The Society for Pediatric Anesthesia recommendations for the use of opioids in children during the perioperative period

Peer Reviewedhttps://deepblue.lib.umich.edu/bitstream/2027.42/149726/1/pan13639_am.pdfhttps://deepblue.lib.umich.edu/bitstream/2027.42/149726/2/pan13639.pd

The Input Catalogue for the OMC camera onboard INTEGRAL

The Optical Monitoring Camera (OMC) onboard INTEGRAL (launched on October 17, 2002) has been designed to obtain V-Johnson photometry simultaneously with high energy observations at X-ray (3–35 keV) and (15 keV–10 MeV) performed by the main instruments onboard INTEGRAL. Due to technical limitations on the data processing electronics and the available telemetry, it is necessary to know, a priori, the objects to be monitored within the field of view (FOV) of the OMC. The OMC Input Catalogue – and subsequent provides this information: astrometric and photometric reference stars for calibration and scientific targets for accurate photometric variability studies.

OMC: An Optical Monitoring Camera for INTEGRAL - Instrument description and performance

The Optical Monitoring Camera (OMC) will observe the optical emission from the prime targets of the gammaray instruments onboard the ESA mission INTEGRAL, with the support of the JEM-X monitor in the X-ray domain. This capability will provide invaluable diagnostic information on the nature and the physics of the sources over a broad wavelength range. Its main scientific objectives are: ( 1) to monitor the optical emission from the sources observed by the gamma- and X-ray instruments, measuring the time and intensity structure of the optical emission for comparison with variability at high energies, and ( 2) to provide the brightness and position of the optical counterpart of any gamma- or X-ray transient taking place within its field of view. The OMC is based on a refractive optics with an aperture of 50 mm focused onto a large format CCD (1024 x 2048 pixels) working in frame transfer mode (1024 x 1024 pixels imaging area). With a field of view of 5degrees x 5degrees it will be able to monitor sources down to magnitude V = 18. Typical observations will perform a sequence of different integration times, allowing for photometric uncertainties below 0.1 mag for objects with V less than or equal to 16