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

Les observations IRAS-LSR et spectrophotometriques a 3 μm terrestres de 24 sources IR sont presentees. Les spectres IR sont analyses. Les proprietes des molecules interstellaires sont etudiees

/pdf/polycyclic-aromatic-hydrocarbons-in-the-near-infrared-2a2zbjmjf0.pdf

Polycyclic aromatic hydrocarbons in the near-infrared spectra of 24 IRAS sources

Distribution of Ethane and Methane Emission on Neptune

Les observations spectroscopiques IR, dans l'intervalle 3-4 μm, de 7 sources IRAS ayant des caracteristiques d'hydrocarbures aromatiques polycycliques (PAH) sont presentees. Les caracteristiques de la region 3.35-3.6 μm sont analysees.

Three micron spectroscopy of IRAS sources - Observed and laboratory signatures of PAHs

We present near-IR spectroscopic observations of the central sources in 17 circumstellar shells from a sample of more than 400 “bubbles” discovered in the Spitzer/MIPSGAL 24 µm survey of the Galactic plane and in the Cygnus-X region. To identify the natures of these shells, we have obtained J, H, and K band spectra with a resolution �2600 of the stars at their centers. We observed 14 MIPSGAL bubbles (MBs), WR149, and 2 objects in the Cygnus-X region (WR138a and BD+43 3710), our sample being about 2.5 magnitudes fainter in K band than previous studies of the central sources of MBs. We use spectroscopic diagnostics and spectral libraries of late and early type stars to constrain the natures of our targets. We find five late type giants. The equivalent widths of their CO 2.29 µm features allow us to determine the spectral types of the stars and hence derive extinction along the line of sight, distance, and physical size of the shells. We also find twelve early type stars, in nine MBs and the 3 comparison objects. We find that the subtype inferred from the near-IR for WR138a (WN9h) and WR149 (WN5h) agrees with that derived from optical observations. A careful analysis of the literature and the environment of BD+43 3710 allows us to rule out the carbon star interpretation previously suggested. Our near-IR spectrum suggests that it is a B5 supergiant. At the centers of the nine MBs, we find a WC5-6 star possibly of low-mass, a candidate O5-6 V star, a B0 supergiant, a B/A type giant, and five LBV candidates. We also report the detections of emission lines arising from at least two shells with typical extents (� 10 ′′ ) in agreement with those in the mid-IR. We summarize the findings on the natures of the MBs since their discovery, with 30% of them now known. Most MBs with central sources detected in the near- to mid-IR have been identified and are red and blue giants, supergiants, or stars evolving toward these phases including, in particular, a handful of newly discovered Wolf-Rayet stars and a significant number of LBV candidates.

PALOMAR/TRIPLESPEC OBSERVATIONS OF SPITZER/MIPSGAL 24 µm CIRCUMSTELLAR SHELLS: UNVEILING THE NATURE OF THEIR CENTRAL SOURCES

Titan at 3 microns: Newly identified spectral features and an improved analysis of haze opacity

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