The Sloan Digital Sky Survey (SDSS) will provide the data to support detailed investigations of the distribution of luminous and nonluminous matter in the universe: a photometrically and astrometrically calibrated digital imaging survey of π sr above about Galactic latitude 30° in five broad optical bands to a depth of g' ~ 23 mag, and a spectroscopic survey of the approximately 106 brightest galaxies and 105 brightest quasars found in the photometric object catalog produced by the imaging survey. This paper summarizes the observational parameters and data products of the SDSS and serves as an introduction to extensive technical on-line documentation.

https://iopscience.iop.org/article/10.1086/301513/pdf

The Sloan Digital Sky Survey: Technical summary

The Sloan Digital Sky Survey (SDSS) will provide the data to support detailed investigations of the distribution of luminous and non- luminous matter in the Universe: a photometrically and astrometrically calibrated digital imaging survey of pi steradians above about Galactic latitude 30 degrees in five broad optical bands to a depth of g' about 23 magnitudes, and a spectroscopic survey of the approximately one million brightest galaxies and 10^5 brightest quasars found in the photometric object catalog produced by the imaging survey. This paper summarizes the observational parameters and data products of the SDSS, and serves as an introduction to extensive technical on-line documentation.

The Sloan Digital Sky Survey: Technical Summary

The Swift mission, scheduled for launch in 2004, is a multiwavelength observatory for gamma-ray burst (GRB) astronomy. It is a first-of-its-kind autonomous rapid-slewing satellite for transient astronomy and pioneers the way for future rapid-reaction and multiwavelength missions. It will be far more powerful than any previous GRB mission, observing more than 100 bursts yr � 1 and performing detailed X-ray and UV/optical afterglow observations spanning timescales from 1 minute to several days after the burst. The objectives are to (1) determine the origin of GRBs, (2) classify GRBs and search for new types, (3) study the interaction of the ultrarelativistic outflows of GRBs with their surrounding medium, and (4) use GRBs to study the early universe out to z >10. The mission is being developed by a NASA-led international collaboration. It will carry three instruments: a newgeneration wide-field gamma-ray (15‐150 keV) detector that will detect bursts, calculate 1 0 ‐4 0 positions, and trigger autonomous spacecraft slews; a narrow-field X-ray telescope that will give 5 00 positions and perform spectroscopy in the 0.2‐10 keV band; and a narrow-field UV/optical telescope that will operate in the 170‐ 600 nm band and provide 0B3 positions and optical finding charts. Redshift determinations will be made for most bursts. In addition to the primary GRB science, the mission will perform a hard X-ray survey to a sensitivity of � 1m crab (� 2;10 � 11 ergs cm � 2 s � 1 in the 15‐150 keV band), more than an order of magnitude better than HEAO 1 A-4. A flexible data and operations system will allow rapid follow-up observations of all types of

/pdf/the-swift-gamma-ray-burst-mission-4u7rpzic8d.pdf

The Swift Gamma-Ray Burst Mission

Final published version including significant revisions. Twenty four pages, fourteen figures. Original version April 2006; final version published in MNRAS August 2007

/pdf/the-ukirt-infrared-deep-sky-survey-ukidss-3x4ktxmdiw.pdf

The UKIRT Infrared Deep Sky Survey (UKIDSS)

Supermassive black holes (BHs) have been found in 85 galaxies by dynamical modeling of spatially resolved kinematics. The Hubble Space Telescope revolutionized BH research by advancing the subject from its proof-of-concept phase into quantitative studies of BH demographics. Most influential was the discovery of a tight correlation between BH mass and the velocity dispersion σ of the bulge component of the host galaxy. Together with similar correlations with bulge luminosity and mass, this led to the widespread belief that BHs and bulges coevolve by regulating each other's growth. Conclusions based on one set of correlations from in brightest cluster ellipticals to in the smallest galaxies dominated BH work for more than a decade. New results are now replacing this simple story with a richer and more plausible picture in which BHs correlate differently with different galaxy components. A reasonable aim is to use this progress to refine our understanding of BH-galaxy coevolution. BHs with masses of 105−106M...

https://www.annualreviews.org/doi/suppl/10.1146/annurev-astro-082708-101811/suppl_file/aa51_kormendy_supmat.pdf

Coevolution (Or Not) of Supermassive Black Holes and Host Galaxies

Widespread methane precipitation on Titan has been predicted by several authors since methane saturation in the upper troposphere was measured by the Huygens probe over its landing site. Recently, observational evidence of widespread morning drizzle has been suggested based on detection of a dark morning site in surface-subtracted 2 μm spectroimages obtained from ground-based observations. We have obtained similar new spectroimages of Titan observed at Gemini-North Observatory at several rotational phase angles and have analyzed them using the same image processing technique. By comparing images at different phases, we show that the presumed dark drizzling regions in the surface-subtracted images are mainly negative renditions of bright surface regions. No evidence of spectroscopically verifiable drizzling is apparent in our cloudless Titan images. At present, constraining models of Titan's hydrological cycle to produce a diurnal response would be premature.

/pdf/no-evidence-of-morning-or-large-scale-drizzle-on-titan-3diepxea02.pdf

No evidence of morning or large-scale drizzle on titan

Searches for the R(O) line of the CH4v3 band at 3.3 μm give CH4/CO ≤3.3 x 10−2 in AFGL 961 (Rosette Nebula) and ≤2.4 x 10−3 in AFGL 989 (NGC 2264). The results are consistent with ion-molecule models, but the observations may not sample regions where gas-grain effects could enhance methane abundances.

Search for interstellar methane

A search for H line emission, reported to have been detected toward the young star HD 141569A and possibly originating in a clump of planet-forming gas orbiting the star, has yielded negative results. Observations made at the United Kingdom Infrared Telescope and the Subaru Telescope during 2001-2005 covered 11 major transitions of H from 3.42 to 3.99 μm. No H emission lines were detected; one marginal detection at 3.9855 μm in 2002 June was not confirmed in later spectra. The upper limits to the line strengths were significantly lower than the previously reported detections. Supplemental slit-scanning spectroscopy using adaptive optics was performed within 038 of HD 141569A to search for extended emission from H, but no emission was detected. We compare our upper limit to the luminosity in H from HD 141569A with that possible from a gas giant protoplanet and also from a jovian mass exoplanet in close orbit about its central star.

https://iopscience.iop.org/article/10.1086/430754/pdf

Search for h~3^+ in hd 141569a

We present near-infrared spectroscopy and unified atmosphere/wind models of the brightest He I 2.058 μm emission line star (hereafter denoted AF) in the Galactic center. The near-infrared spectrum of this star exhibits broad emission lines of He I and H, with the strongest line at 2.058 μm showing shallow P-Cygni absorption, strengthening the stellar wind interpretation for the origin of the lines. None of the higher excitation lines typical of classical Wolf-Rayet stars are detected. From the atmosphere models we conclude that the star is undergoing extensive mass loss (M˙∼6 to 10×10 −5 M ○. yr −1 ), has a luminosity of 2 to 3 10 5 L ○. , a moderate end velocity (V∞∼700 km s −1 ) and a strongly enhanced helium abundance (N He /N H >.5)

The nature of the brightest galactic center He I emission line star

/pdf/near-infrared-spectroscopy-of-supernova-2017eaw-in-2017-53alcly7kh.pdf

Near-infrared Spectroscopy of Supernova 2017eaw in 2017: Carbon Monoxide and Dust Formation in a Type II-P Supernova

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