulation reported by Liu et al.. The folded B-band light curve shows a ˜6-day periodicity with a significance slightly larger than 3σ. The low statistical significance of this modulation, along with the lack of detection in the V band

The Sloan Digital Sky Survey III/Apache Point Observatory Galactic Evolution Experiment (SDSS-III/APOGEE) is a large-scale spectroscopic survey of Galactic stars and star clusters. The SDSS-III/APOGEE survey is designed to produce high-S/N, R = 22,500 spectra that cover a wavelength range of 1.51 to 1.68 microns. By utilizing APOGEE's excellent

The Sloan Digital Sky Survey III/Apache Point Observatory Galactic Evolution Experiment (SDSS-III/APOGEE) is a high resolution H-band (1.51-1.68 μ) spectroscopic survey covering all Galactic populations within the Milky Way. During the survey's three-year lifetime, we plan to target 100,000 Galactic stars, mostly red giants, from within the disk

With the aim of investigating galaxies with two strong simultaneous starbursts, we have extracted a sample of galaxies with double-peaked emission lines in their global spectra from the Sloan Digital Sky Survey (SDSS) spectral data base. We then fitted the emission lines Hα, Hβ, [O III]λ5007, [N II]λ6584, [S II]λ6717 and [S II]λ6731 of 129 spectra