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

We present late-time IR (1-5 mu m) and optical observations of the type IIn SN 1998S up to about 1200 days post-explosion. The shape and evolution of the Ho, and HeI 1.083 mu m line profiles indicate a powerful interaction with a massive progenitor wind and provide evidence of dust condensation within the ejecta. 1.5-2.5 mu m spectra, and HKL'M' photometry reveal strong 113, emission due to hot dust in the ejecta and/or circumstellar medium (CSM). For the origin of the IR emission we favour dust condensation (at least 10(-3) M circle dot) in a cool dense shell (CDS) as the main IR, source but do not rule out a contribution from the CSM. The late-time evolution of the intrinsic (K-L') colour of type H supernovae (SNe) may be a potentially useful tool for determining the presence or absence of a massive CSM around their progenitors.

Dust signatures from late-time infrared and optical observations of SN1998S

We follow the evolution of the infrared excess and the dustshell of Sakurai's Object by modelling the dust emission. The optical depth,dust temperature, and shell thickness parameters from the models are presented.Fits of DUSTY models to infrared spectra between 1997 May and 1999September illustrate the development of the dust from small grains to a rangeof grain sizes with an almost constant 60% graphite – 40% amorphous carbonmixture. The size of the infrared emitting region continues to growand may now be big enough to resolve. This may help to answerquestions such as the morphology of the dust shell, and whether the dustshell is `blobby' or smooth.

Modelling the dust around Sakurai's Object

We report the discovery of Bralpha and Brgamma emission in the infrared spectrum of the B0.2 V star tau Scorpii. The widths and strengths of the lines suggest that they are formed in a region of much higher density than is inferred from the UV resonance lines. This situation is similar to that found in Oe and Be stars. We show that the IR emission lines in tau Scorpii can be produced in a circumstellax disc of moderate density, without producing noticeable emission in Halpha. It is possible that a class of 'hidden' Be stars exists whose emission is prominent in the IR recombination lines but not in Halpha.

Infrared emission lines in tau Scorpii: a pole-on Be star ?

Recent detection of a large number of apparently isolated massive stars within the inner 80 pc of the Galactic Center has raised fundamental questions regarding massive star formation in a such a dense and harsh environment. Are these isolated stars the results of tidal interactions between clusters, are they escapees from a disrupted cluster, or do they represent a new mode of massive star formation in isolation? Noting that most of the isolated massive stars have spectral analogs in the Quintuplet Cluster, we have undertaken a combined analysis of the infrared spectra of both selected Quintuplet stars and the isolated objects using Gemini North spectroscopy. We present preliminary results, aiming at α-elements vs iron abundances, stellar properties, ages and radial velocities which will differentiate the top-heavy and star-formation scenarios.

/pdf/the-massive-star-population-at-the-center-of-the-milky-way-1ztox04dpm.pdf

The Massive Star Population at the Center of the Milky Way

Further Observations of H and He in the Very Center of the Galaxy

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